| Title: | A flat Universe from high-resolution maps of the cosmic microwave background radiation | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; De Gasperis, G.; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P. V.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), AB(Department of Physics, Queen Mary and Westfield College, Mile End Road, London E1 4NS, UK.), AC(Jet Propulsion Laboratory, Pasadena, California 91109, USA), AD(CITA University of Toronto, Toronto M5S 3H8, Canada.), AE(Center for Particle Astrophysics, University of California at Berkeley, 301 Le Conte Hall, Berkeley, California 94720, USA), AF(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy.), AG(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106, USA), AH(California Institute of Technology, Mail Code 59-33, Pasadena, California 91125, USA), AI(Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy.), AJ(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106, USA), AK(Astrophysics, University of Oxford, Keble Road, OX1 3RH, UK.), AL(PCC, College de France, 11 pl. Marcelin Berthelot, 75231 Paris Cedex 05, France .), AM(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), AN(California Institute of Technology, Mail Code 59-33, Pasadena, California 91125, USA), AO(California Institute of Technology, Mail Code 59-33, Pasadena, California 91125, USA), AP(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), AQ(Center for Particle Astrophysics, University of California at Berkeley, 301 Le Conte Hall, Berkeley, California 94720, USA), AR(California Institute of Technology, Mail Code 59-33, Pasadena, California 91125, USA), AS(ENEA Centro Ricerche di Frascati, Via E. Fermi 45, 00044 Frascati, Italy.), AT(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), AU(California Institute of Technology, Mail Code 59-33, Pasadena, California 91125, USA), AV(Department of Physics and Astronomy, University of Massachusetts, Amherst, Massachusetts 01003, USA), AW(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), AX(Department of Physics and Astronomy, University of Toronto, Toronto M5S 3H8, Canada.), AY(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106, USA), AZ(Department of Physics and Astronomy, University of Toronto, Toronto M5S 3H8, Canada.), BA(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy.), BB(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), BC(CITA University of Toronto, Toronto M5S 3H8, Canada.), BD(CITA University of Toronto, Toronto M5S 3H8, Canada.), BE(Istituto Nazionale di Geofisica, Via di Vigna Murata 605, 00143, Roma, Italy .), BF(Istituto Nazionale di Geofisica, Via di Vigna Murata 605, 00143, Roma, Italy .), BG(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106, USA), BH(ENEA Centro Ricerche di Frascati, Via E. Fermi 45, 00044 Frascati, Italy.), BI(Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy.), BJ(Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy.) | |
| Publication: | Nature, Volume 404, Issue 6781, pp. 955-959 (2000). (Nature Homepage) | |
| Publication Date: | 04/2000 | |
| Origin: | NATURE | |
| Bibliographic Code: | 2000Natur.404..955D |
Abstract
The blackbody radiation left over from the Big Bang has been transformed by the expansion of the Universe into the nearly isotropic 2.73K cosmic microwave background. Tiny inhomogeneities in the early Universe left their imprint on the microwave background in the form of small anisotropies in its temperature. These anisotropies contain information about basic cosmological parameters, particularly the total energy density and curvature of the Universe. Here we report the first images of resolved structure in the microwave background anisotropies over a significant part of the sky. Maps at four frequencies clearly distinguish the microwave background from foreground emission. We compute the angular power spectrum of the microwave background, and find a peak at Legendre multipole lpeak = (197 +/- 6), with an amplitude ΔT200 = (69 +/- 8)μK. This is consistent with that expected for cold dark matter models in a flat (euclidean) Universe, as favoured by standard inflationary models.
| Title: | Ionization balance for optically thin plasmas: Rate coefficients for all atoms and ions of the elements H to NI | |
| Authors: | Mazzotta, P.; Mazzitelli, G.; Colafrancesco, S.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, I-00133 Roma, Italy), AB(Associazione EURATOM-ENEA sulla Fusione, C.R. Frascati, CP 65-00044 Frascati Roma, Italy), AC(Osservatorio Astronomico di Roma, via dell’Osservatorio, I-00040 Monteporzio, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, I-00133 Roma, Italy) | |
| Publication: | Astronomy and Astrophysics Supplement, v.133, p.403-409 (A&AS Homepage) | |
| Publication Date: | 12/1998 | |
| Origin: | A&AS | |
| Astronomy Keywords: | ATOMIC DATA, PLASMAS, RADIATION MECHANISMS: THERMAL, X-RAYS: GENERAL | |
| DOI: | 10.1051/aas:1998330 | |
| Bibliographic Code: | 1998A&AS..133..403M |
Abstract
We present in this paper new and updated calculations of the ionization equilibrium for all the elements from H to Ni. We collected for these elements all the data available in the literature for the ionization and radiative plus dielectronic recombination rates. In particular, the dielectronic rates have been fitted with a single formula and the related coefficients are tabulated. Our results are compared with previous works. Tables 1 and 2 are available only in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
| Title: | A Measurement of the CMB <EE> Spectrum from the 2003 Flight of BOOMERANG | |
| Authors: | Montroy, T. E.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; De Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Physics Department, Case Western Reserve University, Rockefeller Building, 10900 Euclid Avenue, Cleveland, OH 44106.), AB(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK.), AC(Jet Propulsion Laboratory, Pasadena, CA 91109; Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720; Space Sciences Laboratory, University of California, Berkeley, CA 94720.), AF(IFAC-CNR, 50127 Florence, Italy.), AG(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy.), AH(Theoretical Physics Group, Imperial College SW7 2BW, London, UK.), AI(IPAC, California Institute of Technology, Pasadena, CA 91125.), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy.), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), AM(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AN(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), AO(IPAC, California Institute of Technology, Pasadena, CA 91125.), AP(Theoretical Physics Group, Imperial College SW7 2BW, London, UK.), AQ(Physics Department, Case Western Reserve University, Rockefeller Building, 10900 Euclid Avenue, Cleveland, OH 44106; Department of Physics, University of California, Santa Barbara, CA 93106.), AR(Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AS(Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AT(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AU(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK.), AV(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada.), AW(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy; INFN, Sezione di Roma 1, 00133 Rome, Italy.), AX(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.), AY(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada; Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AZ(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada.), BA(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BB(Physics Department, University of Alberta, Edmonton, AB T6G 2J1, Canada.), BC(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BD(Institut d’Astrophysique, 75014 Paris, France), BE(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BF(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), BG(Physics Department, Case Western Reserve University, Rockefeller Building, 10900 Euclid Avenue, Cleveland, OH 44106.), BH(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BI(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), BJ(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 647, Issue 2, pp. 813-822. (ApJ Homepage) | |
| Publication Date: | 08/2006 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Instrumentation: Detectors | |
| DOI: | 10.1086/505560 | |
| Bibliographic Code: | 2006ApJ…647..813M |
Abstract
We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A.=82.5d, decl.=-45deg. The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero <EE> signal in the range 201<l<1000 with a significance of 4.8 σ, a 2 σ upper limit of 8.6 μK2 for any <BB> contribution, and a 2 σ upper limit of 7.0 μK2 for the <EB> spectrum. Estimates of foreground intensity fluctuations and the nondetection of <BB> and <EB> signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a ΛCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.
| Title: | A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG | |
| Authors: | Jones, W. C.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; De Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Lange, A. E.; MacTavish, C. J.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Physics Department, California Institute of Technology, MS 59-33, 1200 East California Boulevard, Pasadena, CA 91125 wcj@astro.caltech.edu), AB(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK.), AC(Jet Propulsion Laboratory, Pasadena, CA 91109.), AD(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Toronto, ON M5S 3H8, Canada.), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720; Space Sciences Laboratory, University of California, Berkeley, CA 94720.), AF(IFAC-CNR, 50127 Florence, Italy.), AG(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy.), AH(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Toronto, ON M5S 3H8, Canada; Theoretical Physics Group, Imperial College, London SW7 2BW, UK.), AI(IPAC, California Institute of Technology, Pasadena, CA 91125.), AJ(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), AK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy.), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), AM(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), AN(Instituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), AO(IPAC, California Institute of Technology, Pasadena, CA 91125.), AP(Theoretical Physics Group, Imperial College, London SW7 2BW, UK.), AQ(Department of Physics, University of California, Santa Barbara, CA 93106; Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), AR(Physics Department, California Institute of Technology, MS 59-33, 1200 East California Boulevard, Pasadena, CA 91125 wcj@astro.caltech.edu), AS(Department of Physics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AT(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), AU(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, UK.), AV(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy; INFN, Sezione di Roma 1, 00133 Rome, Italy.), AW(Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), AX(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.), AY(Department of Physics, University of Toronto, Toronto, ON M5S 3H8, Canada; Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AZ(Department of Physics, University of Toronto, Toronto, ON M5S 3H8, Canada.), BA(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), BB(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Toronto, ON M5S 3H8, Canada; Department of Physics, University of Alberta, Edmonton, AB T6G 2J1, Canada.), BC(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), BD(Institut d’Astrophysique de Paris, 75014 Paris, France), BE(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), BF(Instituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), BG(Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), BH(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), BI(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), BJ(Dipartimento di Fisica, Università di Roma “La Sapienza”, 00185 Rome, Italy.), BK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 647, Issue 2, pp. 823-832. (ApJ Homepage) | |
| Publication Date: | 08/2006 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Observations, Instrumentation: Detectors | |
| DOI: | 10.1086/505559 | |
| Bibliographic Code: | 2006ApJ…647..823J |
Abstract
We report on observations of the cosmic microwave background (CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization-sensitive bolometer (PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument (HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50<=l<=1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l>~900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement.
| Title: | Fine-scale anisotropy of the cosmic microwave background in a universe dominated by cold dark matter | |
| Authors: | Vittorio, N.; Silk, J. | |
| Affiliation: | AA(California, University, Berkeley, CA; Roma, Università , Rome, Italy), AB(California, University, Berkeley, CA) | |
| Publication: | Astrophysical Journal, Part 2 – Letters to the Editor (ISSN 0004-637X), vol. 285, Oct. 15, 1984, p. L39-L43. NATO-supported research. (ApJL Homepage) | |
| Publication Date: | 10/1984 | |
| Category: | Space Radiation | |
| Origin: | STI | |
| NASA/STI Keywords: | BACKGROUND RADIATION, BIG BANG COSMOLOGY, DARK MATTER, MASS TO LIGHT RATIOS, RELIC RADIATION, WEAK INTERACTIONS (FIELD THEORY), ANISOTROPY, BRIGHTNESS TEMPERATURE, DENSITY DISTRIBUTION, GALACTIC EVOLUTION, HUBBLE CONSTANT, MICROWAVES | |
| DOI: | 10.1086/184361 | |
| Bibliographic Code: | 1984ApJ…285L..39V |
Abstract
The fine-scale anisotropy of the cosmic microwave background radiation has been studied in cosmological models with a scale-invariant primordial adiabatic density fluctuation spectrum dominated by cold, weakly interacting particles. Normalization of the present fluctuation spectrum to the observed galaxy distribution results in excessive temperature anisotropy when compared to a recent upper limit on 4.5 arcmin unless the density parameter exceeds 0.4. When this result is combined with the requirement that the universe be at least 13 billion years old, it is found that if the cosmological constant is zero, then the density parameter is between roughly 0.4 and 1 and the Hubble constant is between roughly 60 km/s/Mpc and 50 km/s/Mpc.
| Title: | A Measurement of Ω from the North American Test Flight of Boomerang | |
| Authors: | Melchiorri, A.; Ade, P. A. R.; de Bernardis, P.; Bock, J. J.; Borrill, J.; Boscaleri, A.; Crill, B. P.; De Troia, G.; Farese, P.; Ferreira, P. G.; Ganga, K.; de Gasperis, G.; Giacometti, M.; Hristov, V. V.; Jaffe, A. H.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; Miglio, L.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Romeo, G.; Ruhl, J. E.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; Dipartimento di Fisica, Università Tor Vergata, Roma, Italy; Departement de Physique Theorique, Universite de Geneve, Switzerland), AB(Queen Mary and Westfield College, London, England, UK), AC(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AD(California Institute of Technology, Pasadena, CA; Jet Propulsion Laboratory, Pasadena, CA), AE(Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA; National Energy Research Scientific Computing Center, Lawrence Berkeley National Laboratory, Berkeley, CA), AF(Istituto Ricerca Onde Elettromagneitche/Consiglio Nazionale delle Richerche, Firenze, Italy), AG(California Institute of Technology, Pasadena, CA), AH(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AI(Department of Physics, University of California, Santa Barbara, Santa Barbara, CA), AJ(Departement de Physique Theorique, Universite de Geneve, Switzerland; Centro Multidisciplinar de Astrofisica, Instituto Superior Tecnico, Lisbon, Portugal; Theory Division, European Laboratory for Particle Physics (CERN), Geneva, Switzerland), AK(California Institute of Technology, Pasadena, CA; Physique Corpusculaire et Cosmologie, College de France, 11 place Marcelin Berthelot, 75231 Paris Cedex 05, France), AL(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy), AM(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AN(California Institute of Technology, Pasadena, CA), AO(Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA), AP(California Institute of Technology, Pasadena, CA), AQ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AR(Department of Physics and Astronomy, University of Massachusetts, Amherst, MA), AS(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; Departments of Physics and Astronomy, University of Toronto, Toronto, ON, Canada), AT(Departments of Physics and Astronomy, University of Toronto, Toronto, ON, Canada), AU(Istituto Ricerca Onde Elettromagneitche/Consiglio Nazionale delle Richerche, Firenze, Italy), AV(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AW(Istituto Nazionale di Geofisica, Roma, Italy), AX(Department of Physics, University of California, Santa Barbara, Santa Barbara, CA), AY(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy) | |
| Publication: | The Astrophysical Journal, Volume 536, Issue 2, pp. L63-L66. (ApJL Homepage) | |
| Publication Date: | 06/2000 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Dark Matter, Methods: Data Analysis | |
| DOI: | 10.1086/312744 | |
| Bibliographic Code: | 2000ApJ…536L..63M |
Abstract
We use the angular power spectrum of the cosmic microwave background, measured during the North American test flight of the Boomerang experiment, to constrain the geometry of the universe. Within the class of cold dark matter models, we find that the overall fractional energy density of the universe Ω is constrained to be 0.85<=Ω<=1.25 at the 68% confidence level. Combined with the COBE measurement, the data on degree scales from the Microwave Anisotropy Telescope in Chile, and the high-redshift supernovae data, we obtain new constraints on the fractional matter density and the cosmological constant.
| Title: | Cosmological Parameters from the 2003 Flight of BOOMERANG | |
| Authors: | MacTavish, C. J.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; De Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Jones, W. C.; Kisner, T. S.; Lange, A. E.; Lewis, A. M.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Department of Physics, University of Toronto, 60 St. George St., Toronto, ON M5S 1A7, Canada.), AB(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AC(Jet Propulsion Laboratory, Pasadena, CA 91109.), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AE(National Energy Research Scientific Computing Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720.), AF(IFAC-CNR, 50127 Florence, Italy.), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy.), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada; Department of Physics, Imperial College, London SW7 2BW, UK.), AI(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125.), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AK(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy.), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), AM(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AN(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), AO(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125.), AP(Department of Physics, Imperial College, London SW7 2BW, UK.), AQ(Department of Physics, California Institute of Technology, Pasadena, CA 91125.), AR(Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), AS(Department of Physics, California Institute of Technology, Pasadena, CA 91125.), AT(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AU(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), AV(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AW(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy; INFN, Sezione di Roma 1, 00133 Rome, Italy.), AX(Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), AY(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.), AZ(Department of Physics, University of Toronto, 60 St. George St., Toronto, ON M5S 1A7, Canada; Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), BA(Department of Physics, University of Toronto, 60 St. George St., Toronto, ON M5S 1A7, Canada.), BB(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BC(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada; Department of Physics, University of Alberta, Edmonton, AB T6G 2J1, Canada.), BD(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BE(Institute d’Astrophysique de Paris, 75014 Paris, France), BF(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BG(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), BH(Department of Physics, Case Western Reserve University, Cleveland, OH 44106.), BI(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BJ(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), BK(Dipartimento di Fisica, Università di Roma La Sapienza, 00185 Rome, Italy.), BL(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 647, Issue 2, pp. 799-812. (ApJ Homepage) | |
| Publication Date: | 08/2006 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Cosmological Parameters, Polarization | |
| DOI: | 10.1086/505558 | |
| Bibliographic Code: | 2006ApJ…647..799M |
Abstract
We present the cosmological parameters from the CMB intensity and polarization power spectra of the 2003 Antarctic flight of the BOOMERANG telescope. The BOOMERANG data alone constrain the parameters of the ΛCDM model remarkably well and are consistent with constraints from a multiexperiment combined CMB data set. We add LSS data from the 2dF and SDSS redshift surveys to the combined CMB data set and test several extensions to the standard model including running of the spectral index, curvature, tensor modes, the effect of massive neutrinos, and an effective equation of state for dark energy. We also include an analysis of constraints to a model that allows a CDM isocurvature admixture.
| Title: | A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG | |
| Authors: | Piacentini, F.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; De Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), AB(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AC(Jet Propulsion Laboratory, Pasadena, CA 91109; Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720; Space Sciences Laboratory, University of California, Berkeley, CA 94720.), AF(IFAC-CNR, 50127 Florence, Italy.), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy.), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada; Theoretical Physics Group, Imperial College, London 5W7 2BW, UK.), AI(IPAC, California Institute of Technology, Pasadena, CA 91125.), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), AK(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy.), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), AM(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), AN(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), AO(IPAC, California Institute of Technology, Pasadena, CA 91125.), AP(Theoretical Physics Group, Imperial College, London 5W7 2BW, UK.), AQ(Physics Department, Case Western Reserve University, Cleveland, OH 44106; Department of Physics, University of California, Santa Barbara, CA 93106.), AR(Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AS(Observational Cosmology, California Institute of Technology, Pasadena, CA 91125.), AT(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), AU(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AV(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada.), AW(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy; INFN, Sezione di Roma 1, 00133 Rome, Italy.), AX(Physics Department, Case Western Reserve University, Cleveland, OH 44106.), AY(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.), AZ(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada.), BA(Physics Department, University of Toronto, Toronto, ON M5S 3H8, Canada.), BB(Department of Physics, University of Alberta, Edmonton, AB T6G 2J1, Canada.), BC(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), BD(Institut d’Astrophysique, 75104 Paris, France), BE(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), BF(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy.), BG(Physics Department, Case Western Reserve University, Cleveland, OH 44106.), BH(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), BI(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139.), BJ(Dipartimento di Fisica, Università di Roma La Sapienza, Piazzale Aldo Moro 2, 00185 Rome, Italy.), BK(Dipartimento di Fisica, Università di Roma Tor Vergata, 00133 Rome, Italy; INFN, Sezione di Roma 2, 00133 Rome, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 647, Issue 2, pp. 833-839. (ApJ Homepage) | |
| Publication Date: | 08/2006 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background | |
| DOI: | 10.1086/505557 | |
| Bibliographic Code: | 2006ApJ…647..833P |
Abstract
We present a measurement of the polarization-temperature angular cross power spectra, <TE> and <TB>, of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant <TE> correlation in the l-range between 50 and 950 with a statistical significance of >3.5 σ. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the “concordance model” that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.
Abstract
The European Space Agency’s Planck satellite was launched on 14 May 2009, and has been surveying the sky stably and continuously since 13 August 2009. Its performance is well in line with expectations, and it will continue to gather scientific data until the end of its cryogenic lifetime. We give an overview of the history of Planck in its first year of operations, and describe some of the key performance aspects of the satellite. This paper is part of a package submitted in conjunction with Planck’s Early Release Compact Source Catalogue, the first data product based on Planck to be released publicly. The package describes the scientific performance of the Planck payload, and presents results on a variety of astrophysical topics related to the sources included in the Catalogue, as well as selected topics on diffuse emission.
Corresponding author: J. A. Tauber, e-mail: jtauber@rssd.esa.int
| Title: | Measurement of a Peak in the Cosmic Microwave Background Power Spectrum from the North American Test Flight of Boomerang | |
| Authors: | Mauskopf, P. D.; Ade, P. A. R.; de Bernardis, P.; Bock, J. J.; Borrill, J.; Boscaleri, A.; Crill, B. P.; DeGasperis, G.; De Troia, G.; Farese, P.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hanany, S.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Lee, A. T.; Masi, S.; Melchiorri, A.; Melchiorri, F.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Richards, P. L.; Romeo, G.; Ruhl, J. E.; Scannapieco, E.; Scaramuzzi, F.; Stompor, R.; Vittorio, N. | |
| Affiliation: | AA(Department of Physics and Astronomy, University of Massachusetts, Amherst, MA; Department of Physics and Astronomy, University of Wales, Cardiff, Wales, UK), AB(Queen Mary and Westfield College, London, England, UK), AC(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AD(California Institute of Technology, Pasadena, CA; Jet Propulsion Laboratory, Pasadena, CA), AE(Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA; National Energy Research Scientific Computing Center, LBNL, Berkeley, CA), AF(Istituto Ricerca Onde Elettromagneitche/Consiglio Nazionale delle Ricerche, Firenze, Italy), AG(California Institute of Technology, Pasadena, CA), AH(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AI(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AJ(Department of Physics, University of California, Santa Barbara, Santa Barbara, CA), AK(Centro Multidisciplinar de Astrofisica, Instituto Superior Tecnico, Lisbon, Portugal; Theory Division, CERN, Geneva, Switzerland), AL(Physique Corpusculaire et Cosmologie, College de France, 11 Place Marcelin Berthelot, 75231 Paris Cedex 05, France; Infrared Processing and Analysis Center, Pasadena, CA), AM(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AN(Department of Physics, University of Minnesota, Minnealpolis, MN), AO(California Institute of Technology, Pasadena, CA), AP(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AQ(Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA), AR(California Institute of Technology, Pasadena, CA), AS(Department of Physics, University of California, Berkeley, Berkeley, CA), AT(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AU(Departement de Physique Theorique, Universite de Geneve, Switzerland), AV(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AW(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AX(Department of Physics, University of California, Santa Barbara, Santa Barbara, CA), AY(Departments of Physics and Astronomy, University of Toronto, Toronto, ON, Canada), AZ(Istituto Ricerca Onde Elettromagneitche/Consiglio Nazionale delle Ricerche, Firenze, Italy), BA(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BB(Department of Physics, University of California, Berkeley, Berkeley, CA), BC(Istituto Nazionale di Geofisica, Roma, Italy), BD(Department of Physics, University of California, Santa Barbara, Santa Barbara, CA), BE(Department of Physics, University of California, Berkeley, Berkeley, CA), BF(Ente per le Nuove Tecnologie, l’Energia, e l’Ambiente, Frascati, Italy), BG(Department of Physics, University of California, Berkeley, Berkeley, CA), BH(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy) | |
| Publication: | The Astrophysical Journal, Volume 536, Issue 2, pp. L59-L62. (ApJL Homepage) | |
| Publication Date: | 06/2000 | |
| Origin: | UCP | |
| Astronomy Keywords: | Balloons, Cosmology: Cosmic Microwave Background, Cosmology: Observations, Instrumentation: Photometers, Methods: Data Analysis, Telescopes | |
| DOI: | 10.1086/312743 | |
| Bibliographic Code: | 2000ApJ…536L..59M |
Abstract
We describe a measurement of the angular power spectrum of anisotropies in the cosmic microwave background (CMB) at scales of 0.3d to 5° from the North American test flight of the Boomerang experiment. Boomerang is a balloon-borne telescope with a bolometric receiver designed to map CMB anisotropies on a long-duration balloon flight. During a 6 hr test flight of a prototype system in 1997, we mapped more than 200 deg2 at high Galactic latitudes in two bands centered at 90 and 150 GHz with a resolution of 26′ and 16.5′ FWHM, respectively. Analysis of the maps gives a power spectrum with a peak at angular scales of 1° with an amplitude 70 μKCMB.
Abstract
We present the first all-sky sample of galaxy clusters detected blindly by the Planck satellite through the Sunyaev-Zeldovich (SZ) effect from its six highest frequencies. This early SZ (ESZ) sample is comprised of 189 candidates, which have a high signal-to-noise ratio ranging from 6 to 29. Its high reliability (purity above 95%) is further ensured by an extensive validation process based on Planck internal quality assessments and by external cross-identification and follow-up observations. Planck provides the first measured SZ signal for about 80% of the 169 previously-known ESZ clusters. Planck furthermore releases 30 new cluster candidates, amongst which 20 meet the ESZ signal-to-noise selection criterion. At the submission date, twelve of the 20 ESZ candidates were confirmed as new clusters, with eleven confirmed using XMM-Newton snapshot observations, most of them with disturbed morphologies and low luminosities. The ESZ clusters are mostly at moderate redshifts (86% with z below 0.3) and span more than a decade in mass, up to the rarest and most massive clusters with masses above 1 × 1015 Msun.
Corresponding author: M. Douspis, e-mail: marian.douspis@ias.u-psud.frAppendix is available in electronic form at http://www.aanda.org
| Title: | Planck pre-launch status: The Planck mission | |
| Authors: | Tauber, J. A.; Mandolesi, N.; Puget, J.-L.; Banos, T.; Bersanelli, M.; Bouchet, F. R.; Butler, R. C.; Charra, J.; Crone, G.; Dodsworth, J.; Efstathiou, G.; Gispert, R.; Guyot, G.; Gregorio, A.; Juillet, J. J.; Lamarre, J.-M.; Laureijs, R. J.; Lawrence, C. R.; Nørgaard-Nielsen, H. U.; Passvogel, T.; Reix, J. M.; Texier, D.; Vibert, L.; Zacchei, A.; Ade, P. A. R.; Aghanim, N.; Aja, B.; Alippi, E.; Aloy, L.; Armand, P.; Arnaud, M.; Arondel, A.; Arreola-Villanueva, A.; Artal, E.; Artina, E.; Arts, A.; Ashdown, M.; Aumont, J.; Azzaro, M.; Bacchetta, A.; Baccigalupi, C.; Baker, M.; Balasini, M.; Balbi, A.; Banday, A. J.; Barbier, G.; Barreiro, R. B.; Bartelmann, M.; Battaglia, P.; Battaner, E.; Benabed, K.; Beney, J.-L.; Beneyton, R.; Bennett, K.; Benoit, A.; Bernard, J.-P.; Bhandari, P.; Bhatia, R.; Biggi, M.; Biggins, R.; Billig, G.; Blanc, Y.; Blavot, H.; Bock, J. J.; Bonaldi, A.; Bond, R.; Bonis, J.; Borders, J.; Borrill, J.; Boschini, L.; Boulanger, F.; Bouvier, J.; Bouzit, M.; Bowman, R.; Bréelle, E.; Bradshaw, T.; Braghin, M.; Bremer, M.; Brienza, D.; Broszkiewicz, D.; Burigana, C.; Burkhalter, M.; Cabella, P.; Cafferty, T.; Cairola, M.; Caminade, S.; Camus, P.; Cantalupo, C. M.; Cappellini, B.; Cardoso, J.-F.; Carr, R.; Catalano, A.; Cayón, L.; Cesa, M.; Chaigneau, M.; Challinor, A.; Chamballu, A.; Chambelland, J. P.; Charra, M.; Chiang, L.-Y.; Chlewicki, G.; Christensen, P. R.; Church, S.; Ciancietta, E.; Cibrario, M.; Cizeron, R.; Clements, D.; Collaudin, B.; Colley, J.-M.; Colombi, S.; Colombo, A.; Colombo, F.; Corre, O.; Couchot, F.; Cougrand, B.; Coulais, A.; Couzin, P.; Crane, B.; Crill, B.; Crook, M.; Crumb, D.; Cuttaia, F.; Dörl, U.; da Silva, P.; Daddato, R.; Damasio, C.; Danese, L.; D’Aquino, G.; D’Arcangelo, O.; Dassas, K.; Davies, R. D.; Davies, W.; Davis, R. J.; de Bernardis, P.; de Chambure, D.; de Gasperis, G.; de La Fuente, M. L.; de Paco, P.; de Rosa, A.; de Troia, G.; de Zotti, G.; Dehamme, M.; Delabrouille, J.; Delouis, J.-M.; Désert, F.-X.; di Girolamo, G.; Dickinson, C.; Doelling, E.; Dolag, K.; Domken, I.; Douspis, M.; Doyle, D.; Du, S.; Dubruel, D.; Dufour, C.; Dumesnil, C.; Dupac, X.; Duret, P.; Eder, C.; Elfving, A.; Enßlin, T. A.; Eng, P.; English, K.; Eriksen, H. K.; Estaria, P.; Falvella, M. C.; Ferrari, F.; Finelli, F.; Fishman, A.; Fogliani, S.; Foley, S.; Fonseca, A.; Forma, G.; Forni, O.; Fosalba, P.; Fourmond, J.-J.; Frailis, M.; Franceschet, C.; Franceschi, E.; François, S.; Frerking, M.; Gómez-Reñasco, M. F.; Górski, K. M.; Gaier, T. C.; Galeotta, S.; Ganga, K.; GarcÃa Lázaro, J.; Garnica, A.; Gaspard, M.; Gavila, E.; Giard, M.; Giardino, G.; Gienger, G.; Giraud-Heraud, Y.; Glorian, J.-M.; Griffin, M.; Gruppuso, A.; Guglielmi, L.; Guichon, D.; Guillaume, B.; Guillouet, P.; Haissinski, J.; Hansen, F. K.; Hardy, J.; Harrison, D.; Hazell, A.; Hechler, M.; Heckenauer, V.; Heinzer, D.; Hell, R.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Herreros, J. M.; Hervier, V.; Heske, A.; Heurtel, A.; Hildebrandt, S. R.; Hills, R.; Hivon, E.; Hobson, M.; Hollert, D.; Holmes, W.; Hornstrup, A.; Hovest, W.; Hoyland, R. J.; Huey, G.; Huffenberger, K. M.; Hughes, N.; Israelsson, U.; Jackson, B.; Jaffe, A.; Jaffe, T. R.; Jagemann, T.; Jessen, N. C.; Jewell, J.; Jones, W.; Juvela, M.; Kaplan, J.; Karlman, P.; Keck, F.; Keihänen, E.; King, M.; Kisner, T. S.; Kletzkine, P.; Kneissl, R.; Knoche, J.; Knox, L.; Koch, T.; Krassenburg, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lagache, G.; Lagorio, E.; Lami, P.; Lande, J.; Lange, A.; Langlet, F.; Lapini, R.; Lapolla, M.; Lasenby, A.; Le Jeune, M.; Leahy, J. P.; Lefebvre, M.; Legrand, F.; Le Meur, G.; Leonardi, R.; Leriche, B.; Leroy, C.; Leutenegger, P.; Levin, S. M.; Lilje, P. B.; Lindensmith, C.; Linden-Vørnle, M.; Loc, A.; Longval, Y.; Lubin, P. M.; Luchik, T.; Luthold, I.; Macias-Perez, J. F.; Maciaszek, T.; MacTavish, C.; Madden, S.; Maffei, B.; Magneville, C.; Maino, D.; Mambretti, A.; Mansoux, B.; Marchioro, D.; Maris, M.; Marliani, F.; Marrucho, J.-C.; MartÃ-Canales, J.; MartÃnez-González, E.; MartÃn-Polegre, A.; Martin, P.; Marty, C.; Marty, W.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McDonald, A.; McGrath, P.; Mediavilla, A.; Meinhold, P. R.; Mélin, J.-B.; Melot, F.; Mendes, L.; Mennella, A.; Mervier, C.; Meslier, L.; Miccolis, M.; Miville-Deschenes, M.-A.; Moneti, A.; Montet, D.; Montier, L.; Mora, J.; Morgante, G.; Morigi, G.; Morinaud, G.; Morisset, N.; Mortlock, D.; Mottet, S.; Mulder, J.; Munshi, D.; Murphy, A.; Murphy, P.; Musi, P.; Narbonne, J.; Naselsky, P.; Nash, A.; Nati, F.; Natoli, P.; Netterfield, B.; Newell, J.; Nexon, M.; Nicolas, C.; Nielsen, P. H.; Ninane, N.; Noviello, F.; Novikov, D.; Novikov, I.; O’Dwyer, I. J.; Oldeman, P.; Olivier, P.; Ouchet, L.; Oxborrow, C. A.; Pérez-Cuevas, L.; Pagan, L.; Paine, C.; Pajot, F.; Paladini, R.; Pancher, F.; Panh, J.; Parks, G.; Parnaudeau, P.; Partridge, B.; Parvin, B.; Pascual, J. P.; Pasian, F.; Pearson, D. P.; Pearson, T.; Pecora, M.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piersanti, O.; Plaige, E.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poulleau, G.; Poutanen, T.; Prézeau, G.; Pradell, L.; Prina, M.; Prunet, S.; Rachen, J. P.; Rambaud, D.; Rame, F.; Rasmussen, I.; Rautakoski, J.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Reiter, J.; Renault, C.; Ricciardi, S.; Rideau, P.; Riller, T.; Ristorcelli, I.; Riti, J. B.; Rocha, G.; Roche, Y.; Pons, R.; Rohlfs, R.; Romero, D.; Roose, S.; Rosset, C.; Rouberol, S.; Rowan-Robinson, M.; Rubiño-MartÃn, J. A.; Rusconi, P.; Rusholme, B.; Salama, M.; Salerno, E.; Sandri, M.; Santos, D.; Sanz, J. L.; Sauter, L.; Sauvage, F.; Savini, G.; Schmelzel, M.; Schnorhk, A.; Schwarz, W.; Scott, D.; Seiffert, M. D.; Shellard, P.; Shih, C.; Sias, M.; Silk, J. I.; Silvestri, R.; Sippel, R.; Smoot, G. F.; Starck, J.-L.; Stassi, P.; Sternberg, J.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Stringhetti, L.; Strommen, D.; Stute, T.; Sudiwala, R.; Sugimura, R.; Sunyaev, R.; Sygnet, J.-F.; Türler, M.; Taddei, E.; Tallon, J.; Tamiatto, C.; Taurigna, M.; Taylor, D.; Terenzi, L.; Thuerey, S.; Tillis, J.; Tofani, G.; Toffolatti, L.; Tommasi, E.; Tomasi, M.; Tonazzini, E.; Torre, J.-P.; Tosti, S.; Touze, F.; Tristram, M.; Tuovinen, J.; Tuttlebee, M.; Umana, G.; Valenziano, L.; Vallée, D.; van der Vlis, M.; van Leeuwen, F.; Vanel, J.-C.; van-Tent, B.; Varis, J.; Vassallo, E.; Vescovi, C.; Vezzu, F.; Vibert, D.; Vielva, P.; Vierra, J.; Villa, F.; Vittorio, N.; Vuerli, C.; Wade, L. A.; Walker, A. R.; Wandelt, B. D.; Watson, C.; Werner, D.; White, M.; White, S. D. M.; Wilkinson, A.; Wilson, P.; Woodcraft, A.; Yoffo, B.; Yun, M.; Yurchenko, V.; Yvon, D.; Zhang, B.; Zimmermann, O.; Zonca, A.; Zorita, D. | |
| Affiliation: | AA(European Space Agency, Astrophysics Division, ESTEC, Keplerlaan 1, 2201AZ Noordwijk, The Netherlands jtauber@rssd.esa.int), AB(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), AC(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), AD(Thales Alenia Space France, 100 Boulevard du Midi, Cannes la Bocca, France), AE(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy), AF(Institut d’Astrophysique de Paris, CNRS UMR7095, & UPMC, Université Pierre & Marie Curie, 98bis boulevard Arago, Paris, France), AG(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), AH(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), AI(European Space Agency, Herschel-Planck Project, ESTEC, Keplerlaan 1, Noordwijk, The Netherlands), AJ(European Space Agency, Herschel-Planck Project, European Space Operations Centre – ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), AK(University of Cambridge, Institute of Astronomy, Madingley Road, Cambridge, UK), AL(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), AM(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), AN(University of Trieste, Department of Physics, via A. 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Moruzzi 1, Pisa, Italy), PY(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), PZ(LPSC, Université Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de Grenoble, 53 avenue des Martyrs, 38026 Grenoble Cedex, France), QA(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), QB(Institut d’Astrophysique de Paris, CNRS UMR7095, & UPMC, Université Pierre & Marie Curie, 98bis boulevard Arago, Paris, France), QC(Thales Alenia Space France, 100 Boulevard du Midi, Cannes la Bocca, France), QD(Optical Science Laboratory, University College London, Gower Street, London, UK), QE(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), QF(European Space Agency, Herschel-Planck Project, ESTEC, Keplerlaan 1, Noordwijk, The Netherlands), QG(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), QH(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), QI(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), QJ(University of Cambridge, Cavendish Laboratory, Astrophysics group, J J Thomson Avenue, Cambridge, UK), QK(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), QL(Thales Alenia Space Italia, Collegno 253, Turin, Italy), QM(Department of Physics, University of Oxford, 1 Keble Road, Oxford, UK), QN(Thales Alenia Space Italia, S.S. Padana Superiore, 290, Vimodrone, Milano, Italy), QO(Astrium GmbH, Friedrichshafen, Germany), QP(Department of Physics, University of California, Berkeley, California, USA), QQ(CEA Saclay, IrfU/SPP Bat 141, Gif-sur-Yvette, France), QR(LPSC, Université Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de Grenoble, 53 avenue des Martyrs, 38026 Grenoble Cedex, France), QS(European Space Agency, Astrophysics Division, ESTEC, Keplerlaan 1, 2201AZ Noordwijk, The Netherlands), QT(Space Sciences Laboratory, University of California, Berkeley, California, USA), QU(University of Cambridge, Institute of Astronomy, Madingley Road, Cambridge, UK), QV(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), QW(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), QX(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), QY(Astrium GmbH, Friedrichshafen, Germany), QZ(Cardiff University, Department of Physics and Astronomy, Queens Buildings, 5 The Parade, Cardiff, Wales, UK), RA(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), RB(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Garching bei München, Germany), RC(Institut d’Astrophysique de Paris, CNRS UMR7095, & UPMC, Université Pierre & Marie Curie, 98bis boulevard Arago, Paris, France), RD(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), RE(Thales Alenia Space Italia, S.S. Padana Superiore, 290, Vimodrone, Milano, Italy), RF(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), RG(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), RH(Laboratoire de l’Accélerateur Linéaire, Université Paris-Sud, CNRS/IN2P3, Orsay, France), RI(European Space Agency, Planck Science Office – ESAC, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain), RJ(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), RK(European Space Agency, Herschel-Planck Project, ESTEC, Keplerlaan 1, Noordwijk, The Netherlands), RL(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), RM(INAF – Arcetri Astrophysical Observatory, Largo Enrico Fermi 5, Florence, Italy), RN(Departamento de FÃsica, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo, Spain), RO(Agenzia Spaziale Italiana, viale Liegi 26, Roma, Italy), RP(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy), RQ(CNR – ISTI, Area della Ricerca, via G. Moruzzi 1, Pisa, Italy), RR(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), RS(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), RT(Laboratoire de l’Accélerateur Linéaire, Université Paris-Sud, CNRS/IN2P3, Orsay, France), RU(Laboratoire de l’Accélerateur Linéaire, Université Paris-Sud, CNRS/IN2P3, Orsay, France), RV(MilliLab, VTT Information Technology, Tietotie 3, Espoo, Finland), RW(European Space Agency, Herschel-Planck Project, European Space Operations Centre – ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), RX(INAF Osservatorio Astrofisico di Catania, via S. Sofia, Catania, Italy), RY(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), RZ(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), SA(European Space Agency, Herschel-Planck Project, ESTEC, Keplerlaan 1, Noordwijk, The Netherlands), SB(University of Cambridge, Institute of Astronomy, Madingley Road, Cambridge, UK), SC(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), SD(Institut d’Astrophysique de Paris, CNRS UMR7095, & UPMC, Université Pierre & Marie Curie, 98bis boulevard Arago, Paris, France), SE(MilliLab, VTT Information Technology, Tietotie 3, Espoo, Finland), SF(European Space Agency, Herschel-Planck Project, European Space Operations Centre – ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), SG(Laboratoire d’Astrophysique de Grenoble (CNRS, UMR 5571), 414 Rue de la piscine, Grenoble, France), SH(Laboratoire d’Astrophysique de Grenoble (CNRS, UMR 5571), 414 Rue de la piscine, Grenoble, France), SI(Institut d’Astrophysique de Paris, CNRS UMR7095, & UPMC, Université Pierre & Marie Curie, 98bis boulevard Arago, Paris, France), SJ(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), SK(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), SL(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna, Italy), SM(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), SN(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), SO(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), SP(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), SQ(Department of Physics, University of Illinois at Urbana-Champaign, 1110 West Green Street, Urbana, Illinois, USA), SR(European Space Agency, Herschel-Planck Project, European Space Operations Centre – ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), SS(European Space Agency, Herschel-Planck Project, European Space Operations Centre – ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), ST(Departments of Astronomy and Physics, University of California, Berkeley, California, USA), SU(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Garching bei München, Germany), SV(Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, UK), SW(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), SX(Cardiff University, Department of Physics and Astronomy, Queens Buildings, 5 The Parade, Cardiff, Wales, UK), SY(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), SZ(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), TA(National University of Ireland (NUI), Department of Experimental Physics, Maynooth, Co. Kildare, Dublin, Ireland), TB(CEA Saclay, IrfU/SPP Bat 141, Gif-sur-Yvette, France), TC(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), TD(Laboratoire d’Astrophysique de Grenoble (CNRS, UMR 5571), 414 Rue de la piscine, Grenoble, France), TE(INAF/IASF Milano, via E. Bassini 15, Milano, Italy), TF(Sener IngenierÃa y Sistemas S.A., C. Severo Ochoa (Parq. Tecnológico De Madrid) 4, Tres Cantos, Spain) | |
| Publication: | Astronomy and Astrophysics, Volume 520, id.A1 (A&A Homepage) | |
| Publication Date: | 09/2010 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | cosmic microwave background, space vehicles: instruments, instrumentation: detectors, instrumentation: polarimeters, submillimeter: general, radio continuum: general | |
| DOI: | 10.1051/0004-6361/200912983 | |
| Bibliographic Code: | 2010A&A…520A…1T |
Abstract
The European Space Agency’s Planck satellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity ({{Δ T}over T} 2 × 10-6) and angular resolution ( 5 arcmin). Planck will provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planck to measure polarization across a wide frequency range (30-350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planck scientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.
| Title: | Large-scale velocity fields as a test of cosmological models | |
| Authors: | Vittorio, N.; Juszkiewicz, R.; Davis, M. | |
| Affiliation: | AA(California, University, Berkeley), AB(California, University, Berkeley), AC(California, University, Berkeley) | |
| Publication: | Nature (ISSN 0028-0836), vol. 323, Sept. 11, 1986, p. 132, 133. ESA-supported research. (Nature Homepage) | |
| Publication Date: | 09/1986 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, BAYES THEOREM, COSMOLOGY, VELOCITY DISTRIBUTION, BLACK BODY RADIATION, DARK MATTER, HUBBLE CONSTANT, MASS FLOW, UNIVERSE | |
| DOI: | 10.1038/323132a0 | |
| Bibliographic Code: | 1986Natur.323..132V |
Abstract
It has been suggested that the Hubble expansion on large scales is distorted by bulk matter flows of surprisingly large amplitude. Using Bayesian statistics of conditional probability, the authors show here that a high amplitude for large-scale matter flows can be used to rule out, at the 95% confidence level or better, both hot dark matter and cold dark matter models of the growth of structure in the Universe. No random-phase initial conditions with constant-curvature initial perturbations are likely to be consistent with bulk flows relative to the cosmic microwave background exceeding 700 km s-1 on scales of 50h-1Mpc.
Abstract
A brief description of the methodology of construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC), including the Early Cold Cores (ECC) and the Early Sunyaev-Zeldovich (ESZ) cluster catalogue is provided. The catalogue is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is ≥90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143GHz while the SExtractor technique was used between 217 and 857GHz. The 10σ photometric flux density limit of the catalogue at |b| > 30° is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in “clean” regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. In addition, two early release catalogs that contain 915 cold molecular cloud core candidates and 189 SZ cluster candidates that have been generated using multifrequency algorithms are presented. The entire source list, with more than 15000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities.
Corresponding author: R.-R. Chary, e-mail: rchary@caltech.edu
| Title: | Instrument, method, brightness, and polarization maps from the 2003 flight of BOOMERanG | |
| Authors: | Masi, S.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Ehlers, P.; Hivon, E.; Hristov, V.; Iacoangeli, A.; Jaffe, A. H.; Jones, W. C.; Kisner, T. S.; Lange, A. E.; MacTavish, C. J.; Marini Bettolo, C.; Mason, P.; Mauskopf, P. D.; Montroy, T. E.; Nati, F.; Nati, L.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Torbet, E.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy silvia.masi@roma1infn.it), AB(School of Physics and Astronomy, Cardiff University, Wales, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA), AD(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, ON, Canada), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, University of California, Berkeley, CA, USA), AF(IFAC-CNR, Firenze, Italy), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AH(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, ON, Canada; Department of Physics, Imperial College, London, UK), AI(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, USA), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AK(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), AM(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AN(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), AO(Department of Astronomy and Astrophysics, University of Toronto, ON, Canada), AP(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, USA), AQ(Department of Astronomy, California Institute of Technology, Pasadena, CA, USA), AR(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AS(Department of Physics, Imperial College, London, UK), AT(Department of Astronomy, California Institute of Technology, Pasadena, CA, USA), AU(Physics Department, Case Western Reserve University, Cleveland, OH, USA; Department of Physics, University of California, Santa Barbara, CA, USA), AV(Department of Astronomy, California Institute of Technology, Pasadena, CA, USA), AW(Department of Physics, University of Toronto, ON, Canada), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Department of Astronomy, California Institute of Technology, Pasadena, CA, USA), AZ(School of Physics and Astronomy, Cardiff University, Wales, UK), BA(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BB(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BC(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BD(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy), BE(Department of Astronomy and Astrophysics, University of Toronto, ON, Canada; Department of Physics, University of Toronto, ON, Canada), BF(Department of Physics, University of Toronto, ON, Canada), BG(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BH(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, ON, Canada; Department of Physics, University of Alberta, Edmonton, AB, Canada), BI(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BJ(Institut d’Astrophysique de Paris, Paris, France), BK(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BL(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), BM(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BN(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BO(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), BP(Department of Physics, University of California, Santa Barbara, CA, USA), BQ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BR(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy) | |
| Publication: | Astronomy and Astrophysics, Volume 458, Issue 3, November II 2006, pp.687-716 (A&A Homepage) | |
| Publication Date: | 11/2006 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | instrumentation: polarimeters, techniques: polarimetric, ISM: clouds, ISM: HII regions, cosmic microwave background | |
| DOI: | 10.1051/0004-6361:20053891 | |
| Bibliographic Code: | 2006A&A…458..687M |
Abstract
Aims.We present the boomerang-03 experiment, and the maps of the Stokes parameters I, Q, U of the microwave sky obtained during a 14 day balloon flight in 2003.
Methods: .Using a balloon-borne mm-wave telescope with polarization sensitive bolometers, three regions of the southern sky were surveyed: a deep survey (~90 square degrees) and a shallow survey (~750 square degrees) at high Galactic latitudes (both centered at RA ≃ 5.5 h, Dec ≃ -45°) and a survey of ~300 square degrees across the Galactic plane at RA ≃ 9.1 h, dec ≃ -47°. All three surveys were carried out in three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ~10′.
Results: .The 145 GHz maps of Stokes I are dominated by Cosmic Microwave Background (CMB) temperature anisotropy, which is mapped with high signal to noise ratio. The measured anisotropy pattern is consistent with the pattern measured in the same region by boomerang-98 and by WMAP. The 145 GHz maps of Stokes Q and U provide a robust statistical detection of polarization of the CMB when subjected to a power spectrum analysis. The amplitude of the detected polarization is consistent with that of the CMB in the ΛCDM cosmological scenario. At 145 GHz, in the CMB surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps, and give upper limits for any other non-CMB component. When compared to monitors of different interstellar components, the intensity maps of the surveyed section of the Galactic plane show that a variety of emission mechanisms is present in that region.
Abstract
All-sky data from the Planck survey and the Meta-Catalogue of X-ray detected Clusters of galaxies (MCXC) are combined to investigate the relationship between the thermal Sunyaev-Zeldovich (SZ) signal and X-ray luminosity. The sample comprises ~1600 X-ray clusters with redshifts up to ~1 and spans a wide range in X-ray luminosity. The SZ signal is extracted for each object individually, and the statistical significance of the measurement is maximised by averaging the SZ signal in bins of X-ray luminosity, total mass, or redshift. The SZ signal is detected at very high significance over more than two decades in X-ray luminosity (1043erg s-1 ≲ L500E(z)-7/3 ≲ 2 × 1045erg s-1). The relation between intrinsic SZ signal and X-ray luminosity is investigated and the measured SZ signal is compared to values predicted from X-ray data. Planck measurements and X-ray based predictions are found to be in excellent agreement over the whole explored luminosity range. No significant deviation from standard evolution of the scaling relations is detected. For the first time the intrinsic scatter in the scaling relation between SZ signal and X-ray luminosity is measured and found to be consistent with the one in the luminosity – mass relation from X-ray studies. There is no evidence of any deficit in SZ signal strength in Planck data relative to expectations from the X-ray properties of clusters, underlining the robustness and consistency of our overall view of intra-cluster medium properties.
Corresponding author: R. Piffaretti, e-mail: rocco.piffaretti@cea.fr
| Title: | The dynamical evolution of clusters of galaxies | |
| Authors: | Cavaliere, A.; Santangelo, P.; Tarquini, G.; Vittorio, N. | |
| Affiliation: | AA(Roma II, Università , Rome, Italy), AB(IBM Italia S.p.A., Rome, Italy), AC(Roma I, Università , Rome, Italy), AD(California, University, Berkeley; Roma I, Università , Rome, Italy) | |
| Publication: | Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 305, June 15, 1986, p. 651-667. Research supported by Ministero della Pubblica Istruzione and CNR. (ApJ Homepage) | |
| Publication Date: | 06/1986 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | GALACTIC CLUSTERS, GALACTIC EVOLUTION, HEAO 2, INTERGALACTIC MEDIA, X RAY SOURCES, GRAVITATIONAL COLLAPSE, MORPHOLOGY, SPACE PLASMAS | |
| DOI: | 10.1086/164279 | |
| Bibliographic Code: | 1986ApJ…305..651C |
Abstract
The authors have simulated the dynamical evolution of clusters of galaxies, using a direct N-body integrator, from a large set of statistically equivalent initial conditions. They have also mapped the corresponding X-ray emission from the intracluster plasma at various evolutionary stages in a full three-dimensional description. The simulations are compared with recent observations both in the optical and in the X-ray band, with the purpose of testing the predictive ability for morphologies of the hierarchical clustering scenario. The results describe closely the observed variety of cluster morphologies and predict that only < 30% of the clusters as massive as Coma should be in a relaxed phase, the rest being still in a slowly evolving, clumpy or multicomponent and unrelaxed stage.
| Title: | COBRAS/SAMBA. A mission dedicated to imaging the anisotropies of the cosmic microwave background. Report on the phase A study. | |
| Authors: | Bersanelli, M.; Bouchet, F. R.; Efstathiou, G.; Griffin, M.; Lamarre, J. M.; Mandolesi, N.; Norgaard-Nielsen, H. U.; Pace, O.; Polny, J.; Puget, J. L.; Tauber, J.; Vittorio, N.; Volonté, S. | |
| Publication: | COBRAS/SAMBA. A mission dedicated to imaging the anisotropies of the cosmic microwave background. Report on the phase A study., by Bersanelli, M.; Bouchet, F. R.; Efstathiou, G.; Griffin, M.; Lamarre, J. M.; Mandolesi, N.; Norgaard-Nielsen, H. U.; Pace, O.; Polny, J.; Puget, J. L.; Tauber, J.; Vittorio, N.; Volonté, S.. European Space Agency, Paris (France), Feb 1996, XII + 115, | |
| Publication Date: | 02/1996 | |
| Origin: | ARI | |
| Bibliographic Code: | 1996cmdt.book…..B |
Abstract
COBRAS (Cosmic Background Radiation Anisotropy Satellite) and SAMBA (Satellite for Measurement of Background Anisotropies) were both conceived as 1 meter class telescopes, each carrying broad-band detection systems at four different frequencies, in the case of COBRAS in the range 30 to 130 GHz, and in that of SAMBA 140 to 800 GHz. This report summarizes the results of the scientific and technical study activities of the COBRAS/SAMBA phase A.
Abstract
Using Planck maps of six regions of low Galactic dust emission with a total area of about 140 deg2, we determine the angular power spectra of cosmic infrared background (CIB) anisotropies from multipole ℓ = 200 to ℓ = 2000 at 217, 353, 545 and 857 GHz. We use 21-cm observations of Hi as a tracer of thermal dust emission to reduce the already low level of Galactic dust emission and use the 143 GHz Planck maps in these fields to clean out cosmic microwave background anisotropies. Both of these cleaning processes are necessary to avoid significant contamination of the CIB signal. We measure correlated CIB structure across frequencies. As expected, the correlation decreases with increasing frequency separation, because the contribution of high-redshift galaxies to CIB anisotropies increases with wavelengths. We find no significant difference between the frequency spectrum of the CIB anisotropies and the CIB mean, with ΔI / I = 15% from 217 to 857 GHz. In terms of clustering properties, the Planck data alone rule out the linear scale- and redshift-independent bias model. Non-linear corrections are significant. Consequently, we develop an alternative model that couples a dusty galaxy, parametric evolution model with a simple halo-model approach. It provides an excellent fit to the measured anisotropy angular power spectra and suggests that a different halo occupation distribution is required at each frequency, which is consistent with our expectation that each frequency is dominated by contributions from different redshifts. In our best-fit model, half of the anisotropy power at ℓ = 2000 comes from redshifts z < 0.8 at 857 GHz and z < 1.5 at 545 GHz, while about 90% come from redshifts z > 2 at 353 and 217 GHz, respectively.
Corresponding author: G. Lagache, e-mail: guilaine.lagache@ias.u-psud.fr
Abstract
An all sky map of the apparent temperature and optical depth of thermal dust emission is constructed using the Planck-HFI (350μm to 2 mm) andIRAS(100μm) data. The optical depth maps are correlated with tracers of the atomic (Hi) and molecular gas traced by CO. The correlation with the column density of observed gas is linear in the lowest column density regions at high Galactic latitudes. At high NH, the correlation is consistent with that of the lowest NH, for a given choice of the CO-to-H2 conversion factor. In the intermediate NH range, a departure from linearity is observed, with the dust optical depth in excess of the correlation. This excess emission is attributed to thermal emission by dust associated with a dark gas phase, undetected in the available Hi and CO surveys. The 2D spatial distribution of the dark gas in the solar neighbourhood (|bII| > 10°) is shown to extend around known molecular regions traced by CO. The average dust emissivity in the Hi phase in the solar neighbourhood is found to be τD/NHtot = 5.2×10-26 cm2 at 857 GHz. It follows roughly a power law distribution with a spectral index β = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. Taking into account the spectral shape of the dust optical depth, the emissivity is consistent with previous values derived fromFIRAS measurements at high latitudes within 10%. The threshold for the existence of the dark gas is found at NHtot = (8.0±0.58)×1020 H cm-2 (AV = 0.4mag). Assuming the same high frequency emissivity for the dust in the atomic and the molecular phases leads to an average XCO = (2.54 ± 0.13) × 1020 H2 cm-2/(K km s-1). The mass of dark gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighbourhood. The Galactic latitude distribution shows that its mass fraction is relatively constant down to a few degrees from the Galactic plane. A possible explanation for the dark gas lies in a dark molecular phase, where H2 survives photodissociation but CO does not. The observed transition for the onsetof this phase in the solar neighbourhood (AV= 0.4mag) appears consistent with recent theoretical predictions. It is also possible that up to half of the dark gas could be in atomic form, due to optical depth effects in the Hi measurements.
Corresponding author: J.-P. Bernard, e-mail: Jean-Philippe.Bernard@cesr.fr
| Title: | A Map-Making algorithm for the Planck Surveyor. | |
| Authors: | Natoli, P.; de Gasperis, G.; Gheller, C.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AC(Cineca, Via Magnanelli 6/3, 40033 Caselecchio di Reno (BO), Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy) | |
| Publication: | Astronomy and Astrophysics, v.372, p.346-356 (2001) (A&A Homepage) | |
| Publication Date: | 06/2001 | |
| Origin: | A&A | |
| Astronomy Keywords: | COSMIC MICROWAVE BACKGROUND ANISOTROPIES, METHODS: DATA ANALYSIS | |
| DOI: | 10.1051/0004-6361:20010393 | |
| Bibliographic Code: | 2001A&A…372..346N |
Abstract
We present a parallel implementation of a map-making algorithm for CMB anisotropy experiments which is both fast and efficient. We show for the first time a Maximum Likelihood, minimum variance map obtained by processing the entire data stream expected from the Planck Surveyor, under the assumption of a symmetric beam profile. Here we restrict ourselves to the case of the 30 GHz channel of the Planck Low Frequency Instrument. The extension to Planck higher frequency channels is straightforward. If the satellite pointing periodicity is good enough to average data that belong to the same sky circle, then the code runs very efficiently on workstations. The serial version of our code also runs on very competitive time-scales the map-making pipeline for current and forthcoming balloon borne experiments.
| Title: | Planck pre-launch status: The Planck-LFI programme | |
| Authors: | Mandolesi, N.; Bersanelli, M.; Butler, R. C.; Artal, E.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartelmann, M.; Bennett, K.; Bhandari, P.; Bonaldi, A.; Borrill, J.; Bremer, M.; Burigana, C.; Bowman, R. C.; Cabella, P.; Cantalupo, C.; Cappellini, B.; Courvoisier, T.; Crone, G.; Cuttaia, F.; Danese, L.; D’Arcangelo, O.; Davies, R. D.; Davis, R. J.; de Angelis, L.; de Gasperis, G.; de Rosa, A.; de Troia, G.; de Zotti, G.; Dick, J.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Dörl, U.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.; Falvella, M. C.; Finelli, F.; Frailis, M.; Franceschi, E.; Gaier, T.; Galeotta, S.; Gasparo, F.; Giardino, G.; Gomez, F.; Gonzalez-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F.; Hell, R.; Herranz, D.; Herreros, J. M.; Hildebrandt, S.; Hovest, W.; Hoyland, R.; Huffenberger, K.; Janssen, M.; Jaffe, T.; Keihänen, E.; Keskitalo, R.; Kisner, T.; Kurki-Suonio, H.; Lähteenmäki, A.; Lawrence, C. R.; Leach, S. M.; Leahy, J. P.; Leonardi, R.; Levin, S.; Lilje, P. B.; López-Caniego, M.; Lowe, S. R.; Lubin, P. M.; Maino, D.; Malaspina, M.; Maris, M.; Marti-Canales, J.; Martinez-Gonzalez, E.; Massardi, M.; Matarrese, S.; Matthai, F.; Meinhold, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Morgante, G.; Morigi, G.; Morisset, N.; Moss, A.; Nash, A.; Natoli, P.; Nesti, R.; Paine, C.; Partridge, B.; Pasian, F.; Passvogel, T.; Pearson, D.; Pérez-Cuevas, L.; Perrotta, F.; Polenta, G.; Popa, L. A.; Poutanen, T.; Prezeau, G.; Prina, M.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Ricciardi, S.; Riller, T.; Rocha, G.; Roddis, N.; Rohlfs, R.; Rubiño-Martin, J. A.; Salerno, E.; Sandri, M.; Scott, D.; Seiffert, M.; Silk, J.; Simonetto, A.; Smoot, G. F.; Sozzi, C.; Sternberg, J.; Stivoli, F.; Stringhetti, L.; Tauber, J.; Terenzi, L.; Tomasi, M.; Tuovinen, J.; Türler, M.; Valenziano, L.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L.; White, M.; White, S.; Wilkinson, A.; Zacchei, A.; Zonca, A. | |
| Affiliation: | AA(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy mandolesi@iasfbo.inaf.it), AB(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, 20133 Milano, Italy), AC(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AD(Dep. Ing. de Comunicaciones (DICOM), Universidad de Cantabria Av. De Los Castros S/N, 39005 Santander, Spain), AE(SISSA/ISAS, Scuola Internazionale di Studi Superiori Avanzati/International Schools for Advanced Studies, Astrophysics Sector, via Beirut 2-4, Sezione di Trieste, 34014 Trieste, Italy; INFN, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, via Valerio, 2, 34127 Trieste, Italy; INAF – OATs, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy), AF(Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AG(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany; CESR, Centre d’Étude Spatiale des Rayonnements, 9 Av du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France), AH(Instituto de Fisica de Cantabria, CSIC- Universidad de Cantabria, Avenida de los Castros s/n, 39005 Santander, Spain), AI(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AJ(Research and Scientific Support Department of ESA, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands), AK(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), AL(INAF – OAPd, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, 35122 Padova, Italy), AM(University of California, Berkeley Space Sciences Lab 7 Gauss Way Berkeley, CA 94720, USA; Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley CA 94720, USA), AN(Research and Scientific Support Department of ESA, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands), AO(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AP(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), AQ(Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy; Dipartimento di Fisica, Università di Roma “La Sapienza”, p.le A. Moro 2, 00185 Roma, Italy), AR(Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley CA 94720, USA), AS(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, 20133 Milano, Italy), AT(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland), AU(Herschel/Planck Project, Scientific Projects Dpt of ESA, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands), AV(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AW(SISSA/ISAS, Scuola Internazionale di Studi Superiori Avanzati/International Schools for Advanced Studies, Astrophysics Sector, via Beirut 2-4, Sezione di Trieste, 34014 Trieste, Italy), AX(IFP-CNR, Istituto di Fisica del Plasma, Consiglio Nazionale delle Ricerche, via Roberto Cozzi, 53, 20125 Milano, Italy), AY(Jodrell Bank Centre for Astrophysics, University of Manchester, M13 9PL, UK), AZ(Jodrell Bank Centre for Astrophysics, University of Manchester, M13 9PL, UK), BA(ASI, Agenzia Spaziale Italiana, Viale Liegi, 26, 00198 Roma, Italy), BB(Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), BC(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), BD(Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), BE(INAF – OAPd, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, 35122 Padova, Italy), BF(SISSA/ISAS, Scuola Internazionale di Studi Superiori Avanzati/International Schools for Advanced Studies, Astrophysics Sector, via Beirut 2-4, Sezione di Trieste, 34014 Trieste, Italy), BG(Jodrell Bank Centre for Astrophysics, University of Manchester, M13 9PL, UK), BH(Instituto de Fisica de Cantabria, CSIC- Universidad de Cantabria, Avenida de los Castros s/n, 39005 Santander, Spain), BI(Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway; Centre of Mathematics for Applications, University of Oslo, PO Box 1053 Blindern, 0316 Oslo, Norway), BJ(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), BK(ESA – ESAC, European Space Agency, European Space Astronomy Centre, Villafranca del Castillo, Apdo. 50727, 28080 Madrid, Spain), BL(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), BM(Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway; Centre of Mathematics for Applications, University of Oslo, PO Box 1053 Blindern, 0316 Oslo, Norway), BN(ASI, Agenzia Spaziale Italiana, Viale Liegi, 26, 00198 Roma, Italy), BO(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy; INAF-OABo, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), BP(INAF – OATs, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, via G.B. 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Moro 2, 00185 Roma, Italy), DI(ESA/ESAC/RSSD, European Space Agency, European Space Astronomy Centre, Research and Scientific Support Department, PO Box – Apdo. de correos 78, 28691 Villanueva de la Cañada, Madrid, Spain), DJ(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, 20133 Milano, Italy), DK(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), DL(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), DM(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland), DN(Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T 1Z1, Canada), DO(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DP(Dipartimento di Fisica, Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy; INFN, Istituto Nazionale di Fisica Nucleare, Sezione di Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy; ASI, Agenzia Spaziale Italiana, Science Data Center, c/o ESRIN, via G. Galilei, 00044 Frascati, Italy; INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), DQ(Osservatorio Astrofisico di Arcetri, L.go E. Fermi 5, Firenze, Italy), DR(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DS(Department of Astronomy, Haverford College, Haverford, PA 19041, USA), DT(INAF – OATs, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy), DU(Herschel/Planck Project, Scientific Projects Dpt of ESA, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands), DV(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DW(Herschel/Planck Project, Scientific Projects Dpt of ESA, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands), DX(SISSA/ISAS, Scuola Internazionale di Studi Superiori Avanzati/International Schools for Advanced Studies, Astrophysics Sector, via Beirut 2-4, Sezione di Trieste, 34014 Trieste, Italy), DY(ASI, Agenzia Spaziale Italiana, Science Data Center, c/o ESRIN, via G. Galilei, 00044 Frascati, Italy; Dipartimento di Fisica, Università di Roma “La Sapienza”, p.le A. Moro 2, 00185 Roma, Italy; INAF-OARo, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), DZ(Institute for Space Sciences, Bucharest-Magurele, Str. Atomostilor, 409, Po Box Mg-23, Ro-077125, Romania), EA(Helsinki Institute of Physics, PO Box 64, 00014 Helsinki, Finland; University of Helsinki, Department of Physics, PO Box 64, 00014 Helsinki, Finland; Metsähovi Radio Observatory, TKK, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland), EB(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), EC(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), ED(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), EE(Instituto de AstrofÃsica de Canarias, C/ vÃa Láctea s/n, 38200, La Laguna, Tenerife, Spain), EF(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), EG(INAF – IASF Bologna, Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy; University of California, Berkeley Space Sciences Lab 7 Gauss Way Berkeley, CA 94720, USA; Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley CA 94720, USA), EH(MPA – Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), EI(Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Drive, Pasadena, CA 91109, USA), EJ(Jodrell Bank Centre for Astrophysics, University of Manchester, M13 9PL, UK), EK(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland), EL(Instituto de AstrofÃsica de Canarias, C/ vÃa Láctea s/n, 38200, La Laguna, Tenerife, Spain), EM(Istituto di Scienza e Technologie dellInformazione “Alessandro Faedo”, CNR, Consiglio Nazionale delle Ricerche, Area della Ricerca di Pisa, via G. 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Tiepolo 11, 34131 Trieste, Italy), FM(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, 20133 Milano, Italy) | |
| Publication: | Astronomy and Astrophysics, Volume 520, id.A3 (A&A Homepage) | |
| Publication Date: | 09/2010 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | cosmic microwave background, space vehicles: instruments, instrumentation: detectors, instrumentation: polarimeters, submillimeter: general, telescopes | |
| DOI: | 10.1051/0004-6361/200912837 | |
| Bibliographic Code: | 2010A&A…520A…3M |
Abstract
This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27-77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration, performance, and verification phases will be completed, after which Planck will begin its operational life, in which LFI will have an integral part.
Abstract
We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (~10ks) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (4 < S/N < 6), and a further 15 in a programme to observe a sample of S/N > 5 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N ≤ 4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about ~70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z = 0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09 ≲ z ≲ 0.54, with a median redshift of z ~ 0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y500. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y500-YX relation established for X-ray selected objects, where YXis the product of the gas mass and temperature.
Corresponding author: E. Pointecouteau, e-mail: etienne.pointecouteau@irap.omp.eu
| Title: | Planck early results. III. First assessment of the Low Frequency Instrument in-flight performance | |
| Authors: | Mennella, A.; Butler, R. C.; Curto, A.; Cuttaia, F.; Davis, R. J.; Dick, J.; Frailis, M.; Galeotta, S.; Gregorio, A.; Kurki-Suonio, H.; Lawrence, C. R.; Leach, S.; Leahy, J. P.; Lowe, S.; Maino, D.; Mandolesi, N.; Maris, M.; MartÃnez-González, E.; Meinhold, P. R.; Morgante, G.; Pearson, D.; Perrotta, F.; Polenta, G.; Poutanen, T.; Sandri, M.; Seiffert, M. D.; Suur-Uski, A.-S.; Tavagnacco, D.; Terenzi, L.; Tomasi, M.; Valiviita, J.; Villa, F.; Watson, R.; Wilkinson, A.; Zacchei, A.; Zonca, A.; Aja, B.; Artal, E.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Bartolo, N.; Battaglia, P.; Bennett, K.; Bonaldi, A.; Bonavera, L.; Borrill, J.; Bouchet, F. R.; Burigana, C.; Cabella, P.; Cappellini, B.; Chen, X.; Colombo, L.; Cruz, M.; Danese, L.; D’Arcangelo, O.; Davies, R. D.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falvella, M. C.; Finelli, F.; Foley, S.; Franceschet, C.; Franceschi, E.; Gaier, T. C.; Génova-Santos, R. T.; George, D.; Gómez, F.; González-Nuevo, J.; Górski, K. M.; Gruppuso, A.; Hansen, F. K.; Herranz, D.; Herreros, J. M.; Hoyland, R. J.; Hughes, N.; Jewell, J.; Jukkala, P.; Juvela, M.; Kangaslahti, P.; Keihänen, E.; Keskitalo, R.; Kilpia, V.-H.; Kisner, T. S.; Knoche, J.; Knox, L.; Laaninen, M.; Lähteenmäki, A.; Lamarre, J.-M.; Leonardi, R.; León-Tavares, J.; Leutenegger, P.; Lilje, P. B.; López-Caniego, M.; Lubin, P. M.; Malaspina, M.; Marinucci, D.; Massardi, M.; Matarrese, S.; Matthai, F.; Melchiorri, A.; Mendes, L.; Miccolis, M.; Migliaccio, M.; Mitra, S.; Moss, A.; Natoli, P.; Nesti, R.; Nørgaard-Nielsen, H. U.; Pagano, L.; Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.; Pettorino, V.; Pietrobon, D.; Pospieszalski, M.; Prézeau, G.; Prina, M.; Procopio, P.; Puget, J.-L.; Quercellini, C.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Ricciardi, S.; Robbers, G.; Rocha, G.; Roddis, N.; Rubino-MartÃn, J. A.; Savelainen, M.; Scott, D.; Silvestri, R.; Simonetto, A.; Sjoman, P.; Smoot, G. F.; Sozzi, C.; Stringhetti, L.; Tauber, J. A.; Tofani, G.; Toffolatti, L.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Varis, J.; Vielva, P.; Vittorio, N.; Wade, L. A.; Watson, C.; White, S. D. M.; Winder, F. | |
| Affiliation: | AA(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy aniello.mennella@fisica.unimi.it; INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AB(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), AC(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), AD(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), AE(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), AF(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AG(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AH(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AI(Dipartimento di Fisica, Università degli Studi di Trieste, via A. 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Padana Superiore 290, 20090, Vimodrone (MI), Italy), DW(Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway; Centre of Mathematics for Applications, University of Oslo, Blindern, Oslo, Norway), DX(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), DY(Department of Physics, University of California, Santa Barbara, California, USA), DZ(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), EA(Dipartimento di Matematica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), EB(INAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, Padova, Italy), EC(Dipartimento di Fisica G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131, Padova, Italy), ED(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), EE(Dipartimento di Fisica, Università La Sapienza, P. le A. Moro 2, Roma, Italy), EF(European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Ca nada, Madrid, Spain), EG(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090, Vimodrone (MI), Italy), EH(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), EI(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EJ(Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), EK(Dipartimento di Fisica, Università di Ferrara, via Saragat 1, 44122, Ferrara, Italy; Agenzia Spaziale Italiana Science Data Center, c/o ESRIN, via Galileo Galilei, Frascati, Italy; INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), EL(INAF – Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, Firenze, Italy), EM(DTU Space, National Space Institute, Juliane Mariesvej 30, Copenhagen, Denmark), EN(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EO(Spitzer Science Center, 1200 E. California Blvd., Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), EP(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), EQ(Haverford College Astronomy Department, 370 Lancaster Avenue, Haverford, Pennsylvania, USA), ER(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), ES(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), ET(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EU(National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22903-2475, USA), EV(California Institute of Technology, Pasadena, California, USA; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EW(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EX(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), EY(Institut d’Astrophysique Spatiale, CNRS (UMR 8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), EZ(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), FA(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), FB(Instituto de AstrofÃsica de Canarias, C/vÃa Láctea s/n, La Laguna, Tenerife, Spain; Dpto. AstrofÃsica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain), FC(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), FD(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), FE(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), FF(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), FG(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), FH(Instituto de AstrofÃsica de Canarias, C/vÃa Láctea s/n, La Laguna, Tenerife, Spain; Dpto. AstrofÃsica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain), FI(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland; Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland), FJ(Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), FK(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090, Vimodrone (MI), Italy), FL(Istituto di Fisica del Plasma, CNR-ENEA-EURATOM Association, via R. Cozzi 53, Milano, Italy), FM(DA-Design Oy, Keskuskatu 29, Jokioinen, Finland), FN(Department of Physics, University of California, Berkeley, California, USA; Lawrence Berkeley National Laboratory, Berkeley, California, USA; Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), FO(Istituto di Fisica del Plasma, CNR-ENEA-EURATOM Association, via R. Cozzi 53, Milano, Italy), FP(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), FQ(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), FR(INAF – Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, Firenze, Italy), FS(Departamento de FÃsica, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo, Spain), FT(MilliLab, VTT Technical Research Centre of Finland, Tietotie 3, Espoo, Finland), FU(ISDC Data Centre for Astrophysics, University of Geneva, Ch. d’Écogia 16, Versoix, Switzerland), FV(INAF – Osservatorio Astrofisico diCatania, via S. Sofia 78, Catania, Italy), FW(INAF/IASF Bologna, via Gobetti 101, Bologna, Italy), FX(MilliLab, VTT Technical Research Centre of Finland, Tietotie 3, Espoo, Finland), FY(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), FZ(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), GA(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), GB(European Space Agency, ESOC, Robert-Bosch-Str. 5, Darmstadt, Germany), GC(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), GD(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK) | |
| Publication: | Astronomy & Astrophysics, Volume 536, id.A3 (A&A Homepage) | |
| Publication Date: | 12/2011 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | cosmic background radiation, cosmology: observations, space vehicles: instruments, instrumentation: detectors | |
| DOI: | 10.1051/0004-6361/201116480 | |
| Bibliographic Code: | 2011A&A…536A…3M |
Abstract
The scientific performance of the Planck Low Frequency Instrument (LFI) after one year of in-orbit operation is presented. We describe the main optical parameters and discuss photometric calibration, white noise sensitivity, and noise properties. A preliminary evaluation of the impact of the main systematic effects is presented. For each of the performance parameters, we outline the methods used to obtain them from the flight data and provide a comparison with pre-launch ground assessments, which are essentially confirmed in flight.
Corresponding author: A. Mennella, e-mail: aniello.mennella@fisica.unimi.it
| Title: | Planck pre-launch status: Design and description of the Low Frequency Instrument | |
| Authors: | Bersanelli, M.; Mandolesi, N.; Butler, R. C.; Mennella, A.; Villa, F.; Aja, B.; Artal, E.; Artina, E.; Baccigalupi, C.; Balasini, M.; Baldan, G.; Banday, A.; Bastia, P.; Battaglia, P.; Bernardino, T.; Blackhurst, E.; Boschini, L.; Burigana, C.; Cafagna, G.; Cappellini, B.; Cavaliere, F.; Colombo, F.; Crone, G.; Cuttaia, F.; D’Arcangelo, O.; Danese, L.; Davies, R. D.; Davis, R. J.; de Angelis, L.; de Gasperis, G. C.; de La Fuente, L.; de Rosa, A.; de Zotti, G.; Falvella, M. C.; Ferrari, F.; Ferretti, R.; Figini, L.; Fogliani, S.; Franceschet, C.; Franceschi, E.; Gaier, T.; Garavaglia, S.; Gomez, F.; Gorski, K.; Gregorio, A.; Guzzi, P.; Herreros, J. M.; Hildebrandt, S. R.; Hoyland, R.; Hughes, N.; Janssen, M.; Jukkala, P.; Kettle, D.; Kilpiä, V. H.; Laaninen, M.; Lapolla, P. M.; Lawrence, C. R.; Lawson, D.; Leahy, J. P.; Leonardi, R.; Leutenegger, P.; Levin, S.; Lilje, P. B.; Lowe, S. R.; Lubin, P. M.; Maino, D.; Malaspina, M.; Maris, M.; Marti-Canales, J.; Martinez-Gonzalez, E.; Mediavilla, A.; Meinhold, P.; Miccolis, M.; Morgante, G.; Natoli, P.; Nesti, R.; Pagan, L.; Paine, C.; Partridge, B.; Pascual, J. P.; Pasian, F.; Pearson, D.; Pecora, M.; Perrotta, F.; Platania, P.; Pospieszalski, M.; Poutanen, T.; Prina, M.; Rebolo, R.; Roddis, N.; Rubiño-Martin, J. A.; Salmon, M. J.; Sandri, M.; Seiffert, M.; Silvestri, R.; Simonetto, A.; Sjoman, P.; Smoot, G. F.; Sozzi, C.; Stringhetti, L.; Taddei, E.; Tauber, J.; Terenzi, L.; Tomasi, M.; Tuovinen, J.; Valenziano, L.; Varis, J.; Vittorio, N.; Wade, L. A.; Wilkinson, A.; Winder, F.; Zacchei, A.; Zonca, A. | |
| Affiliation: | AA(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy; INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Bassini 15, 20133 Milano, Italy), AB(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), AC(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), AD(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy; INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Bassini 15, 20133 Milano, Italy), AE(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), AF(Universidad de Cantabria, Departamento de Ingenieria de Comunicaciones, Av. de Los Castros s/n, 39005 Santander, Spain), AG(Universidad de Cantabria, Departamento de Ingenieria de Comunicaciones, Av. de Los Castros s/n, 39005 Santander, Spain), AH(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AI(SISSA/ISAS, Astrophysics Sector, Via Beirut 4, 34014 Trieste, Italy; INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy), AJ(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AK(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AL(CESR, Centre d’Étude Spatiale des Rayonnements, 9 Av. du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France; MPA Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AM(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AN(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AO(Instituto de Fisica de Cantabria, CSIC, Universidad de Cantabria, Av. de los Castros s/n, 39005 Santander, Spain), AP(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), AQ(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AR(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), AS(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AT(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy; INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Bassini 15, 20133 Milano, Italy), AU(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy), AV(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), AW(Herschel/Planck Project, Scientific Projects Dpt of ESA, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands), AX(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), AY(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), AZ(SISSA/ISAS, Astrophysics Sector, Via Beirut 4, 34014 Trieste, Italy), BA(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), BB(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), BC(ASI, Agenzia Spaziale Italiana, viale Liegi, 26, 00198 Roma, Italy), BD(Dipartimento di Fisica, Università degli Studi di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy), BE(Universidad de Cantabria, Departamento de Ingenieria de Comunicaciones, Av. de Los Castros s/n, 39005 Santander, Spain), BF(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), BG(INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy), BH(ASI, Agenzia Spaziale Italiana, viale Liegi, 26, 00198 Roma, Italy), BI(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), BJ(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), BK(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), BL(INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy), BM(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy), BN(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), BO(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), BP(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), BQ(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), BR(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), BS(Dipartimento di Fisica, Università degli Studi di Trieste, via A. Valerio 2, 34127 Trieste, Italy), BT(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), BU(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), BV(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), BW(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), BX(DA-Design Oy, Keskuskatu 29, 31600 Jokioinen, Finland), BY(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), BZ(DA-Design Oy, Keskuskatu 29, 31600 Jokioinen, Finland), CA(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), CB(DA-Design Oy, Keskuskatu 29, 31600 Jokioinen, Finland), CC(Ylinen Electronics Oy, Teollisuustie 9A, 02700 Kauniainen, Finland), CD(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), CE(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), CF(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), CG(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), CH(Department of Physics, University of California, Santa Barbara, CA 93106, USA), CI(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), CJ(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), CK(Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway), CL(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), CM(Department of Physics, University of California, Santa Barbara, CA 93106, USA), CN(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy), CO(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), CP(INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy), CQ(Herschel/Planck Project, Scientific Projects Dpt of ESA, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands), CR(Instituto de Fisica de Cantabria, CSIC, Universidad de Cantabria, Av. de los Castros s/n, 39005 Santander, Spain), CS(Universidad de Cantabria, Departamento de Ingenieria de Comunicaciones, Av. de Los Castros s/n, 39005 Santander, Spain), CT(Department of Physics, University of California, Santa Barbara, CA 93106, USA), CU(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), CV(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), CW(Dipartimento di Fisica, Università degli Studi di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy), CX(INAF – Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy), CY(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), CZ(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DA(Haverford College, 370 Lancaster Avenue, Haverford, PA 19041, USA), DB(Universidad de Cantabria, Departamento de Ingenieria de Comunicaciones, Av. de Los Castros s/n, 39005 Santander, Spain), DC(INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy), DD(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DE(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), DF(INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy; SISSA/ISAS, Astrophysics Sector, Via Beirut 4, 34014 Trieste, Italy), DG(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), DH(National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903-2475, USA), DI(University of Helsinki, Department of Physics, PO Box 64, 00014 Helsinki, Finland; Helsinki Institute of Physics, University of Helsinki, PO Box 64, 00014, Finland; Metsähovi Radio Observatory, Helsinki University of Technology, Metsähovintie 114, 02540, Kylmälä, Finland), DJ(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DK(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), DL(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), DM(Instituto de Astrofisica de Canarias, C/ via Lactea s/n, 38200 La Laguna, Tenerife, Spain), DN(Instituto de Fisica de Cantabria, CSIC, Universidad de Cantabria, Av. de los Castros s/n, 39005 Santander, Spain), DO(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), DP(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), DQ(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), DR(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), DS(DA-Design Oy, Keskuskatu 29, 31600 Jokioinen, Finland), DT(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), DU(Istituto di Fisica del Plasma, CNR, via Cozzi 53, 20125 Milano, Italy), DV(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), DW(Thales Alenia Space Italia S.p.A., S.S. Padana Superiore 290, 20090 Vimodrone, Milano, Italy), DX(European Space Agency (ESA), Astrophysics Division, Keplerlaan 1, 2201AZ Noordwijk, The Netherlands), DY(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), DZ(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy), EA(MilliLab, VTT Technical Research Centre of Finland, PO Box 1000, 02044 VTT, Finland), EB(INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via P. Gobetti, 101, 40129 Bologna, Italy), EC(MilliLab, VTT Technical Research Centre of Finland, PO Box 1000, 02044 VTT, Finland), ED(Dipartimento di Fisica, Università degli Studi di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy), EE(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA), EF(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), EG(Jodrell Bank Centre for Astrophysics, Alan Turing Building, The University of Manchester, Manchester, M13 9PL, UK), EH(INAF – Osservatorio Astronomico di Trieste, via Tiepolo, 11, 34143 Trieste, Italy), EI(Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy; INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, via Bassini 15, 20133 Milano, Italy) | |
| Publication: | Astronomy and Astrophysics, Volume 520, id.A4 (A&A Homepage) | |
| Publication Date: | 09/2010 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | cosmic microwave background, cosmology: observations, space vehicles: instruments | |
| DOI: | 10.1051/0004-6361/200912853 | |
| Bibliographic Code: | 2010A&A…520A…4B |
Abstract
In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA programme dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100-850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art indium phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference signals. The front end is cooled to 20 K for optimal sensitivity and the reference loads are cooled to 4 K to minimise low-frequency noise. We provide an overview of the LFI, discuss the leading scientific requirements, and describe the design solutions adopted for the various hardware subsystems. The main drivers of the radiometric, optical, and thermal design are discussed, including the stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results of ground calibration are provided in a set of companion papers.
Abstract
Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10-60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and Ï Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20-40 GHz and are detected at high significances of 17.1σ for Perseus and 8.4σ for Ï Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In Ï Ophiuchi, the ~30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50-100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright Hii regions that show evidence for AME, and are well fitted by spinning dust models.
Corresponding author: C. Dickinson, Clive.Dickinson@manchester.ac.uk
Abstract
We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y500 – N200) for the MaxBCG cluster catalogue. Employing a multi-frequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N200 – M500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M500 ≈ 5 × 1013 Msun. The observed Y500 – N200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y500 – N200relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters.
Corresponding author: J. G. Bartlett, e-mail: bartlett@apc.univ-paris7.fr
Abstract
We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters (z < 0.5) detected at high signal-to-noise in the first Planck all-sky data set. The sample spans approximately a decade in total mass, 2 × 1014 Msun < M500 < 2 × 1015 Msun, where M500 is the mass corresponding to a total density contrast of 500. Combining these high quality Planck measurements with deep XMM-Newton X-ray data, we investigate the relations between DA2 Y500, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass Mg,500, temperature TX, luminosity LX,500, SZ signal analogue YX,500 = Mg,500 × TX, and total mass M500. After correction for the effect of selection bias on the scaling relations, we find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. The present data yield an exceptionally robust, high-quality local reference, and illustrate Planck’s unique capabilities for all-sky statistical studies of galaxy clusters.
Corresponding author: G. W. Pratt, e-mail: gabriel.pratt@cea.fr
| Title: | Spherical needlets for cosmic microwave background data analysis | |
| Authors: | Marinucci, D.; Pietrobon, D.; Balbi, A.; Baldi, P.; Cabella, P.; Kerkyacharian, G.; Natoli, P.; Picard, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Matematica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma), AB(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma), AC(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma; INFN Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma), AD(Dipartimento di Matematica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma), AE(University of Oxford, Astrophysics, Keble Road, Oxford OX1 3RH), AF(Université de Paris 10 and Laboratoire de Probabilités et Modèles Aléatoires), AG(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma; INFN Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma), AH(Université de Paris 7 and Laboratoire de Probabilités et Modèles Aléatoires), AI(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma; INFN Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, 00133 Roma) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 383, Issue 2, pp. 539-545. (MNRAS Homepage) | |
| Publication Date: | 01/2008 | |
| Origin: | MNRAS | |
| Astronomy Keywords: | methods: data analysis , cosmic microwave background , cosmology: observations | |
| DOI: | 10.1111/j.1365-2966.2007.12550.x | |
| Bibliographic Code: | 2008MNRAS.383..539M |
Abstract
We discuss spherical needlets and their properties. Needlets are a form of spherical wavelets which do not rely on any kind of tangent plane approximation and enjoy good localization properties in both pixel and harmonic space; moreover needlet coefficients are asymptotically uncorrelated at any fixed angular distance, which makes their use in statistical procedures very promising. In view of these properties, we believe needlets may turn out to be especially useful in the analysis of cosmic microwave background (CMB) data on the incomplete sky, as well as of other cosmological observations. As a final advantage, we stress that the implementation of needlets is computationally very convenient and may rely completely on standard data analysis packages such as HEALPix.
Abstract
This paper presents the first results from a comparison of Planck dust maps at 353, 545 and 857GHz, along with IRAS data at 3000 (100 μm) and 5000GHz (60 μm), with Green Bank Telescope 21-cm observations of Hi in 14 fields covering more than 800 deg2 at high Galactic latitude. The main goal of this study is to estimate the far-infrared to sub-millimeter (submm) emissivity of dust in the diffuse local interstellar medium (ISM) and in the intermediate-velocity (IVC) and high-velocity clouds (HVC) of the Galactic halo. Galactic dust emission for fields with average Hi column density lower than 2 × 1020 cm-2 is well correlated with 21-cm emission because in such diffuse areas the hydrogen is predominantly in the neutral atomic phase. The residual emission in these fields, once the Hi-correlated emission is removed, is consistent with the expected statistical properties of the cosmic infrared background fluctuations. The brighter fields in our sample, with an average Hi column density greater than 2 × 1020 cm-2, show significant excess dust emission compared to the Hi column density. Regions of excess lie in organized structures that suggest the presence of hydrogen in molecular form, though they are not always correlated with CO emission. In the higher Hi column density fields the excess emission at 857 GHz is about 40% of that coming from the Hi, but over all the high latitude fields surveyed the molecular mass faction is about 10%. Dust emission from IVCs is detected with high significance by this correlation analysis. Its spectral properties are consistent with, compared to the local ISM values, significantly hotter dust (T ~ 20K), lower submm dust opacity normalized per H-atom, and a relative abundance of very small grains to large grains about four times higher. These results are compatible with expectations for clouds that are part of the Galactic fountain in which there is dust shattering and fragmentation. Correlated dust emission in HVCs is not detected; the average of the 99.9% confidence upper limits to the emissivity is 0.15 times the local ISM value at 857 and 3000GHz, in accordance with gas phase evidence for lower metallicity and depletion in these clouds. Unexpected anti-correlated variations of the dust temperature and emission cross-section per H atom are identified in the local ISM and IVCs, a trend that continues into molecular environments. This suggests that dust growth through aggregation, seen in molecular clouds, is active much earlier in the cloud condensation and star formation processes.
Corresponding author: M.-A. Miville-Deschênes, e-mail: mamd@ias.u-psud.fr
Abstract
The integrated spectral energy distributions (SED) of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) appear significantly flatter than expected from dust models based on their far-infrared and radio emission. The still unexplained origin of this millimetre excess is investigated here using the Planck data. The integrated SED of the two galaxies before subtraction of the foreground (Milky Way) and background (CMB fluctuations) emission are in good agreement with previous determinations, confirming the presence of the millimetre excess. In the context of this preliminary analysis we do not propose a full multi-component fitting of the data, but instead subtract contributions unrelated to the galaxies and to dust emission. The background CMB contribution is subtracted using an internal linear combination (ILC) method performed locally around the galaxies. The foreground emission from the Milky Way is subtracted as a Galactic Hi template, and the dust emissivity is derived in a region surrounding the two galaxies and dominated by Milky Way emission. After subtraction, the remaining emission of both galaxies correlates closely with the atomic and molecular gas emission of the LMC and SMC. The millimetre excess in the LMC can be explained by CMB fluctuations, but a significant excess is still present in the SMC SED. The Planck and IRAS-IRIS data at 100 μm are combined to produce thermal dust temperature and optical depth maps of the two galaxies. The LMC temperature map shows the presence of a warm inner arm already found with the Spitzer data, but which also shows the existence of a previously unidentified cold outer arm. Several cold regions are found along this arm, some of which are associated with known molecular clouds. The dust optical depth maps are used to constrain the thermal dust emissivity power-law index (β). The average spectral index is found to be consistent with β = 1.5 and β = 1.2 below 500μm for the LMC and SMC respectively, significantly flatter than the values observed in the Milky Way. Also, there is evidence in the SMC of a further flattening of the SED in the sub-mm, unlike for the LMC where the SED remains consistent with β = 1.5. The spatial distribution of the millimetre dustexcess in the SMC follows the gas and thermal dust distribution. Different models are explored in order to fit the dust emission in the SMC. It is concluded that the millimetre excess is unlikely to be caused by very cold dust emission and that it could be due to a combination of spinning dust emission and thermal dust emission by more amorphous dust grains than those present in our Galaxy.
Corresponding author: J.-P. Bernard, e-mail: jean-philippe.bernard@cesr.fr
Abstract
Planck allows unbiased mapping of Galactic sub-millimetre and millimetre emission from the most diffuse regions to the densest parts of molecular clouds. We present an early analysis of the Taurus molecular complex, on line-of-sight-averaged data and without component separation. The emission spectrum measured by Planck and IRAS can be fitted pixel by pixel using a single modified blackbody. Some systematic residuals are detected at 353 GHz and 143 GHz, with amplitudes around -7% and +13%, respectively, indicating that the measured spectra are likely more complex than a simple modified blackbody. Significant positive residuals are also detected in the molecular regions and in the 217 GHz and 100 GHz bands, mainly caused by the contribution of the J = 2 → 1 and J = 1 → 0 12CO and 13CO emission lines. We derive maps of the dust temperature T, the dust spectral emissivity index β, and the dust optical depth at 250 μm Ï„250. The temperature map illustrates the cooling of the dust particles in thermal equilibrium with the incident radiation field, from 16 – 17 K in the diffuse regions to 13 – 14 K in the dense parts. The distribution of spectral indices is centred at 1.78, with a standard deviation of 0.08 and a systematic error of 0.07. We detect a significant T – β anti-correlation. The dust optical depth map reveals the spatial distribution of the column density of the molecular complex from the densest molecular regions to the faint diffuse regions. We use near-infrared extinction and Hi data at 21-cm to perform a quantitative analysis of the spatial variations of the measured dust optical depth at 250 μm per hydrogen atom Ï„250/NH. We report an increase of Ï„250/NHby a factor of about 2 between the atomic phase and the molecular phase, which has a strong impact on the equilibrium temperature of the dust particles.
Corresponding author: A. Abergel, e-mail: alain.abergel@ias.u-psud.fr
Abstract
Spectral energy distributions (SEDs) and radio continuum spectra are presented for a northern sample of 104 extragalactic radio sources, based on the Planck Early Release Compact Source Catalogue (ERCSC) and simultaneous multifrequency data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous observations ranging from radio to gamma-rays. This is the first extensive frequency coverage in the radio and millimetre domains for an essentially complete sample of extragalactic radio sources, and it shows how the individual shocks, each in their own phase of development, shape the radio spectra as they move in the relativistic jet. The SEDs presented in this paper were fitted with second and third degree polynomials to estimate the frequencies of the synchrotron and inverse Compton (IC) peaks, and the spectral indices of low and high frequency radio data, including the Planck ERCSC data, were calculated. SED modelling methods are discussed, with an emphasis on proper, physical modelling of the synchrotron bump using multiple components. Planck ERCSC data also suggest that the original accelerated electron energy spectrum could be much harder than commonly thought, with power-law indexaround 1.5 instead of the canonical 2.5. The implications of this are discussed for the acceleration mechanisms effective in blazar shocks. Furthermore in many cases the Planck data indicate that gamma-ray emission must originate in the same shocks that produce the radio emission.
Tables 1 and 4, Figs. 18-121 are available in electronic form at http://www.aanda.org
Abstract
The data reported in Planck’s Early Release Compact Source Catalogue (ERCSC) are exploited to measure the number counts (dN/dS) of extragalactic radio sources at 30, 44, 70, 100, 143 and 217 GHz. Due to the full-sky nature of the catalogue, this measurement extends to the rarest and brightest sources in the sky. At lower frequencies (30, 44, and 70 GHz) our counts are in very good agreement with estimates based on WMAP data, being somewhat deeper at 30 and 70 GHz, and somewhat shallower at 44 GHz. Planck’s source counts at 143 and 217 GHz join smoothly with the fainter ones provided by the SPT and ACT surveys over small fractions of the sky. An analysis of source spectra, exploiting Planck’s uniquely broad spectral coverage, finds clear evidence of a steepening of the mean spectral index above about 70 GHz. This implies that, at these frequencies, the contamination of the CMB power spectrum by radio sources below the detection limit is significantly lower than previously estimated.
Corresponding author: J. González-Nuevo, e-mail: gnuevo@sissa.it
| Title: | Scale-invariant density perturbations, anisotropy of the cosmic microwave background, and large-scale peculiar velocity field | |
| Authors: | Vittorio, N.; Silk, J. | |
| Affiliation: | AA(Chicago, University, Chicago, IL; Roma, Università , Rome, Italy), AB(California, University, Berkeley, CA) | |
| Publication: | Astrophysical Journal, Part 2 – Letters to the Editor (ISSN 0004-637X), vol. 293, June 1, 1985, p. L1-L5. NASA-supported research. (ApJL Homepage) | |
| Publication Date: | 06/1985 | |
| Category: | Space Radiation | |
| Origin: | STI | |
| NASA/STI Keywords: | ANISOTROPY, BACKGROUND RADIATION, COSMOLOGY, DENSITY DISTRIBUTION, RELIC RADIATION, GALACTIC CLUSTERS, MICROWAVES, MISSING MASS (ASTROPHYSICS), VELOCITY DISTRIBUTION | |
| DOI: | 10.1086/184479 | |
| Bibliographic Code: | 1985ApJ…293L…1V |
Abstract
The large-scale peculiar velocity field and the large- and intermediate-angular scale anisotropy of the cosmic microwave background are studied in inflationary cosmological models of critical density and containing primordial scale-invariant adiabatic density perturbations. Comparison with recent observations by de Vaucouleurs and Peters provides tentative support for a cold dark matter scenario in which the dark matter is not appreciably less clustered than the luminous galaxy distribution.
Abstract
We present the statistical properties of the Cold Clump Catalogue of Planck Objects (C3PO), the first all-sky catalogue of cold objects, in terms of their spatial distribution, dust temperature, distance, mass, and morphology. We have combined Planck and IRAS data to extract 10342 cold sources that stand out against a warmer environment. The sources are distributed over the whole sky, including in the Galactic plane, despite the confusion, and up to high latitudes (>30°). We find a strong spatial correlation of these sources with ancillary data tracing Galactic molecular structures and infrared dark clouds where the latter have been catalogued. These cold clumps are not isolated but clustered in groups. Dust temperature and emissivity spectral index values are derived from their spectral energy distributions using both Planck and IRAS data. The temperatures range from 7K to 19K, with a distribution peaking around 13K. The data are inconsistent with a constant value of the associated spectral index β over the whole temperature range: β varies from 1.4 to 2.8, with a mean value around 2.1. Distances are obtained for approximately one third of the objects. Most of the detections lie within 2kpc of the Sun, but more distant sources are also detected, out to 7kpc. The mass estimates inferred from dust emission range from 0.4 Msun to 2.4 × 105 Msun. Their physical properties show that these cold sources trace a broad range of objects, from low-mass dense cores to giant molecular clouds, hence the “cold clump” terminology. This first statistical analysis of the C3PO reveals at least two colder populations of special interest with temperatures in the range 7 to 12K: cores that mostly lie close to the Sun; and massive cold clumps located in the inner Galaxy. We also describe the statistics of the early cold core (ECC) sample that is a subset of the C3PO, containing only the 915 most reliable detections. The ECC is delivered as a part of the Planck Early Release Compact Source Catalogue (ERCSC).
Corresponding author: L. Montier, e-mail: Ludovic.Montier@irap.omp.eu
Abstract
The all-sky coverage of the Planck Early Release Compact Source Catalogue (ERCSC) provides an unsurpassed survey of galaxies at submillimetre (submm) wavelengths, representing a major improvement in the numbers of galaxies detected, as well as the range of far-IR/submm wavelengths over which they have been observed. We here present the first results on the properties of nearby galaxies using these data. We match the ERCSC catalogue to IRAS-detected galaxies in the Imperial IRAS Faint Source Redshift Catalogue (IIFSCz), so that we can measure the spectral energy distributions (SEDs) of these objects from 60 to 850μm. This produces a list of 1717 galaxies with reliable associations between Planck and IRAS, from which we select a subset of 468 for SED studies, namely those with strong detections in the three highest frequency Planck bands and no evidence of cirrus contamination. The SEDs are fitted using parametric dust models to determine the range of dust temperatures and emissivities. We find evidence for colder dust than has previously been found in external galaxies, with T < 20K. Such cold temperatures are found using both the standard single temperature dust model with variable emissivity β, or a two dust temperature model with β fixed at 2. We also compare our results to studies of distant submm galaxies (SMGs) which have been claimed to contain cooler dust than their local counterparts. We find that including our sample of 468 galaxies significantly reduces the distinction between the two populations. Fits to SEDs of selected objects using more sophisticated templates derived from radiative transfer models confirm the presence of the colder dust found through parametric fitting. We thus conclude that cold (T < 20K) dust is a significant and largely unexplored component of many nearby galaxies.
Corresponding author: D. L. Clements, e-mail: d.clements@imperial.ac.uk
Abstract
Planck has observed the entire sky from 30 GHz to 857GHz. The observed foreground emission contains contributions from different phases of the interstellar medium (ISM). We have separated the observed Galactic emission into the different gaseous components (atomic, molecular and ionised) in each of a number of Galactocentric rings. This technique provides the necessary information to study dust properties (emissivity, temperature, etc.), as well as other emission mechanisms as a function of Galactic radius. Templates are created for various Galactocentric radii using velocity information from atomic (neutral hydrogen) and molecular (12CO) observations. The ionised template is assumed to be traced by free-free emission as observed by WMAP, while 408 MHz emission is used to trace the synchrotron component. Gas emission not traced by the above templates, namely “dark gas”, as evidenced using Planck data, is included as an additional template, the first time such a component has been used in this way. These templates are then correlated with each of the Planck frequency bands, as well as with higher frequency data from IRAS and DIRBE along with radio data at 1.4 GHz. The emission per column density of the gas templates allows us to create distinct spectral energy distributions (SEDs) per Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to 25 THz (12μm). The resulting SEDs allow us to explore the contribution of various emission mechanisms to the Planck signal. Apart from the thermal dust and free-free emission, we have probed the Galaxy for anomalous (e.g., spinning) dust as well as synchrotron emission. We find the dust opacity in the solar neighbourhood, Ï„/NH = 0.92 ± 0.05 × 10-25 cm2at 250 μm, with no significant variation with Galactic radius, even though the dust temperature is seen to vary from over 25 K to under 14 K. Furthermore, we show that anomalous dust emission is present in the atomic, molecular and dark gas phases throughout the Galactic disk. Anomalous emission is not clearly detected in the ionised phase, as free-free emission is seen to dominate. The derived dust propeties associated with the dark gas phase are derived but do not allow us to reveal the nature of this phase. For all environments, the anomalous emission is consistent with rotation from polycyclic aromatic hydrocarbons (PAHs) and, according to our simple model, accounts for (25 ± 5)% (statistical) of the total emission at 30 GHz.
Corresponding author: D. J. Marshall, e-mail: douglas.marshall@irap.omp.eu
| Title: | Planck early results. V. The Low Frequency Instrument data processing | |
| Authors: | Zacchei, A.; Maino, D.; Baccigalupi, C.; Bersanelli, M.; Bonaldi, A.; Bonavera, L.; Burigana, C.; Butler, R. C.; Cuttaia, F.; de Zotti, G.; Dick, J.; Frailis, M.; Galeotta, S.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Keihänen, E.; Keskitalo, R.; Knoche, J.; Kurki-Suonio, H.; Lawrence, C. R.; Leach, S.; Leahy, J. P.; López-Caniego, M.; Mandolesi, N.; Maris, M.; Matthai, F.; Meinhold, P. R.; Mennella, A.; Morgante, G.; Morisset, N.; Natoli, P.; Pasian, F.; Perrotta, F.; Polenta, G.; Poutanen, T.; Reinecke, M.; Ricciardi, S.; Rohlfs, R.; Sandri, M.; Suur-Uski, A.-S.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Tomasi, M.; Valiviita, J.; Villa, F.; Zonca, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Bartolo, N.; Bedini, L.; Bennett, K.; Binko, P.; Borrill, J.; Bouchet, F. R.; Bremer, M.; Cabella, P.; Cappellini, B.; Chen, X.; Colombo, L.; Cruz, M.; Curto, A.; Danese, L.; Davies, R. D.; Davis, R. J.; de Gasperis, G.; de Rosa, A.; de Troia, G.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Dörl, U.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falvella, M. C.; Finelli, F.; Franceschi, E.; Gaier, T. C.; Gasparo, F.; Génova-Santos, R. T.; Giardino, G.; Gómez, F.; Gruppuso, A.; Hansen, F. K.; Hell, R.; Herranz, D.; Hovest, W.; Huynh, M.; Jewell, J.; Juvela, M.; Kisner, T. S.; Knox, L.; Lähteenmäki, A.; Lamarre, J.-M.; Leonardi, R.; León-Tavares, J.; Lilje, P. B.; Lubin, P. M.; Maggio, G.; Marinucci, D.; MartÃnez-González, E.; Massardi, M.; Matarrese, S.; Meharga, M. T.; Melchiorri, A.; Migliaccio, M.; Mitra, S.; Moss, A.; Nørgaard-Nielsen, H. U.; Pagano, L.; Paladini, R.; Paoletti, D.; Partridge, B.; Pearson, D.; Pettorino, V.; Pietrobon, D.; Prézeau, G.; Procopio, P.; Puget, J.-L.; Quercellini, C.; Rachen, J. P.; Rebolo, R.; Robbers, G.; Rocha, G.; Rubiño-MartÃn, J. A.; Salerno, E.; Savelainen, M.; Scott, D.; Seiffert, M. D.; Silk, J. I.; Smoot, G. F.; Sternberg, J.; Stivoli, F.; Stompor, R.; Tofani, G.; Toffolatti, L.; Tuovinen, J.; Türler, M.; Umana, G.; Vielva, P.; Vittorio, N.; Vuerli, C.; Wade, L. A.; Watson, R.; White, S. D. M.; Wilkinson, A. | |
| Affiliation: | AA(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AB(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy; INAF/IASF Milano, via E. Bassini 15, Milano, Italy), AC(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AD(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy; INAF/IASF Milano, via E. Bassini 15, Milano, Italy), AE(INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy), AF(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy; Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW, 1710, Australia), AG(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), AH(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), AI(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), AJ(INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy; SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AK(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AL(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AM(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), AN(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AO(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478, Warszawa, Poland), AP(Dipartimento di Fisica, Università degli Studi di Trieste, via A. Valerio 2, Trieste, Italy), AQ(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland), AR(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland), AS(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), AT(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland; Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland), AU(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), AV(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AW(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), AX(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), AY(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), AZ(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), BA(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), BB(Department of Physics, University of California, Santa Barbara, California, USA), BC(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy; INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), BD(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BE(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), BF(Dipartimento di Fisica, Università di Ferrara, via Saragat 1, 44122, Ferrara, Italy; Agenzia Spaziale Italiana Science Data Center, c/o ESRIN, via Galileo Galilei, Frascati, Italy; INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BG(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), BH(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), BI(Agenzia Spaziale Italiana Science Data Center, c/o ESRIN, via Galileo Galilei, Frascati, Italy; INAF – Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy), BJ(Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland; Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland; Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540, Kylmälä, Finland), BK(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), BL(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BM(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), BN(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BO(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland; Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland), BP(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), BQ(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), BR(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BS(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano, Italy; INAF/IASF Milano, via E. Bassini 15, Milano, Italy), BT(Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway), BU(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), BV(Department of Physics, University of California, Santa Barbara, California, USA), BW(Université de Toulouse, UPS-OMP, IRAP, 31028, Toulouse Cedex 4, France; CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028, Toulouse Cedex 4, France; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), BX(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), BY(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), BZ(Dipartimento di Fisica G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131, Padova, Italy), CA(CNR – ISTI, Area della Ricerca, via G. Moruzzi 1, Pisa, Italy), CB(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), CC(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), CD(Lawrence Berkeley National Laboratory, Berkeley, California, USA; Space Sciences Laboratory, University of California, Berkeley, California, USA), CE(Institut d’Astrophysique de Paris, CNRS UMR7095, Université Pierre & Marie Curie, 98 bis boulevard Arago, Paris, France), CF(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), CG(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), CH(INAF/IASF Milano, via E. Bassini 15, Milano, Italy), CI(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, 91125, USA), CJ(Department of Physics and Astronomy, University of Southern California, Los Angeles, California, USA; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), CK(Departamento de Matemáticas, EstadÃstica y Computación, Universidad de Cantabria, Avda. de los Castros s/n, Santander, Spain), CL(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), CM(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), CN(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), CO(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), CP(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), CQ(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), CR(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), CS(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), CT(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), CU(INAF/IASF Milano, via E. Bassini 15, Milano, Italy; Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway), CV(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), CW(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK), CX(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), CY(Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway), CZ(Agenzia Spaziale Italiana, Viale Liegi 26, Roma, Italy), DA(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), DB(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), DC(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), DD(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), DE(Instituto de AstrofÃsica de Canarias, C/VÃa Láctea s/n, La Laguna, Tenerife, Spain; Dpto. AstrofÃsica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain), DF(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), DG(Instituto de AstrofÃsica de Canarias, C/VÃa Láctea s/n, La Laguna, Tenerife, Spain), DH(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), DI(Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway), DJ(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), DK(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), DL(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), DM(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, 91125, USA), DN(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), DO(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland), DP(Lawrence Berkeley National Laboratory, Berkeley, California, USA), DQ(Department of Physics, University of California, One Shields Avenue, Davis, California, USA), DR(Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540, Kylmälä, Finland; Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland), DS(LERMA, CNRS, Observatoire de Paris, 61 Avenue de l’Observatoire, Paris, France), DT(European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain; European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands; Department of Physics, University of California, Santa Barbara, California, USA), DU(Aalto University Metsähovi Radio Observatory, Metsähovintie 114, 02540, Kylmälä, Finland), DV(Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway; Centre of Mathematics for Applications, University of Oslo, Blindern, Oslo, Norway), DW(Department of Physics, University of California, Santa Barbara, California, USA), DX(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), DY(Dipartimento di Matematica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), DZ(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), EA(INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy), EB(Dipartimento di Fisica G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131, Padova, Italy), EC(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), ED(Dipartimento di Fisica, Università La Sapienza, P. le A. Moro 2, Roma, Italy), EE(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), EF(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EG(Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), EH(DTU Space, National Space Institute, Juliane Mariesvej 30, Copenhagen, Denmark), EI(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EJ(Spitzer Science Center, 1200 E. California Blvd., Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), EK(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), EL(Haverford College Astronomy Department, 370 Lancaster Avenue, Haverford, Pennsylvania, USA), EM(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EN(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), EO(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EP(California Institute of Technology, Pasadena, California, USA; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), EQ(INAF/IASF Bologna, via Gobetti , 101, Bologna, Italy), ER(Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France), ES(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), ET(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), EU(Instituto de AstrofÃsica de Canarias, C/VÃa Láctea s/n, La Laguna, Tenerife, Spain; Dpto. AstrofÃsica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain), EV(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), EW(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), EX(Instituto de AstrofÃsica de Canarias, C/VÃa Láctea s/n, La Laguna, Tenerife, Spain; Dpto. AstrofÃsica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain), EY(CNR – ISTI, Area della Ricerca, via G. Moruzzi 1, Pisa, Italy), EZ(Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland; Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland), FA(Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada), FB(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), FC(Department of Physics, University of Oxford, 1 Keble Road, Oxford, UK), FD(Department of Physics, University of California, Berkeley, California, USA; Lawrence Berkeley National Laboratory, Berkeley, California, USA; Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), FE(European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ, Noordwijk, The Netherlands), FF(INRIA, Laboratoire de Recherche en Informatique, Université Paris-Sud 11, Bâtiment 490, 91405, Orsay Cedex, France), FG(Astroparticule et Cosmologie, CNRS (UMR7164), Université Denis Diderot Paris 7, Bâtiment Condorcet, 10 rue A. Domon et Léonie Duquet, Paris, France), FH(INAF – Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, Firenze, Italy), FI(Departamento de FÃsica, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo, Spain), FJ(MilliLab, VTT Technical Research Centre of Finland, Tietotie 3, Espoo, Finland), FK(ISDC Data Centre for Astrophysics, University of Geneva, ch. d’Ecogia 16, Versoix, Switzerland), FL(INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, Catania, Italy), FM(Instituto de FÃsica de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, Santander, Spain), FN(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy), FO(INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), FP(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), FQ(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), FR(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), FS(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK) | |
| Publication: | Astronomy & Astrophysics, Volume 536, id.A5 (A&A Homepage) | |
| Publication Date: | 12/2011 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | methods: data analysis, cosmic background radiation, cosmology: observations, surveys | |
| DOI: | 10.1051/0004-6361/201116484 | |
| Bibliographic Code: | 2011A&A…536A…5Z |
Abstract
We describe the processing of data from the Low Frequency Instrument (LFI) used in production of the Planck Early Release Compact Source Catalogue (ERCSC). In particular, we discuss the steps involved in reducing the data from telemetry packets to cleaned, calibrated, time-ordered data (TOD) and frequency maps. Data are continuously calibrated using the modulation of the temperature of the cosmic microwave background radiation induced by the motion of the spacecraft. Noise properties are estimated from TOD from which the sky signal has been removed using a generalized least square map-making algorithm. Measured 1/f noise knee-frequencies range from ~100 mHz at 30 GHz to a few tens of mHz at 70GHz. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices required to compute statistical uncertainties on LFI and Planck products are also produced. Main beams are estimated down to the ≈-10dB level using Jupiter transits, which are also used for geometrical calibration of the focal plane.
Corresponding author: A. Zacchei, e-mail: zacchei@oats.inaf.it
| Title: | Search for Non-Gaussian Signals in the BOOMERANG Maps: Pixel-Space Analysis | |
| Authors: | Polenta, G.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; De Troia, G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Jaffe, A. H.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Prunet, S.; Romeo, G.; Ruhl, J. E.; Vittorio, N.; Zeppilli, A. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AB(Queen Mary and Westfield College, Mile End Road, London E1 4NS, UK.), AC(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109.), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada.), AE(National Energy Research Scientific Computing Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720.), AF(IROE-CNR, 64 Via Panciatichi, I-50127 Firenze, Italy.), AG(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada.), AH(Physics Department, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125.), AI(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AJ(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, I-00133 Roma, Italy.), AK(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AL(Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125.), AM(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AN(Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125.), AO(Physics Department, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125.), AP(Astrophysics Group, Blackett Laboratory, Imperial College, Prince Consort Road, London SW7 2BZ, UK.), AQ(Physics Department, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125.), AR(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AS(Department of Physics and Astronomy, University of Wales, Cardiff CF24 3YB, Wales, UK.), AT(Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford OX1 3RH, UK.), AU(Department of Physics, University of California at Santa Barbara, Broida Hall, Building 572, Santa Barbara, CA 93106-9530.), AV(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, I-00133 Roma, Italy.), AW(Department of Astronomy and Astrophysics, University of Toronto, 60 St. George Street, Room 1403, Toronto, ON M5S 3H8, Canada.), AX(IROE-CNR, 64 Via Panciatichi, I-50127 Firenze, Italy.), AY(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.), AZ(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada.), BA(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada.), BB(Istituto Nazionale di Geofisica e Vulcanologia, Via di Vigna Murata, 606, I-00143 Roma, Italy.), BC(Department of Physics, University of California at Santa Barbara, Broida Hall, Building 572, Santa Barbara, CA 93106-9530.), BD(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, I-00133 Roma, Italy.), BE(Dipartimento di Fisica, Università di Roma, “La Sapienza”, Piazzale Aldo Moro, 2, I-00185 Roma, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 572, Issue 1, pp. L27-L31. (ApJL Homepage) | |
| Publication Date: | 06/2002 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background | |
| DOI: | 10.1086/341484 | |
| Bibliographic Code: | 2002ApJ…572L..27P |
Abstract
We search the BOOMERANG (Balloon Observations Of Millimetric Extragalactic Radiation ANd Geophysics) maps of the anisotropy of the cosmic microwave background (CMB) for deviations from Gaussianity. In this Letter, we focus on analysis techniques in pixel space and compute skewness, kurtosis, and Minkowski functionals for the BOOMERANG maps and for Gaussian simulations of the CMB sky. We do not find any significant deviation from Gaussianity in the high galactic latitude section of the 150 GHz map. We do find deviations from Gaussianity at lower latitudes and at 410 GHz, and we ascribe them to Galactic dust contamination. Using non-Gaussian simulations of instrumental systematic effects, of foregrounds, and of sample non-Gaussian cosmological models, we set upper limits to the non-Gaussian component of the temperature field in the BOOMERANG maps. For fluctuations distributed as a 1 degree of freedom χ2 mixed to the main Gaussian component, our upper limits are in the few percentile range.
| Title: | Fast Spherical Harmonic Analysis: A Quick Algorithm for Generating and/or Inverting Full-Sky, High-Resolution Cosmic Microwave Background Anisotropy Maps | |
| Authors: | Muciaccia, P. F.; Natoli, P.; Vittorio, N. | |
| Publication: | Astrophysical Journal Letters v.488, p.L63 (ApJL Homepage) | |
| Publication Date: | 10/1997 | |
| Origin: | APJ | |
| DOI: | 10.1086/310921 | |
| Bibliographic Code: | 1997ApJ…488L..63M |
Abstract
We present a fast algorithm for generating full-sky, high-resolution (~5′) simulations of the cosmic microwave background anisotropy pattern. We also discuss the inverse problem, that of evaluating from such a map the full set of alm values and the spectral coefficients Cl . We show that using an equidistant cylindrical projection of the sky substantially speeds up the calculations. Thus, generating and/or inverting a full-sky, high-resolution map can be easily achieved with present-day computer technology.
Abstract
We present first results on PLCKG266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate isa bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02, and estimate the cluster mass to be M500 = (7.8 ± 0.8) × 1014 Msun. PLCKG266.6-27.3 is an exceptional system: its luminosity of LX [0.5-2.0 keV] = (1.4 ± 0.05) × 1045 erg s-1equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z ~ 1. Moreover, unlike the majority of high-redshift clusters, PLCKG266.6-27.3 appears to be highly relaxed. This observation confirms Planck’s capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function.
Corresponding author: M. Arnaud, monique.arnaud@cea.fr
| Title: | Primordial non-Gaussianity: local curvature method and statistical significance of constraints on fNL from WMAP data | |
| Authors: | Cabella, P.; Liguori, M.; Hansen, F. K.; Marinucci, D.; Matarrese, S.; Moscardini, L.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy), AB(Dipartimento di Fisica `Galileo Galilei’, Università di Padova and INFN, Via Marzolo 8, I-35131 Padova, Italy), AC(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy), AD(Dipartimento di Matematica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy), AE(Dipartimento di Fisica `Galileo Galilei’, Università di Padova and INFN, Via Marzolo 8, I-35131 Padova, Italy), AF(Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, I-40127 Bologna, Italy), AG(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy; INFN, Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 358, Issue 2, pp. 684-692. (MNRAS Homepage) | |
| Publication Date: | 04/2005 | |
| Origin: | MNRAS | |
| Astronomy Keywords: | methods: numerical, methods: statistical, cosmic microwave background, cosmology: observations, cosmology: theory | |
| DOI: | 10.1111/j.1365-2966.2005.08833.x | |
| Bibliographic Code: | 2005MNRAS.358..684C |
Abstract
We test the consistency of estimates of the non-linear coupling constant fNL using non-Gaussian cosmic microwave background (CMB) maps generated by the method described in the work of Liguori, Matarrese & Moscardini. This procedure to obtain non-Gaussian maps differs significantly from the method used in previous works on the estimation of fNL. Nevertheless, using spherical wavelets, we find results in very good agreement with Mukherjee & Wang, showing that the two ways of generating primordial non-Gaussian maps give equivalent results. Moreover, we introduce a new method for estimating the non-linear coupling constant from CMB observations by using the local curvature of the temperature fluctuation field. We present both Bayesian credible regions (assuming a flat prior) and proper (frequentist) confidence intervals on fNL, and discuss the relation between the two approaches. The Bayesian approach tends to yield lower error bars than the frequentist approach, suggesting that a careful analysis of the different interpretations is needed. Using this method, we estimate fNL=-10+270-260 at the 2σ level (Bayesian) and fNL=-10+310-270 (frequentist). Moreover, we find that the wavelet and the local curvature approaches, which provide similar error bars, yield approximately uncorrelated estimates of fNL and therefore, as advocated in the work of Cabella et al., the estimates may be combined to reduce the error bars. In this way, we obtain fNL=-5 +/- 85 and fNL=-5 +/- 175 at the 1σ and 2σ level respectively using the frequentist approach.
| Title: | Implications for Quintessence Models from MAXIMA-1 and BOOMERANG-98 | |
| Authors: | Balbi, A.; Baccigalupi, C.; Matarrese, S.; Perrotta, F.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università Tor Vergata, Roma, I-00133, Italy.), AB(International School for Advanced Studies, via Beirut 4, 34014 Trieste, Italy.), AC(Dipartimento di Fisica “Galileo Galilei”, Università di Padov; and Instituto Nazionale di Fisica Nucleare, Sezione di Padova, Via Marzolo 8, 35131 Padova, Italy; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85748 Garching bei München, Germany), AD(International School for Advanced Studies, via Beirut 4, 34014 Trieste, Italy.), AE(Dipartimento di Fisica, Università Tor Vergata, Roma, I-00133, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 547, Issue 2, pp. L89-L92. (ApJL Homepage) | |
| Publication Date: | 02/2001 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Observations, Cosmology: Theory, Equation of State | |
| DOI: | 10.1086/318904 | |
| Bibliographic Code: | 2001ApJ…547L..89B |
Abstract
Prompted by the recent MAXIMA-1 and BOOMERANG-98 measurements of the cosmic microwave background (CMB) anisotropy power spectrum and motivated by the results from the observation of high-redshift Type Ia supernovae, we investigate CMB anisotropies in quintessence models in order to characterize the nature of the dark energy today. We perform a Bayesian likelihood analysis, using the MAXIMA-1 and BOOMERANG-98 published band powers, in combination with the COBE/Differential Microwave Radiometer, to explore the space of quintessence parameters: the quintessence energy density Ωφ and equation of state wφ. We restrict our analysis to flat, scale-invariant, inflationary adiabatic models. We find that this simple class of inflationary models, with a quintessence component Ωφ<~0.7, -1<=wφ<~-0.5, is in good agreement with the data. Within the assumptions of our analysis, pure quintessence models seem to be slightly favored, although the simple cosmological constant scenario is consistent with the data.
Abstract
We perform a detailed investigation of sources from the Cold Cores Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability of the detections, validate the separation between warm and cold dust emission components, provide the first glimpse at the nature, internal morphology and physical characterictics of the Planck-detected sources. We focus on a sub-sample of ten sources from the C3PO list, selected to sample different environments, from high latitude cirrus to nearby (150pc) and remote (2kpc) molecular complexes. We present Planck surface brightness maps and derive the dust temperature, emissivity spectral index, and column densities of the fields. With the help of higher resolution Herschel and AKARI continuum observations and molecular line data, we investigate the morphology of the sources and the properties of the substructures at scales below the Planck beam size. The cold clumps detected by Planck are found to be located on large-scale filamentary (or cometary) structures that extend up to 20pc in the remote sources. The thickness of these filaments ranges between 0.3 and 3pc, for column densities NH2 ~ 0.1 to 1.6 × 1022 cm-2, and with linear mass density covering a broad range, between 15 and 400 Msun pc-1. The dust temperatures are low (between 10 and 15K) and the Planck cold clumps correspond to local minima of the line-of-sight averaged dust temperature in these fields. These low temperatures are confirmed when AKARI and Herschel data are added to the spectral energy distributions. Herschel data reveal a wealth of substructure within the Planck cold clumps. In all cases (except two sources harbouring young stellar objects), the substructures are found to be colder, with temperatures as low as 7K. Molecular line observations provide gas column densities which are consistent with those inferred from the dust. The linewidths are all supra-thermal, providing large virial linear mass densities in the range 10 to 300 Msun pc-1, comparable within factors of a few, to the gas linear mass densities. The analysis of this small set of cold clumps already probes a broad variety of structures in the C3PO sample, probably associated with different evolutionary stages, from cold and starless clumps, to young protostellar objects still embedded in their cold surrounding cloud. Because of the all-sky coverage and its sensitivity, Planck is able to detect and locate the coldest spots in massive elongated structures that may be the long-searched for progenitors of stellar clusters.
Appendix A is available in electronic form at http://www.aanda.orgCorresponding author: I. Ristorcelli, e-mail: isabelle.ristorcelli@irap.omp.eu
Abstract
The performance of the Planck instruments in space is enabled by their low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two detector technologies with widely different temperature and cooling needs. Active coolers could satisfy these needs; a helium cryostat, as used by previous cryogenic space missions (IRAS, COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided by three V-groove radiators and a large telescope baffle. The active coolers are a hydrogen sorption cooler (<20 K), a 4He Joule-Thomson cooler (4.7 K), and a 3He-4He dilution cooler (1.4 K and 0.1 K). The flight system was at ambient temperature at launch and cooled in space to operating conditions. The HFI bolometer plate reached 93 mK on 3 July 2009, 50 days after launch. The solar panel always faces the Sun, shadowing the rest of Planck, andoperates at a mean temperature of 384 K. At the other end of the spacecraft, the telescope baffle operates at 42.3 K and the telescope primary mirror operates at 35.9 K. The temperatures of key parts of the instruments are stabilized by both active and passive methods. Temperature fluctuations are driven by changes in the distance from the Sun, sorption cooler cycling and fluctuations in gas-liquid flow, and fluctuations in cosmic ray flux on the dilution and bolometer plates. These fluctuations do not compromise the science data.
Abstract
Planck’s all-sky surveys at 30-857 GHz provide an unprecedented opportunity to follow the radio spectra of a large sample of extragalactic sources to frequencies 2-20 times higher than allowed by past, large-area, ground-based surveys. We combine the results of the Planck Early Release Compact Source Catalog (ERCSC) with quasi-simultaneous ground-based observations as well as archival data at frequencies below or overlapping Planck frequency bands, to validate the astrometry and photometry of the ERCSC radio sources and study the spectral features shown in this new frequency window opened by Planck. The ERCSC source positions and flux density scales are found to be consistent with the ground-based observations. We present and discuss the spectral energy distributions of a sample of “extreme” radio sources, to illustrate the richness of the ERCSC for the study of extragalactic radio sources. Variability is found to play a role in the unusual spectral features of some of these sources.
Corresponding author: B. Partridge, e-mail: bpartrid@haverford.edu
| Title: | Intracluster Comptonization of the Cosmic Microwave Background: Mean Spectral Distortion and Cluster Number Counts | |
| Authors: | Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y.; Vittorio, N. | |
| Publication: | Astrophysical Journal v.479, p.1 (ApJ Homepage) | |
| Publication Date: | 04/1997 | |
| Origin: | APJ | |
| Astronomy Keywords: | COSMOLOGY: COSMIC MICROWAVE BACKGROUND, COSMOLOGY: OBSERVATIONS, GALAXIES: CLUSTERS: GENERAL, INSTRUMENTATION: DETECTORS | |
| DOI: | 10.1086/303845 | |
| Bibliographic Code: | 1997ApJ…479….1C |
Abstract
The mean sky-averaged Comptonization parameter, y bar , describing the scattering of the cosmic microwave background (CMB) by hot gas in clusters of galaxies, is calculated in an array of flat and open cosmological and dark matter models. The models are globally normalized to fit cluster X-ray data, and intracluster gas is assumed to have evolved in a manner consistent with current observations. We predict values of y bar lower than the COBE/FIRAS upper limit. The corresponding values of the overall optical thickness to Compton scattering are <~10-4 for relevant parameter values. Of more practical importance are number counts of clusters across which a net flux (with respect to the CMB) higher than some limiting value can be detected. Such number counts are specifically predicted for the COBRAS/SAMBA and BOOMERANG missions.
| Title: | Can a relic cosmological constant reconcile inflationary predictions with the observations? | |
| Authors: | Vittorio, N.; Silk, J. | |
| Affiliation: | AA(California, University, Berkeley, CA; Roma, Università , Rome, Italy), AB(California, University, Berkeley) | |
| Publication: | Astrophysical Journal, Part 2 – Letters to the Editor (ISSN 0004-637X), vol. 297, Oct. 1, 1985, p. L1-L4. (ApJL Homepage) | |
| Publication Date: | 10/1985 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | BARYONS, BIG BANG COSMOLOGY, MISSING MASS (ASTROPHYSICS), RELIC RADIATION, ANISOTROPY, BACKGROUND RADIATION, GLOBULAR CLUSTERS, MICROWAVES | |
| DOI: | 10.1086/184545 | |
| Bibliographic Code: | 1985ApJ…297L…1V |
Abstract
The small-scale anisotropy in pure baryonic universes, with and without a cosmological constant, is calculated. If we restrict ourselves to the inflationary requirement of a flat universe, pure baryonic models are not consistent with the present upper limits on the fine-scale anisotropy even if recourse is made to a cosmological constant Lambda = 1 – Omega0. However, a cold dark matter-dominated model may be consistent with the observations if (Omega0)(h) greater than or equal to 0.05 and Lambda = 1 – omega0. Such a scheme might reconcile the astronomical determinations of Omega0 with the inflationary prediction of a flat universe.
| Title: | The integrated bispectrum as a test of cosmic microwave background non-Gaussianity: detection power and limits on fNL with WMAP data | |
| Authors: | Cabella, P.; Hansen, F. K.; Liguori, M.; Marinucci, D.; Matarrese, S.; Moscardini, L.; Vittorio, N. | |
| Affiliation: | AA(Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH), AB(Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, Blindern, 0315 Oslo, Norway), AC(Particle Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500, USA; Dipartimento di Fisica `Galileo Galilei’, Università di Padova, Via Marzolo 8, I-35131 Padova, Italy; INFN, Sezione di Padova, Via Marzolo 8, I-35131 Padova, Italy), AD(Dipartimento di Matematica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy), AE(Dipartimento di Fisica `Galileo Galilei’, Università di Padova, Via Marzolo 8, I-35131 Padova, Italy; INFN, Sezione di Padova, Via Marzolo 8, I-35131 Padova, Italy), AF(Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, I-40127 Bologna, Italy), AG(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy; INFN, Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 369, Issue 1, pp. 819-824. (MNRAS Homepage) | |
| Publication Date: | 06/2006 | |
| Origin: | MNRAS | |
| Astronomy Keywords: | methods: numerical: methods: statistical: cosmic microwave background: cosmology: observations: cosmology: theory, methods: numerical, methods: statistical, cosmic microwave background, cosmology: observations, cosmology: theory | |
| DOI: | 10.1111/j.1365-2966.2006.10339.x | |
| Bibliographic Code: | 2006MNRAS.369..819C |
Abstract
We propose a fast and efficient bispectrum statistic for cosmic microwave background (CMB) temperature anisotropies to constrain the amplitude of the primordial non-Gaussian signal measured in terms of the non-linear coupling parameter fNL. We show how the method can achieve a remarkable computational advantage by focusing on subsets of the multipole configurations, where the non-Gaussian signal is more concentrated. The detection power of the test increases roughly linearly with the maximum multipole, as shown in the ideal case of an experiment without noise and gaps. The CPU-time scales as l3max instead of l5max for the full bispectrum, which for Planck resolution lmax ~ 3000 means an improvement in speed of a factor of 107 compared with the full bispectrum analysis with minor loss in precision. This approach is complementary to the fast method introduced by Komatsu, Spergel & Wandelt using a reconstruction of the primordial fluctuation field. We find that the introduction of a galactic cut partially destroys the optimality of the configuration, which will then need to be dealt with in the future. We find for an ideal experiment with lmax = 2000 that upper limits of fNL < 8 can be obtained at 1σ. For the case of the WMAP experiment, we would be able to put limits of |fNL| < 40 if no galactic cut were present. Using the real data with a galactic cut, we obtain an estimate of -80 < fNL < 80 and -160 < fNL < 160 at 1 and 2σ, respectively.
| Title: | Cosmic microwave background anisotropy induced by gas in clusters of galaxies | |
| Authors: | Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y.; Vittorio, N. | |
| Affiliation: | AA(Osservatorio Astronomico di Roma, Monteporzio, Italy), AB(Osservatorio Astronomico di Roma, Monteporzio, Italy), AC(Tel Aviv University, Tel Aviv, Israel), AD(Tel Aviv University, Tel Aviv, Israel) | |
| Publication: | Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 433, no. 2, p. 454-463 (ApJ Homepage) | |
| Publication Date: | 10/1994 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ANISOTROPY, ASTRONOMICAL MODELS, BACKGROUND RADIATION, COSMOLOGY, DARK MATTER, GALACTIC CLUSTERS, INTERSTELLAR GAS, MICROWAVES, RADIO ASTRONOMY, COMPTON EFFECT, COSMIC BACKGROUND EXPLORER SATELLITE, GALACTIC EVOLUTION, INFRARED SPECTROMETERS, RED SHIFT | |
| DOI: | 10.1086/174657 | |
| Bibliographic Code: | 1994ApJ…433..454C |
Abstract
The spectral change induced by Compton scattering of the cosmic microwave background (CMB) radiation off hot electron gas in clusters of galaxies is an important component of the anisotropy on arcminute scales. The level and spatial characteristics of this anisotropy are explored in detail in the context of flat cold (taking 0.8 and 1 for the index of the density fluctuation power spectrum) and mixed dark matter models. Properties of intracluster gas and its evolution are directly modeled based on X-ray measurements, with an implied decrease in the gas mass fraction with increasing redshift. Our calculations yield levels of rms temperature anisotropy, (delta T/T)rms, approximately = a few 10-6 for a wide range of angular scales and in the context of realistic models for the intracluster gas evolution and spatial distribution. This is the minimum level of anisotropy expected on sub-degree angular scales if the universe underwent a phase of late reheating.
| Title: | X-ray clusters and gravitiational instability theories | |
| Authors: | Colafrancesco, S.; Vittorio, N. | |
| Affiliation: | AA(Osservatorio Astronomico di Roma, Monteporzio, Italy), AB(Osservatorio Astronomico di Roma, Monteporzio, Italy) | |
| Publication: | Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 443-458 (ApJ Homepage) | |
| Publication Date: | 02/1994 | |
| Category: | Astronomy | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, BACKGROUND RADIATION, COSMOLOGY, DARK MATTER, GALACTIC CLUSTERS, GALACTIC EVOLUTION, GRAVITATION THEORY, MATHEMATICAL MODELS, MICROWAVE EMISSION, MISSING MASS (ASTROPHYSICS), X RAY ASTRONOMY, ANISOTROPY, HEAO 2, LUMINOSITY, LUMINOUS INTENSITY | |
| DOI: | 10.1086/173740 | |
| Bibliographic Code: | 1994ApJ…422..443C |
Abstract
We discuss the expected evolution of X-ray clusters of galaxies in different models for structure formation: these are cold dark matter, hybrid, and baryonic isocurvature models. We compare the theoretical predictions with the observed X-ray local luminosity function and with the counts obtained from the Extended Medium Sensitivity Survey (EMSS) of the HEAO 2 satellite. For properly comparing our predictions with the EMSS data we apply several corrections to the theoretical X-ray luminosities and fluxes. We find that the most effective correction comes from considering the finite size of the EMSS detection cell in the HEAO 2 Imaging Proportional Counter cluster images. The available X-ray data are extremely selective. The allow to reject baryonic isocurvature models, as well as hybrid models where hot dark matter provides approximately 30% of the critical density. The model which performs by far better than the others considered here is a low-density (Omega0 = 0.2, h = 0.75) vacuum-dominated cold dark matter model, with an initial scale-free density fluctuation spectrum. In all models, the brighter X-ray clusters are rare objects originating from the high peaks of the initial density field. This implies that optical galaxies are biased tracers of the mass density field, unless the cluster collapse occurs on timescales longer than those of the ideal pressureless sphere. We discuss our results in the light of the Cosmic Background Explorer Satellite – Differential Microwave Radiometer (COBE-DMR) detection of large scale anisotropy of the cosmic microwave background.
| Title: | ROMA: A map-making algorithm for polarised CMB data sets | |
| Authors: | de Gasperis, G.; Balbi, A.; Cabella, P.; Natoli, P.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy giancarlo.degasperis@roma2.infn.it), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; Sezione INFN Roma 2, via della Ricerca Scientifica 1, 00133, Roma, Italy), AC(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; Sezione INFN Roma 2, via della Ricerca Scientifica 1, 00133, Roma, Italy), AE(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; Sezione INFN Roma 2, via della Ricerca Scientifica 1, 00133, Roma, Italy) | |
| Publication: | Astronomy and Astrophysics, Volume 436, Issue 3, June IV 2005, pp.1159-1165 (A&A Homepage) | |
| Publication Date: | 06/2005 | |
| Origin: | EDP Sciences | |
| Astronomy Keywords: | cosmology: cosmic microwave background, methods: statistical, methods: data analysis | |
| DOI: | 10.1051/0004-6361:20042512 | |
| Bibliographic Code: | 2005A&A…436.1159D |
Abstract
We present ROMA, a parallel code to produce joint optimal
temperature and polarisation maps out of multidetector CMB
observations. ROMA is a fast, accurate, and robust implementation of
the iterative generalised least-squares approach to map-making. We
benchmark ROMA on realistic simulated data from the last
polarisation-sensitive flight of BOOMERanG.
| Title: | Microwave background anisotropy and decaying-particle models for a flat universe | |
| Authors: | Vittorio, N.; Silk, J. | |
| Affiliation: | AA(California, University, Berkeley, CA; Roma, Università , Rome, Italy), AB(California, University, Berkeley, CA) | |
| Publication: | Physical Review Letters (ISSN 0031-9007), vol. 54, May 20, 1985, p. 2269-2272. (PhRvL Homepage) | |
| Publication Date: | 05/1985 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ANISOTROPY, BACKGROUND RADIATION, BIG BANG COSMOLOGY, RELIC RADIATION, UNIVERSE, BARYONS, MASS DISTRIBUTION, MICROWAVE FREQUENCIES, MISSING MASS (ASTROPHYSICS), NEUTRINOS, RED SHIFT | |
| DOI: | 10.1103/PhysRevLett.54.2269 | |
| Bibliographic Code: | 1985PhRvL..54.2269V |
Abstract
The fine-scale anisotropy of the cosmic microwave background radiation, induced by primordial scale-invariant adiabatic density fluctuations, has been studied in flat cosmological models dominated by relativistic particles from the recent decay of a massive relic-particle species. The authors find that, if the relic-particle species consists of massive, unstable neutrinos, there is appreciable, and probably excessive, fine-scale anisotropy in the cosmic microwave background.
| Title: | Probing Dark Energy with the Cosmic Microwave Background: Projected Constraints from the Wilkinson Microwave Anisotropy Probe and Planck | |
| Authors: | Balbi, A.; Baccigalupi, C.; Perrotta, F.; Matarrese, S.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università Tor Vergata, and INFN, Sezione di Roma 2, Via della Ricerca Scientifica 1, I-00133 Rome, Italy balbi@roma2.infn.it vittorio@roma2.infn.it), AB(SISSA/ISAS, Via Beirut 4, I-34014 Trieste, Italy perrotta@sissa.it bacci@sissa.it), AC(SISSA/ISAS, Via Beirut 4, I-34014 Trieste, Italy perrotta@sissa.it bacci@sissa.it), AD(Dipartimento di Fisica “Galileo Galilei”, Università di Padova, and INFN, Sezione di Padova, Via Marzolo 8, I-35131 Padua, Italy matarrese@pd.infn.it), AE(Dipartimento di Fisica, Università Tor Vergata, and INFN, Sezione di Roma 2, Via della Ricerca Scientifica 1, I-00133 Rome, Italy balbi@roma2.infn.it vittorio@roma2.infn.it) | |
| Publication: | The Astrophysical Journal, Volume 588, Issue 1, pp. L5-L8. (ApJL Homepage) | |
| Publication Date: | 05/2003 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Observations, Cosmology: Theory, Equation of State | |
| DOI: | 10.1086/375360 | |
| Bibliographic Code: | 2003ApJ…588L…5B |
Abstract
We investigate the accuracy attainable by forthcoming space-based observations of the cosmic microwave background (CMB) temperature and polarization anisotropy in constraining the dark energy density parameter ΩQ and equation of state wQ=pQ/ÏQ. Despite degeneracies among parameters, it is possible for high-precision observations such as those from the Wilkinson Microwave Anisotropy Probe and Planck to provide interesting information on the nature of the dark energy. Furthermore, we show that imposing a flat universe constraint makes it possible to obtain tight limits in the space of dark energy parameters even from the CMB alone.
| Title: | Testing the isotropy of the cosmic microwave background – The ULISSE experiment | |
| Authors: | de Bernardis, P.; Masi, S.; Melchiorri, F.; Melchiorri, B.; Vittorio, N. | |
| Affiliation: | AA(Roma I, Università , Rome, Italy), AB(Roma I, Università , Rome, Italy), AC(Roma I, Università , Rome, Italy), AD(CNR, Istituto di Fisica dell’Atmosfera, Rome, Italy), AE(Roma II, Università , Rome, Italy) | |
| Publication: | Astrophysical Journal, Part 2 – Letters (ISSN 0004-637X), vol. 396, no. 2, Sept. 10, 1992, p. L57-L60. Research supported by MURST and CNR. (ApJL Homepage) | |
| Publication Date: | 09/1992 | |
| Category: | Space Radiation | |
| Origin: | STI | |
| NASA/STI Keywords: | BALLOON SOUNDING, COSMOLOGY, RADIATION DISTRIBUTION, RELIC RADIATION, ATMOSPHERIC EFFECTS, BACKGROUND RADIATION, BALLOON-BORNE INSTRUMENTS, BARYONS, DARK MATTER | |
| DOI: | 10.1086/186516 | |
| Bibliographic Code: | 1992ApJ…396L..57D |
Abstract
The balloon-borne experiment ULISSE, operating at millimetric wavelengths, set a very stringet upper limit to the differential (single-subtracted) cosmic microwave background anisotrophy at 6 deg: Delta-T is less than or approximately equal to 35 micro-K. This limit is obtained with a likelihood-ratio analysis; the size and power of the test are 5 and less than or equal to 80 percent, respectively. The implications of this upper bound for flat cold dark matter and open baryonic-dominated cosmologies are discussed.
| Title: | Foreground influence on primordial non-Gaussianity estimates: needlet analysis of WMAP 5-year data | |
| Authors: | Cabella, P.; Pietrobon, D.; Veneziani, M.; Balbi, A.; Crittenden, R.; de Gasperis, G.; Quercellini, C.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy), AB(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy; Institute of Cosmology and Gravitation, Dennis Sciama Building Burnaby Road Portsmouth, Portsmouth PO1 3FX), AC(Dipartimento di Fisica, Università di Roma `La Sapienza’, Rome, Italy), AD(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy; INFN Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1, 00133 Roma, Italy), AE(Institute of Cosmology and Gravitation, Dennis Sciama Building Burnaby Road Portsmouth, Portsmouth PO1 3FX), AF(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy), AG(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy), AH(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Rome, Italy; INFN Sezione di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1, 00133 Roma, Italy) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 2, pp. 961-968. (MNRAS Homepage) | |
| Publication Date: | 06/2010 | |
| Origin: | WILEY | |
| Astronomy Keywords: | methods: data analysis, cosmic background radiation, early Universe | |
| Abstract Copyright: | (c) Journal compilation © 2010 RAS | |
| DOI: | 10.1111/j.1365-2966.2010.16542.x | |
| Bibliographic Code: | 2010MNRAS.405..961C |
Abstract
We constrain the amplitude of primordial non-Gaussianity in the cosmic microwave background data taking into account the presence of foreground residuals in the maps. We generalize the needlet bispectrum estimator marginalizing over the amplitudes of thermal dust, free-free and synchrotron templates. We apply our procedure to Wilkinson Microwave Anisotropy Probe 5-year data, finding fNL = 38 +/- 47 (1σ), while the analysis without marginalization provides fNL = 35 +/- 42. Splitting the marginalization over each foreground separately, we found that the estimates of fNL are positively cross-correlated of 17 and 12 per cent with the dust and synchrotron, respectively, while a negative cross-correlation of about -10 per cent is found for the free-free component.
| Title: | Holes in cosmology | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Affiliation: | AA(Roma, Università , Rome; CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AB(Roma, Università , Rome; CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AC(Roma, Università , Rome; CNR, Istituto di Astrofisica Spaziale, Frascati, Italy) | |
| Publication: | Astronomy and Astrophysics, vol. 117, no. 2, Jan. 1983, p. 365-367. (A&A Homepage) | |
| Publication Date: | 01/1983 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, COSMOLOGY, GALACTIC CLUSTERS, GALACTIC EVOLUTION, HUBBLE CONSTANT, SPACE DENSITY, CONSERVATION LAWS, MASS DISTRIBUTION, PERTURBATION THEORY, RELATIVISTIC THEORY, SYMMETRY, UNIVERSE, VACUUM | |
| Bibliographic Code: | 1983A&A…117..365O |
Abstract
The fact that the three-dimensional structure of the Universe consists of holes surrounded by matter is explained in terms of hyperbolic energy inhomogeneities. No mass condensation arises and the hole results from the overall mass expulsion from the assumed center of spherical symmetry. Mass conservation leads to the formation of a higher density spherical shell at the boundary of the hole. A matter ridge forms around each hole and expands faster than the Hubble flow; the collision of two such ridges may lead to the formation of a Zel’dovich pancake. The simplifying assumptions of spherical symmetry and of an Einstein-de Sitter background are used in the analysis, which can easily be extended to a more general background. In the model, the depth and width of a hole as well as the shape of the ridge around it are shown to depend in a simple way on the parameters; this may be used to infer the nature of the initial perturbations.
| Title: | The formation of cavities around cosmological condensations | |
| Authors: | Occhionero, F.; Veccia-Scavalli, L.; Vittorio, N. | |
| Affiliation: | AA(CNR, Istituto di Astrofisica Spaziale, Frascati; Osservatorio Astronomico, Rome, Italy), AB(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AC(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy) | |
| Publication: | Astronomy and Astrophysics, vol. 97, no. 1, Apr. 1981, p. 169-174. (A&A Homepage) | |
| Publication Date: | 04/1981 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, BLACK HOLES (ASTRONOMY), COSMOLOGY, GALACTIC CLUSTERS, GALACTIC EVOLUTION, DENSITY DISTRIBUTION, HUBBLE CONSTANT, MASS DISTRIBUTION, PERTURBATION THEORY, RADIAL VELOCITY | |
| Comment: | A&AA ID. AAA029.162.031 | |
| Bibliographic Code: | 1981A&A….97..169O |
Abstract
Motivated by the observations which show the existence of large scale holes in the matter distribution in superclusters of galaxies, this paper studies the development of density gradients in initially uniform cosmological models due to the onset of energy perturbations in the Hubble flow. Spherical symmetry is assumed and the density profiles are described by means of Tolman models which asymptotically become uniform Friedmann-Robertson-Walker Universes. In previous work the formation of cavities around mass condensations originated by uniform, spherical energy perturbations was pointed out. Here it is shown that cavities do form also around more realistic continuous energy perturbations, which yield continuous density profiles. Thus an interesting initial condition for the development of cosmological condensations and the surrounding cavities consists of energy perturbations rather than density perturbations, of the Hubble flow.
| Title: | First results from the BOOMERanG experiment | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Pongetti, F.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AB(Department of Physics, Queen Mary and Westfield College, London, United Kingdom), AC(Jet Propulsion Laboratory, Pasadena, California), AD(CITA University of Toronto, Canada), AE(NERSC-LBNL, Berkeley, California; Center for Particle Astrophysics, University of California at Berkeley), AF(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy), AG(Department of Physics, University of California at Santa Barbara), AH(California Institute of Technology, Pasadena), AI(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AK(Department of Physics, University of California at Santa Barbara), AL(Astrophysics, University of Oxford, United Kingdom), AM(California Institute of Technology, Pasadena; Astrophysics, University of Oxford, United Kingdom), AN(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AO(California Institute of Technology, Pasadena), AP(California Institute of Technology, Pasadena), AQ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AR(Center for Particle Astrophysics, University of California at Berkeley), AS(California Institute of Technology, Pasadena), AT(ENEA Centro Ricerche di Frascati, Italy), AU(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AV(California Institute of Technology, Pasadena), AW(Physics and Astronomy Department, Cardiff University, United Kingdom), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy; Departments of Physics and Astronomy, University of Toronto, Canada), AZ(Department of Physics, University of California at Santa Barbara), BA(Departments of Physics and Astronomy, University of Toronto, Canada), BB(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy), BC(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BD(CITA University of Toronto, Canada), BE(Istituto Nazionale di Geofisica, Roma, Italy), BF(CITA University of Toronto, Canada), BG(Istituto Nazionale di Geofisica, Roma, Italy), BH(Istituto Nazionale di Geofisica, Roma, Italy), BI(Department of Physics, University of California at Santa Barbara), BJ(ENEA Centro Ricerche di Frascati, Italy), BK(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BL(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy) | |
| Publication: | Cosmology and Particle Physics: CAPP 2000. AIP Conference Proceedings, Volume 555, pp. 85-94 (2001). (AIPC Homepage) | |
| Publication Date: | 02/2001 | |
| Origin: | AIP | |
| PACS Keywords: | Background radiations, Observational cosmology, Radio, microwave | |
| DOI: | 10.1063/1.1363510 | |
| Bibliographic Code: | 2001AIPC..555…85D |
Abstract
We report the first results from the BOOMERanG experiment, which mapped at 90, 150, 240 and 410 GHz a wide (3%) region of the microwave sky with minimal local contamination. From the data of the best 150 GHz detector we find evidence for a well defined peak in the power spectrum of temperature fluctuations of the Cosmic Microwave Background, localized at =197+/-6, with an amplitude of (68+/-8)μKCMB. The location, width and amplitude of the peak is suggestive of acoustic oscillations in the primeval plasma. In the framework of inflationary adiabatic cosmological models the measured spectrum allows a Bayesian estimate of the curvature of the Universe and of other cosmological parameters. With reasonable priors we find Ω=(1.07+/-0.06) and ns=(1.00+/-0.08) (68%C.L.) in excellent agreement with the expectations from the simplest inflationary theories. We also discuss the limits on the density of baryons, of cold dark matter and on the cosmological constant. .
| Title: | Dynamical Models for Clusters of Galaxies | |
| Authors: | Occhionero, F.; Vignato, A.; Vittorio, N. | |
| Publication: | Astronomy and Astrophysics, Vol. 70, p. 265 (1978) (A&A Homepage) | |
| Publication Date: | 11/1978 | |
| Origin: | ADS | |
| Comment: | A&AA ID. AAA022.160.023 | |
| Bibliographic Code: | 1978A&A….70..265O |
Abstract
| Title: | BOOMERanG constraints on primordial non-Gaussianity from analytical Minkowski functionals | |
| Authors: | Natoli, P.; de Troia, G.; Hikage, C.; Komatsu, E.; Migliaccio, M.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; di Stefano, G.; Hivon, E.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Polenta, G.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy; INFN, Sezione di Tor Vergata, Via della Ricerca Scientifica 1, I-00133 Roma, Italy), AB(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AC(Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA; School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA), AD(Texas Cosmology Center, University of Texas at Austin, 1 University Station, C1400, Austin, TX 78712, USA), AE(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AF(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA), AG(Jet Propulsion Laboratory, Pasadena, CA 91109-8099, USA), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St George Street, Toronto, Ontario M5S 3H8, Canada), AI(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA; Space Sciences Laboratory, UC Berkeley, CA 94720, USA), AJ(IFAC-CNR, I-50127 Firenze, Italy), AK(Theoretical Physics Group, Imperial College, London SW7 2BZ), AL(Jet Propulsion Laboratory, Pasadena, CA 91109-8099, USA), AM(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy), AN(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AO(Department of Physics, MIT, Cambridge, MA 02139, USA), AP(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), AQ(Institut d’Astrophysique, Paris 75014, France), AR(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA; Space Sciences Laboratory, UC Berkeley, CA 94720, USA), AS(Department of Physics, Princeton University, Princeton, NJ 08544, USA), AT(Observational Cosmology, California Institute of Technology, Pasadena, CA 91125, USA), AU(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy), AV(School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA), AW(Astrophysics Group, Imperial College, London SW7 2BZ), AX(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy; INFN, Sezione di Roma 1, I-00185 Roma, Italy), AY(Physics Department, Case Western Reserve University, Cleveland, OH 44106, USA), AZ(Physics Department, University of Toronto, Toronto, Ontario M5S 3H8, Canada), BA(Physics Department, University of Toronto, Toronto, Ontario M5S 3H8, Canada), BB(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy), BC(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF – Osservatorio Astronomico di Roma, I-00040 Monte Porzio Catone, Italy), BD(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA; Space Sciences Laboratory, UC Berkeley, CA 94720, USA), BE(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), BF(Physics Department, Case Western Reserve University, Cleveland, OH 44106, USA), BG(Department of Physics, MIT, Cambridge, MA 02139, USA), BH(Dipartimento di Fisica, Università La Sapienza, I-00185 Roma, Italy), BI(Dipartimento di Fisica, Università di Roma `Tor Vergata’, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy) | |
| Publication: | Monthly Notices of the Royal Astronomical Society, Volume 408, Issue 3, pp. 1658-1665. (MNRAS Homepage) | |
| Publication Date: | 11/2010 | |
| Origin: | WILEY | |
| Astronomy Keywords: | methods: analytical, methods: statistical, early Universe, cosmic background radiation, cosmology: observations | |
| Abstract Copyright: | (c) Journal compilation © 2010 RAS | |
| DOI: | 10.1111/j.1365-2966.2010.17228.x | |
| Bibliographic Code: | 2010MNRAS.408.1658N |
Abstract
We use Minkowski functionals (MFs) to constrain a primordial non-Gaussian contribution to the cosmic microwave background intensity field as observed in the 150- and 145-GHz BOOMERanG maps from the 1998 and 2003 flights, respectively, performing for the first time a joint analysis of the two data sets. A perturbative expansion of the MF formulae in the limit of a weakly non-Gaussian field yields analytical formulae, derived by Hikage et al., which can be used to constrain the coupling parameter fNL without the need for non-Gaussian simulations. We find -770 < fNL < 500 at 95 per cent CL, significantly improving the previous constraints by De Troia et al. on the BOOMERanG 2003 data set. These are the best fNL limits to date for suborbital probes.
| Title: | Searching for Non-Gaussian Signals in the BOOMERANG 2003 CMB Maps | |
| Authors: | De Troia, G.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; Di Stefano, G.; Ferreira, P. G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Kunz, M.; Jones, W. C.; Lange, A. E.; Liguori, M.; Masi, S.; Matarrese, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy; Dipartimento di Fisica, Università La Sapienza, Roma, Italy.), AB(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AC(Jet Propulsion Laboratory, Pasadena, CA; Observational Cosmology, California Institute of Technology, Pasadena, CA.), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada.), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA; Space Sciences Laboratory, University of California, Berkeley, CA.), AF(IFAC-CNR, Firenze, Italy.), AG(Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK.), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada; Theoretical Physics Group, Imperial College, London, UK.), AI(IPAC, California Institute of Technology, Pasadena, CA.), AJ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy.), AK(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy.), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA.), AM(Istituto Nazionale di Geofisicae Vulcanologia, Roma, Italy.), AN(Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK.), AO(Institut d’Astrophysique, Paris, France), AP(Theoretical Physics Group, Imperial College, London, UK.), AQ(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA; Space Sciences Laboratory, University of California, Berkeley, CA.), AR(Département de Physique Théorique, Université de Genève, Switzerland.), AS(Jet Propulsion Laboratory, Pasadena, CA; Observational Cosmology, California Institute of Technology, Pasadena, CA.), AT(Observational Cosmology, California Institute of Technology, Pasadena, CA.), AU(Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK.), AV(Dipartimento di Fisica, Università La Sapienza, Roma, Italy.), AW(Dipartimento di Fisica G. Galilei, Università di Padova and INFN, Sezione di Padova, Italy.), AX(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK.), AY(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada.), AZ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy.), BA(Sierra Lobo, Inc., 11401 Hoover Road, Milan, OH 44846.), BB(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy; INFN, Sezione di Tor Vergata, Roma, Italy.), BC(Physics Department, University of Toronto, Toronto, ON.), BD(Physics Department, University of Toronto, Toronto, ON.), BE(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; European Space Astronomy Centre (ESAC), European Space Agency, Madrid, Spain.), BF(Department of Physics, University of Alberta, Edmonton, AB, Canada.), BG(Dipartimento di Fisica, Università La Sapienza, Roma, Italy.), BH(Institut d’Astrophysique, Paris, France), BI(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; INAF-Osservatorio Astronomico di Padova, Italy.), BJ(Istituto Nazionale di Geofisicae Vulcanologia, Roma, Italy.), BK(Physics Department, Case Western Reserve University, Cleveland, OH.), BL(Dipartimento di Fisica, Università La Sapienza, Roma, Italy.), BM(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA.), BN(Dipartimento di Fisica, Università La Sapienza, Roma, Italy; APC, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France), BO(Dipartimento di Fisica, Università Tor Vergata, Roma, Italy; INFN, Sezione di Tor Vergata, Roma, Italy.) | |
| Publication: | The Astrophysical Journal, Volume 670, Issue 2, pp. L73-L76. (ApJL Homepage) | |
| Publication Date: | 12/2007 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background | |
| DOI: | 10.1086/524402 | |
| Bibliographic Code: | 2007ApJ…670L..73D |
Abstract
We analyze the BOOMERANG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non-Gaussian, primordial contribution to CMB fluctuations. We perform a pixel-space analysis restricted to a portion of the map chosen in view of high-sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high-quality simulated data, including non-Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERANG data for the nonlinear coupling parameter fNL as -300<fNL<650 at 68% CL and -800<fNL<1050 at 95% CL.
| Title: | Unbiased estimation of an angular power spectrum | |
| Authors: | Polenta, G.; Marinucci, D.; Balbi, A.; de Bernardis, P.; Hivon, E.; Masi, S.; Natoli, P.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma ‘La Sapienza’, Italy), AB(Dipartimento di Matematica, Università di Roma ‘Tor Vergata’, Italy), AC(Dipartimento di Fisica, Università di Roma ‘Tor Vergata’, Italy), AD(Dipartimento di Fisica, Università di Roma ‘La Sapienza’, Italy), AE(IPAC, California Institute of Technology, USA), AF(Dipartimento di Fisica, Università di Roma ‘La Sapienza’, Italy), AG(Dipartimento di Fisica, Università di Roma ‘Tor Vergata’, Italy), AH(Dipartimento di Fisica, Università di Roma ‘Tor Vergata’, Italy) | |
| Publication: | Journal of Cosmology and Astroparticle Physics, Issue 11, id. 001 (2005). (JCAP Homepage) | |
| Publication Date: | 11/2005 | |
| Origin: | IOP | |
| DOI: | 10.1088/1475-7516/2005/11/001 | |
| Bibliographic Code: | 2005JCAP…11..001P |
Abstract
We discuss the derivation of the analytic properties of the cross-power spectrum estimator from multi-detector CMB anisotropy maps. The method is computationally convenient and it provides unbiased estimates under very broad assumptions. We also propose a new procedure for testing for the presence of residual bias due to inappropriate noise subtraction in pseudo-C_{\ell } estimates. We derive the analytic behaviour of this procedure under the null hypothesis, and use Monte Carlo simulations to investigate its efficiency properties, which appear very promising. For instance, for full sky maps with isotropic white noise, the test is able to identify an error of 1% on the noise amplitude estimate.
| Title: | Foreground Contributions to 0.2-2° CMB Anisotropies | |
| Authors: | Toffolatti, L.; Danese, L.; Franceschini, A.; Mandolesi, N.; Smoot, G. F.; Bersanelli, M.; Vittorio, N.; Lasenby, A.; Partridge, R. B.; Davies, R.; Sironi, G.; Cesarsky, C.; Lachieze-Rey, M.; Martinez-Gonzalez, E.; Beckman, J.; Rebolo, R.; Sáez, D.; de Bernardis, P.; dall’Oglio, G.; Crane, P.; Janssen, M.; Puget, J. L.; Bussoletti, E.; Raffelt, G.; Encrenaz, P.; Natale, V.; Tofani, G.; Merluzzi, P.; Scaramella, R.; Efstathiou, G. | |
| Affiliation: | AA(Osservatorio Astronomico di Padova, Padova, Italy), AB(Osservatorio Astronomico di Padova, Padova, Italy), AC(Osservatorio Astronomico di Padova, Padova, Italy), AD(Osservatorio Astronomico di Padova, Padova, Italy), AE(Osservatorio Astronomico di Padova, Padova, Italy), AF(Osservatorio Astronomico di Padova, Padova, Italy), AG(Osservatorio Astronomico di Padova, Padova, Italy), AH(Osservatorio Astronomico di Padova, Padova, Italy), AI(Osservatorio Astronomico di Padova, Padova, Italy), AJ(Osservatorio Astronomico di Padova, Padova, Italy), AK(Osservatorio Astronomico di Padova, Padova, Italy), AL(Osservatorio Astronomico di Padova, Padova, Italy), AM(Osservatorio Astronomico di Padova, Padova, Italy), AN(Osservatorio Astronomico di Padova, Padova, Italy), AO(Osservatorio Astronomico di Padova, Padova, Italy), AP(Osservatorio Astronomico di Padova, Padova, Italy), AQ(Osservatorio Astronomico di Padova, Padova, Italy), AR(Osservatorio Astronomico di Padova, Padova, Italy), AS(Osservatorio Astronomico di Padova, Padova, Italy), AT(Osservatorio Astronomico di Padova, Padova, Italy), AU(Osservatorio Astronomico di Padova, Padova, Italy), AV(Osservatorio Astronomico di Padova, Padova, Italy), AW(Osservatorio Astronomico di Padova, Padova, Italy), AX(Osservatorio Astronomico di Padova, Padova, Italy), AY(Osservatorio Astronomico di Padova, Padova, Italy), AZ(Osservatorio Astronomico di Padova, Padova, Italy), BA(Osservatorio Astronomico di Padova, Padova, Italy), BB(Osservatorio Astronomico di Padova, Padova, Italy), BC(Osservatorio Astronomico di Padova, Padova, Italy), BD(Osservatorio Astronomico di Padova, Padova, Italy) | |
| Publication: | Astrophysical Letters and Communications, Vol. 32, p.125 | |
| Publication Date: | 00/1995 | |
| Origin: | AUTHOR; ADS | |
| Keywords: | Cosmic background radiation: galaxy: general infrared: galaxies radio sources | |
| Bibliographic Code: | 1995ApL&C..32..125T |
Abstract
We examine the extent to which galactic and extragalactic foregrounds can hamper the detection of primordial Cosmic Microwave background (CMB) anisotropies. We limit our discussion to intermediate angular scales, 10′< theta < 2 deg, since many current as well as future experiments have been designed to map CMB anisotropies at these angular scales. In fact, scales of > 10′ are of crucial importance to test both the conditions in the early Universe and current theories of the gravitational collapse.
| Title: | Measuring CMB polarization with Boomerang | |
| Authors: | Montroy, T.; Ade, P. A. R.; Balbi, A.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Ganga, K.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C.; Melchiorri, A.; Nati, F.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Torbet, E.; Tegmark, M.; Vittorio, N. | |
| Affiliation: | AA(tom@cmb.phys.cwru.edu), AB(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK), AC(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AD(Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AE(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ont., Canada), AF(National Energy Research Scientific Computing Center, LBNL, Berkeley, CA, USA; Center for Particle Astrophysics, University of California, Berkeley, CA, USA), AG(IFAC-CNR, Firenze, Italy), AH(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AI(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ont., Canada), AJ(CSU Dominguez Hills, Carson, CA, USA), AK(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AL(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AM(Physics Department, University of Pennsylvania, Philadelphia, PA, USA), AN(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AO(Istituto Nazionale di Geofisica, Roma, Italy), AP(IPAC, California Institute of Technology, Pasadena, CA, USA), AQ(IPAC, California Institute of Technology, Pasadena, CA, USA), AR(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AS(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AT(Astrophysics Group, Imperial College, London, UK), AU(Physics Department, Case Western Reserve University, Cleveland, OH, USA; Department of Physics, University of California, Santa Barbara, CA, USA), AV(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AW(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK), AZ(Physics Department, University of Toronto, Toronto, Ont., Canada), BA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BB(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BC(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), BD(Physics Department, University of Toronto, Toronto, Ont., Canada), BE(Physics Department, University of Toronto, Toronto, Ont., Canada), BF(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BG(Physics Department, University of Alberta, Edmonton, Alta., Canada), BH(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BI(Institut d’Astrophysique, Paris, France), BJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BK(Istituto Nazionale di Geofisica, Roma, Italy), BL(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BM(Department of Physics, University of California, Santa Barbara, CA, USA), BN(Physics Department, University of Pennsylvania, Philadelphia, PA, USA), BO(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy) | |
| Publication: | New Astronomy Reviews, Volume 47, Issue 11-12, p. 1057-1065. (NewAR Homepage) | |
| Publication Date: | 12/2003 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.newar.2003.09.011 | |
| Bibliographic Code: | 2003NewAR..47.1057M |
Abstract
Boomerang is a balloon-borne telescope designed for long duration (LDB) flights around Antarctica. The second LDB flight of Boomerang took place in January 2003. The primary goal of this flight was to measure the polarization of the CMB. The receiver uses polarization sensitive bolometers at 145 GHz. Polarizing grids provide polarization sensitivity at 245 and 345 GHz. We describe the Boomerang telescope noting changes made for 2003 LDB flight, and discuss some of the issues involved in the measurement of polarization with bolometers. Lastly, we report on the 2003 flight and provide an estimate of the expected results.
| Title: | Polarization of the microwave background: theoretical framework. | |
| Authors: | Melchiorri, A.; Vittorio, N. | |
| Publication: | NATO Advanced Study Institute on the Cosmological Background Radiation, p. 419 – 440 | |
| Publication Date: | 00/1997 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Polarization, Cosmic Microwave Background: Dark Matter, Cosmic Microwave Background: Anisotropy | |
| Bibliographic Code: | 1997cbr..conf..419M |
Abstract
The authors present a brief review of the polarization properties of the cosmic microwave background in dark matter models for structure formation. Quite independently of the model parameters, the polarization level is expected to be ≡10% of the anisotropy signal at angular scales ≤1°. Detections of polarization at larger angular scales would provide strong evidence in favour of an early reionization of the intergalactic medium.
| Title: | Subdegree Sunyaev-Zel’dovich Signal from Multifrequency BOOMERANG Observations | |
| Authors: | Veneziani, M.; Amblard, A.; Cooray, A.; Piacentini, F.; Pietrobon, D.; Serra, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; DeGasperis, G.; de Oliveira-Costa, A.; DeTroia, G.; Di Stefano, G.; Ganga, K. M.; Hivon, E.; Jones, W. C.; Kisner, T. S.; Lange, A. E.; MacTavish, C. J.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Polenta, G.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Vittorio, N. | |
| Affiliation: | AA(Center for Cosmology, University of California, Irvine, CA 92697, USA; Dipartimento di Fisica, Università di Roma La Sapienza”, Rome, Italy; APC, Université Paris Diderot, 75013 Paris, France” marcella.veneziani@roma1.infn.it), AB(Center for Cosmology, University of California, Irvine, CA 92697, USA amblard@uci.edu), AC(Center for Cosmology, University of California, Irvine, CA 92697, USA), AD(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), AE(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Institute of Cosmology and Gravitation, University of Portsmouth, UK), AF(Center for Cosmology, University of California, Irvine, CA 92697, USA), AG(Department of Physics and Astronomy, Cardiff University, Cardiff, UK), AH(Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA), AI(CITA, University of Toronto, Toronto, ON M5S 3H8, Canada), AJ(Computational Research Division, LBNL, Berkeley, CA 94720, USA), AK(IFAC-CNR, 50127, Firenze, Italy), AL(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), AM(Theoretical Physics Group, Imperial College, London, UK), AN(Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA), AO(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), AP(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), AQ(Department of Physics, MIT, Cambridge, MA 02139, USA), AR(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), AS(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), AT(APC, Université Paris Diderot, 75013 Paris, France), AU(Institut d’Astrophysique de Paris, 75014 Paris, France), AV(Department of Physics, Princeton University, Princeton, NJ 08544, USA), AW(Case Western Reserve University, Cleveland, OH 44106, USA), AX(Jet Propulsion Laboratory, Pasadena, CA 91109, USA), AY(Astrophysics Group, Imperial College, London, UK), AZ(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BA(Department of Physics and Astronomy, Cardiff University, Cardiff, UK), BB(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BC(Case Western Reserve University, Cleveland, OH 44106, USA), BD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), BE(Physics Department, University of Toronto, Toronto ON, Canada), BF(Physics Department, University of Toronto, Toronto ON, Canada), BG(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF-Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy), BH(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Space Sciences Laboratory, UC Berkeley CA, USA), BI(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), BJ(Case Western Reserve University, Cleveland, OH 44106, USA), BK(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BL(Department of Physics, MIT, Cambridge, MA 02139, USA), BM(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy) | |
| Publication: | The Astrophysical Journal Letters, Volume 702, Issue 1, pp. L61-L65 (2009). (ApJL Homepage) | |
| Publication Date: | 09/2009 | |
| Origin: | IOP | |
| Astronomy Keywords: | cosmic microwave background, cosmological parameters, cosmology: observations, large-scale structure of universe | |
| DOI: | 10.1088/0004-637X/702/1/L61 | |
| Bibliographic Code: | 2009ApJ…702L..61V |
Abstract
The Sunyaev-Zel’dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB data sets. Using CMB anisotropies measured at three frequencies by the BOOMERANG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 μK (2σ) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERANG SZ data alone is σSZ 8 < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find σSZ 8 < 0.92 (95% c.l.).
| Title: | Non-iterative methods to estimate the in-flight noise properties of CMB detectors | |
| Authors: | Natoli, P.; Marinucci, D.; Cabella, P.; de Gasperis, G.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AB(Dipartimento di Studi Geoeconomici e Statistici, Università di Roma “La Sapienza”, via del Castro Laurenziano 9, 00161 Roma, Italy), AC(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AE(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy) | |
| Publication: | Astronomy and Astrophysics, v.383, p.1100-1112 (2002) (A&A Homepage) | |
| Publication Date: | 03/2002 | |
| Origin: | A&A | |
| Astronomy Keywords: | COSMOLOGY: COSMIC MICROWAVE BACKGROUND, METHODS: STATISTICAL, DATA ANALYSIS | |
| DOI: | 10.1051/0004-6361:20011788 | |
| Bibliographic Code: | 2002A&A…383.1100N |
Abstract
We present a new approach for statistical inference on noise properties of CMB anisotropy data. We consider a Maximum Likelihood parametric estimator to recover the full dependence structure of the noise process. We also consider a semiparametric procedure which is only sensitive to the low frequency behavior of the noise spectral density. Both approaches are statistically robust and computationally convenient in the case of long memory noise, even under nonstationary circumstances. We show that noise properties can be consistently derived by such procedures without resorting to currently used iterative noise-signal methods. More importantly, we show that optimal (GLS) CMB maps can be obtained from the observed timestream with the only knowledge of the noise memory parameter, the outcome of our estimators.
| Title: | Evolution of groups of galaxies | |
| Authors: | Cavaliere, A.; Santangelo, P.; Tarquini, G.; Vittorio, N. | |
| Publication: | Clustering in the Universe, Proceedings of a Colloquium, held at Meudon Observatory, 1982. Edited by D. Gerbal and A. Mazure. Gif-sur-Yvette: Editions Frontieres, 1983., p.25 | |
| Publication Date: | 00/1983 | |
| Origin: | ADS | |
| Bibliographic Code: | 1983clun.proc…25C |
Abstract
The merging process in groups of galaxies is studied by direct numerical simulations that include a mass spectrum, an initial Hubble expansion and the presence of dark mass. The authors find that a large merger forms while small galaxies easily survive for long time; that the merger follows a de Vaucouleurs law out to large radii; that the X-ray emission from the associated intragroup gas is strongly peaked towards the central merger.
| Title: | Sub-degree CMB anisotropy from space. II. In-flight calibration | |
| Authors: | Bersanelli, M.; Muciaccia, P. F.; Natoli, P.; Vittorio, N.; Mandolesi, N. | |
| Affiliation: | AA(Istituto di Fisica Cosmica, CNR, Milano, Italy), AB(Dipartimento di Fisica, Università di Tor Vergata, Roma, Italy), AC(Istituto TESRE, CNR, Bologna, Italy) | |
| Publication: | A & A Supplement series, Vol. 121, February 1997, 393-404 (A&AS Homepage) | |
| Publication Date: | 02/1997 | |
| Origin: | A&AS | |
| Astronomy Keywords: | COSMIC MICROWAVE BACKGROUND, RADIO CONTINUUM: GENERAL, SPACE VEHICLES | |
| DOI: | 10.1051/aas:1997322 | |
| Bibliographic Code: | 1997A&AS..121..393B |
Abstract
In the context of the COBRAS/SAMBA mission study, we discuss in-flight calibration of extended sky maps of the microwave sky using celestial sources. We simulate the observations in order to assess the accuracy obtainable for absolute and relative calibration of the Low Frequency Instrument (LFI), operating in the 30-130 GHz range. Accurate calibration can be achieved using the CMB dipole signal, Delta TD. With conservative assumptions on the effect of Galactic contamination, we find that the CMB dipole will provide absolute calibration accuracy ~0.7% (limited by the COBE-DMR uncertainty on Delta TD) on time-scales of about 10 days at all frequencies and for the entire mission lifetime. Long-term calibration with accuracy < 0.2% can be obtained using the spacecraft orbital velocity. Additional, independent calibration will be provided by the observation of external planets. We also describe the capability of the proposed scanning technique to detect and remove long-term instrumental drifts, and show that these effects, if present, can be controlled and removed with an overall negligible impact on the data uncertainty.
| Title: | Linear clustering of galaxies in low-density universes | |
| Authors: | Occhionero, F.; Vittorio, N.; Carnevali, P.; Santangelo, P. | |
| Affiliation: | AA(CNR, Laboratorio di Astrofisica Spaziale, Frascati; Osservatorio Astronomico, Rome, Italy), AB(CNR, Laboratorio di Astrofisica Spaziale, Frascati, Italy), AC(CNR, Laboratorio di Astrofisica Spaziale, Frascati, Italy), AD(CNR, Laboratorio di Astrofisica Spaziale, Frascati, Italy) | |
| Publication: | Astronomy and Astrophysics, vol. 86, no. 1-2, June 1980, p. 212-216. (A&A Homepage) | |
| Publication Date: | 06/1980 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, COSMOLOGY, GALACTIC CLUSTERS, GRAVITATION THEORY, ACCELERATION (PHYSICS), CURVATURE, SPACE-TIME FUNCTIONS | |
| Comment: | A&AA ID. AAA027.162.099 | |
| Bibliographic Code: | 1980A&A….86..212O |
Abstract
Assuming that the large scale structure observed in the present universe can be explained by dissipationless gravitational clustering of small (Jeans) masses into larger and larger structures, the theory of linear growth of gravitational instability is applied to the case of a positive cosmological constant. For such a constant, numerical results show that the growing modes of low-density universes still amplify by at least an order of magnitude between z approximately equal to 1/Omega(0) and the present, provided the spatial curvature is positive and suitably large.
| Title: | Observations of the temperature and polarization anisotropies with BOOMERANG 2003 | |
| Authors: | Jones, W. C.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Lange, A. E.; MacTavish, C. J.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T. E.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Physics Department, California Institute of Technology, Pasadena, CA, USA; Jet Propulsion Laboratory, Pasadena, CA, USA), AB(School of Physics and Astronomy, Cardiff University, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA), AD(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Ont., Canada), AE(Computational Research Division, LBNL, Berkeley, CA, USA; Space Sciences Laboratory, University of California at Berkeley, CA, USA), AF(IFAC-CNR, Firenze, Italy), AG(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), AH(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Ont., Canada; Theoretical Physics Group, Imperial College, London, UK), AI(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, USA), AJ(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), AK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), AM(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), AN(Instituto Nazionale di Geofisica e Vulcanologia, Rome, Italy), AO(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA, USA), AP(Theoretical Physics Group, Imperial College, London, UK), AQ(Department of Physics, University of California at Santa Barbara, CA, USA; Department of Physics, Case Western Reserve University, Cleveland, OH, USA), AR(Physics Department, California Institute of Technology, Pasadena, CA, USA), AS(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Ont., Canada; INFN, Sezione di Roma 1, Rome, Italy), AT(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), AU(School of Physics and Astronomy, Cardiff University, UK), AV(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; INFN, Sezione di Roma 1, Rome, Italy), AW(Department of Physics, Case Western Reserve University, Cleveland, OH, USA), AX(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; INFN, Sezione di Roma 2, Rome, Italy), AY(Department of Physics, University of Toronto, Ont., Canada; Department of Astronomy and Astrophysics, University of Toronto, Ont., Canada), AZ(Department of Physics, University of Toronto, Ont., Canada), BA(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BB(Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, Ont., Canada; Department of Physics, University of Alberta, Edmonton, AB, Canada), BC(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BD(Institut d’Astrophysique de Paris, Paris, France), BE(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BF(Instituto Nazionale di Geofisica e Vulcanologia, Rome, Italy), BG(Department of Physics, Case Western Reserve University, Cleveland, OH, USA), BH(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BI(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), BJ(Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy), BK(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; INFN, Sezione di Roma 2, Rome, Italy) | |
| Publication: | New Astronomy Reviews, Volume 50, Issue 11-12, p. 945-950. (NewAR Homepage) | |
| Publication Date: | 12/2006 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.newar.2006.09.014 | |
| Bibliographic Code: | 2006NewAR..50..945J |
Abstract
The BOOMERANG experiment completed its final long duration balloon (LDB) flight over Antarctica in January 2003. The focal plane was upgraded to accommodate four sets of 145 GHz polarization sensitive bolometers (PSBs), identical to those to be flown on the Planck HFI instrument. Approximately, 195 hours of science observations were obtained during this flight, including 75 hours distributed over 1.84% of the sky and an additional 120 hours concentrated on a region covering 0.22% of the sky. We derive the angular power spectra of the cosmic microwave background (CMB) temperature and polarization anisotropies from these data. The temperature anisotropies are detected with high signal to noise on angular scales ranging from several degrees to ˜10 arcminutes. The curl-free (EE) component is detected at ˜4.8σ, and a two-sigma upper limit on the curl (BB) component of 8.6 μK2 is obtained on scales corresponding to ˜0.5°. Both the temperature and polarization anisotropies are found to be consistent with a concordance ΛCDM cosmology that is seeded by adiabatic density perturbations. In addition to the CMB observations, BOOMERANG03 surveyed a ˜300 square degree region centered on the Galactic plane. These observations represent the first light for polarization sensitive bolometers, which are currently operational in two South-Pole based polarimeters, as well as Planck HFI, at frequencies ranging from 100 to 350 GHz (3 mm to 850 μm).
| Title: | CMB power spectrum estimation for the Planck Surveyor | |
| Authors: | Balbi, A.; de Gasperis, G.; Natoli, P.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; INFN, Sezione di Roma II, via della Ricerca Scientifica 1, 00133, Roma, Italy), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy), AC(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; INFN, Sezione di Roma II, via della Ricerca Scientifica 1, 00133, Roma, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133, Roma, Italy; INFN, Sezione di Roma II, via della Ricerca Scientifica 1, 00133, Roma, Italy) | |
| Publication: | Astronomy and Astrophysics, v.395, p.417-421 (2002) (A&A Homepage) | |
| Publication Date: | 11/2002 | |
| Origin: | A&A | |
| Astronomy Keywords: | cosmic microwave background, methods: data analysis | |
| DOI: | 10.1051/0004-6361:20021288 | |
| Bibliographic Code: | 2002A&A…395..417B |
Abstract
We use an iterative generalized least squares map-making algorithm, in conjunction with Monte Carlo techniques, to obtain estimates of the angular power spectrum from cosmic microwave background (CMB) maps. This is achieved by characterizing and removing the instrumental noise contribution in multipole space. This technique produces unbiased estimates and can be applied to an arbitrary experiment. In this paper, we use it on realistic simulations of Planck Low Frequency Instrument (LFI) observations, showing that it can lead to fast and reliable estimation of the CMB angular power spectrum from megapixel maps.
| Title: | On the Primordial Helium Content: Cosmic Microwave Background and Stellar Constraints | |
| Authors: | Bono, G.; Balbi, A.; Cassisi, S.; Vittorio, N.; Buonanno, R. | |
| Affiliation: | AA(Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monte Porzio Catone, Italy buonanno@mporzio.astro.it bono@mporzio.astro.it), AB(Dipartimento di Fisica, Università Tor Vergata, and INFN, Sezione di Roma II, Via della Ricerca Scientifica 1, 00133 Rome, Italy balbi@roma2.infn.it Nicola.Vittorio@roma2.infn.it), AC(Osservatorio Astronomico di Collurania, via M. Maggini, 64100 Teramo, Italy cassisi@te.astro.it), AD(Dipartimento di Fisica, Università Tor Vergata, and INFN, Sezione di Roma II, Via della Ricerca Scientifica 1, 00133 Rome, Italy balbi@roma2.infn.it Nicola.Vittorio@roma2.infn.it), AE(Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monte Porzio Catone, Italy; Dipartimento di Fisica, Università Tor Vergata, and INFN, Sezione di Roma II, Via della Ricerca Scientifica 1, 00133 Rome, Italy balbi@roma2.infn.it Nicola.Vittorio@roma2.infn.it buonanno@mporzio.astro.it bono@mporzio.astro.it) | |
| Publication: | The Astrophysical Journal, Volume 568, Issue 2, pp. 463-469. (ApJ Homepage) | |
| Publication Date: | 04/2002 | |
| Origin: | UCP | |
| Astronomy Keywords: | Cosmology: Cosmic Microwave Background, Cosmology: Theory, Stars: Abundances, Stars: Evolution, Stars: Horizontal-Branch | |
| DOI: | 10.1086/338951 | |
| Bibliographic Code: | 2002ApJ…568..463B |
Abstract
We present the results of a joint investigation aimed at constraining the primordial He content (YP) on the basis of both the cosmic microwave background (CMB) anisotropy and two stellar observables, namely, the tip of the red giant branch (TRGB) and the luminosity of the zero-age horizontal branch (ZAHB). Current baryon density estimates based on CMB measurements cover a wide range of values 0.009<~Ωbh2<~0.045, which according to big bang nucleosynthesis models would imply 0.24<~YP<~0.26. We constructed several sets of evolutionary tracks and horizontal-branch (HB) models by adopting YP=0.26 and several metal contents. The comparison between theory and observations suggests that ZAHB magnitudes based on He-enhanced models are 1.5 σ brighter than the empirical ones. The same outcome applies for TRGB bolometric magnitudes. This finding somewhat supports a YP abundance close to the canonical 0.23-0.24 value. More quantitative constraints on this parameter are hampered by the fact that the CMB pattern shows a sizable dependence on both YP and the baryon density only at small angular scales, i.e., at high l in the power spectrum (l>~100). However, this region of the power spectrum could be still affected by deceptive systematic uncertainties. Finally, we suggest using the UV upturn to estimate the He content on Gpc scales. In fact, we find that a strong increase in YP causes a decrease in the UV emission in metal-poor, hot HB structures.
| Title: | Primordial spectrum and density parameter-problem in a power-law inflation | |
| Authors: | Lucchin, F.; Matarrese, S.; Vittorio, N. | |
| Affiliation: | AA(Padova, Università , Padua, Italy), AB(Scuola Internazionale Superiore di Studi Avanzati, Trieste, Italy), AC(California, University, Berkeley) | |
| Publication: | Astronomy and Astrophysics (ISSN 0004-6361), vol. 162, no. 1-2, July 1986, p. 13-15. (A&A Homepage) | |
| Publication Date: | 07/1986 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | BIG BANG COSMOLOGY, GALACTIC EVOLUTION, UNIVERSE, ASTRONOMICAL MODELS, BACKGROUND RADIATION, DARK MATTER, INFLATING, MICROWAVES, SPECTRAL METHODS | |
| Bibliographic Code: | 1986A&A…162…13L |
Abstract
The possibility of defining a valid power-law inflationary model of an open universe with a primordial density fluctuation spectrum flatter than a scale-invariant spectrum is examined. The model is developed by relaxing the Big Bang requirements of exponential growth and no divergence from the perturbation specific binding energy. The accelerated expansion of the power-law model satisfies the horizon conditions of a Friedmann universe. An expression is found for relating the observed density parameter (about 10 percent) to the parameter at the moment of the inflationary phase. A natural large-scale cutoff is found to arise for the perturbations during inflation. The analysis supports a model of the universe as dominated by cold dark matter, and identifies problems inherent in a purely baryonic universe and in interpretation of clustering on the basis of analysis of the cosmic microwave background radiation.
| Title: | Ionization curves and last scattering surfaces in neutrino-dominated universes | |
| Authors: | Bonometto, S.; Lucchin, F.; Occhionero, F.; Vittorio, N. | |
| Affiliation: | AA(Padova, Università , Padua; Scuola Internazionale Superiore di Studi Avanzati, Trieste, Italy), AB(Padova, Università , Padua, Italy), AC(Roma, Università , Rome; CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AD(Roma, Università , Rome, Italy) | |
| Publication: | Astronomy and Astrophysics (ISSN 0004-6361), vol. 123, no. 1, June 1983, p. 118-120. (A&A Homepage) | |
| Publication Date: | 06/1983 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | COSMOLOGY, IONIZATION, NEUTRINOS, RED SHIFT, PARTICLE FLUX DENSITY, SCATTERING | |
| Bibliographic Code: | 1983A&A…123..118B |
Abstract
The ionization curve and redshift distribution of the microwave photon last scatterings in the decoupling epoch are computed for models of the universe dynamically dominated by the energy density in massive neutrinos. The results are compared with the canonical massless neutrino cases. It is found that the presence of neutrinos does significantly modify the ionization degree, but that the changes in the redshift distribution are fairly small.
| Title: | Cavities in high density universes | |
| Authors: | Occhionero, F.; Veccia-Scavalli, L.; Vittorio, N. | |
| Affiliation: | AA(CNR, Istituto di Astrofisica Spaziale, Frascati; Osservatorio Astronomico, Rome, Italy), AB(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AC(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy) | |
| Publication: | Astronomy and Astrophysics, vol. 99, no. 1, June 1981, p. L12-L14. (A&A Homepage) | |
| Publication Date: | 06/1981 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, COSMOLOGY, GRAVITATIONAL EFFECTS, SPACE DENSITY, UNIVERSE, BIG BANG COSMOLOGY, GRAVITATIONAL COLLAPSE, NEUTRINOS, RELATIVITY, SPACE-TIME FUNCTIONS | |
| Comment: | A&AA ID. AAA029.162.161 | |
| Bibliographic Code: | 1981A&A….99L..12O |
Abstract
Occhionero et al. (1981) have constructed a theoretical model in order to explain the large-scale voids which exist between clusters of galaxies. In the model, large cavities develop around matter condensations. However, for a reasonable mass of 10 to the 15th solar masses, and for an Einstein- de Sitter Universe, the typical cavity dimension is of the order of 10 Mpc rather 100 Mpc as required by the observations. In the considered analysis, the algorithm of the previous investigation has been generalized to conduct a study of the issue in cosmological models with arbitrary parameter values. An expression is reported for the typical dimension of the cavities. The possibility is pointed out that matter condensations are in reality neutrino condensations, ordinary baryonic matter being only a one percent contamination of the total. The assumption has to be made that neutrinos are condensed where the galaxies are seen.
| Title: | Noise Estimation in CMB Time-Streams and Fast Iterative Map-Making | |
| Authors: | Prunet, S.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; Bernardis, P. De; Gasperis, G. De; Troia, G. De; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Pongetti, F.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza), AB(Department of Physics, Queen Mary and Westfield College), AC(Jet Propulsion Laboratory), AD(Dipartimento di Fisica, Università di Roma La Sapienza), AE(NERSC-LBNL; Center for Particle Astrophysics, University of California at Berkeley), AF(IROE – CNR), AG(Department of Physics, University of California at Santa Barbara), AH(California Institute of Technology), AI(CITA University of Toronto), AJ(Dipartimento di Fisica, Università di Roma Tor Vergata), AK(CITA University of Toronto), AL(Department of Physics, University of California at Santa Barbara), AM(Astrophysics, University of Oxford), AN(California Institute of Technology;, Astrophysics, University of Oxford), AO(CITA University of Toronto), AP(California Institute of Technology), AQ(California Institute of Technology), AR(CITA University of Toronto), AS(Center for Particle Astrophysics, University of California at Berkeley), AT(California Institute of Technology), AU(ENEA Centro Ricerche di Frascati), AV(CITA University of Toronto), AW(California Institute of Technology), AX(Physics and Astronomy Dept, Cardiff University), AY(CITA University of Toronto), AZ(CITA University of Toronto; Departments of Physics and Astronomy, University of Toronto), BA(Department of Physics, University of California at Santa Barbara), BB(Departments of Physics and Astronomy, University of Toronto), BC(IROE – CNR), BD(CITA University of Toronto), BE(Dipartimento di Fisica, Università di Roma La Sapienza), BF(Istituto Nazionale di Geofisica), BG(Dipartimento di Fisica, Università di Roma La Sapienza), BH(Istituto Nazionale di Geofisica), BI(Istituto Nazionale di Geofisica), BJ(Department of Physics, University of California at Santa Barbara), BK(ENEA Centro Ricerche di Frascati), BL(CITA University of Toronto), BM(Dipartimento di Fisica, Università di Roma Tor Vergata) | |
| Publication: | Mining the Sky: Proceedings of the MPA/ESO/MPE Workshop Held at Garching, Germany, July 31 – August 4, 2000, ESO ASTROPHYSICS SYMPOSIA. ISBN 3-540-42468-7. Edited by A.J. Banday, S. Zaroubi, and M. Bartelmann. Springer-Verlag, 2001, p. 421 | |
| Publication Date: | 00/2001 | |
| Origin: | ADS; SPRINGER | |
| Abstract Copyright: | (c) 2001: Springer-Verlag | |
| DOI: | 10.1007/10849171_53 | |
| Bibliographic Code: | 2001misk.conf..421P |
Abstract
We describe here an iterative method for jointly estimating the noise power spectrum from a CMB experiment’s time-ordered data, together with the maximum-likelihood map. We test the robustness of this method on simulated Boomerang datasets with realistic noise.
| Title: | Searching for non-Gaussian signals in the BOOMERanG 2003 CMB map: Preliminary results | |
| Authors: | de Troia, G.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; di Stefano, G.; Ferreira, P. G.; Hivon, E.; Jaffe, A.; Kisner, T.; Kunz, M.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C.; Melchiorri, A.; Montroy, T.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy), AB(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Canada), AE(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA), AF(IFAC-CNR, Firenze, Italy), AG(Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Canada; Theoretical Physics Group, Imperial College, London, UK), AI(IPAC, California Institute of Technology, Pasadena, CA, USA), AJ(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AK(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), AM(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), AN(Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK), AO(IPAC, California Institute of Technology, Pasadena, CA, USA), AP(Theoretical Physics Group, Imperial College, London, UK), AQ(Physics Department, Case Western Reserve University, Cleveland, OH, USA; Department of Physics, University of California, Santa Barbara, CA, USA), AR(Départment de Physique Théorique, Université de Genève, 24 quai Ernest, Ansermet, Genève 4, Switzerland), AS(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AT(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AU(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AV(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK), AW(Physics Department, University of Toronto, Toronto, Ont., Canada), AX(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AY(Physics Department, Case Western Reserve University, Cleveland, OH, USA), AZ(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy), BA(Physics Department, University of Toronto, Toronto, Ont., Canada), BB(Physics Department, University of Toronto, Toronto, Ont., Canada), BC(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy), BD(Department of Physics, University of Alberta, Edmonton, AB, Canada), BE(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy), BF(Institut dÃ;strophysique, Paris, France), BG(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy), BH(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), BI(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BJ(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy), BK(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), BL(Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy), BM(Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy) | |
| Publication: | New Astronomy Reviews, Volume 51, Issue 3-4, p. 250-255. (NewAR Homepage) | |
| Publication Date: | 03/2007 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.newar.2006.11.064 | |
| Bibliographic Code: | 2007NewAR..51..250D |
Abstract
We analyse the 145 GHz temperature map produced from the 2003 flight of BOOMERanG in search for deviations from Gaussianity. We perform a pixel space analysis computing the map’s skewness, kurtosis and Minkowski functionals, as well as a Fourier space analysis computing the diagonal part the of angular bispectrum. The preliminary results presented here suggest that the data are fully consistent with the Gaussian hypothesis.
| Title: | l-space spectroscopy of the Cosmic Microwave Background with the BOOMERanG experiment | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Contaldi, C. R.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Jones, W. C.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Natoli, P.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Pongetti, F.; Prunet, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), AB(Queen Mary and Westfield College, London, United Kingdom), AC(Jet Propulsion Laboratory, Pasadena, California), AD(C.I.T.A., University of Toronto, Canada), AE(N.E.R.S.C., LBNL, Berkeley, California), AF(IROE-CNR, Firenze, Italy), AG(Department of Physics, University of California, Santa Barbara, California), AH(C.I.T.A., University of Toronto, Canada), AI(California Institute of Technology, Pasadena, California), AJ(Department of Physics, Second University of Rome, Italy), AK(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), AL(Department of Physics, University of California, Santa Barbara, California), AM(IPAC, Caltech, Pasadena, California), AN(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), AO(IPAC, Caltech, Pasadena, California), AP(California Institute of Technology, Pasadena, California), AQ(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), AR(Department of Astronomy, Space Sciences Lab and Center for Particle Astrophysics, University of California, Berkeley, California 94720), AS(California Institute of Technology, Pasadena, California), AT(California Institute of Technology, Pasadena, California), AU(ENEA, Frascati, Italy), AV(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), AW(California Institute of Technology, Pasadena, California), AX(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, United Kingdom), AY(Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford, OX 3RH, United Kingdom), AZ(Department of Physics, Second University of Rome, Italy), BA(Department of Physics, University of California, Santa Barbara, California), BB(Departments of Physics and Astronomy, University of Toronto, Canada), BC(IROE-CNR, Firenze, Italy), BD(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), BE(C.I.T.A., University of Toronto, Canada), BF(Dipartimento di Fisica, Universitá La Sapienza, Roma, P.le A. Moro, 2, 00185, Italy), BG(Istituto Nazionale di Geofisica, Roma, Italy), BH(C.I.T.A., University of Toronto, Canada), BI(Istituto Nazionale di Geofisica, Roma, Italy), BJ(Department of Physics, University of California, Santa Barbara, California), BK(ENEA, Frascati, Italy), BL(Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford, OX 3RH, United Kingdom) | |
| Publication: | EXPERIMENTAL COSMOLOGY AT MILLIMETRE WAVELENGTHS: 2K1BC Workshop. Breuil-Cervinia, Valle d’Aosta, Italy, 9-13 July, 2001. Edited by Marco De Petri and Massimo Gervasi. American Institute of Physics, 2002. AIP Conference Proceedings, Volume 616, pp. 3-11 (2002). (AIPC Homepage) | |
| Publication Date: | 05/2002 | |
| Origin: | STI | |
| PACS Keywords: | Background radiations, Radio, microwave, Observational cosmology | |
| Abstract Copyright: | (c) 2002: American Institute of Physics | |
| Comment: | ISBN: 0735400628 | |
| DOI: | 10.1063/1.1475595 | |
| Bibliographic Code: | 2002AIPC..616….3D |
Abstract
The BOOMERanG experiment has recently produced detailed maps of the Cosmic Microwave Background, where sub-horizon structures are resolved with good signal to noise ratio. A power spectrum (spherical harmonics) analysis of the maps detects three peaks, at multipoles <script>l</script>=(213-13+10),(541-32+20),(845-25+12). In this paper we discuss the data analysis and the implications of these results for cosmology. .
| Title: | The evolution of clusters of galaxies and of their intracluster medium | |
| Authors: | Cavaliere, A.; de Biase, G. A.; Santangelo, P.; Vittorio, N. | |
| Publication: | Clustering in the Universe, Proceedings of a Colloquium, held at Meudon Observatory, 1982. Edited by D. Gerbal and A. Mazure. Gif-sur-Yvette: Editions Frontieres, 1983., p.15 | |
| Publication Date: | 00/1983 | |
| Origin: | ADS | |
| Bibliographic Code: | 1983clun.proc…15C |
Abstract
The authors present first results from simulated evolutionary histories of clusters of galaxies with their intracluster medium (ICM). They adopt a hydrostatic approximation to concentrate on full 3-dimensional morphologies and on detailed mapping of X-ray emission from the ICM. The authors obtain a close correspondence of simulated maps with clumpy, bimodal and nearly symmetric configurations of observed nXD clusters.
| Title: | COBRAS: A Space Mission for Mapping the CMB Structure at 0.5° Resolution | |
| Authors: | Smoot, G. F.; Mandolesi, N.; Bersanelli, M.; Cesarsky, C.; Lachieze-Rey, M.; Danese, L.; Vittorio, N.; de Bernardis, P.; dall’Oglio, G.; Sironi, G.; Crane, P.; Janssen, M.; Partridge, B.; Beckman, J.; Rebolo, R.; Puget, J. L.; Bussoletti, E.; Raffelt, G.; Davies, R.; Encrenaz, P.; Natale, V.; Tofani, G.; Merluzzi, P.; Toffolatti, L.; Scaramella, R.; MartÃnez-Gonzáles, E.; Sáez, D.; Lasenby, A.; Kogut, A.; Efstathiou, G. | |
| Publication: | Astrophysical Letters and Communications, Vol. 32, p.297 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995ApL&C..32..297S |
Abstract
Not Available
| Title: | Evolution of adiabatic fluctuations in massive-neutrino-dominated universe models | |
| Authors: | Bonometto, S. A.; Lucchin, F.; Occhionero, F.; Vittorio, N. | |
| Affiliation: | AA(Padova, Università , Padua; Scuola Internazionale Superiore di Studi Avanzati, Trieste, Italy), AB(Padova, Università , Padua, Italy), AC(Roma, Università , Rome, Italy), AD(Roma, Università , Rome, Italy) | |
| Publication: | Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 477-484. (A&A Homepage) | |
| Publication Date: | 09/1984 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ADIABATIC CONDITIONS, ASTRONOMICAL MODELS, FLUCTUATION THEORY, NEUTRINOS, UNIVERSE, AMPLITUDES, BACKGROUND RADIATION, BIG BANG COSMOLOGY, DARK MATTER, GALACTIC EVOLUTION, MASS, SPHERICAL HARMONICS | |
| Bibliographic Code: | 1984A&A…138..477B |
Abstract
A canonical case of three neutrinos with masses of about 30 eV is discussed theoretically in terms of their influence on linear adiabatic fluctuations in the early universe. The interest in hot dark matter was encouraged by the possibility that gravitational instabilities in massive neutrinos could account for current structures in the universe. Unity is assumed for the density parameter and a value of much less for the baryonic density parameter (0.03). Matter and radiation are treated as fluids and neutrinos in terms of phase space distributions. The discussion focuses on gravitational interactions between the three components, Thomson scattering between electrons and photons, and the evolution of fluctuations to scales of 10 to the 14th to 10 to the 19th solar masses. The growth of fluctuations above 10 to the 15th solar masses is shown to depend on dark matter after matter-radiation decoupling. A dependency is found between the mass scale of a first nonlinear collapse regime and the primeval spectral index.
| Title: | Perturbations of the Hubble flow | |
| Authors: | Occhionero, F.; Vittorio, N.; Carnevali, P.; Santangelo, P. | |
| Affiliation: | AA(CNR, Istituto di Astrofisica Spaziale, Frascati; Osservatorio Astronomico, Rome, Italy), AB(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AC(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy), AD(CNR, Istituto di Astrofisica Spaziale, Frascati, Italy) | |
| Publication: | Astronomy and Astrophysics, vol. 107, no. 1, Mar. 1982, p. 172-177. (A&A Homepage) | |
| Publication Date: | 03/1982 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | BIG BANG COSMOLOGY, DENSITY DISTRIBUTION, ENERGY DISTRIBUTION, HUBBLE CONSTANT, BACKGROUND RADIATION, GALACTIC EVOLUTION, GRAVITATIONAL FIELDS, MICROWAVES, PERTURBATION, RED SHIFT, UNIVERSE | |
| Comment: | A&AA ID. AAA031.162.043 | |
| Bibliographic Code: | 1982A&A…107..172O |
Abstract
The growth of perturbations in an expanding universe in the presence of a nonvanishing cosmological constant is investigated, and it is shown that the amplification of density perturbations is much larger than previously thought. Nonlinear growth after parameterizing a perturbation by its initial redshift and by its density excess or energy deficit relative to the background is also investigated, and a definition for the strength of the perturbation is found along with a prescription of its evolution. The necessary and sufficient condition for binding, and a simple expression for the size of a cavity forming around an energy perturbation are given, and results are presented for the density contrasts in analytical form for bound virialized perturbations, and in numerical form for perturbations marginally bound or at turnaround.
| Title: | Scalar field dark energy and cosmic microwave background | |
| Authors: | Baccigalupi, C.; Balbi, A.; Matarrese, S.; Perrotta, F.; Vittorio, N. | |
| Affiliation: | AA(SISSA/ISAS, Via Beirut 4, 34014, Trieste, Italy bacci@sissa.it), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata” and INFN, Sezione di Roma II, Via della Ricerca Scientifica 1, 00133 Roma, Italy balbi@roma2.infn.it), AC(Dipartimento di Fisica “Galileo Galilei”, Università di Padova and INFN, Sezione di Padova, via Marzolo 8, 35131 Padova, Italy matarrese@Upd.infn.it), AD(Lawrence Berkeley National Laboratory, 1 Cyclotron Road Mailstop 50-205, Berkeley, CA 94720, USA perrotta@materia.lbl.gov), AE(Dipartimento di Fisica, Università di Roma “Tor Vergata” and INFN, Sezione di Roma II, Via della Ricerca Scientifica 1, 00133 Roma, Italy vittorio@roma2.infn.it) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 124, p. 68-71. | |
| Publication Date: | 07/2003 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/S0920-5632(03)02079-6 | |
| Bibliographic Code: | 2003NuPhS.124…68B |
Abstract
A dynamical scalar field represents the simplest generalization of a pure Cosmological Constant as a candidate to explain the recent evidence in favour of the accelerated cosmic expansion. We review the dynamical properties of such a component, and argue that, even if the background expectation value of this field is fixed and the equation of state is the same as a Cosmological Constant, scalar field fluctuations can still be used to distinguish the two components. We compare predicted spectra of Cosmic Microvave Background (CMB) anisotropies in tracking scalar field cosmologies with the present CMB data, in order to get constraints on the amount and equation of state of dark energy. High precision experiments like SNAP, Planck and SNFactory, together with the data on Large Scale Structure, are needed to probe this issue with the necessary accuracy. Here we show the intriguing result that, with a strong prior on the value of the Hubble constant today, the assumption of a flat universe, and consistency relations between amplitude and spectral index of primordial gravitational waves, the present CMB data at 1σ give indication of a dark energy equation of state larger than -1, while the ordinary Cosmological Constant is recovered at 2σ.
| Title: | COBRAS: Goal and Experimental Approach | |
| Authors: | Mandolesi, N.; Smoot, G. F.; Bersanelli, M.; Cesarsky, C.; Lachieze-Rey, M.; Danese, L.; Vittorio, N.; de Bernardis, P.; dall’Oglio, G.; Sironi, G.; Crane, P.; Janssen, M.; Partridge, B.; Beckman, J.; Rebolo, R.; Puget, J. L.; Bussoletti, E.; Raffelt, G.; Davies, R.; Encrenaz, P.; Natale, V.; Tofani, G.; Merluzzi, P.; Toffolatti, L.; Scaramella, R.; MartÃnez-Gonzáles, E.; Sáez, D.; Lasenby, A.; Efstathiou, G. | |
| Publication: | Astrophysical Letters and Communications, Vol. 32, p.309 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995ApL&C..32..309M |
Abstract
Not Available
| Title: | Probing primordial non Gaussianity in the BOOMERanG CMB maps: an analysis based on analytical Minkowski functionals | |
| Authors: | Migliaccio, M.; Natoli, P.; de Troia, G.; Hikage, C.; Komatsu, E.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; di Stefano, G.; Hivon, E.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Masi, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Polenta, G.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AC(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AD(School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA), AE(Texas Cosmology Center, University of Texas at Austin, 1 University Station, C1400, Austin, TX 78712, USA), AF(School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA), AG(Jet Propulsion Laboratory, Pasadena, CA, USA), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada), AI(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA), AJ(IFAC-CNR, Firenze, Italy), AK(Theoretical Physics Group, Imperial College, London), AL(Jet Propulsion Laboratory, Pasadena, CA, USA), AM(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AN(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy), AO(Department of Physics, MIT, Cambridge, MA 02139, USA), AP(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), AQ(Institut d’Astrophysique, Paris, France), AR(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA), AS(Department of Physics, Princeton University, Princeton, NJ 0854, USA), AT(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AU(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AV(School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA), AW(Astrophysics Group, Imperial College, London), AX(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AY(Physics Department, Case Western Reserve University, Cleveland, OH, USA), AZ(Physics Department, University of Toronto, Toronto, Ontario, Canada), BA(Physics Department, University of Toronto, Toronto, Ontario, Canada), BB(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BC(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BD(Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA), BE(Istituto Nazionale di Geofisica e Vulcanologia, 00143 Rome, Italy), BF(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BG(Department of Physics, MIT, Cambridge, MA 02139, USA), BH(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BI(Dipartimento di Fisica, Università di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 194, p. 278-286. | |
| Publication Date: | 10/2009 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.nuclphysbps.2009.07.092 | |
| Bibliographic Code: | 2009NuPhS.194..278M |
Abstract
Minkowski functionals are a powerful tool to constrain the Gaussianity of the Cosmic Microwave Background (CMB). In the limit of a weakly non Gaussian field, a perturbative approach can be derived [Hikage C., Komatsu E., & Matsubara T., 2006, ApJ, 653, 11] that is completely based on analytical formulae without requiring computationally intensive, dedicated Monte Carlo non Gaussian simulations of the CMB anisotropy. We apply this machinery to an intensity map derived from the 1998 and 2003 flights of BOOMERanG, analyzed here together for the first time. We set limits on the non-linear coupling parameter f as -1020<f<390 at 95% CL, markedly improving the previous constraints set by [De Troia G. et al., 2007, ApJ, 670, L73] whose analysis was limited to the BOOMERanG 2003 dataset. These limits are the most stringent ever set among suborbital experiments.
| Title: | BOOMERanG results | |
| Authors: | Polenta, G.; Ade, P. A. R.; Balbi, A.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Ganga, K.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; MacTavish, C.; Bettolo, C. M.; Masi, S.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T.; Nati, F.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Torbet, E.; Tegmark, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AB(Department of Physics and Astronomy, Cardiff University, 5 The Parade, P.O. Box 913, Cardiff CF24 3YB, Wales, UK), AC(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 00133 Roma, Italy), AD(Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA; Observational Cosmology, California Institute of Technology, 1200 East California Boulevard, MC 59-33, Pasadena, CA 91125, USA), AE(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AF(National Energy Research Scientific Computing Center, LBNL, Berkeley, CA 94729-8139, USA; Center for Particle Astrophysics, University of California, Berkeley, CA, USA), AG(IFAC-CNR, via Panciatichi 64, 50127 Firenze, Italy), AH(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 00133 Roma, Italy), AI(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AJ(IPAC, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA), AK(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AL(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 00133 Roma, Italy), AM(Physics Department, University of Pennsylvania, Philadelphia, 209 South 33rd Street, PA 19104-6396, USA), AN(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AO(Istituto Nazionale di Geofisica, via di Vigna Murata 605, 00143 Roma, Italy), AP(IPAC, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA), AQ(IPAC, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA), AR(Observational Cosmology, California Institute of Technology, 1200 East California Boulevard, MC 59-33, Pasadena, CA 91125, USA), AS(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AT(Astrophysics Group, Imperial College, Prince Consort Road, London SW72BZ, UK), AU(Physics Department, Case Western Reserve University, 10900 Evelid Avenue, Cleveland, OH 44106-7079, USA; Department of Physics, University of California, Santa Barbara, CA 93106, USA), AV(IPAC, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA), AW(IPAC, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA), AX(Physics Department, University of Toronto, 60 St. George Street, Toronto, ON M5S3H8, Canada), AY(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AZ(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BA(Department of Physics and Astronomy, Cardiff University, 5 The Parade, P.O. Box 913, Cardiff CF24 3YB, Wales, UK), BB(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BC(Physics Department, Case Western Reserve University, 10900 Evelid Avenue, Cleveland, OH 44106-7079, USA; Department of Physics, University of California, Santa Barbara, CA 93106, USA), BD(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BE(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 00133 Roma, Italy), BF(Physics Department, University of Toronto, 60 St. George Street, Toronto, ON M5S3H8, Canada), BG(Physics Department, University of Toronto, 60 St. George Street, Toronto, ON M5S3H8, Canada), BH(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BI(Physics Department, University of Alberta, Edmonton AB T6G 2J1, Canada), BJ(Institut d’Astrophysique de Paris, CNRS, 98bis Boulevard Arago, Paris F-75014, France), BK(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BL(Istituto Nazionale di Geofisica, via di Vigna Murata 605, 00143 Roma, Italy), BM(Physics Department, Case Western Reserve University, 10900 Evelid Avenue, Cleveland, OH 44106-7079, USA), BN(Department of Physics, University of California, Santa Barbara, CA 93106, USA), BO(Physics Department, University of Pennsylvania, Philadelphia, 209 South 33rd Street, PA 19104-6396, USA), BP(Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 00133 Roma, Italy) | |
| Publication: | Advances in Space Research, Volume 36, Issue 6, p. 1064-1069. (AdSpR Homepage) | |
| Publication Date: | 00/2005 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.asr.2005.06.080 | |
| Bibliographic Code: | 2005AdSpR..36.1064P |
Abstract
The BOOMERanG experiment has mapped the mm/sub-mm sky during two long duration balloon flights from Antarctica, in 1998 and 2003. The first flight observed about 4% of the sky, measuring its brightness at 90, 150, 240 and 410 GHz with resolution of 12′. The faint structure of the Cosmic Microwave Background at horizon and sub-horizon scales is evident in these maps, and the wide frequency coverage allows for a careful estimate of the Galactic foreground. In the second flight a polarization-sensitive version of the instrument has been flown, to measure the linear polarization of the microwave sky at 145, 245 and 345 GHz. In this paper we review the main results from the first flight and report preliminary results obtained in the second flight.
| Title: | CMB polarization with BOOMERANG 2003 | |
| Authors: | Piacentini, F.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Hivon, E.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Marini-Bettolo, C.; Masi, S.; Mauskopf, P. D.; MacTavish, C. J.; Melchiorri, A.; Montroy, T. E.; Nati, F.; Nati, L.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AB(Department of Physics and Astronomy, Cardiff University, Wales, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street Toronto, Ontario, Canada M5S 3H8), AE(Computational Research Division, LBNL, Berkeley, CA, USA; Space Sciences Laboratory, UC Berkeley, CA, USA), AF(Istituto di Fisica Applicata “Nello Carrara”, Consiglio Nazionale delle Ricerce, Firenze, Italy), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street Toronto, Ontario, Canada M5S 3H8; Theoretical Physics Group, Imperial College, London, UK), AI(IPAC, California Institute of Technology, Pasadena, CA, USA), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AK(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), AM(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AN(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), AO(IPAC, California Institute of Technology, Pasadena, CA, USA), AP(Theoretical Physics Group, Imperial College, London, UK), AQ(Physics Department, Case Western Reserve University, Cleveland, OH, USA; Department of Physics, University of California, Santa Barbara, CA, USA), AR(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AS(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AT(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AU(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AV(Department of Physics and Astronomy, Cardiff University, Wales, UK), AW(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street Toronto, Ontario, Canada M5S 3H8), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AY(Physics Department, Case Western Reserve University, Cleveland, OH, USA), AZ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BB(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy), BC(Physics Department, University of Toronto, Toronto, Ont., Canada), BD(Physics Department, University of Toronto, Toronto, Ont., Canada), BE(Department of Physics, University of Alberta, Edmonton, Alta., Canada), BF(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BG(Institut d’Astrophysique, Paris, France), BH(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BI(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), BJ(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BK(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), BM(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BN(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy) | |
| Publication: | New Astronomy Reviews, Volume 51, Issue 3-4, p. 244-249. (NewAR Homepage) | |
| Publication Date: | 03/2007 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.newar.2006.11.058 | |
| Bibliographic Code: | 2007NewAR..51..244P |
Abstract
This paper reports results from the BOOMERANG 2003 flights, devoted to the measurement of intensity and polarization of the cosmic microwave background radiation. In particular, it is focused on the power angular power spectra and on the control of possible contamination from systematic effects and foregrounds.
Abstract
In the 1998-99 flight, BOOMERanG has produced maps of Ëœ 4 % of the sky at high Galactic latitudes, at frequencies of 90, 150, 240 and 410 GHz, with resolution ≳ 10′. The faint structure of the Cosmic Microwave Background at horizon and sub-horizon scales is evident in these maps. These maps compare well to the maps recently obtained at lower frequencies by the WMAP experiment. Here we compare the amplitude and morphology of the structures observed in the two sets of maps. We also outline the polarization sensitive version of BOOMERanG, which was flown early this year to measure the linear polarization of the microwave sky at 150, 240 and 350 GHz.
| Title: | BOOMERANG returns | |
| Authors: | Mauskopf, P. D.; Ade, P. A. R.; Balbi, A.; Cabella, P.; de Gasperis, G.; Natoli, P.; Vittorio, N.; Bock, J. J.; Hristov, V. V.; Jones, W. C.; Lange, A. E.; Bond, J. R.; Contaldi, C. R.; Borrill, J.; Boscaleri, A.; Crill, B. P.; de Bernardis, P.; de Troia, G.; Iacoangeli, A.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.; Polenta, G.; Ricciardi, S.; de Oliveira-Costa, A.; Tegmark, M.; di Stefano, G.; Romeo, G.; Ganga, K.; Hivon, E.; Jaffe, A. H.; Ruhl, J. E.; Kisner, T. S.; Montroy, T.; Torbet, E.; MacTavish, C.; Netterfield, C. B.; Pascale, E.; Pogosyan, D.; Prunet, S. | |
| Affiliation: | AA(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK philip.mauskopf@astro.cf.ac.uk), AB(Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK), AC(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AD(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AE(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AF(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AH(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA; Jet Propulsion Laboratory, Pasadena, CA, USA), AI(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AJ(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AK(Observational Cosmology, California Institute of Technology, Pasadena, CA, USA), AL(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ont., Canada), AM(Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ont., Canada), AN(National Energy Research Scientific Computing Center, LBNL, Berkeley, CA, USA; Center for Particle Astrophysics, University of California, Berkeley, CA, USA), AO(IFAC-CNR, Firenze, Italy), AP(CSU Dominguez Hills, Carson, CA, USA), AQ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AR(Physics Department, University of Pennsylvania, Philadelphia, PA, USA), AS(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AT(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AU(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AV(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AW(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AZ(Physics Department, University of Pennsylvania, Philadelphia, PA, USA), BA(Physics Department, University of Pennsylvania, Philadelphia, PA, USA), BB(Istituto Nazionale di Geofisica, Roma, Italy), BC(Istituto Nazionale di Geofisica, Roma, Italy), BD(IPAC, California Institute of Technology, Pasadena, CA, USA), BE(IPAC, California Institute of Technology, Pasadena, CA, USA), BF(Astrophysics Group, Imperial College, London, UK), BG(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BH(Department of Physics, University of California, Santa Barbara, CA, USA), BI(Physics Department, University of Toronto, Toronto, Ont., Canada), BJ(Physics Department, University of Toronto, Toronto, Ont., Canada), BK(Physics Department, University of Toronto, Toronto, Ont., Canada), BL(Physics Department, University of Alberta, Edmonton, Alta., Canada), BM(Institut d’Astrophysique, Paris, France) | |
| Publication: | New Astronomy Reviews, Volume 47, Issue 8-10, p. 733-740. (NewAR Homepage) | |
| Publication Date: | 11/2003 | |
| Origin: | ELSEVIER | |
| Keywords: | CMB, Sunyaev-Zel’dovich effect, Component separation, CMB polarisation | |
| DOI: | 10.1016/j.newar.2003.07.019 | |
| Bibliographic Code: | 2003NewAR..47..733M |
Abstract
BOOMERANG was one of the first experiments to map large areas of the cosmic microwave background (CMB) with high signal-to-noise during a long duration balloon (LDB) flight in 1998/99. BOOMERANG uses bolometric detectors measuring frequency bands from 90 to 400 GHz, a frequency range that complements the lower frequency range of experiments using HEMT amplifiers such as DASI and WMAP. Here, we discuss the status of the analysis of the B98 data including initial comparison of the B98 data with WMAP and component separation of the B98 maps in order to measure the Sunyaev-Zel’dovich effect. Finally, we describe the second LDB flight of the BOOMERANG telescope in January, 2003 with a receiver designed to map the polarisation of the CMB.
| Title: | BOOMERanG | |
| Authors: | Masi, S.; Ade, P. A. R.; Balbi, A.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; De Gasperis, G.; de Oliveira-Costa, A.; De Troia, G.; di Stefano, G.; Ganga, K.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Kisner, T. S.; Jones, W. C.; Lange, A. E.; Mauskopf, P. D.; Mactavish, C.; Melchiorri, A.; Montroy, T.; Nati, F.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Torbet, E.; Tegmark, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Universitá La Sapienza, Roma), AB(Department of Physics and Astronomy, Cardiff University), AC(Dipartimento di Fisica, Università di Roma Tor Vergata), AD(Jet Propulsion Laboratory, Pasadena), AE(Canadian Institute for Theoretical Astrophysics, University of Toronto), AF(National Energy Research Scientific Computing Center, LBNL, Berkeley), AG(IFAC-CNR, Firenze), AH(Dipartimento di Fisica, Università di Roma Tor Vergata), AI(Canadian Institute for Theoretical Astrophysics, University of Toronto), AJ(Jet Propulsion Laboratory, Pasadena), AK(Dipartimento di Fisica, Universitá La Sapienza, Roma), AL(Dipartimento di Fisica, Università di Roma Tor Vergata), AM(Physics Department, University of Pennsylvania, Philadelphia), AN(Dipartimento di Fisica, Universitá La Sapienza, Roma), AO(Istituto Nazionale di Geofisica, Roma), AP(California Institute of Technology, Pasadena), AQ(California Institute of Technology, Pasadena), AR(Jet Propulsion Laboratory, Pasadena), AS(Dipartimento di Fisica, Universitá La Sapienza, Roma), AT(Center for Particle Astrophysics, University of California), AU(Physics Department, Case Western Reserve University), AV(Jet Propulsion Laboratory, Pasadena), AW(Jet Propulsion Laboratory, Pasadena), AX(Department of Physics and Astronomy, Cardiff University), AY(Physics Department, University of Toronto, Toronto), AZ(Dipartimento di Fisica, Universitá La Sapienza, Roma), BA(Physics Department, Case Western Reserve University), BB(Dipartimento di Fisica, Universitá La Sapienza, Roma), BC(Dipartimento di Fisica, Università di Roma Tor Vergata), BD(Physics Department, University of Toronto, Toronto), BE(Physics Department, University of Toronto, Toronto), BF(Dipartimento di Fisica, Universitá La Sapienza, Roma), BG(Physics Department, University of Alberta), BH(Dipartimento di Fisica, Universitá La Sapienza, Roma), BI(Institut d’Astrophysique), BJ(Dipartimento di Fisica, Universitá La Sapienza, Roma), BK(Istituto Nazionale di Geofisica, Roma), BL(Physics Department, Case Western Reserve University), BM(Physics Department, Case Western Reserve University), BN(Physics Department, University of Pennsylvania, Philadelphia), BO(Dipartimento di Fisica, Università di Roma Tor Vergata) | |
| Publication: | Memorie della Società Astronomica Italiana Supplement, v.2, p.54 (2003) | |
| Publication Date: | 00/2003 | |
| Origin: | MmSAI | |
| Keywords: | Cosmology, Cosmic Microwave Background, Antarctic Astronomy | |
| Bibliographic Code: | 2003MSAIS…2…54M |
Abstract
The BOOMERanG experiment is a balloon-borne microwave telescope devoted to measurements of anisotropy and polarization of the Cosmic Microwave Background Radiation (CMB). The instrument is multiband in order to map the CMB and have a good understanding of all the important contaminating signals, (mainly galactic), and remove them if needed. Observations are carried out at about 38 Km of altitude, during a circum-antarctic Long Duration Balloon flight provided by NASA-NSBF. After two test flights in 1997, the instrument has been flown as a long duration payload in 1998 (covering four bands at 90, 150, 240, 410 GHz), and in 2003 (covering three bands at 150, 245, 345 GHz with polarization sensitive bolometers). Data from the first Antarctic flight are now fully analyzed; data analysis of the second (polarization) flight is currently under way.
| Title: | Constraints on reionization from CMB fluctuations. | |
| Authors: | de Bernardis, P.; Balbi, A.; de Gasperis, G.; Melchiorri, A.; Vittorio, N. | |
| Publication: | 16th Moriond Astrophysics Meeting: Microwave background anisotropies, p. 215 – 218 | |
| Publication Date: | 00/1997 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Anisotropy, Cosmic Microwave Background: Fluctuations, Cosmological Models: Dark Matter | |
| Bibliographic Code: | 1997mba..conf..215D |
Abstract
The authors study the anisotropy of the cosmic microwave background (CMB) in mixed dark matter models, with non scale-invariant primordial power spectra (i.e. n ≠1) and a late, sudden reionization of the intergalactic medium at redshift zrh. They test these models against recent detections of CMB anisotropy at large and intermediate angular scales. The likelihood analysis indicates that mixed dark matter models with blue power spectra (n ≅ 1.24) and a reionization at zrh ≡ 20 are most consistent with the presently available CMB anisotropy data.
| Title: | Sub-degree CMB anisotropy from space. I. Sky coverage and sensitivity. | |
| Authors: | Muciaccia, P. F.; Bersanelli, M.; de Bernardis, P.; Vittorio, N.; Masi, S.; Mandolesi, N. | |
| Publication: | Astronomy and Astrophysics Supplement, v.117, p.569-582 (A&AS Homepage) | |
| Publication Date: | 06/1996 | |
| Origin: | CDS | |
| Astronomy Keywords: | COSMIC MICROWAVE BACKGROUND, SPACE VEHICLES, COSMOLOGY: OBSERVATIONS | |
| Bibliographic Code: | 1996A&AS..117..569M |
Abstract
Decisive progress in cosmology is expected from a space mission dedicated to an extensive mapping of the Cosmic Microwave Background (CMB) with high angular and temperature sensitivity. Based on the European Space Agency COBRAS/SAMBA mission concept, we have studied the attainable sensitivity and sky coverage taking into account the effect of solar-system sources for the two far-Earth candidate orbits (Lagrangian points Moon-Earth L5 and Sun-Earth L2). We also take into account the microwave emission of the Galaxy in limiting the useful sky coverage. Our results provide a quantitative assessment of the relative observational merits of the two orbit options, and show that the Sun-Earth L2 orbit allows significantly better observational conditions.
| Title: | CMB Anisotropy due to Compton Scattering in Clusters of Galaxies. | |
| Authors: | Colafrancesco, S.; Maxxota, P.; Rephaeli, Y.; Vittorio, N. | |
| Publication: | Seventeeth Texas Symposium on Relativistic Astrophysics and Cosmology, Edited by Hans Böhringer, Gregor E. Morfill, and Joachim E. Trümper. Annals of the New York Academy of Sciences, Vol. 759 (New York, NY: The New York Academy of Sciences), 1995., p.722 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| DOI: | 10.1111/j.1749-6632.1995.tb17644.x | |
| Bibliographic Code: | 1995NYASA.759..722C |
Abstract
Not Available
| Title: | Preface | |
| Authors: | Bersanelli, M.; Cortiglioni, S.; Mandolesi, N.; Smoot, G. F.; Vittorio, N. | |
| Publication: | Astrophysical Letters and Communications, Vol. 32, p.1 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995ApL&C..32….1B |
Abstract
Not Available
| Title: | Are Omega{0} = 1 Cold Dark Matter Models Really Acceptable? | |
| Authors: | Vittorio, N. | |
| Publication: | Observational Cosmology. Astronomical Society of the Pacific Conference Series, Volume 51; Proceedings of an International Symposium; held in Milano; Italy; 21-25 September 1992; San Francisco: Astronomical Society of the Pacific (ASP); |c1993; edited by Guido L. Chincarini, Angela Iovino, Tommaso Maccacaro, and Dario Maccagni, p.685 | |
| Publication Date: | 01/1993 | |
| Origin: | ADS | |
| Bibliographic Code: | 1993ASPC…51..685V |
Abstract
Not Available
| Title: | Cosmology with clusters of galaxies | |
| Authors: | Colafrancesco, S.; Vittorio, N. | |
| Publication: | Cosmic Velocity Fields, Proceedings of the 9th IAP Astrophysics Meeting, Institut d’Astrophysique, Paris, July 12-17, 1993. Edited by François R. Bouchet and Marc Lachièze-Rey. Gif-sur-Yvette: Editions Frontieres, 1993., p.533 | |
| Publication Date: | 00/1993 | |
| Origin: | ADS | |
| Bibliographic Code: | 1993cvf..conf..533C |
Abstract
Not Available
| Title: | The cosmic microwave background: 25 years later | |
| Authors: | Mandolesi, N.; Vittorio, N. | |
| Affiliation: | AA(CNR, Istituto di Studio e Tecnologie sulle Radiazioni Extraterrestri, Bologna, Italy), AB(L’Aquila, Università , Italy) | |
| Publication: | Dordrecht, Netherlands, Kluwer Academic Publishers (Astrophysics and Space Science Library. Vol. 164), 1990, 301 p. For individual items see A92-27356 to A92-27369. | |
| Publication Date: | 00/1990 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | BACKGROUND RADIATION, CONFERENCES, EXTRATERRESTRIAL RADIO WAVES, MICROWAVES, RELIC RADIATION, ANISOTROPY, ASTRONOMICAL MAPS, ASTRONOMICAL SPECTROSCOPY, COSMOLOGY, INFRARED ASTRONOMY, RADIATION PRESSURE, RADIO ASTRONOMY, X RAY ASTRONOMY | |
| Bibliographic Code: | 1990ASSL..164…..M |
Abstract
The present conference on the cosmic microwave background (CMB) 25 yr following its discovery encompasses historical effects, small-, medium-, and large-scale CMB anisotropy, the CMB spectrum, other backgrounds, current experimental work, and examinations of observational and theoretical understanding to date. Specific issues addressed include the discovery of the 3 K radiation, theoretical maps of CMB anisotropies, observations of the Suniaev Zel’dovich effect, measurements of the CMB at 3.3 mm, theoretical implications of the CMB spectral distortions, cosmic instability from radiation pressure, and the IR cosmic background radiation. Also addressed are the origin of the extragalactic X-ray background, the components of the cosmic background radiation in other wavelength ranges and their relevance to the microwave background, experimental methods for the investigation of the large-scale CBR anisotropy, and developing astronomical programs for studying the CMB.
| Title: | The large scale structure of the universe | |
| Authors: | Vittorio, N. | |
| Affiliation: | AA(L’Aquila, Università , Italy) | |
| Publication: | IN: Astronomy, cosmology and fundamental physics; Proceedings of the Third ESO-CERN Symposium, Bologna, Italy, May 16-20, 1988 (A90-44077 19-90). Dordrecht, Netherlands and Boston, MA, Kluwer Academic Publishers, 1989, p. 159-180. | |
| Publication Date: | 00/1989 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | ASTRONOMICAL MODELS, COSMOLOGY, SPATIAL DISTRIBUTION, UNIVERSE, DARK MATTER, GALACTIC STRUCTURE, RADIATION DISTRIBUTION, RELIC RADIATION | |
| Bibliographic Code: | 1989ASSL..155..159V |
Abstract
Results from recent observational studies of galactic peculiar velocities and gravity and of the angular distribution of the cosmic microwave background radiation (CMBR) are summarized, with a focus on their implications for theoretical models of galaxy formation and large-scale structure. The data are presented in graphs and discussed in detail. It is found that biased cold-dark-matter models are much less able to account for large-scale coherent flows and inhomogeneities than isocurvature baryonic (IB) models of the type formulated by Peebles (1987). The IB models are also favored when more discriminant tests are applied, based on the orientation of the dipole anisotropy of the galaxy distribution or the misalignment of the apices of this dipole and that of the CMBR temperature. Also discussed are Monte Carlo simulations of CMBR observations, useful for the design of future searches for CMBR temperature anisotropy.
| Title: | The Dynamical Evolution of Clusters and Groups of Galaxies | |
| Authors: | Cavaliere, A.; Santangelo, P.; Tarquini, G.; Vittorio, N. | |
| Publication: | Clusters and Groups of Galaxies. International Meeting held in Trieste, Italy, September 13-16, 1983. Editors, F. Mardirossian, G. Giuricin, M. Mezzetti; Publisher, D. Reidel Pub. Co., Dordrecht, Holland, Boston, MA, Hingham, MA, U.S.A. Sold and distributed in the U.S.A. and Canada by Kluwer Academic Publishers, 1984. LC # QB858.7 .C58 1984. ISBN # 9027717729. P.499, 1984 | |
| Publication Date: | 00/1984 | |
| Origin: | ADS | |
| Comment: | ISBN: 9027717729 | |
| Bibliographic Code: | 1984ASSL..111..499C |
Abstract
Computer simulations of the evolution of clusters and of groups (including degrees of freedom internal to galaxies) test how the dissipationless clustering scenario meets the challenge posed by the observed variety of morphologies and structures.
| Title: | Condensations and Cavities | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Publication: | Early Evolution of the Universe and its Present Structure, Proceedings of IAU Symposium No. 104, held 30 August – 2 September 1982 in Kolymbari, Greece. Edited by G.O. Abell and G. Chincarini. Dordrecht: D. Reidel Publishing Co., p.217, 1983 | |
| Publication Date: | 00/1983 | |
| Origin: | KNUDSEN | |
| Bibliographic Code: | 1983IAUS..104..217O |
Abstract
Not Available
| Title: | Forecasting isocurvature models with CMB lensing information: Axion and curvaton scenarios | |
| Authors: | Santos, L.; Cabella, P.; Balbi, A.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata,†Via della Ricerca Scientica 1, 00133 Roma, Italy), AB(Dipartimento di Fisica, Università di Roma “Tor Vergata,†Via della Ricerca Scientica 1, 00133 Roma, Italy), AC(Dipartimento di Fisica, Università di Roma “Tor Vergata†and INFN, Sezione di Roma Tor Vergata, Via della Ricerca Scientica 1, 00133 Roma, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata†and INFN, Sezione di Roma Tor Vergata, Via della Ricerca Scientica 1, 00133 Roma, Italy) | |
| Publication: | Physical Review D, vol. 86, Issue 2, id. 023002 (PhRvD Homepage) | |
| Publication Date: | 07/2012 | |
| Origin: | APS | |
| PACS Keywords: | Background radiations | |
| DOI: | 10.1103/PhysRevD.86.023002 | |
| Bibliographic Code: | 2012PhRvD..86b3002S |
Abstract
Some inflationary models predict the existence of isocurvature primordial fluctuations, in addition to the well known adiabatic perturbation. Such mixed models are not yet ruled out by available data sets. In this paper we explore the possibility of obtaining better constraints on the isocurvature contribution from future astronomical data. We consider the axion and curvaton inflationary scenarios, and use Planck satellite experimental specifications together with the Sloan Digital Sky Survey galaxy survey to forecast for the best parameter error estimation by means of the Fisher information matrix formalism. In particular, we consider how cosmic microwave background (CMB) lensing information can improve this forecast. We found substantial improvements for all the considered cosmological parameters. In the case of isocurvature amplitude this improvement is strongly model-dependent, varying between less than 1% and above 20% around its fiducial value. Furthermore, CMB lensing enables the degeneracy break between the isocurvature amplitude and correlation phase in one of the models. In this sense, CMB lensing information will be crucial in the analysis of future data.
Abstract
We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N < 5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 < z < 0.94, demonstrating Planck’s capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using YX as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the YSZ-YX relation, with a turnover at YSZ ~ 4 × 10-4 arcmin2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the YX vs. YSZ and X-ray flux FX vs. YSZ relations.
| Title: | The millimeter sky as seen with BOOMERanG | |
| Authors: | Masi, S.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Cabella, P.; Contaldi, C. R.; Crill, B. P.; de Bernardis, P.; de Gasperis, G.; de Oliveira-Costa, A.; de Troia, G.; di Stefano, G.; Ehlers, P.; Hivon, E.; Hristov, V.; Iacoangeli, A.; Jaffe, A. H.; Jones, W. C.; Kisner, T. S.; Lange, A. E.; MacTavish, C. J.; Marini Bettolo, C.; Mason, P.; Mauskopf, P. D.; Montroy, T. E.; Nati, F.; Nati, L.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Prunet, S.; Ricciardi, S.; Romeo, G.; Ruhl, J. E.; Santini, P.; Tegmark, M.; Torbet, E.; Veneziani, M.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AB(Department of Physics and Astronomy, Cardiff University, Wales, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, CalTech, Pasadena, CA, USA), AD(Canadian Institute for Theoretical Astrophysics, University of Toronto, Canada), AE(Computational Research Division, LBNL, Berkeley, CA, USA; Space Sciences Laboratory, UC Berkeley, CA, USA), AF(IFAC-CNR, Firenze, Italy), AG(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AH(Canadian Institute for Theoretical Astrophysics, University of Toronto, Canada; Theoretical Physics Group, Imperial College, London, UK), AI(IPAC, CalTech, Pasadena, CA, USA), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy), AK(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AL(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), AM(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AN(Theoretical Physics Group, Imperial College, London, UK), AO(Physics Department, University of Toronto, Toronto, Ont., Canada), AP(IPAC, CalTech, Pasadena, CA, USA), AQ(Observational Cosmology, CalTech, Pasadena, CA, USA), AR(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AS(Theoretical Physics Group, Imperial College, London, UK), AT(Observational Cosmology, CalTech, Pasadena, CA, USA), AU(Physics Department, Case Western Reserve University, Cleveland, OH, USA; Department of Physics, University of California, Santa Barbara, CA, USA), AV(Observational Cosmology, CalTech, Pasadena, CA, USA), AW(Canadian Institute for Theoretical Astrophysics, University of Toronto, Canada), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Observational Cosmology, CalTech, Pasadena, CA, USA), AZ(Department of Physics and Astronomy, Cardiff University, Wales, UK), BA(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BB(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BC(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BD(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy), BE(Physics Department, University of Toronto, Toronto, Ont., Canada), BF(Physics Department, University of Toronto, Toronto, Ont., Canada), BG(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BH(Department of Physics, University of Alberta, Edmonton, AB, Canada), BI(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BJ(Institut d’Astrophysique, Paris, France), BK(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BL(Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy), BM(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BN(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BO(Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA), BP(Physics Department, Case Western Reserve University, Cleveland, OH, USA), BQ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BR(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy) | |
| Publication: | New Astronomy Reviews, Volume 51, Issue 3-4, p. 236-243. (NewAR Homepage) | |
| Publication Date: | 03/2007 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/j.newar.2006.11.063 | |
| Bibliographic Code: | 2007NewAR..51..236M |
Abstract
BOOMERanG is a balloon-borne, mm-wave scanning telescope, which measured the first images of the CMB with sub-horizon resolution in 1998. In 2003 the instrument has been flown again with polarization sensitive bolometers, and has produced maps of the Stokes parameters I, Q, U of the microwave sky. Three regions of the southern sky were surveyed: a deep (˜90 square degrees) and a shallow survey (˜750 square degrees) at high Galactic latitudes, and a survey of ˜300 square degrees across a southern section of the Galactic plane. The experiment measured simultaneously three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ˜10′. The 145 GHz temperature maps are dominated by Cosmic Microwave Background (CMB) anisotropy, which is mapped with high signal to noise ratio. The map is consistent with the pattern measured in the same region by BOOMERanG-98 and by WMAP. At 145 GHz, in the high latitude surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps. The Q and U maps at high latitudes are dominated by detector noise: a power spectrum analysis allows us to extract from the maps a significant CMB polarization signal.
| Title: | Detection of Anisotropy in the Cosmic Microwave Background at Horizon and Sub-Horizon Scales with the BOOMERanG Experiment | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Pongetti, F.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Publication: | New Cosmological Data and the Values of the Fundamental Parameters, Proceedings of IAU Symposium #201, held 7-11 August 2000 at Manchester, United Kingdom. Edited by A. Lasenby and A. Wilkinson. San Francisco, CA: Astronomical Society of the Pacific (ASP), 2005., p.55 | |
| Publication Date: | 00/2005 | |
| Origin: | ADS | |
| Comment: | ISBN: 1583812121 | |
| Bibliographic Code: | 2005IAUS..201…55D |
Abstract
BOOMERanG has recently resolved with high signal to noise sub-horizon structures on the last scattering surface at z=1000. We shortly review the technical advances which made this possible, and we focus on the current results for maps and power spectra, with special attention to the determination of the total mass-energy density in the Universe.
| Title: | What’s behind acoustic peaks in the cosmic microwave background anisotropies | |
| Authors: | Baccigalupi, C.; Balbi, A.; Matarrese, S.; Perrotta, F.; Vittorio, N. | |
| Affiliation: | AA(SISSA/ISAS, Via Beirut 2-4, 34014 Trieste, Italy), AB(SISSA/ISAS, Via Beirut 2-4, 34014 Trieste, Italy), AC(SISSA/ISAS, Via Beirut 2-4, 34014 Trieste, Italy), AD(SISSA/ISAS, Via Beirut 2-4, 34014 Trieste, Italy), AE(SISSA/ISAS, Via Beirut 2-4, 34014 Trieste, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 110, p. 173-178. | |
| Publication Date: | 07/2002 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/S0920-5632(02)80119-0 | |
| Bibliographic Code: | 2002NuPhS.110..173B |
Abstract
We give a brief review of the physics of acoustic oscillations in Cosmic Microwave Background (CMB) anisotropies. As an example of the impact of their detection in cosmology, we show how the present data on CMB angular power spectrum on sub-degree scales can be used to constrain dark energy cosmological models.
| Title: | The new images of the microwave sky: a concordance cosmology ? | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Contaldi, C. R.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Jones, W. C.; Lange, A. E.; Martinis, L.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Montroy, T.; Natoli, P.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Pongetti, F.; Prunet, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AB(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AC(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AD(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AE(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AF(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AG(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AH(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AI(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AJ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AK(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AL(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AM(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AN(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AO(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AP(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AQ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AR(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AS(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AT(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AU(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AV(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AW(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AX(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AY(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), AZ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BA(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BB(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BC(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BD(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BE(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BF(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BG(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BH(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BI(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BJ(Dipartimento di Fisica, Università La Sapienza, Roma, Italy), BK(Dipartimento di Fisica, Università La Sapienza, Roma, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 110, p. 128-136. | |
| Publication Date: | 07/2002 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/S0920-5632(02)80112-8 | |
| Bibliographic Code: | 2002NuPhS.110..128D |
Abstract
The existence and anisotropy of the cosmic microwave background (CMB), the large scale distribution of Galaxies, the expansion of the Universe and the abundance of light elements can be all be explained with a single cosmological model. In this paper we focus on the CMB anisotropy maps produced by the BOOMERanG experiment and on their impact on cosmology. The images are consistent with the result of acoustic oscillations of the photons-matter plasma in the pre-recombination Universe (z >~ 1000). We show how the instrument and the observations have been optimized and how the basic parameters of the model are derived from the data. These observations of the CMB are gaussian and point to a low curvature Universe (ω ~ 1), as expected in the inflation scenario. In order to fit these observations and other cosmological evidence, the composition of the Universe must have significant contributions from dark matter (ω m ~ 0.3) and dark energy (ωΛ ~ 0.7).
| Title: | CMB polarization: Scientific case and data analysis issues | |
| Authors: | Balbi, A.; Cabella, P.; de Gasperis, G.; Natoli, P.; Vittorio, N. | |
| Affiliation: | AA(INFN, Sezione di Roma II; Dipartimento di Fisica, Università Tor Vergata, Roma I-00133, Italy), AB(Dipartimento di Fisica, Università Tor Vergata, Roma I-00133, Italy), AC(Dipartimento di Fisica, Università Tor Vergata, Roma I-00133, Italy), AD(INFN, Sezione di Roma II; Dipartimento di Fisica, Università Tor Vergata, Roma I-00133, Italy), AE(INFN, Sezione di Roma II; Dipartimento di Fisica, Università Tor Vergata, Roma I-00133, Italy) | |
| Publication: | ASTROPHYSICAL POLARIZED BACKGROUNDS: Workshop on Astrophysical Polarized Backgrounds, held 9-12 October, 2001 in Bologna Italy. Edited by Stefano Cecchini, Stefano Cortiglioni, Robert Sault, and Carla Sbarra. Melville, NY: American Institute of Physics, 2002.. AIP Conference Proceedings, Volume 609, pp. 78-83 (2002). (AIPC Homepage) | |
| Publication Date: | 03/2002 | |
| Origin: | STI | |
| PACS Keywords: | Background radiations, Radiation mechanisms; polarization, Artificial Earth satellites, Radio, microwave | |
| DOI: | 10.1063/1.1471827 | |
| Bibliographic Code: | 2002AIPC..609…78B |
Abstract
We review the science case for studying CMB polarization. We then discuss the main issues related to the analysis of forth-coming polarized CMB data, such as those expected from balloon-borne (e.g. BOOMERanG) and satellite (e.g., Planck) experiments. .
| Title: | Images of the early universe from the BOOMERanG experiment | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Polenta, G.; Pogosyan, D.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AB(Department of Physics, Queen Mary and Westfield College, Mile End Road, London, E1 4NS, United Kingdom), AC(Jet Propulsion Laboratory, Pasadena, California), AD(CITA, University of Toronto, Canada), AE(NERSC-LBNL, Berkeley, California; Center for Particle Astrophysics, University of California at Berkeley, 301 Le Conte Hall, Berkeley, California 94720), AF(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy), AG(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106), AH(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125), AI(Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica I, 00133 Roma, Italy), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AK(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106), AL(Astrophysics, University of Oxford, Keble Road, OX1 3RH, United Kingdom), AM(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125; PCC, College de France, 11 pl. Marcelin Berthelot, 75231 Paris Cedex 05, France), AN(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AO(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125), AP(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125), AQ(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AR(Center for Particle Astrophysics, University of California at Berkeley, 301 Le Conte Hall, Berkeley, California 94720), AS(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125), AT(ENEA Centro Ricerche di Frascati, Via E. Fermi 45, 00044 Frascati, Italy), AU(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AV(California Institute of Technology, Mail Code: 59-33, Pasadena, California 91125), AW(Physics and Astronomy Department, Cardiff University, United Kingdom; Department of Physics and Astronomy, University of Massachusetts Amherst, Massachusetts), AX(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), AY(Departments of Physics and Astronomy, University of Toronto, Canada), AZ(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106), BA(Departments of Physics and Astronomy, University of Toronto, Canada), BB(IROE-CNR, Via Panciatichi 64, 50127 Firenze, Italy), BC(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BD(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BE(CITA, University of Toronto, Canada), BF(CITA, University of Toronto, Canada), BG(Istituto Nazionale di Geofisica, Via di Vigna Murata 605, 00143, Roma, Italy), BH(Istituto Nazionale di Geofisica, Via di Vigna Murata 605, 00143, Roma, Italy), BI(Department of Physics, University of California at Santa Barbara, Santa Barbara, California 93106), BJ(ENEA Centro Ricerche di Frascati, Via E. Fermi 45, 00044 Frascati, Italy), BK(Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, 00185 Roma, Italy), BL(Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica I, 00133 Roma, Italy) | |
| Publication: | RELATIVISTIC ASTROPHYSICS: 20th Texas Symposium. AIP Conference Proceedings, Volume 586, pp. 157-171 (2001). (AIPC Homepage) | |
| Publication Date: | 10/2001 | |
| Origin: | AIP | |
| PACS Keywords: | Cosmology, Observation and data reduction techniques; computer modeling and simulation, Astronomical observations, Background radiations | |
| DOI: | 10.1063/1.1419548 | |
| Bibliographic Code: | 2001AIPC..586..157D |
Abstract
.
| Title: | The Deepest Field | |
| Authors: | de Bernardis, P.; Ade, P. A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Crill, B. P.; de Gasperis, G.; de Troia, G.; Farese, P. C.; Ferreira, P. G.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, P. D.; Melchiorri, A.; Miglio, L.; Montroy, T.; Netterfield, C. B.; Pascale, E.; Piacentini, F.; Pogosyan, D.; Polenta, G.; Pongetti, F.; Prunet, S.; Rao, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.; Sforna, D.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AB(Department of Physics, Queen Mary and Westfield College, London, UK), AC(Jet Propulsion Laboratory, Pasadena, CA, USA), AD(CITA University of Toronto, Canada), AE(NERSC-LBNL, Berkeley, CA, USA, and Center for Particle Astrophysics, University of California at Berkeley, USA), AF(IROE – CNR, Via Panciatichi 64, 50127 Firenze, Italy), AG(Department of Physics, University of California at Santa Barbara, USA), AH(California Institute of Technology, Pasadena, USA), AI(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy), AJ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AK(Department of Physics, University of California at Santa Barbara, USA), AL(Astrophysics, University of Oxford, UK), AM(California Institute of Technology, Pasadena, USA, and 12 PCC, College de France, Paris, France), AN(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AO(California Institute of Technology, Pasadena, USA), AP(California Institute of Technology, Pasadena, USA), AQ(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AR(Center for Particle Astrophysics, University of California at Berkeley, USA), AS(California Institute of Technology, Pasadena, USA), AT(ENEA Centro Ricerche di Frascati, Italy), AU(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AV(California Institute of Technology, Pasadena, USA), AW(Physics and Astronomy Dept, Cardiff University, UK), AX(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), AY(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy, and Departments of Physics and Astronomy, University of Toronto, Canada), AZ(Department of Physics, University of California at Santa Barbara, USA), BA(Departments of Physics and Astronomy, University of Toronto, Canada), BB(IROE – CNR, Via Panciatichi 64, 50127 Firenze, Italy), BC(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BD(CITA University of Toronto, Canada), BE(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BF(Istituto Nazionale di Geofisica, Roma, Italy), BG(CITA University of Toronto, Canada), BH(Istituto Nazionale di Geofisica, Roma, Italy), BI(Istituto Nazionale di Geofisica, Roma, Italy), BJ(Department of Physics, University of California at Santa Barbara, USA), BK(ENEA Centro Ricerche di Frascati, Italy), BL(Dipartimento di Fisica, Università di Roma La Sapienza, Roma, Italy), BM(Dipartimento di Fisica, Università di Roma Tor Vergata, Roma, Italy) | |
| Publication: | Deep Fields: Proceedings of the ESO Workshop Held at Garching, Germany, 9-12 October 2000, ESO ASTROPHYSICS SYMPOSIA. ISBN 3-540-42799-6. Edited by S. Cristiani, A. Renzini, and R.E. Williams. Springer-Verlag, 2001, p. 362 | |
| Publication Date: | 00/2001 | |
| Origin: | AUTHOR; SPRINGER | |
| Abstract Copyright: | (c) 2001: Springer-Verlag | |
| Comment: | ISBN: 3-540-42799-6 | |
| DOI: | 10.1007/10854354_101 | |
| Bibliographic Code: | 2001defi.conf..362D |
Abstract
The Cosmic Microwave Background (CMB) anisotropy experiments are starting to map the last scattering surface at z ˜ 1100 with significant detail and accuracy. Here we focus on the results of the BOOMERanG experiment, which mapped the CMB over ˜ 3% of the sky, detecting hundreds of hot and cold spots in the microwave sky. The analysis of the characteristic sizes and shapes of the temperature fluctuations provides direct evidence for acoustic oscillations in the primeval plasma and for a flat geometry of our universe.
| Title: | Limits on the gravitational-wave contribution from the cosmic microwave background anisotropies | |
| Authors: | Melchiorri, A.; Sazhin, M. V.; Shulga, V. V.; Vittorio, N. | |
| Publication: | Nuclear Physics B Proceedings Supplements, Vol. 80, Proceedings of the Texas Symposium on Relativistic Astrophysics and Cosmology held in Paris, France, 14-18 December, 1998. CDROM contents., p.02/06 | |
| Publication Date: | 01/2000 | |
| Origin: | ADS | |
| Bibliographic Code: | 2000NuPhS..80C0206M |
Abstract
Not Available
| Title: | X-ray spectra from hot thin plasmas: first results from a new, updated plasma code | |
| Authors: | Mazzotta, P.; Mazzitelli, P.; Colafrancesco, S.; Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy), AB(Associazione EURATOM-ENEA sulla Fusione, C.R. Frascati, CP 65-00044 Frascati Roma, Italy), AC(Osservatorio Astronomico di Roma, via dell’Osservatorio, 00040 Monteporzio, Italy), AD(Dipartimento di Fisica, Università di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 69, Issue 1-3, p. 585-588. | |
| Publication Date: | 01/1999 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/S0920-5632(98)00300-4 | |
| Bibliographic Code: | 1999NuPhS..69..585M |
Abstract
We present in this paper new and updated calculations of the ionization equilibrium for all the elements from He to Ni. Moreover, we discuss some preliminary results on the application of such calculations to a new spectral code for the X-ray continuum and line emission from hot plasmas.
| Title: | Evolution of distant X-ray clusters of galaxies: the BeppoSAX data | |
| Authors: | Colafrancesco, S.; Antonelli, A.; Mazzotta, P.; Vittorio, N. | |
| Affiliation: | AA(Osservatorio Astronomico di Roma, Via dell’Osservatorio 2, 00040 Monteporzio, Italy), AB(II Università di Roma “Tor Vergata”, Roma, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 69, Issue 1-3, p. 573-580. | |
| Publication Date: | 01/1999 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/S0920-5632(98)00295-3 | |
| Bibliographic Code: | 1999NuPhS..69..573C |
Abstract
We present the results of the Beppo-SAX observations of two distant z~0.3 galaxy clusters: A348 and A33. We outline the main results of the data analysis and discuss the cosmological relevance of these new data for the evolution of the Inter Galactic Medium (IGM) in distant clusters of galaxies.
| Title: | Ionization balance for optically thin plasmas (Mazzotta+ 1998) | |
| Authors: | Mazzotta, P.; Mazzitelli, G.; Colafrancesco, S.; Vittorio, N. | |
| Publication: | VizieR On-line Data Catalog: J/A+AS/133/403. Originally published in: 1998A&AS..133..403M | |
| Publication Date: | 07/1998 | |
| Origin: | SIMBAD | |
| Keywords: | Atomic physics | |
| Comment: | table1.dat 378×86 Fitting coefficients for dielectronic; recombination rates ; table2.dat 1138×181 Ionization equilibrium | |
| Bibliographic Code: | 1998yCat..41330403M |
Abstract
Fitting coefficients for dielectronic recombination rates of formula (7) of the paper are detailed in two tables. (2 data files).
| Title: | The T – L Correlation for Distant Galaxy Clusters | |
| Authors: | Colafrancesco, S.; Mazzotta, P.; Vittorio, N. | |
| Affiliation: | AA(Osservatorio Astronomico di Roma, Via dell’Osservatorio 2, Monteporzio (Roma), Italy), AB(Dip. di Fisica, II Università di Roma “Tor Vergata”, Roma, Italy), AC(Dip. di Fisica, II Università di Roma “Tor Vergata”, Roma, Italy) | |
| Publication: | Large Scale Structure: Tracks and Traces. Proceedings of the 12th Potsdam Cosmology Workshop, held in Potsdam, September 15th to 19th, 1997. Eds. V. Mueller, S. Gottloeber, J.P. Muecket, J. Wambsganss World Scientific 1998, p. 159-163. | |
| Publication Date: | 00/1998 | |
| Origin: | AUTHOR | |
| Bibliographic Code: | 1998lsst.conf..159C |
Abstract
In this paper we discuss the constrains that high-quality observations of clusters at $z \sim 0.3$ can pose on the evolution of their intra cluster (IC) gas and on the overall cosmological parameters.
| Title: | Intracluster comptonization of the CMB in CDM cosmologies. | |
| Authors: | Vittorio, N.; Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y. | |
| Publication: | 16th Moriond Astrophysics Meeting: Microwave background anisotropies, p. 401 – 406 | |
| Publication Date: | 00/1997 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Scattering, Cosmic Microwave Background: Clusters of Galaxies, Cosmic Microwave Background: Cosmology | |
| Bibliographic Code: | 1997mba..conf..401V |
Abstract
The authors present calculations of the mean sky-averaged Comptonization parameter describing the scattering of the CMB by hot gas in clusters of galaxies, in an array of flat and open CDM cosmologies. The models are globally normalized to fit cluster X-ray data, and the intracluster gas is assumed to have evolved in a manner consistent with current observations. The authors also discuss the rms temperature fluctuations induced by a population of evolving clusters. Finally, they predict the number counts of clusters across which a net flux (with respect to the CMB) higher than some limiting value can be detected. Such number counts are specifically predicted for the COBRAS/SAMBA mission.
| Title: | Evolution of clusters of galaxies. | |
| Authors: | Colafrancesco, S.; Vittorio, N.; Mazzotta, P. | |
| Publication: | 16th Moriond Astrophysics Meeting: Microwave background anisotropies, p. 395 – 400 | |
| Publication Date: | 00/1997 | |
| Origin: | ARI | |
| ARI Keywords: | Clusters of Galaxies: Evolution | |
| Bibliographic Code: | 1997mba..conf..395C |
Abstract
In this paper the authors discuss theoretical predictions for the local abundance of galaxy clusters and their evolution. They also discuss the constraints set by two different databases: the X-ray luminosity function and the temperature function.
| Title: | Imaging and calibration of the CMB anisotropies below 130 GHz. | |
| Authors: | Bersanelli, M.; Mandolesi, N.; Maino, D.; Vittorio, N.; Muciaccia, P. F.; Natoli, P. | |
| Publication: | 16th Moriond Astrophysics Meeting: Microwave background anisotropies, p. 173 – 178 | |
| Publication Date: | 00/1997 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Anisotropy | |
| Bibliographic Code: | 1997mba..conf..173B |
Abstract
The authors outline the main features of the COBRAS/SAMBA Low Frequency Instrument (LFI), which is designed to image the CMB anisotropies in the frequency range 30 – 130 GHz. The instrument is based on an array of corrugated feed horns coupled with passively cooled, low-noise HEMT receivers employing microwave integrated circuits technology. The authors describe the receiver concept and present simulations of the in-flight instrument calibration using the CMB dipole signal.
| Title: | N-body simulations of the large-scale structure of the universe in models with blue primordial perturbation spectra. | |
| Authors: | Moscardini, L.; Lucchin, F.; Colafrancesco, S.; de Gasperis, G.; Mei, S.; Vittorio, N.; Matarrese, S.; Mollerach, S. | |
| Publication: | Astrophysical Letters and Communications, Vol. 33, Nos. 1 – 5, p. 119 – 125 | |
| Publication Date: | 02/1996 | |
| Origin: | ARI | |
| ARI Keywords: | Universe: Large-Scale Structure, Universe: Dark Matter, Universe: Galaxy Clustering, N-Body Simulations: Cosmology | |
| Bibliographic Code: | 1996ApL&C..33..119M |
Abstract
Recently, there has been growing interest on primordial “blue” (n > 1) perturbation spectra, motivated both by a composite set of observational data on large scales (CMB anisotropies, bulk flows, etc.), and from the point of view of theoretical model building (e.g. hybrid inflation). In order to put some observational constraints on this type of spectra, both in the frame of purely Cold Dark Matter (CDM) and in Mixed Dark Matter (MDM) scenarios, the authors run N-body simulations and they study the spatial clustering properties and the peculiar velocities. The main results show that a blue MDM model can reproduce the APM-Stromlo variance of count-in-cells and the POTENT bulk flows; on the contraray, a pure CDM model with blue primordial spectrum produces too small-scale power.
| Title: | Dark Matter in the Universe: A Review (contribution not received) | |
| Authors: | Vittorio, N. | |
| Publication: | The Dark Side of the Universe; Experimental Efforts and Theoretical Framework, Proceedings of the Second Workshop held 13-14 November, 1995 in Roma, Italy. Edited by Rita Bernabei and Antonella Incicchitti. Singapore: World Scientific, 1996., p.1 | |
| Publication Date: | 00/1996 | |
| Origin: | ADS | |
| Bibliographic Code: | 1996dsu..conf….1V |
Abstract
Not Available
| Title: | Cosmology with clusters of galaxies | |
| Authors: | Colafrancesco, S.; Antonuccio-Delogu, V.; Vittorio, N. | |
| Publication: | Memorie della Società Astronomia Italiana, Vol. 66, p.183 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995MmSAI..66..183C |
Abstract
Not Available
| Title: | Large Scale Structure of the Universe from Blue Primordial Perturbation Spectra | |
| Authors: | Moscardini, L.; Lucchin, F.; Colafrancesco, S.; de Gasperis, G.; Mei, S.; Vittorio, N.; Matarrese, S.; Mollerach, S. | |
| Publication: | Large Scale Structure in the Universe, Proceedings of an International Workshop, held in Potsdam, Germany, 18-24 September 1994. Edited by Jan P. Mücket, Stefan Gottloeber, and Volker Müller. Singapore: World Scientific, 1995, p.128 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995lssu.conf..128M |
Abstract
Not Available
| Title: | Cosmic microwave background anisotropies and structure formation in the universe. | |
| Authors: | Vittorio, N. | |
| Publication: | Extragalactic Background Radiation Meeting, p. 209 – 222 | |
| Publication Date: | 00/1995 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Anisotropy, Cosmic Microwave Background: Clusters of Galaxies | |
| Bibliographic Code: | 1995ebr..proc..209V |
Abstract
The author discusses the implications of the COBE/DMR detection of cosmic microwave background anisotropies on inflationary models for the large scale structure of the universe. The author also discusses the constraints set on these models from current upper limits on, and recent detection of cosmic microwave background anisotropies at small and intermediate angular scales, and from the local abundance of X-ray galaxy clusters.
| Title: | Observational constraints on blue primordial spectra | |
| Authors: | Moscardini, L.; Colafrancesco, S.; de Gasperis, G.; Lucchin, F.; Matarrese, S.; Mei, S.; Mollerach, S.; Vittorio, N. | |
| Publication: | Clustering in the Universe, Proceedings of the 30th Rencontres de Moriond, Moriond Astrophysics Meeting, held in Les Arcs, Savoie, France, March 11-18, 1995. Edited by S. Maurogordato, C. Balkowski, C. Tao, and J. Tran Thanh Van. Paris: Editions Frontiers, 1995., p.221 | |
| Publication Date: | 00/1995 | |
| Origin: | ADS | |
| Bibliographic Code: | 1995clun.conf..221M |
Abstract
Not Available
| Title: | Capri CMB workshop | |
| Authors: | Bersanelli, M.; Cortiglioni, S.; Mandolesi, N.; Smoot, G. F.; Vittorio, N. | |
| Publication: | Proceedings of a workshop held in Anacapri (Capri), Italy, 20-24 September 1993, New York: Gordon and Breach Science Publishers, |c1995, edited by Bersanelli, M.; Cortiglioni, S.; Mandolesi, N.; Smoot, G.F.; Vittorio, N. | |
| Publication Date: | 00/1995 | |
| Origin: | ESO | |
| Keywords: | BACKGROUND RADIATION, MICROWAVE BACKGROUND, CONFERENCES | |
| Bibliographic Code: | 1995ccw..conf…..B |
Abstract
Not Available
| Title: | Cosmic microwave background anisotropies and the large scale structure of the universe | |
| Authors: | Vittorio, N. | |
| Affiliation: | AA(Dipartimento di Fisica, Università di Roma “Tor Vergata” Via della Ricerca Scientifica, 00133 Roma, Italy) | |
| Publication: | Nuclear Physics B Proceedings Supplements, Volume 35, p. 85-93. | |
| Publication Date: | 05/1994 | |
| Origin: | ELSEVIER | |
| DOI: | 10.1016/0920-5632(94)90226-7 | |
| Bibliographic Code: | 1994NuPhS..35…85V |
Abstract
We discuss the implications of the COBE/DMR detection of Cosmic Microwave Background anisotropies on inflationary models for the large scale structure of the universe. We also discuss the constraints set on these models from current upper limits on the Cosmic Microwave Background anisotropies at small and intermediate angular scales, and from the local abundance of X-ray galaxy clusters.
| Title: | Introduction | |
| Authors: | Silk, J.; Vittorio, N. | |
| Publication: | “Galaxy formation, International School of Physics “Enrico Fermi”, Proceedings of the International School of Physics “Enrico Fermi”, course 122, Varenna on Lake Como, 21-31 July 1992, Amsterdam: North-Holland, |c1994, edited by Silk, Joseph; Vittorio, N, p.XI” | |
| Publication Date: | 01/1994 | |
| Origin: | ADS | |
| Bibliographic Code: | 1994gafo.confD..11S |
Abstract
Not Available
| Title: | Galaxy formation | |
| Authors: | Silk, Joseph; Vittorio, N. | |
| Publication: | “International School of Physics “Enrico Fermi”, Proceedings of the International School of Physics “Enrico Fermi”, course 122, Varenna on Lake Como, 21-31 July 1992, Amsterdam: North-Holland, |c1994, edited by Silk, Joseph; Vittorio, N.” | |
| Publication Date: | 00/1994 | |
| Origin: | ESO | |
| Keywords: | GALAXY FORMATION, MICROWAVE BACKGROUND, LARGE SCALE STRUCTURE, COSMOLOGY, CONFERENCES | |
| Bibliographic Code: | 1994gafo.conf…..S |
Abstract
Not Available
| Title: | Cosmic microwave background anisotropies and the large scale structure of the universe. | |
| Authors: | Vittorio, N. | |
| Publication: | “The Dark Side of the Universe – Experimental Efforts | |
| Publication Date: | 00/1994 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Anisotropy, Cosmic Microwave Background: Universe, Large-Scale Structure: Universe | |
| Bibliographic Code: | 1994dsu..conf….1V |
Abstract
The author discusses the implications of the COBE/DMR detection of cosmic microwave background anisotropies on inflationary models for the large scale structure of the universe. She also discusses the constraints set on these models from current upper limits on the cosmic microwave background anisotropies at small and intermediate angular scales.
| Title: | The large scale structure of the Universe | |
| Authors: | Vittorio, N. | |
| Publication: | Memorie della Società Astronomia Italiana, Vol. 64, p.909 | |
| Publication Date: | 00/1993 | |
| Origin: | ADS | |
| Bibliographic Code: | 1993MmSAI..64..909V |
Abstract
Not Available
| Title: | Cosmic Microwave Background Anisotropies and Structure Formation in the Universe | |
| Authors: | Vittorio, N. | |
| Publication: | Extragalactic Background Radiation: A Meeting in Honor of Riccardo Giacconi, Proceedings of the Space Telescope Science Institute Symposium, held in Baltimore, Maryland May 18–20, 1993, Ed. by Daniela Calzetti, Mario Livio, and Piero Madau, Cambridge University Press, p. 209. | |
| Publication Date: | 00/1993 | |
| Origin: | AUTHOR | |
| Bibliographic Code: | 1993ebr..proc..209V |
Abstract
Not Available
| Title: | Book-Review – the Cosmic Microwave Background – 25 Years | |
| Authors: | Mandolesi, N.; Vittorio, N.; Kaufmann, P. | |
| Publication: | Space Science Reviews, Vol. 59, NO. 3/4, P.411, 1992 (SSRv Homepage) | |
| Publication Date: | 00/1992 | |
| Origin: | KNUDSEN | |
| Bibliographic Code: | 1992SSRv…59..411M |
Abstract
Not Available
| Title: | Large scale anisotropy of the cosmic microwave background | |
| Authors: | Vittorio, N.; et al. | |
| Publication: | “Physical Cosmology, Proceedings of the 2nd Rencontresde Blois: “25th Anniversary of the Cosmic Background Radiation Discovery”, Chateau de Blois, France, August 28th – September 1st, 1990. Edited by Alain Blanchard. L. Celnikier, M. Lachieze-Rey and J. Tran Thanh Van. Gif-sur-Yvette: Editions Frontieres, 1991, p.135″ | |
| Publication Date: | 00/1991 | |
| Origin: | ADS | |
| Bibliographic Code: | 1991phco.conf..135V |
Abstract
Not Available
| Title: | Cold Dark Matter Cosmologies and Cosmic Microwave Background Anisotropy at Small and Intermediate Angular Scales | |
| Authors: | Vittorio, N.; Muciaccia, P. F. | |
| Publication: | Astroparticle Physics, Proceeings of the International School of Astroparticle Physics held 6-12 January, 1991 at the Houston Advanced Research Center (HARC). Edited by D.V. Nanopoulos. Singapore: World Scientific, 1991., p.321 | |
| Publication Date: | 00/1991 | |
| Origin: | ADS | |
| Bibliographic Code: | 1991asph.conf..321V |
Abstract
Not Available
| Title: | Cosmological background radiation. | |
| Authors: | Vittorio, N.; Lachièze-Rey, M. | |
| Publication: | Recherche, Vol. 21, No. 227, p. 1468 – 1475 | |
| Publication Date: | 12/1990 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmic Microwave Background: Cosmology | |
| Bibliographic Code: | 1990Rech…21.1468V |
Abstract
Not Available
| Title: | Book-Review – the Cosmic Microwave Background – 25 Years Later | |
| Authors: | Mandolesi, N.; Vittorio, N. | |
| Publication: | Journal of the British Astronomical Society, Vol.100, NO. 6/DEC, P.316, 1990 (JBAA Homepage) | |
| Publication Date: | 12/1990 | |
| Origin: | KNUDSEN | |
| Bibliographic Code: | 1990JBAA..100Q.316M |
Abstract
Not Available
| Title: | The large-scale structure of the Universe: theory and observatioal constraints | |
| Authors: | Silk, J.; Vittorio, N. | |
| Publication: | “Confrontation between Theories and Observations in Cosmology: Present Status and Future Programmes. International School of Physics “Enrico Fermi”, Proceedings of the International School of Physics “Enrico Fermi”, course 105, Varenna on Lake Como, July 21-31, 1987, Amsterdam: North-Holland, Edited by Jean Audouze, 1990., p.137″ | |
| Publication Date: | 00/1990 | |
| Origin: | ADS | |
| Bibliographic Code: | 1990cbto.conf..137S |
Abstract
Introduction Observational cosmology The expansion of the Universe The redshift-magnitude test The number count test The density of luminous matter Primordial nucleosynthesis The cosmic black-body radiation Dark matter Prediction from inflation Particle physics candidates Large-scale structure Galaxy correlations Peculiar velocities Cluster correlations Hubble bubbles Large-scale streaming motions Origin of large-scale structure Particle physics cosmology Primordial fluctuations Pertubation theory Introduction Growth rate Protential fluctuations Peculiar velocity Collisional fluid: baryons and radiation before recombination Collisionless medium: weakly interacting massive particles Random Gaussian field Definition Fourier analysis Potential fluctuations Peculiar velocity Statistics The general approach Normalization Scenarios Hot and cold dark matter Biasing Pancakes, strings and explosions Large-scale peculiar velocity field CMB dipole anisotropy Virgocentric infall Large-scale drifts Theoretical implications Model predictions The cosmic microwave background Introduction Large-scale anisotropy Intermediate-angular-scale anisotropy Small-scale anisotropy Statistics Galaxy formation Dissipation Biasing and dwarfs Morphology Conclusions
| Title: | Monte Carlo Simulations of a CBR Anisotropy Experiment | |
| Authors: | Vittorio, N.; de Bernardis, P.; Masi, S.; Scaramella, R. | |
| Publication: | Large Scale Structure and Motions in the Universe, Proceedings of an International meeting held in Trieste, Italy, April 6-9, 1988. Edited by M. Mezzetti, G. Giuricin, F. Mardirossian, M. Ramella. ISBN 0-7923-0082-3; 1989, Astrophysics and Space Science Library, Vol. 151, p.455 | |
| Publication Date: | 00/1989 | |
| Origin: | ADS | |
| Comment: | ISBN: 0-7923-0082-3 | |
| Bibliographic Code: | 1989ASSL..151..455V |
Abstract
Not Available
| Title: | On the Large Scale Anisotropy of the Cosmic Microwave Background | |
| Authors: | Scaramella, R.; Vittorio, N. | |
| Publication: | Large Scale Structure and Motions in the Universe, Proceedings of an International meeting held in Trieste, Italy, April 6-9, 1988. Edited by M. Mezzetti, G. Giuricin, F. Mardirossian, M. Ramella. ISBN 0-7923-0082-3; 1989, Astrophysics and Space Science Library, Vol. 151, p.435 | |
| Publication Date: | 00/1989 | |
| Origin: | ADS | |
| Comment: | ISBN: 0-7923-0082-3 | |
| Bibliographic Code: | 1989ASSL..151..435S |
Abstract
Not Available
| Title: | Discussion Panel: X-Ray Background – An Important Cosmological Signal | |
| Authors: | Cowsik, R.; Mandelbrot, B.; Primack, J.; Salpeter, E. E.; Sato, H.; Vittorio, N. | |
| Publication: | Large Scale Structures of the Universe: Proceedings of the 130th Symposium of the International Astronomical Union, dedicated to the memory of Marc A. Aaronson (1950-1987) held in Balatonfured, Hungary, June 15-20, 1987. Edited by Jean Audouze, Marie-Christine Pelletan and Sandor Szalay. International Astronomical Union. Symposium no. 130, Kluwer Academic Publishers, Dordrecht, p.479-480 | |
| Publication Date: | 00/1988 | |
| Origin: | ADS | |
| Bibliographic Code: | 1988IAUS..130..479C |
Abstract
Not Available
| Title: | Large scale anisotropy of the infrared background – Primordial fluctuations vs. local emission | |
| Authors: | de Bernardis, P.; Masi, S.; Melchiorri, F.; Vittorio, N. | |
| Affiliation: | AA(Roma I, Università , Rome, Italy), AB(Roma I, Università , Rome, Italy), AC(Roma I, Università , Rome, Italy), AD(Roma I, Università , Rome, Italy) | |
| Publication: | IN: Texas Symposium on Relativistic Astrophysics, 13th, Chicago, IL, Dec. 14-19, 1986, Proceedings (A88-49551 21-90). Singapore and Teaneck, NJ, World Scientific Publishing Co., 1987, p. 236-239. | |
| Publication Date: | 00/1987 | |
| Category: | Astronomy | |
| Origin: | STI | |
| NASA/STI Keywords: | COSMIC DUST, COSMIC RAYS, GALACTIC EVOLUTION, INFRARED ASTRONOMY, MICROWAVES, RELIC RADIATION, ANISOTROPY, INFRARED ASTRONOMY SATELLITE, TEMPERATURE EFFECTS | |
| Bibliographic Code: | 1987txra.symp..236D |
Abstract
Results of studies on the cosmic microwave background large scale anisotropy are presented, assuming that density fluctuations are initially Gaussian distributed. A lower limit to the observable quadrupole anisotropy was derived, neglecting instrument noise and local effects. Maps of the dust emission at the millimeter wavelengths were produced assuming alpha between 1.5 and 2. The dust emissivity in the spherical harmonics was analyzed after subtracting the galactic plane from the full sky map. Preliminary results for the dipole and quadrupole component of the dust emission are given.
| Title: | List of Participants | |
| Authors: | Stodolsky, L.; Szalay, A.; Vittorio, N. | |
| Publication: | Cosmology and Particle Physics, Proceedings of the Theoretical Workshop on Cosmology and Particle Physics, held July 28th – August 15th, 1986, in Berkeley, Ca. Edited by Ian Hinchliffe. Singapore: World Scientific, 1987., p.201 | |
| Publication Date: | 00/1987 | |
| Origin: | ADS | |
| Bibliographic Code: | 1987cpp..conf..201S |
Abstract
Not Available
| Title: | Double inflation: A possible resolution of the large-scale structure problem | |
| Authors: | Turner, M. S.; Villumsen, J. V.; Vittorio, N.; Silk, J.; Juszkiewicz, R. | |
| Affiliation: | AA(Fermi National Accelerator Lab., Batavia, IL.), AB(Fermi National Accelerator Lab., Batavia, IL.), AC(Fermi National Accelerator Lab., Batavia, IL.), AD(Fermi National Accelerator Lab., Batavia, IL.), AE(Fermi National Accelerator Lab., Batavia, IL.) | |
| Publication: | Unknown | |
| Publication Date: | 11/1986 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | COMPUTERIZED SIMULATION, DARK MATTER, MODELS, UNIVERSE, COSMOLOGY, GALACTIC EVOLUTION, MASS | |
| Bibliographic Code: | 1986STIN…8720865T |
Abstract
A model is presented for the large-scale structure of the universe in which two successive inflationary phases resulted in large small-scale and small large-scale density fluctuations. This bimodal density fluctuation spectrum in an Omega = 1 universe dominated by hot dark matter leads to large-scale structure of the galaxy distribution that is consistent with recent observational results. In particular, large, nearly empty voids and significant large-scale peculiar velocity fields are produced over scales of approx 100 Mpc, while the small-scale structure over less than or equal to 10 Mpc resembles that in a low density universe, as observed. Detailed analytical calculations and numerical simulations are given of the spatial and velocity correlations.
| Title: | The large-scale peculiar velocity field in flat models of the universe | |
| Authors: | Vittorio, N.; Turner, M. S. | |
| Affiliation: | AA(California Univ., Berkeley.), AB(California Univ., Berkeley.) | |
| Publication: | Unknown | |
| Publication Date: | 10/1986 | |
| Category: | Astrophysics | |
| Origin: | STI | |
| NASA/STI Keywords: | MASS, MODELS, UNIVERSE, VELOCITY DISTRIBUTION, BIG BANG COSMOLOGY, DARK MATTER, RELATIVITY | |
| Bibliographic Code: | 1986STIN…8720864V |
Abstract
The inflationary Universe scenario predicts a flat Universe and both adiabatic and isocurvature primordial density perturbations with the Zel’dovich spectrum. The two simplest realizations, models dominated by hot or cold dark matter, seem to be in conflict with observations. Flat models are examined with two components of mass density, where one of the components of mass density is smoothly distributed and the large-scale (greater than or equal to 10h/1 MpC) peculiar velocity field for these models is considered. For the smooth component relativistic particles, a relic cosmological term, and light strings are considered. At present the observational situation is unsettled; but, in principle, the large-scale peculiar velocity field is a very powerful discriminator between these different models.
| Title: | Cosmic Microwave Background Radiation Anisotropies in Universes Dominated by Weakly Interacting Massive Particles | |
| Authors: | Vittorio, N. | |
| Publication: | Acta Cosmologica, Vol. 14, P. 25, 1986 | |
| Publication Date: | 00/1986 | |
| Origin: | KNUDSEN | |
| Bibliographic Code: | 1986AcC….14…25V |
Abstract
The cosmic microwave background (CMB) has proved to be one of the most important tests for galaxy formation theories. Density fluctuations, which later will evolve in galaxies and cluster of galaxies, necessarily induce angular anisotropies on the CMB at the epoch of the last scattering. The author evaluates the angular anisotropies on small, intermediate and large angular scales in universes dominated by a weakly interacting massive component. Since the residual fluctuation spectrum depends on the particle species, unique predictions are made for the anisotropy of the background radiation.
| Title: | Galaxy formation, nonbaryonic matter and cosmic strings. | |
| Authors: | Schramm, D. N.; Vittorio, N. | |
| Publication: | Comments Nucl. Part. Phys., Vol. 15, No. 1, p. 1 – 8 | |
| Publication Date: | 00/1985 | |
| Origin: | ARI | |
| ARI Keywords: | Cosmology:Dark Matter, Cosmology:Galaxy Formation, Dark Matter:Cosmology, Galaxy Formation:Cosmology | |
| Bibliographic Code: | 1985CNPPh..15….1S |
Abstract
Not Available
| Title: | Cold Dark Matter | |
| Authors: | Occhionero, F.; Achilli, S.; Scaramella, R.; Vittorio, N. | |
| Publication: | Bulletin of the American Astronomical Society, Vol. 16, p.487 | |
| Publication Date: | 03/1984 | |
| Origin: | ADS | |
| Bibliographic Code: | 1984BAAS…16..487O |
Abstract
Not Available
| Title: | Curvature Fluctuations as Progenitors of Largescale Holes | |
| Authors: | Vittorio, N.; Santangelo, P.; Occhionero, F. | |
| Publication: | Clusters and Groups of Galaxies. International Meeting held in Trieste, Italy, September 13-16, 1983. Editors, F. Mardirossian, G. Giuricin, M. Mezzetti; Publisher, D. Reidel Pub. Co., Dordrecht, Holland, Boston, MA, Hingham, MA, U.S.A. Sold and distributed in the U.S.A. and Canada by Kluwer Academic Publishers, 1984. LC # QB858.7 .C58 1984. ISBN # 9027717729. P.479, 1984 | |
| Publication Date: | 00/1984 | |
| Origin: | ADS | |
| Comment: | ISBN: 9027717729 | |
| Bibliographic Code: | 1984ASSL..111..479V |
Abstract
The authors extend previous work to study the formation and evolution of deep holes, under the assumption that they arise from curvature or energy perturbations in the Hubble flow. The algorithm, which makes use of the spherically symmetric and pressureless Tolman-Bondi solution, can embed a perturbation in any cosmological background. After recalling previous results on the central depth of the hole and its radial dimension, the authors give specific examples of density and peculiar velocity profiles, which may have a bearing on whether galaxy formation is a dissipative or dissipationless process.
| Title: | Radiation Perturbations in a Three Component Universe | |
| Authors: | Vittorio, N.; Occhionero, F.; Lucchin, F.; Bonometto, S. | |
| Publication: | Clusters and Groups of Galaxies. International Meeting held in Trieste, Italy, September 13-16, 1983. Editors, F. Mardirossian, G. Giuricin, M. Mezzetti; Publisher, D. Reidel Pub. Co., Dordrecht, Holland, Boston, MA, Hingham, MA, U.S.A. Sold and distributed in the U.S.A. and Canada by Kluwer Academic Publishers, 1984. LC # QB858.7 .C58 1984. ISBN # 9027717729. P.441, 1984 | |
| Publication Date: | 00/1984 | |
| Origin: | ADS | |
| Comment: | ISBN: 9027717729 | |
| Bibliographic Code: | 1984ASSL..111..441V |
Abstract
The authors study numerically the evolution of initial adiabatic perturbations in a universe with critical density containing three components: massive neutrinos or the like, baryonic matter and radiation. The evaluation at decoupling of the residual perturbation in the radiation field shows that the common expectations on the neutrino influence on the monopole and the dipole components are likely to be modified. Thus, the lack of detection of distortions in the cosmic microwave background may remain an unresolved problem.
| Title: | Spherical Simulations of the Cellular Structure of the Universe | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Publication: | General Relativity and Gravitation, Vol. 1, Classical Relativity. Proceedings of the 10th International Conference on General Relativity and Gravitation, held July 4-9, 1983, in Padova, Italy. Edited by B. Bertotti, F. de Felice and A. Pascolini. Published by Consiglio Nazionale delle Ricerche, Rome, 1983, p. 857 | |
| Publication Date: | 07/1983 | |
| Origin: | ADS | |
| Bibliographic Code: | 1983grg1.conf..857O |
Abstract
Not Available
| Title: | Mw Background Small Scale Fluctuations in Neutrino Dominated Universe Models | |
| Authors: | Bonometto, S. A.; Lucchin, F.; Occhionero, F.; Vittorio, N. | |
| Publication: | General Relativity and Gravitation, Vol. 1, Classical Relativity. Proceedings of the 10th International Conference on General Relativity and Gravitation, held July 4-9, 1983, in Padova, Italy. Edited by B. Bertotti, F. de Felice and A. Pascolini. Published by Consiglio Nazionale delle Ricerche, Rome, 1983, p. 793 | |
| Publication Date: | 07/1983 | |
| Origin: | ADS | |
| Bibliographic Code: | 1983grg1.conf..793B |
Abstract
Not Available
| Title: | Spherical voids in cosmology (Λ > 0). | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Publication: | Bulletin of the Astronomical Society, Vol. 15, No. 3, p. 878 | |
| Publication Date: | 06/1983 | |
| Origin: | ARI | |
| ARI Keywords: | Galaxy Voids:Universe, Universe:Galaxy Voids | |
| Bibliographic Code: | 1983BAAS…15..878O |
Abstract
Not Available
| Title: | Spherical simulations of the cellular structure of the universe | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Publication: | Clustering in the Universe, Proceedings of a Colloquium, held at Meudon Observatory, 1982. Edited by D. Gerbal and A. Mazure. Gif-sur-Yvette: Editions Frontieres, 1983., p.103 | |
| Publication Date: | 00/1983 | |
| Origin: | ADS | |
| Bibliographic Code: | 1983clun.proc..103O |
Abstract
The large scale holes observed in the Universe can be described by spherically symmetric perturbations in the Hubble flow; the pressureless Tolman-Bondi solution is apt to this purpose. Earlier work of the authors for an Einstein-de Sitter space is extended by determining a perturbation ansatz capable of digging a deep hole and of generating a mild density contrast in the surrounding ridge. The results are generalized to study the depth of the hole in arbitrary backgrounds.
| Title: | Spherical Voids in Cosmology | |
| Authors: | Occhionero, F.; Santangelo, P.; Vittorio, N. | |
| Publication: | Bulletin of the American Astronomical Society, Vol. 14, p.961 | |
| Publication Date: | 09/1982 | |
| Origin: | ADS | |
| Bibliographic Code: | 1982BAAS…14..961O |
Abstract
Not Available
| Title: | Synthetic clusters of galaxies: mapping of the intracluster gas from the X-ray emission. | |
| Authors: | Cavaliere, A.; de Biase, G. A.; Santangelo, P.; Vittorio, N. | |
| Publication: | Memorie della Societa Astronomica Italiana, Vol. 53, No. 1, p. 301 – 314 | |
| Publication Date: | 00/1982 | |
| Origin: | ARI | |
| ARI Keywords: | Clusters of Galaxies:Intergalactic Gas, Clusters of Galaxies:Models, Clusters of Galaxies:X Rays, Intergalactic Gas:Clusters of Galaxies, X Rays:Clusters of Galaxies | |
| Bibliographic Code: | 1982MmSAI..53..301C |
Abstract
The authors present synthetic maps of X-ray brightness from an interactive system of codes designed to model the fully 3-D configurations and the time evolution of galaxy clusters, including galaxies and the intracluster medium by a combination of a gravitational N-body model and a gas-dynamical code.
| Title: | Baryon and Massive Neutrino Normal Modes in a Massive Neutrino Dominated Universe | |
| Authors: | Occhionero, F.; Vittorio, N.; Boccadoro, M.; de Luca, S. | |
| Publication: | Bulletin of the American Astronomical Society, Vol. 13, p.844 | |
| Publication Date: | 03/1981 | |
| Origin: | ADS | |
| Comment: | A&AA ID. AAA031.162.162 | |
| Bibliographic Code: | 1981BAAS…13..844O |
Abstract
Not Available
| Title: | Dynamical Models for Clusters of Galaxies | |
| Authors: | Occhionero, F.; Veccia-Scavalli, L.; Vittorio, N. | |
| Publication: | Bulletin of the American Astronomical Society, Vol. 13, p.533 | |
| Publication Date: | 03/1981 | |
| Origin: | ADS | |
| Comment: | A&AA ID. AAA030.160.025 | |
| Bibliographic Code: | 1981BAAS…13..533O |
Abstract
Not Available
| Title: | Dynamical models for clusters of galaxies. | |
| Authors: | Occhionero, F.; Vignato, A.; Vittorio, N. | |
| Publication: | Stars and star systems, p. A14 | |
| Publication Date: | 00/1978 | |
| Origin: | ARI | |
| ARI Keywords: | Clusters of Galaxies:Models | |
| Comment: | A&AA ID. AAA026.160.050 | |
| Bibliographic Code: | 1978sss..meet..A14O |
Abstract
Not Available