PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

被引：194

作者：

Andre, Philippe

Baccigalupi, Carlo

Banday, Anthony

Barbosa, Domingos

Barreiro, Belen

Bartlett, James

Bartolo, Nicola

Battistelli, Elia

Battye, Richard

Bendo, George

Benoit, Alain

Bernard, Jean-Philippe

Bersanelli, Marco

Bethermin, Matthieu

Bielewicz, Pawel

Bonaldi, Anna

Bouchet, Francois

Boulanger, Francois

Brand, Jan

Bucher, Martin

Burigana, Carlo

Cai, Zhen-Yi

Camus, Philippe

Casas, Francisco

Casasola, Viviana

Castex, Guillaume

Challinor, Anthony

Chluba, Jens

Chon, Gayoung

Colafrancesco, Sergio

Comis, Barbara

Cuttaia, Francesco

D'Alessandro, Giuseppe

Da Silva, Antonio

Davis, Richard

de Avillez, Miguel

de Bernardis, Paolo

de Petris, Marco

de Rosa, Adriano

de Zotti, Gianfranco

Delabrouille, Jacques

Desert, Francois-Xavier

Dickinson, Clive

Diego, Jose Maria

Dunkley, Joanna

Ensslin, Torsten

Errard, Josquin

Falgarone, Edith

Ferreira, Pedro

Ferriere, Katia

机构：

[1] Laboratoire d’Astrophysique de Paris-Saclay, Gif-sur-Yvette Cedex

[2] SISSA, Via Bonomea 265, Trieste

[3] Université de Toulouse, UPS-OMP, IRAP, Toulouse cedex 4

[4] CNRS, IRAP, 9 Av. colonel Roche, BP 44346, Toulouse cedex 4

[5] Grupo de Radio Astronomia Basic Sciences & Enabling Technologies Instituto de Telecomunicações, Campus Universitario de Santiago, Aveiro

[6] Instituto de Fìsica de Cantabria (CSIC-Universidad de Cantabria) Avda. de los Castros s/n, Santander

[7] APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris, 10, rue Alice Domon et Léonie Duquet, Paris Cedex 13, Cité

[8] Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA

[9] Dipartimento di Fisica e Astronomia “G. Galilei”, Università degli studi di Padova, via Marzolo 8, Padova

[10] INFN, Sezione di Padova, via Marzolo 8, Padova

[11] Dipartimento di Fisica, Università di Roma La Sapienza, P.le A. Moro 2, Roma

[12] Jordell Bank Centre for Astrophysics, School of Physics & Astronomy, University of Manchester, Oxford Road, Manchester

[13] U.K. ALMA Regional Centre Node, Jordell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester

[14] Physics & Astronomy, University of Manchester, Oxford Road, Manchester

[15] Institut Néel, CNRS, Université Joseph Fourier Grenoble I, 25 rue des Martyrs, Grenoble

[16] Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano

[17] INAF/IASF Milano, Via E. Bassini 15, Milano

[18] European Southern Observatory, Karl-Schwarzschild-Str. 2, Garching

[19] Institut d’Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, Paris

[20] UPMC Univ Paris 06, UMR7095, 98 bis Boulevard Arago, Paris

[21] Institut d’Astrophysique Spatiale, CNRS, UMR8617, Université Paris-Sud 11, Bâtiment 121, Orsay

[22] INFN, Sezione di Ferrara, Ferrara

[23] INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, Bologna

[24] Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, Via Saragat 1, Ferrara

[25] Department of Astronomy, Xiamen University, Xiamen

[26] Center for Astrophysics, University of Science and Technology of China, Hefei

[27] INAF-Osservatorio Astronomico di Arcetri, Largo Enrico Fermi 5, Firenze

[28] Dipartimento di Fisica e Astronomia, Università di Bologna, Viale Berti Pichat 6/2, Bologna

[29] Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge

[30] Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge

[31] Centre for Theoretical Cosmology, DAMTP, University of Cambridge, Wilberforce Road, Cambridge

[32] Johns Hopkins University, Bloomberg Center 435, 3400 N Charles St, Baltimore

[33] Max-Planck-Institut Für Extraterrestriche Physik, Garching

[34] School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg

[35] Laboratoire de Physique Subatomique et de Cosmologie, Université Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de Grenoble, 53 rue des Martyrs, Grenoble cedex

[36] Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, Porto

[37] Department of Mathematics, University of Evora, R. Romao Ramalho 58, Evora

[38] Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstr. 36, Berlin

[39] INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova

[40] IPAG: Institut de Planétologie et d’Astrophysique de Grenoble, Université Joseph Fourier, Grenoble 1 / CNRS-INSU, UMR 5272, Grenoble

[41] Astrophysics, University of Oxford, Keble Road, Oxford

[42] Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Garching

[43] Lawrence Berkeley National Laboratory 1, Cyclotron Rd, MS 48R4047, Berkeley, 94718, 8151, CA

[44] LERMA, CNRS, Observatoire de Paris, 59 Avenue de l’Observatoire, Paris

[45] INFN, Sezione di Bologna, Via Irnerio 44, Bologna

[46] Institut de Ciencies de L’Espai (IEEC-CSIC), Facultat de Ciencies, Campus UAB, Torre C5, par 2a planta, Cerdanyola (Barcelona)

[47] Instituto de Fisica Teorica CSIC-UAM, c/ Nicolas Cabrera, 13 Universidad Autonoma de Madrid, Cantoblanco, Madrid

[48] Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh

[49] Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9008, Nijmegen

[50] Leiden Observatory, Leiden University, P.O. Box 9511, Leiden

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2014年 / 02期

关键词：

CMBR detectors; CMBR experiments; cosmological parameters from CMBR; MICROWAVE BACKGROUND SPECTRUM; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; DARK-MATTER; RELATIVISTIC CORRECTIONS; SUBMILLIMETER GALAXIES; THERMAL HISTORY; COSMOLOGICAL RECOMBINATION; MAGNETIC-FIELDS; HERSCHEL-ATLAS;

D O I：

10.1088/1475-7516/2014/02/006

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 10 6 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during inflation and from gravitational lensing, as well as the ultimate search for primordial non-Gaussianity using CMB polarization, which is less contaminated by foregrounds on small scales than the temperature anisotropies; (4) a search for distortions from a perfect blackbody spectrum, which include some nearly certain signals and others that are more speculative but more informative; and (5) a study of the role of the magnetic field in star formation and its interaction with other components of the interstellar medium of our Galaxy. These are but a few of the highlights presented here along with a description of the proposed instrument.

引用

页数：69

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