Planck intermediate results: XLIII. Spectral energy distribution of dust in clusters of galaxies

Tutkimustuotos: Lehtiartikkelivertaisarvioitu

Tutkijat

  • R. Adam
  • P. A R Ade
  • N. Aghanim
  • M. Ashdown
  • J. Aumont
  • C. Baccigalupi
  • A. J. Banday
  • R. B. Barreiro
  • N. Bartolo
  • E. Battaner
  • K. Benabed
  • A. Benoit-Lévy
  • M. Bersanelli
  • P. Bielewicz
  • I. Bikmaev
  • A. Bonaldi
  • J. R. Bond
  • J. Borrill
  • F. R. Bouchet
  • R. Burenin
  • C. Burigana
  • E. Calabrese
  • J. F. Cardoso
  • A. Catalano
  • H. C. Chiang
  • P. R. Christensen
  • E. Churazov
  • L. P L Colombo
  • C. Combet
  • B. Comis
  • F. Couchot
  • B. P. Crill
  • A. Curto
  • F. Cuttaia
  • L. Danese
  • R. J. Davis
  • P. De Bernardis
  • A. De Rosa
  • G. De Zotti
  • J. Delabrouille
  • F. X. Désert
  • J. M. Diego
  • H. Dole
  • O. Doré
  • M. Douspis
  • A. Ducout
  • X. Dupac
  • F. Elsner
  • T. A. Enßlin
  • F. Finelli
  • O. Forni
  • M. Frailis
  • A. A. Fraisse
  • E. Franceschi
  • S. Galeotta
  • K. Ganga
  • R. T. Génova-Santos
  • M. Giard
  • Y. Giraud-Héraud
  • E. Gjerløw
  • J. González-Nuevo
  • K. M. Górski
  • A. Gregorio
  • A. Gruppuso
  • J. E. Gudmundsson
  • F. K. Hansen
  • D. L. Harrison
  • C. Hernández-Monteagudo
  • D. Herranz
  • S. R. Hildebrandt
  • E. Hivon
  • M. Hobson
  • A. Hornstrup
  • W. Hovest
  • G. Hurier
  • A. H. Jaffe
  • T. R. Jaffe
  • W. C. Jones
  • E. Keihänen
  • R. Keskitalo
  • I. Khamitov
  • T. S. Kisner
  • R. Kneissl
  • J. Knoche
  • M. Kunz
  • H. Kurki-Suonio
  • G. Lagache
  • J. M. Lamarre
  • A. Lasenby
  • M. Lattanzi
  • C. R. Lawrence
  • R. Leonardi
  • F. Levrier
  • M. Liguori
  • P. B. Lilje
  • M. Linden-Vørnle
  • M. López-Caniego
  • J. F. Macías-Pérez
  • B. Maffei
  • G. Maggio
  • N. Mandolesi
  • A. Mangilli
  • M. Maris
  • P. G. Martin
  • E. Martínez-González
  • S. Masi
  • S. Matarrese
  • A. Melchiorri
  • A. Mennella
  • M. Migliaccio
  • M. A. Miville-Deschênes
  • A. Moneti
  • L. Montier
  • G. Morgante
  • D. Mortlock
  • D. Munshi
  • J. A. Murphy
  • P. Naselsky
  • F. Nati
  • P. Natoli
  • H. U. Nørgaard-Nielsen
  • D. Novikov
  • I. Novikov
  • C. A. Oxborrow
  • L. Pagano
  • F. Pajot
  • D. Paoletti
  • F. Pasian
  • O. Perdereau
  • L. Perotto
  • V. Pettorino
  • F. Piacentini
  • M. Piat
  • S. Plaszczynski
  • E. Pointecouteau
  • G. Polenta
  • N. Ponthieu
  • G. W. Pratt
  • S. Prunet
  • J. L. Puget
  • J. P. Rachen
  • R. Rebolo
  • M. Reinecke
  • M. Remazeilles
  • C. Renault
  • A. Renzi
  • I. Ristorcelli
  • G. Rocha
  • C. Rosset
  • M. Rossetti
  • G. Roudier
  • J. A. Rubiño-Martín
  • B. Rusholme
  • D. Santos
  • G. Savini
  • D. Scott
  • V. Stolyarov
  • R. Stompor
  • R. Sudiwala
  • R. Sunyaev
  • D. Sutton
  • A. S. Suur-Uski
  • J. F. Sygnet
  • J. A. Tauber
  • L. Terenzi
  • L. Toffolatti
  • M. Tomasi
  • M. Tristram
  • M. Tucci
  • L. Valenziano
  • J. Valiviita
  • F. Van Tent
  • P. Vielva
  • F. Villa
  • L. A. Wade
  • I. K. Wehus
  • D. Yvon
  • A. Zacchei
  • A. Zonca

Organisaatiot

  • CNRS/IN2P3
  • Cardiff University
  • CNRS/IN2P3
  • Kavli Institute for Cosmology Cambridge
  • International School for Advanced Studies
  • IRAP
  • Instituto de Física de Cantabria (CSIC-Universidad de Cantabria)
  • Universit'a di Rome Sapienza
  • Instituto Carlos I de Física Teórica y Computacional
  • UMR7095
  • INAF/IASF Milano
  • Kazan Federal University
  • University of Manchester
  • University of Toronto
  • University of California at Berkeley
  • Institut d 'Astrophysique de Paris
  • Space Research Institute, Russian Academy of Sciences
  • University of Oxford
  • Princeton University
  • Niels Bohr Institute
  • Jet Propulsion Laboratory, California Institute of Technology
  • Universite Paris-Sud
  • Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
  • Università La Sapienza
  • Université Pierre and Marie Curie
  • CNRS Centre National de la Recherche Scientifique
  • Urbanización Villafranca Del Castillo
  • Max-Planck-Institut für Astrophysik
  • Osservatorio Astronomico di Trieste
  • Instituto Astrofisico de Canarias
  • University of Oslo
  • University of Warsaw
  • Stockholm University
  • University of Cambridge
  • Danmarks Tekniske Universitet
  • Imperial College London
  • University of Helsinki
  • Lawrence Berkeley National Laboratory
  • Akdeniz University
  • European Southern Observatory Santiago
  • LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres
  • Torre C
  • Department of Experimental Physics
  • Russian Academy of Sciences
  • Institut für Theoretische Astrophysik
  • Osservatorio Astronomico Roma
  • Université Paris Diderot
  • Università di Roma Tor Vergata
  • California Institute of Technology
  • University College London
  • University of British Columbia
  • Special Astrophysical Observatory, Russian Academy of Sciences
  • ESTEC - European Space Research and Technology Centre
  • Università degli Studi e-Campus
  • Université de Genève
  • University of California at Santa Barbara

Kuvaus

Although infrared (IR) overall dust emission from clusters of galaxies has been statistically detected using data from the Infrared Astronomical Satellite (IRAS), it has not been possible to sample the spectral energy distribution (SED) of this emission over its peak, and thus to break the degeneracy between dust temperature and mass. By complementing the IRAS spectral coverage with Planck satellite data from 100 to 857 GHz, we provide new constraints on the IR spectrum of thermal dust emission in clusters of galaxies. We achieve this by using a stacking approach for a sample of several hundred objects from the Planck cluster sample. This procedure averages out fluctuations from the IR sky, allowing us to reach a significant detection of the faint cluster contribution. We also use the large frequency range probed by Planck, together with componentseparation techniques, to remove the contamination from both cosmic microwave background anisotropies and the thermal Sunyaev-Zeldovich effect (tSZ) signal, which dominate at ν ≤ 353 GHz. By excluding dominant spurious signals or systematic effects, averaged detections are reported at frequencies 353 GHz ≤ ν ≤ 5000 GHz.We confirm the presence of dust in clusters of galaxies at low and intermediate redshifts, yielding an SED with a shape similar to that of the Milky Way. Planck's resolution does not allow us to investigate the detailed spatial distribution of this emission (e.g. whether it comes from intergalactic dust or simply the dust content of the cluster galaxies), but the radial distribution of the emission appears to follow that of the stacked SZ signal, and thus the extent of the clusters. The recovered SED allows us to constrain the dust mass responsible for the signal and its temperature.

Yksityiskohdat

AlkuperäiskieliEnglanti
ArtikkeliA 104
Sivumäärä12
JulkaisuAstronomy and Astrophysics
Vuosikerta596
TilaJulkaistu - 1 joulukuuta 2016
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

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