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

被引：0

作者：

Adam, R. ^{[73
]}

Ade, P.A.R. ^{[87
]}

Aghanim, N. ^{[58
]}

Ashdown, M. ^{[7
,67
]}

Aumont, J. ^{[58
]}

Baccigalupi, C. ^{[85
]}

Banday, A.J. ^{[12
,96
]}

Barreiro, R.B. ^{[63
]}

Bartolo, N. ^{[30
,64
]}

Battaner, E. ^{[97
,98
]}

Benabed, K. ^{[59
,95
]}

Benoit-Lévy, A. ^{[26
,59
,95
]}

Bersanelli, M. ^{[33
,48
]}

Bielewicz, P. ^{[12
,80
,85
]}

Bikmaev, I. ^{[3
,22
]}

Bonaldi, A. ^{[66
]}

Bond, J.R. ^{[11
]}

Borrill, J. ^{[15
,90
]}

Bouchet, F.R. ^{[59
,88
]}

Burenin, R. ^{[78
,89
]}

Burigana, C. ^{[31
,47
,49
]}

Calabrese, E. ^{[92
]}

Cardoso, J.-F. ^{[1
,59
,72
]}

Catalano, A. ^{[70
,73
]}

Chiang, H.C. ^{[8
,28
]}

Christensen, P.R. ^{[36
,81
]}

Churazov, E. ^{[77
,89
]}

Colombo, L.P.L. ^{[25
,65
]}

Combet, C. ^{[73
]}

Comis, B. ^{[73
]}

Couchot, F. ^{[69
]}

Crill, B.P. ^{[13
,65
]}

Curto, A. ^{[7
,63
,67
]}

Cuttaia, F. ^{[47
]}

Danese, L. ^{[85
]}

Davis, R.J. ^{[66
]}

De Bernardis, P. ^{[32
]}

De Rosa, A. ^{[47
]}

De Zotti, G. ^{[44
,85
]}

Delabrouille, J. ^{[1
]}

Désert, F.-X. ^{[54
]}

Diego, J.M. ^{[63
]}

Dole, H. ^{[57
,58
]}

Doré, O. ^{[13
,65
]}

Douspis, M. ^{[58
]}

Ducout, A. ^{[55
,59
]}

Dupac, X. ^{[39
]}

Elsner, F. ^{[26
,59
,95
]}

Enßlin, T.A. ^{[77
]}

Finelli, F. ^{[47
,49
]}

机构：

[1] APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10 rue Alice Domon et Léonie Duquet, Paris Cedex 13,75205, France

[2] Aalto University Metsähovi Radio Observatory and Dept of Radio Science and Engineering, PO Box 13000, Aalto,00076, Finland

[3] Academy of Sciences of Tatarstan, Bauman Str., 20, Kazan,420111, Russia

[4] African Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg, Cape Town,7945, South Africa

[5] Agenzia Spaziale Italiana Science Data Center, via del Politecnico snc, Roma,00133, Italy

[6] Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, Marseille,13388, France

[7] Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge,CB3 0HE, United Kingdom

[8] Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Westville Campus, Private Bag X54001, Durban,4000, South Africa

[9] Atacama Large Millimeter/submillimeter Array, ALMA Santiago Central Offices, Alonso de Cordova 3107, Vitacura, Casilla, Santiago,763 0355, Chile

[10] CGEE, SCS Qd 9, Lote C, Torre C, 40 andar, Ed. Parque Cidade Corporate, Brasília, DF,CEP 70308-200, Brazil

[11] CITA, University of Toronto, 60 St. George St., Toronto,ON,M5S 3H8, Canada

[12] CNRS, IRAP, 9 Av. colonel Roche, Toulouse Cedex 4,31028, France

[13] California Institute of Technology, Pasadena,CA, United States

[14] Centro de Estudios de Física Del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, planta 2, Teruel,44001, Spain

[15] Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley,CA,94720, United States

[16] Consejo Superior de Investigaciones Científicas (CSIC), Madrid,28049, Spain

[17] DSM/Irfu/SPP, CEA-Saclay, Gif-sur-Yvette Cedex,91191, France

[18] DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, Lyngby,2800 Kgs., Denmark

[19] Département de Physique Théorique, Université de Genève, 24, Quai E. Ansermet, Genève 4,1211, Switzerland

[20] Departamento de Astrofísica, Universidad de la Laguna (ULL), La Laguna, Tenerife,38206, Spain

[21] Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo,33077, Spain

[22] Department of Astronomy and Geodesy, Kazan Federal University, Kremlevskaya Str., 18, Kazan,420008, Russia

[23] Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, Nijmegen,6500 GL, Netherlands

[24] Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver,BC, Canada

[25] Department of Physics and Astronomy, Dana and David Dornsife College of Letter, Arts and Sciences, University of Southern California, Los Angeles,CA,90089, United States

[26] Department of Physics and Astronomy, University College London, London,WC1E 6BT, United Kingdom

[27] Department of Physics, Gustaf Hällströmin Katu 2a, University of Helsinki, Helsinki,00100, Finland

[28] Department of Physics, Princeton University, Princeton,NJ,08544, United States

[29] Department of Physics, University of California, Santa Barbara,CA,93106, United States

[30] Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, Padova,35131, Italy

[31] Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, via Saragat 1, Ferrara,44122, Italy

[32] Dipartimento di Fisica, Università la Sapienza, P. le A. Moro 2, Roma,00133, Italy

[33] Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, Milano,20133, Italy

[34] Dipartimento di Fisica, Università degli Studi di Trieste, via A. Valerio 2, Trieste,34127, Italy

[35] Dipartimento di Matematica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma,00133, Italy

[36] Discovery Center, Niels Bohr Institute, Blegdamsvej 17, Copenhagen,1165, Denmark

[37] Discovery Center, Niels Bohr Institute, Copenhagen University, Blegdamsvej 17, Copenhagen,1165, Denmark

[38] European Southern Observatory, ESO Vitacura, Alonso de Cordova 3107, Vitacura, Casilla ,Santiago,19001, Chile

[39] European Space Agency, ESAC, Planck Science Office, Camino Bajo Del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain

[40] European Space Agency, ESTEC, Keplerlaan 1, Noordwijk,2201 AZ, Netherlands

[41] Gran Sasso Science Institute, INFN, viale F. Crispi 7, L' Aquila,67100, Italy

[42] HGSFP, University of Heidelberg, Theoretical Physics Department, Philosophenweg 16, Heidelberg,69120, Germany

[43] Helsinki Institute of Physics, Gustaf Hällströmin Katu 2, University of Helsinki, Helsinki,35131, Finland

[44] INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova,35131, Italy

[45] INAF-Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy

[46] INAF-Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy

[47] INAF/IASF Bologna, via Gobetti 101, Bologna, Italy

[48] INAF/IASF Milano, via E. Bassini 15, Milano, Italy

[49] INFN, Sezione di Bologna, viale Berti Pichat 6/2, Bologna,40127, Italy

[50] INFN, Sezione di Ferrara, via Saragat 1, Ferrara,44122, Italy

来源：

Astronomy and Astrophysics | 2016年 / 596卷

关键词：

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. © ESO 2016;

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