Adam, R. and Ade, P.A.R. and Aghanim, N. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Banday, A.J. and Barreiro, R.B. and Bartolo, N. and Battaner, E. and Benabed, K. and Benoit-Lévy, A. and Bersanelli, M. and Bielewicz, P. and Bikmaev, I. and Bonaldi, A. and Bond, J.R. and Borrill, J. and Bouchet, F.R. and Burenin, R. and Burigana, C. and Calabrese, E. and Cardoso, J.-F. and Catalano, A. and Chiang, H.C. and Christensen, P.R. and Churazov, E. and Colombo, L.P.L. and Combet, C. and Comis, B. and Couchot, F. and Crill, B.P. and Curto, A. and Cuttaia, F. and Danese, L. and Davis, R.J. and De Bernardis, P. and de Rosa, A. and de Zotti, G. and Delabrouille, J. and Desert, F.-X. and Diego, J.M. and Dole, H. and Dore, O. and Douspis, M. and Ducout, A. and Dupac, X. and Elsner, F. and Enßlin, T.A. and Finelli, F. and Forni, O. and Frailis, M. and Fraisse, A.A. and Franceschi, E. and Galeotta, S. and Ganga, K. and Genova-Santos, R.T. and Giard, M. and Giraud-Héraud, Y. and Gjerløw, E. and Gonzalez-Nuevo, J. and Gorski, K.M. and Gregorio, A. and Gruppuso, A. and Gudmundsson, J.E. and Hansen, F.K. and Harrison, D. and Hernandez-Monteagudo, C. and Herranz, D. and Hildebrandt, S.R. and Hivon, E. and Hobson, M. and Hornstrup, A. and Hovest, W. and Hurier, G. and Jaffe, A.H. and Jaffe, T.R. and Jones, W.C. and Keihanen, E. and Keskitalo, R. and Khamitov, I. and Kisner, T.S. and Kneissl, R. and Knoche, J. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and Lahteenmaki, A. and Lamarre, J.-M. and Lasenby, A. and Lattanzi, M. and Lawrence, C.R. and Leonardi, R. and Levrier, F. and Liguori, M. and Lilje, P.B. and Linden-Vornle, M. and Lopez-Caniego, M. and Macias-Perez, J.F. and Maffei, B. and Maggio, G. and Mandolesi, N. and Mangilli, A. and Maris, M. and Martin, P.G. and Martinez-Gonzalez, E. and Masi, S. and Matarrese, S. and Melchiorri, A. and Mennella, A. and Migliaccio, M. and Miville-Deschenes, M.-A. and Moneti, A. and Montier, L. and Morgante, G. and Mortlock, D. and Munshi, D. and Murphy, J.Anthony and Naselsky, P. and Nati, F. and Natoli, P. and Norgaard-Nielsen, H.U. and Novikov, D. and Novikov, I. and Oxborrow, C.A. and Pagano, L. and Pajot, F. and Paoletti, D. and Pasian, F. and Perdereau, O. and Perotto, L. and Pettorino, V. and Piacentini, F. and Piat, M. and Plaszczynski, S. and Pointecouteau, E. and Polenta, G. and Ponthieu, N. and Pratt, G.W. and Prunet, S. and Puget, J.-L. and Rachen, J.P. and Rebolo, R. and Reinecke, M. and Remazeilles, M. and Renault, C. and Renzi, A. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Rossetti, M. and Roudier, G. and Rubino-Martin, J.A. and Rusholme, B. and Santos, D. and Savelainen, M. and Savini, G. and Scott, D. and Stolyarov, V. and Stompor, R. and Sudiwala, R. and Sunyaev, R. and Sutton, D. and Suur-Uski, A.-S. and Sygnet, J.-F. and Tauber, J.A. and Terenzi, L. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Tucci, M. and Valenziano, L. and Valiviita, J. and Van Tent, B. and Vielva, P. and Villa, F. and Wade, L.A. and Wehus, I. and Yvon, D. and Zacchei, A. and Zonca, A. (2016) Planck intermediate results XLIII. Spectral energy distribution of dust in clusters of galaxies. Astronomy & Astrophysics, 596 (A104). ISSN 0004-6361

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Abstract

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 component-separation 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.

Item Type:	Article
Keywords:	Planck Collaboration; galaxies: clusters: intracluster medium; galaxies: clusters: general; diffuse radiation; infrared: general;
Academic Unit:	Faculty of Science and Engineering > Experimental Physics
Item ID:	14326
Identification Number:	https://doi.org/10.1051/0004-6361/201628522
Depositing User:	Dr. Anthony Murphy
Date Deposited:	12 Apr 2021 15:20
Journal or Publication Title:	Astronomy & Astrophysics
Publisher:	EDP Sciences
Refereed:	Yes
URI:	Publisher
Use Licence:	This item is available under a Creative Commons Attribution Non Commercial Share Alike Licence (CC BY-NC-SA). Details of this licence are available here

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