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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.
Planck intermediate results : XLIII. Spectral energy distribution of dust in clusters of galaxies / 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, A. Lähteenmäki, 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, M. Savelainen, 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. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 596(2016 Dec), pp. A 104.1-A 104.12. [10.1051/0004-6361/201628522]
Planck intermediate results : XLIII. Spectral energy distribution of dust in clusters of galaxies
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;A. Lähteenmäki;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;M. Savelainen;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
2016
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 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.
Planck intermediate results : XLIII. Spectral energy distribution of dust in clusters of galaxies / 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, A. Lähteenmäki, 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, M. Savelainen, 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. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 596(2016 Dec), pp. A 104.1-A 104.12. [10.1051/0004-6361/201628522]
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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, A. Lähteenmäki, 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, M. Savelainen, 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
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Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.