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The survey of galaxy clusters performed by Planck through the Sunyaev-Zeldovich effect has already discovered many interesting objects, thanks to the whole coverage of the sky. One of the SZ candidates detected in the early months of the mission near to the signal to noise threshold, PLCKG214.6+37.0, was later revealed by XMM-Newton to be a triple system of galaxy clusters. We have further investigated this puzzling system with a multi-wavelength approach and we present here the results from a deep XMM-Newton re-observation. The characterisation of the physical properties of the three components has allowed us to build a template model to extract the total SZ signal of this system with Planck data. We partly reconciled the discrepancy between the expected SZ signal from X-rays and the observed one, which are now consistent at less than 1.2 sigma. We measured the redshift of the three components with the iron lines in the X-ray spectrum, and confirmed that the three clumps are likely part of the same supercluster structure. The analysis of the dynamical state of the three components, as well as the absence of detectable excess X-ray emission, suggest that we are witnessing the formation of a massive cluster at an early phase of interaction.
Planck intermediate results. 6. : the dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters / P.A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A.J. Banday, R.B. Barreiro, J.G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J.-P. Bernard, M. Bersanelli, R. Bhatia, H. Böhringer, A. Bonaldi, J.R. Bond, J. Borrill, F. R. Bouchet, H. Bourdin, C. Burigana, P. Cabella, J.-F. Cardoso, G. Castex, A. Catalano, L. Cayón, A. Chamballu, L.-Y. Chiang, G. Chon, P.R. Christensen, D.L. Clements, S. Colafrancesco, S. Colombi, L.P.L. Colombo, B. Comis, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, L. Danese, R. J. Davis, P. de Bernardis, G. de Gasperis, G. de Zotti, J. Delabrouille, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou,
T. A. Ensslin, H. K. Eriksen, F. Finelli, I. Flores-Cacho, O. Forni, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, M. Gilfanov, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, P. Heinämäki, A. Hempel, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, G. Hurier, T. R. Jaffe, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, E. Keihänen, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.-M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, R. Leonardi, P. B. Lilje, M. López-Caniego, G. Luzzi, J. F. Macías-Pérez, D. Maino, N. Mandolesi, M. Maris, F. Marleau, D. J. Marshall, E. Martínez González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, A. Melchiorri, J.-B. Melin, L. Mendes, A. Mennella, S. Mitra, 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, F. Noviello, S. Osborne, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, R. Piffaretti, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J.-L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, M. Roman, C. Rosset, M. Rossetti, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G. F. Smoot, J.-L. Starck, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, J. Tuovinen, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L.A. Wade, B.D. Wandelt, N. Welikala, D. Yvon, A. Zacchei, S. Zaroubi, A. Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 550(2013), pp. A132.1-A132.14.
Planck intermediate results. 6. : the dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters
P. A. R. Ade;N. Aghanim;M. Arnaud;M. Ashdown;F. Atrio Barandela;J. Aumont;C. Baccigalupi;A. Balbi;A. J. Banday;R. B. Barreiro;J. G. Bartlett;E. Battaner;K. Benabed;A. Benoît;J. P. Bernard;M. Bersanelli;R. Bhatia;H. Böhringer;A. Bonaldi;J. R. Bond;J. Borrill;F. R. Bouchet;H. Bourdin;C. Burigana;P. Cabella;J. F. Cardoso;G. Castex;A. Catalano;L. Cayón;A. Chamballu;L. Y. Chiang;G. Chon;P. R. Christensen;D. L. Clements;S. Colafrancesco;S. Colombi;L.P.L. Colombo;B. Comis;A. Coulais;B. P. Crill;F. Cuttaia;A. Da Silva;H. Dahle;L. Danese;R. J. Davis;P. de Bernardis;G. de Gasperis;G. de Zotti;J. Delabrouille;J. M. Diego;K. Dolag;H. Dole;S. Donzelli;O. Doré;U. Dörl;M. Douspis;X. Dupac;G. Efstathiou;T. A. Ensslin;H. K. Eriksen;F. Finelli;I. Flores Cacho;O. Forni;M. Frailis;E. Franceschi;M. Frommert;S. Galeotta;K. Ganga;R. T. Génova Santos;M. Giard;M. Gilfanov;Y. Giraud Héraud;J. González Nuevo;K. M. Górski;A. Gregorio;A. Gruppuso;F. K. Hansen;D. Harrison;P. Heinämäki;A. Hempel;S. Henrot Versillé;C. Hernández Monteagudo;D. Herranz;S. R. Hildebrandt;E. Hivon;M. Hobson;W. A. Holmes;G. Hurier;T. R. Jaffe;A. H. Jaffe;T. Jagemann;W. C. Jones;M. Juvela;E. Keihänen;T. S. Kisner;R. Kneissl;J. Knoche;L. Knox;M. Kunz;H. Kurki Suonio;G. Lagache;A. Lähteenmäki;J. M. Lamarre;A. Lasenby;C. R. Lawrence;M. Le Jeune;R. Leonardi;P. B. Lilje;M. López Caniego;G. Luzzi;J. F. Macías Pérez;D. Maino;N. Mandolesi;M. Maris;F. Marleau;D. J. Marshall;E. Martínez González;S. Masi;M. Massardi;S. Matarrese;P. Mazzotta;S. Mei;A. Melchiorri;J. B. Melin;L. Mendes;A. Mennella;S. Mitra;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;F. Noviello;S. Osborne;F. Pajot;D. Paoletti;F. Pasian;G. Patanchon;O. Perdereau;L. Perotto;F. Perrotta;F. Piacentini;M. Piat;E. Pierpaoli;R. Piffaretti;S. Plaszczynski;E. Pointecouteau;G. Polenta;N. Ponthieu;L. Popa;T. Poutanen;G. W. Pratt;S. Prunet;J. L. Puget;J. P. Rachen;R. Rebolo;M. Reinecke;M. Remazeilles;C. Renault;S. Ricciardi;T. Riller;I. Ristorcelli;G. Rocha;M. Roman;C. Rosset;M. Rossetti;J. A. Rubiño Martín;B. Rusholme;M. Sandri;G. Savini;D. Scott;G. F. Smoot;J. L. Starck;R. Sudiwala;R. Sunyaev;D. Sutton;A. S. Suur Uski;J. F. Sygnet;J. A. Tauber;L. Terenzi;L. Toffolatti;M. Tomasi;M. Tristram;J. Tuovinen;L. Valenziano;B. Van Tent;P. Vielva;F. Villa;N. Vittorio;L. A. Wade;B. D. Wandelt;N. Welikala;D. Yvon;A. Zacchei;S. Zaroubi;A. Zonca
2013
Abstract
The survey of galaxy clusters performed by Planck through the Sunyaev-Zeldovich effect has already discovered many interesting objects, thanks to the whole coverage of the sky. One of the SZ candidates detected in the early months of the mission near to the signal to noise threshold, PLCKG214.6+37.0, was later revealed by XMM-Newton to be a triple system of galaxy clusters. We have further investigated this puzzling system with a multi-wavelength approach and we present here the results from a deep XMM-Newton re-observation. The characterisation of the physical properties of the three components has allowed us to build a template model to extract the total SZ signal of this system with Planck data. We partly reconciled the discrepancy between the expected SZ signal from X-rays and the observed one, which are now consistent at less than 1.2 sigma. We measured the redshift of the three components with the iron lines in the X-ray spectrum, and confirmed that the three clumps are likely part of the same supercluster structure. The analysis of the dynamical state of the three components, as well as the absence of detectable excess X-ray emission, suggest that we are witnessing the formation of a massive cluster at an early phase of interaction.
Planck intermediate results. 6. : the dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters / P.A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A.J. Banday, R.B. Barreiro, J.G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J.-P. Bernard, M. Bersanelli, R. Bhatia, H. Böhringer, A. Bonaldi, J.R. Bond, J. Borrill, F. R. Bouchet, H. Bourdin, C. Burigana, P. Cabella, J.-F. Cardoso, G. Castex, A. Catalano, L. Cayón, A. Chamballu, L.-Y. Chiang, G. Chon, P.R. Christensen, D.L. Clements, S. Colafrancesco, S. Colombi, L.P.L. Colombo, B. Comis, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, L. Danese, R. J. Davis, P. de Bernardis, G. de Gasperis, G. de Zotti, J. Delabrouille, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou,
T. A. Ensslin, H. K. Eriksen, F. Finelli, I. Flores-Cacho, O. Forni, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, M. Gilfanov, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, P. Heinämäki, A. Hempel, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, G. Hurier, T. R. Jaffe, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, E. Keihänen, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.-M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, R. Leonardi, P. B. Lilje, M. López-Caniego, G. Luzzi, J. F. Macías-Pérez, D. Maino, N. Mandolesi, M. Maris, F. Marleau, D. J. Marshall, E. Martínez González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, A. Melchiorri, J.-B. Melin, L. Mendes, A. Mennella, S. Mitra, 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, F. Noviello, S. Osborne, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, R. Piffaretti, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J.-L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, M. Roman, C. Rosset, M. Rossetti, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G. F. Smoot, J.-L. Starck, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, J. Tuovinen, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L.A. Wade, B.D. Wandelt, N. Welikala, D. Yvon, A. Zacchei, S. Zaroubi, A. Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 550(2013), pp. A132.1-A132.14.
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P.A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A.J. Banday, R.B. Barreiro, J.G. Bartlett, E. ...espandi
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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.