Abstract
We present first results on PLCKG266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate isa bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02, and estimate the cluster mass to be M 500 = (7.8 ± 0.8) × 1014 M. PLCKG266.6-27.3 is an exceptional system: its luminosity of LX [0.5-2.0 keV] = (1.4 ± 0.05) × 1045 erg s-1 equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z ~ 1. Moreover, unlike the majority of high-redshift clusters, PLCKG266.6-27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function.
| Original language | English (US) |
|---|---|
| Article number | A26 |
| Journal | Astronomy and Astrophysics |
| Volume | 536 |
| DOIs | |
| State | Published - 2011 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Cosmic background radiation
- Cosmology
- Galaxies
- X-rays
- clusters
- galaxies
- general
- intracluster medium
- observations
Fingerprint Dive into the research topics of 'Planck early results. XXVI. Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z ~ 1'. Together they form a unique fingerprint.
Cite this
- APA
- Author
- BIBTEX
- Harvard
- Standard
- RIS
- Vancouver
}
Planck early results. XXVI. Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z ~ 1. / Aghanim, N.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Bernard, J. P.; Bersanelli, M.; Bhatia, R.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borgani, S.; Borrill, J.; Bouchet, F. R.; Brown, M. L.; Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cappellini, B.; Carvalho, P.; Catalano, A.; Cayón, L.; Chiang, L. Y.; Chiang, C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements, D. L.; Colafrancesco, S.; Colombi, S.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; 'Arcangelo, O. D.; Davis, R. J.; De Bernardis, P.; De Gasperis, G.; De Zotti, G.; Delabrouille, J.; Delouis, J. M.; Démoclès, J.; Désert, F. X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; González-Nuevo, J.; González-Riestra, R.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Heinämäki, P.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Hurier, G.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leonardi, R.; Leroy, C.; Liddle, A.; Lilje, P. B.; López-Caniego, M.; Luzzi, G.; MacÍas-Pérez, J. F.; Maino, D.; Mandolesi, N.; Marleau, F.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J. B.; Mendes, L.; Mennella, A.; Miville-Deschênes, M. A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.; Natoli, P.; Nevalainen, J.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paladini, R.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Pierpaoli, E.; Piffaretti, R.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rubiño-Martín, J. A.; Saar, E.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott, D.; Smoot, G. F.; Starck, J. L.; Sutton, D.; Sygnet, J. F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Türler, M.; Valenziano, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Weller, J.; White, S. D.M.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
In: Astronomy and Astrophysics, Vol. 536, A26, 2011.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Planck early results. XXVI. Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z ~ 1
AU - Aghanim, N.
AU - Arnaud, M.
AU - Ashdown, M.
AU - Atrio-Barandela, F.
AU - Aumont, J.
AU - Baccigalupi, C.
AU - Balbi, A.
AU - Banday, A. J.
AU - Barreiro, R. B.
AU - Bartlett, J. G.
AU - Battaner, E.
AU - Benabed, K.
AU - Benoît, A.
AU - Bernard, J. P.
AU - Bersanelli, M.
AU - Bhatia, R.
AU - Böhringer, H.
AU - Bonaldi, A.
AU - Bond, J. R.
AU - Borgani, S.
AU - Borrill, J.
AU - Bouchet, F. R.
AU - Brown, M. L.
AU - Burigana, C.
AU - Cabella, P.
AU - Cantalupo, C. M.
AU - Cappellini, B.
AU - Carvalho, P.
AU - Catalano, A.
AU - Cayón, L.
AU - Chiang, L. Y.
AU - Chiang, C.
AU - Chon, G.
AU - Christensen, P. R.
AU - Churazov, E.
AU - Clements, D. L.
AU - Colafrancesco, S.
AU - Colombi, S.
AU - Crill, B. P.
AU - Cuttaia, F.
AU - Da Silva, A.
AU - Dahle, H.
AU - Danese, L.
AU - 'Arcangelo, O. D.
AU - Davis, R. J.
AU - De Bernardis, P.
AU - De Gasperis, G.
AU - De Zotti, G.
AU - Delabrouille, J.
AU - Delouis, J. M.
AU - Démoclès, J.
AU - Désert, F. X.
AU - Dickinson, C.
AU - Diego, J. M.
AU - Dole, H.
AU - Donzelli, S.
AU - Doré, O.
AU - Douspis, M.
AU - Dupac, X.
AU - Efstathiou, G.
AU - Enßlin, T. A.
AU - Eriksen, H. K.
AU - Finelli, F.
AU - Flores-Cacho, I.
AU - Forni, O.
AU - Fosalba, P.
AU - Frailis, M.
AU - Franceschi, E.
AU - Fromenteau, S.
AU - Galeotta, S.
AU - Ganga, K.
AU - Génova-Santos, R. T.
AU - Giard, M.
AU - González-Nuevo, J.
AU - González-Riestra, R.
AU - Górski, K. M.
AU - Gregorio, A.
AU - Gruppuso, A.
AU - Hansen, F. K.
AU - Harrison, D.
AU - Heinämäki, P.
AU - Hernández-Monteagudo, C.
AU - Hildebrandt, S. R.
AU - Hivon, E.
AU - Hobson, M.
AU - Hurier, G.
AU - Jaffe, A. H.
AU - Jones, W. C.
AU - Juvela, M.
AU - Keihänen, E.
AU - Keskitalo, R.
AU - Kisner, T. S.
AU - Kneissl, R.
AU - Kurki-Suonio, H.
AU - Lagache, G.
AU - Lähteenmäki, A.
AU - Lamarre, J. M.
AU - Lasenby, A.
AU - Lawrence, C. R.
AU - Le Jeune, M.
AU - Leach, S.
AU - Leonardi, R.
AU - Leroy, C.
AU - Liddle, A.
AU - Lilje, P. B.
AU - López-Caniego, M.
AU - Luzzi, G.
AU - MacÍas-Pérez, J. F.
AU - Maino, D.
AU - Mandolesi, N.
AU - Marleau, F.
AU - Martínez-González, E.
AU - Masi, S.
AU - Matarrese, S.
AU - Mazzotta, P.
AU - Meinhold, P. R.
AU - Melchiorri, A.
AU - Melin, J. B.
AU - Mendes, L.
AU - Mennella, A.
AU - Miville-Deschênes, M. A.
AU - Moneti, A.
AU - Montier, L.
AU - Morgante, G.
AU - Mortlock, D.
AU - Munshi, D.
AU - Naselsky, P.
AU - Natoli, P.
AU - Nevalainen, J.
AU - Nørgaard-Nielsen, H. U.
AU - Noviello, F.
AU - Novikov, D.
AU - Novikov, I.
AU - O'Dwyer, I. J.
AU - Osborne, S.
AU - Paladini, R.
AU - Pasian, F.
AU - Patanchon, G.
AU - Pearson, T. J.
AU - Perdereau, O.
AU - Perotto, L.
AU - Perrotta, F.
AU - Piacentini, F.
AU - Pierpaoli, E.
AU - Piffaretti, R.
AU - Platania, P.
AU - Pointecouteau, E.
AU - Polenta, G.
AU - Ponthieu, N.
AU - Popa, L.
AU - Poutanen, T.
AU - Pratt, G. W.
AU - Prézeau, G.
AU - Prunet, S.
AU - Puget, J. L.
AU - Rachen, J. P.
AU - Rebolo, R.
AU - Reinecke, M.
AU - Renault, C.
AU - Ricciardi, S.
AU - Riller, T.
AU - Ristorcelli, I.
AU - Rocha, G.
AU - Rubiño-Martín, J. A.
AU - Saar, E.
AU - Sandri, M.
AU - Savini, G.
AU - Schaefer, B. M.
AU - Scott, D.
AU - Smoot, G. F.
AU - Starck, J. L.
AU - Sutton, D.
AU - Sygnet, J. F.
AU - Tauber, J. A.
AU - Terenzi, L.
AU - Toffolatti, L.
AU - Tomasi, M.
AU - Tristram, M.
AU - Türler, M.
AU - Valenziano, L.
AU - Vielva, P.
AU - Villa, F.
AU - Vittorio, N.
AU - Wade, L. A.
AU - Wandelt, B. D.
AU - Weller, J.
AU - White, S. D.M.
AU - White, M.
AU - Yvon, D.
AU - Zacchei, A.
AU - Zonca, A.
N1 - Copyright: Copyright 2013 Elsevier B.V., All rights reserved.
PY - 2011
Y1 - 2011
N2 - We present first results on PLCKG266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate isa bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02, and estimate the cluster mass to be M 500 = (7.8 ± 0.8) × 1014 M. PLCKG266.6-27.3 is an exceptional system: its luminosity of LX [0.5-2.0 keV] = (1.4 ± 0.05) × 1045 erg s-1 equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z ~ 1. Moreover, unlike the majority of high-redshift clusters, PLCKG266.6-27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function.
AB - We present first results on PLCKG266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate isa bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02, and estimate the cluster mass to be M 500 = (7.8 ± 0.8) × 1014 M. PLCKG266.6-27.3 is an exceptional system: its luminosity of LX [0.5-2.0 keV] = (1.4 ± 0.05) × 1045 erg s-1 equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z ~ 1. Moreover, unlike the majority of high-redshift clusters, PLCKG266.6-27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function.
KW - Cosmic background radiation
KW - Cosmology
KW - Galaxies
KW - X-rays
KW - clusters
KW - galaxies
KW - general
KW - intracluster medium
KW - observations
UR - http://www.scopus.com/inward/record.url?scp=82955194922&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=82955194922&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201117430
DO - 10.1051/0004-6361/201117430
M3 - Article
AN - SCOPUS:82955194922
VL - 536
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A26
ER -