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普朗克早期结果XXVI：用普朗克探测并用XMM-牛顿法确认z~1处异常X射线发光的大质量星系团PLCK G266 .6-27.3

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

Planck Collaboration, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, … 展开作者

Planck Collaboration, 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, S. Borgani, J. Borrill, F. R. Bouchet, M. L. Brown, C. Burigana, P. Cabella, C. M. Cantalupo, B. Cappellini, P. Carvalho, A. Catalano, L. Cayón, L. -Y Chiang, C. Chiang, G. Chon, P. R. Christensen, E. Churazov, D. L. Clements, S. Colafrancesco, S. Colombi, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, L. Danese, O. D'Arcangelo, R. J. Davis, P. de Bernardis, G. de Gasperis, G. de Zotti, J. Delabrouille, J. -M. Delouis, J. Démoclès, F. -X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, I. Flores-Cacho, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, S. Fromenteau, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, J. González-Nuevo, R. González-Riestra, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, P. Heinämäki, C. Hernández-Monteagudo, S. R. Hildebrandt, E. Hivon, M. Hobson, G. Hurier, A. H. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, S. Leach, R. Leonardi, C. Leroy, A. Liddle, P. B. Lilje, M. López-Caniego, G. Luzzi, J. F. Macías-Pérez, D. Maino, N. Mandolesi, F. Marleau, E. Martínez-González, S. Masi, S. Matarrese, P. Mazzotta, P. R. Meinhold, A. Melchiorri, J. -B. Melin, L. Mendes, A. Mennella, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, P. Natoli, J. Nevalainen, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, I. J. O'Dwyer, S. Osborne, R. Paladini, F. Pasian, G. Patanchon, T. J. Pearson, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, E. Pierpaoli, R. Piffaretti, P. Platania, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, G. Prézeau, S. Prunet, J. -L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, J. A. Rubiño-Martín, E. Saar, M. Sandri, G. Savini, B. M. Schaefer, D. Scott, G. F. Smoot, J. -L. Starck, D. Sutton, J. -F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Türler, L. Valenziano, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, J. Weller, S. D. M. White, M. White, D. Yvon, A. Zacchei, A. Zonca

备注：
6 pages, 3 figures; final version accepted for publication in A&A ; minor changes in Sec.2.,3.2 and 4.1; Table 1: misprint on R500 error corrected; abundance value added
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摘要：

我们目前的第一个结果PLCK G266.6-27.3，一个星系团候选人在信噪比为5的普朗克全天巡天检测。XMM-牛顿验证观测使我们能够确认候选者是真正的星系团。利用这些X射线数据，我们测量了一个精确的红移，z = 0.94 +/- 0.02，并估计星系团的质量为M_500 =（7.8 +/- 0.8）e+14太阳质量。PLCK G266.6-27.3是一个特殊的星系，它的光度为LX（0.5-2.0 keV）=（1.4 +/- 0.05）e+45 erg/s，相当于z > 0.5宇宙中已知的两个最亮的星系团，是z~1时质量最大的星系团之一。此外，与大多数高红移星团不同，PLCK G266.6-27.3似乎是高度松弛的。这一观测结果证实了普朗克探测高红移、高质量星系团的能力，并为系统研究质量函数指数尾部的种群演化开辟了道路。

英文摘要：

We present first results on PLCK G266.6-27.3, 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 is a 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)e+14 solar masses. PLCK G266.6-27.3 is an exceptional system: its luminosity of L_X(0.5-2.0 keV)=(1.4 +/- 0.05)e+45 erg/s, 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, PLCK G266.6-27.3 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.

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