Planck intermediate results. II. Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters
Planck intermediate results. II. Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters
复制标题
普朗克中间结果。
DOI：
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发表时间：
2012
期刊：
影响因子：
--
通讯作者：
A. Zonca
中科院分区：
文献类型：
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作者：
Planck;A. C. N. Aghanim;M. Arnaud;M. Ashdown;J. Aumont;C. Baccigalupi;A. Balbi;A. Banday;R. B. Barreiro;E. Battaner;R. Battye;K. Benabed;A. Benoȋt;J. Bernard;M. Bersanelli;R. Bhatia;I. Bikmaev;H. Bohringer;A. Bonaldi;J. Bond;J. Borrill;F. Bouchet;H. Bourdin;M. Brown;M. Bucher;R. Burenin;C. Burigana;R. C. Butler;P. Cabella;P. Carvalho;A. Catalano;L. Cay'on;A. Chamballu;R. Chary;L. Chiang;G. Chon;D. Clements;S. Colafrancesco;S. Colombi;B. Crill;F. Cuttaia;A. Silva;H. Dahle;R. Davies;R. Davis;P. Bernardis;G. Gasperis;A. Rosa;G. Zotti;J. Delabrouille;J. D'emocles;C. Dickinson;J. Diego;K. Dolag;H. Dole;S. Donzelli;O. Dor'e;M. Douspis;X. Dupac;T. Ensslin;H. Eriksen;F. Feroz;F. Finelli;I. Flores;O. Forni;P. Fosalba;M. Frailis;E. Franceschi;S. Fromenteau;S. Galeotta;K. Ganga;R. G'enova;M. Giard;Y. Giraud;J. Gonz'alez;K. M. G'orski;K. Grainge;A. Gregorio;A. Gruppuso;F. Hansen;D. Harrison;S. Henrot;C. Hern'andez;D. Herranz;S. Hildebrandt;E. Hivon;M. Hobson;W. Holmes;K. Huffenberger;G. Hurier;N. Hurley;T. Jagemann;M. Juvela;E. Keihanen;I. Khamitov;R. Kneissl;J. Knoche;M. Kunz;H. Kurki;G. Lagache;J. Lamarre;A. Lasenby;C. Lawrence;M. Jeune;S. Leach;R. Leonardi;A. Liddle;P. Lilje;M. Linden;M. L'opez;G. Luzzi;J. Mac'ias;C. MacTavish;D. Maino;N. Mandolesi;M. Maris;F. Marleau;D. Marshall;E. Mart'inez;S. Masi;M. Massardi;S. Matarrese;F. Matthai;P. Mazzotta;A. Melchiorri;J. Melin;L. Mendes;A. Mennella;S. Mitra;M. Miville;L. Montier;G. Morgante;D. Munshi;P. Naselsky;P. Natoli;F. Noviello;M. Olamaie;S. Osborne;F. Pajot;D. Paoletti;F. Pasian;G. Patanchon;T. Pearson;O. Perdereau;Y. Perrott;F. Perrotta;F. Piacentini;E. Pierpaoli;P. Platania;E. Pointecouteau;G. Polenta;L. Popa;T. Poutanen;G. Pratt;J. Puget;J. Rachen;R. Rebolo;M. Reinecke;M. Remazeilles;C. Renault;S. Ricciardi;I. Ristorcelli;G. Rocha;C. Rodr'iguez;C. Rosset;M. Rossetti;J. Rubino;B. Rusholme;R. Saunders;G. Savini;M. Schammel;D. Scott;T. W. Shimwell;G. Smoot;J. Starck;F. Stivoli;V. Stolyarov;R. Sunyaev;D. Sutton;A.;J. Sygnet;J. Tauber;L. Terenzi;L. Toffolatti;M. Tomasi;M. Tristram;L. Valenziano;B. Tent;P. Vielva;F. Villa;N. Vittorio;L. Wade;B. Wandelt;D. Yvon;A. Zacchei;A. Zonca
比较了普朗克星系团和地面干涉仪ArcMinin Microkelvin成像仪对11个星系团的Sunyaev-Zeldovich测量结果。假设星系团的气体压强分布是一个普遍的球对称广义纳瓦罗、弗伦克和怀特模型，我们联合约束了积分的康普顿-Y参数(Y500)和每个星系团的尺度半径(θ500)。我们从这两台仪器得到的Y500−θ5002D参数空间中的八个星系团的约束条件显著重叠，尽管总的来说，AMI有发现Sunyaev-Zeldovich信号的角尺寸更小且比普朗克更弱的趋势。样本中剩余的三个星系团，即A1413、A1914和新发现的普朗克星系团PLCKESZ G139.59+24.18存在显著差异。通过使用详细的模拟，证明了对普朗克和AMI数据的分析的稳健性，这些模拟也排除了来自残留点(射电)源和漫射天体物理前景的混淆，作为对所发现的差异的可能解释。对于我们的星系团样本的一个子集，我们通过采用与X射线观测最匹配的GNFW剖面形状重复分析，研究了我们的结果对假设压力剖面的依赖性。通常，从X射线数据中采用最适合的轮廓形状并不能解决在这五个簇的子集中发现的差异。虽然基于小样本，但我们的结果表明，所采用的GNFW模型可能不够灵活，不足以描述普遍的团簇。
A comparison is presented of Sunyaev-Zeldovich measurements for 11 galaxy clusters as obtained by Planck and by the ground-based interferometer, the Arcminute Microkelvin Imager. Assuming a universal spherically-symmetric Generalised Navarro, Frenk and White (GNFW) model for the cluster gas pressure profile, we jointly constrain the integrated Compton-Y parameter (Y500) and the scale radius (θ500) of each cluster. Our resulting constraints in the Y500 − θ500 2D parameter space derived from the two instruments overlap significantly for eight of the clusters, although, overall, there is a tendency for AMI to find the Sunyaev-Zeldovich signal to be smaller in angular size and fainter than Planck. Significant discrepancies exist for the three remaining clusters in the sample, namely A1413, A1914, and the newly-discovered Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis of both the Planck and AMI data is demonstrated through the use of detailed simulations, which also discount confusion from residual point (radio) sources and from diffuse astrophysical foregrounds as possible explanations for the discrepancies found. For a subset of our cluster sample, we have investigated the dependence of our results on the assumed pressure profile by repeating the analysis adopting the best-fitting GNFW profile shape which best matches X-ray observations. Adopting the best-fitting profile shape from the X-ray data does not, in general, resolve the discrepancies found in this subset of five clusters. Though based on a small sample, our results suggest that the adopted GNFW model may not be sufficiently flexible to describe clusters universally.
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.