Planck 2015 results: XXI. The integrated Sachs-Wolfe effect-猫眼课题宝

DOI：

10.1051/0004-6361/201525831

发表时间：

2015-02

期刊：

Astronomy and Astrophysics

影响因子：

6.5

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

P. Ade;N. Aghanim;M. Arnaud;M. Ashdown;J. Aumont;C. Baccigalupi;A. Banday;R. B. Barreiro;N. Bartolo;S. Basak;E. Battaner;K. Benabed;A. Benoit;A. Benoit-Lévy;J. Bernard;M. Bersanelli;P. Bielewicz;J. Bock;A. Bonaldi;L. Bonavera;J. Bond;J. Borri;F. Bouchet;M. Bucher;C. Burigana;R. C. Butler;E. Calabrese;J. Cardoso;B. Casaponsa;A. Catalano;A. Challinor;A. Chamballu;H. Chiang;P. Christensen;S. Church;D. Clements;S. Colombi;L. Colombo;C. Combet;F. Couchot;A. Coulais;B. Crill;A. Curto;F. Cuttaia;L. Danese;R. Davies;R. Davis;P. Bernardis;A. D. Rosa;G. Zotti;J. Delabrouille;F. Désert;J. Diego;H. Dole;S. Donzelli;O. Doré;M. Douspis;A. Ducout;X. Dupac;G. Efstathiou;F. Elsner;T. Ensslin;H. Eriksen;J. Fergusson;R. Fernández-Cobos;F. Finelli;O. Forni;M. Frailis;A. Fraisse;E. Franceschi;A. Frejsel;S. Galeotta;S. Galli;K. Ganga;R. Génova-Santos;M. Girad;Y. Giraud-Héraud;E. Gjerløw;J. González-Nuevo;K. Górski;S. Gratton;A. Gregorio;A. Gruppuso;J. Gudmundsson;F. Hansen;D. Hanson;D. Harrison;S. Henrot-Versillé;C. Hernández-Monteagudo;D. Herranz;S. Hildebrandt;E. Hivon;M. Hobson;W. Holmes;A. Hornstrup;W. Hovest;K. Huffenberger;G. Hurier;S. Ilic;A. Jaffe;T. Jaffe;W. Jones;M. Juvela;E. Keihänen;R. Keskitalo;T. Kisner;R. Kneiss;J. Knoche;M. Kunz;H. Kurki-Suonio;G. Lagache;A. Lähteenmäki;J. Lamarre;M. Langer;A. Lasenby;M. Lattanzi;C. Lawrence;R. Leonardi;J. Lesgourgues;F. Levrier;M. Liguori;P. Lilje;M. Linden-Vørnle;M. López-Caniego;P. Lubin;Yin-Zhe Ma;J. Macı́as-Pérez;G. Maggio;D. Maino;N. Mandolesi;A. Mangilli;A. Marcos-Caballero;M. Maris;P. Martin;E. Martinez-Gonzalez;S. Masi;S. Matarrese;P. McGehee;P. Meinhold;A. Melchiorri;L. Mendes;A. Mennella;M. Migliaccio;S. Mitra;M. Miville-Deschênes;A. Moneti;L. Montier;G. Morgante;D. Mortlock;A. Moss;D. Munshi;J. Murphy;P. Naselsky;F. Nati;P. Natoli;C. Netterfield;H. Nørgaard-Nielsen;F. Noviello;D. Novikov;I. Novikov;C. A. Oxborrow;F. Paci;L. Pagano;F. Pajot;D. Paoletti;F. Pasian;G. Patanchon;O. Perdereau;L. Perotto;Francesco Perrotta;V. Pettorino;F. Piacentini;M. Piat;E. Pierpaoli;D. Pietrobon;S. Plaszczynski;E. Pointecouteau;G. Polenta;L. Popa;G. Pratt;G. Prezeau;S. Prunet;J. Puget;J. Rachen;W. Reach;R. Rebolo;M. Reinecke;M. Remazeilles;C. Renault;A. Renzi;I. Ristorcelli;G. Rocha;C. Rosset;M. Rossetti;G. Roudier;J. Rubiño-Martín;B. Rusholme;M. Sandri;D. Santos;M. Savelainen;G. Savini;B. M. Schaefer;D. Scott;M. Seiffert;E. Shellard;L. Spencer;V. Stolyarov;R. Stompor;R. Sudiwala;R. Sunyaev;D. Sutton;A.-S. Suur-Uski;J. Sygnet;J. Tauber;L. Terenzi;L. Toffolatti;M. Tomasi;M. Tristram;M. Tucci;J. Tuovinen;L. Valenziano;J. Valiviita;F. V. Tent;P. Vielva;F. Villa;L. Wade;B. Wandelt;I. Wehus;D. Yvon;A. Zacchei;A. Zonca

本文介绍了普朗克2015年温度和偏振数据发布的综合萨克斯-沃尔夫（ISW）效应的研究。从不同的角度探讨了由大尺度时变引力势引起的次级宇宙微波背景辐射各向异性。CMB与不同的大尺度结构（LSS）示踪剂交叉相关：来自NVSS目录的射电源;来自光学SDSS和红外WISE调查的星系;以及普朗克2015会聚透镜图。CMB与示踪剂的联合互相关产生4σ的检测，其中大部分信噪比是由于普朗克透镜和NVSS射电目录。事实上，从普朗克数据中仅在103 σ处检测到ISW效应（通过ISW透镜双谱），这与通过结合来自上述所有星系目录的互相关信号所达到的检测水平相似。我们研究了ISW效应对暗能量参数的约束能力，特别是，我们发现ΩΛ在大于3σ时被检测到。由于2015年版本中可用的偏振尺度不允许CMB-LSS互相关可探测性的显着改善，因此仅使用普朗克温度数据进行互相关分析。然而，普朗克偏振数据被用来研究先前通过孔径测光在已知超星系团和超空洞位置的堆积CMB特征上报告的异常大的ISW信号，这与ΛCDM的预期相冲突。我们发现，目前的普朗克极化数据并不排除这种信号可能是由ISW效应。此外，叠加的普朗克透镜映射的位置上的超结构表现出积极的交叉相关，这些大规模的结构。最后，我们改进了我们以前的重建的ISW温度波动的信息编码在所有前面提到的LSS示踪剂相结合。特别是，我们构建了一个地图的ISW二次各向异性和相应的不确定性地图，从模拟中获得。我们还探讨了由2 MASS测光红移巡天（2 MPZ）跟踪的大尺度结构所引起的ISW各向异性的重建，通过直接将密度场反演为引力势场。

This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. This secondary cosmic microwave background (CMB) anisotropy caused by the large-scale time-evolving gravitational potential is probed from different perspectives. The CMB is cross-correlated with different large-scale structure (LSS) tracers: radio sources from the NVSS catalogue; galaxies from the optical SDSS and the infrared WISE surveys; and the Planck 2015 convergence lensing map. The joint cross-correlation of the CMB with the tracers yields a detection at 4σ where most of the signal-to-noise is due to the Planck lensing and the NVSS radio catalogue. In fact, the ISW effect is detected from the Planck data only at ≈3σ (through the ISW-lensing bispectrum), which is similar to the detection level achieved by combining the cross-correlation signal coming from all the galaxy catalogues mentioned above. We study the ability of the ISW effect to place constraints on the dark-energy parameters; in particular, we show that ΩΛ is detected at more than 3σ. This cross-correlation analysis is performed only with the Planck temperature data, since the polarization scales available in the 2015 release do not permit significant improvement of the CMB-LSS cross-correlation detectability. Nevertheless, the Planck polarization data are used to study the anomalously large ISW signal previously reported through the aperture photometry on stacked CMB features at the locations of known superclusters and supervoids, which is in conflict with ΛCDM expectations. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. In addition, the stacking of the Planck lensing map on the locations of superstructures exhibits a positive cross-correlation with these large-scale structures. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. We also explore the reconstruction of the ISW anisotropies caused by the large-scale structure traced by the 2MASS Photometric Redshift Survey (2MPZ) by directly inverting the density field into the gravitational potential field.

Planck 2015 results: XXI. The integrated Sachs-Wolfe effect

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