Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam
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DOI：
10.3847/1538-4357/ab3424
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发表时间：
2019-04
期刊：
The Astrophysical Journal
影响因子：
--
通讯作者：
T. Namikawa;Y. Chinone;H. Miyatake;M. Oguri;R. Takahashi;A. Kusaka;N. Katayama;S. Adachi;M. Aguilar;H. Aihara;Aamir Ali;R. Armstrong;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;S. Beckman;F. Bianchini;D. Boettger;J. Borrill;K. Cheung;L. Corbett;K. Crowley;H. E. Bouhargani;T. Elleflot;J. Errard;G. Fabbian;C. Feng;N. Galitzki;N. Goeckner-wald;J. Groh;T. Hamada;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;O. Jeong;D. Kaneko;B. Keating;Adrian T. Lee;D. Leon;E. Linder;L. Lowry;A. Mangu;F. Matsuda;Y. Minami;S. Miyazaki;H. Murayama;M. Navaroli;H. Nishino;A. Nishizawa;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;J. Speagle;R. Stompor;A. Suzuki;Philip J. Tait;O. Tajima;M. Takada;S. Takakura;S. Takatori;D. Tanabe;Masayuki Tanaka;G. Teply;C. Tsai;C. Vergés;B. Westbrook;Yuyang Zhou;The Polarbear Collaboration;The H.E.S.S. Collaboration
T. Namikawa;Y. Chinone;H. Miyatake;M. Oguri;R. Takahashi;A. Kusaka;N. Katayama;S. Adachi;M. Aguilar;H. Aihara;Aamir Ali;R. Armstrong;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;S. Beckman;F. Bianchini;D. Boettger;J. Borrill;K. Cheung;L. Corbett;K. Crowley;H. E. Bouhargani;T. Elleflot;J. Errard;G. Fabbian;C. Feng;N. Galitzki;N. Goeckner-wald;J. Groh;T. Hamada;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;O. Jeong;D. Kaneko;B. Keating;Adrian T. Lee;D. Leon;E. Linder;L. Lowry;A. Mangu;F. Matsuda;Y. Minami;S. Miyazaki;H. Murayama;M. Navaroli;H. Nishino;A. Nishizawa;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;J. Speagle;R. Stompor;A. Suzuki;Philip J. Tait;O. Tajima;M. Takada;S. Takakura;S. Takatori;D. Tanabe;Masayuki Tanaka;G. Teply;C. Tsai;C. Vergés;B. Westbrook;Yuyang Zhou;The Polarbear Collaboration;The H.E.S.S. Collaboration
中科院分区：
其他
文献类型：
--
作者：
T. Namikawa;Y. Chinone;H. Miyatake;M. Oguri;R. Takahashi;A. Kusaka;N. Katayama;S. Adachi;M. Aguilar;H. Aihara;Aamir Ali;R. Armstrong;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;S. Beckman;F. Bianchini;D. Boettger;J. Borrill;K. Cheung;L. Corbett;K. Crowley;H. E. Bouhargani;T. Elleflot;J. Errard;G. Fabbian;C. Feng;N. Galitzki;N. Goeckner-wald;J. Groh;T. Hamada;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;O. Jeong;D. Kaneko;B. Keating;Adrian T. Lee;D. Leon;E. Linder;L. Lowry;A. Mangu;F. Matsuda;Y. Minami;S. Miyazaki;H. Murayama;M. Navaroli;H. Nishino;A. Nishizawa;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;J. Speagle;R. Stompor;A. Suzuki;Philip J. Tait;O. Tajima;M. Takada;S. Takakura;S. Takatori;D. Tanabe;Masayuki Tanaka;G. Teply;C. Tsai;C. Vergés;B. Westbrook;Yuyang Zhou;The Polarbear Collaboration;The H.E.S.S. Collaboration

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我们提出了第一次测量的透镜势之间的互相关，从宇宙微波背景（CMB）的偏振数据重建，和宇宙剪切场从星系的形状。该测量是使用Polarbear CMB实验和Subaru Hyper Suprime-Cam（HSC）调查的数据进行的。通过分析11 deg 2的重叠区域，我们拒绝了3.5σ的零假设，并将互谱的振幅限制为，其中是基于平坦Λ冷暗物质宇宙学相对于普朗克2018预测归一化的振幅。第一次测量这种交叉光谱而不依赖于CMB温度测量是可能的，这是由于北极熊深地图的噪声水平为1.66 μK弧分，以及深HSC数据的高星系数密度为。我们提出了一个详细的研究的系统预算表明，在我们的研究结果中，剩余的系统是微不足道的小，这表明了这种互相关技术的未来潜力。
We present the first measurement of cross-correlation between the lensing potential, reconstructed from cosmic microwave background (CMB) polarization data, and the cosmic shear field from galaxy shapes. This measurement is made using data from the Polarbear CMB experiment and the Subaru Hyper Suprime-Cam (HSC) survey. By analyzing an 11 deg2 overlapping region, we reject the null hypothesis at 3.5σ and constrain the amplitude of the cross-spectrum to , where is the amplitude normalized with respect to the Planck 2018 prediction, based on the flat Λ cold dark matter cosmology. The first measurement of this cross-spectrum without relying on CMB temperature measurements is possible owing to the deep Polarbear map with a noise level of ∼6 μK arcmin, as well as the deep HSC data with a high galaxy number density of . We present a detailed study of the systematics budget to show that residual systematics in our results are negligibly small, which demonstrates the future potential of this cross-correlation technique.