A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of polarbear Data

A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of polarbear Data
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DOI：
10.3847/1538-4357/aa8e9f
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发表时间：
2017-05
期刊：
The Astrophysical Journal
影响因子：
--
通讯作者：
T. C. C. P. Ade-T.-C.-C.-P.-Ade-103029307;M. Aguilar;Y. Akiba;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;F. Bianchini;D. Boettger;J. Borrill;S. Chapman;Y. Chinone;K. Crowley;A. Cukierman;M. Dobbs;A. Ducout;R. Dunner;T. Elleflot;J. Errard;G. Fabbian;S. Feeney;C. Feng;T. Fujino;N. Galitzki;A. Gilbert;N. Goeckner-wald;J. Groh;T. Hamada;G. Hall;N. Halverson;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;Y. Inoue;G. Jaehnig;A. Jaffe;O. Jeong;D. Kaneko;N. Katayama;B. Keating;R. Keskitalo;T. Kisner;N. Krachmalnicoff;A. Kusaka;M. Jeune;A. Lee;E. Leitch;D. Leon;E. Linder;L. Lowry;F. Matsuda;T. Matsumura;Y. Minami;J. Montgomery;M. Navaroli;H. Nishino;H. Paar;J. Peloton;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;P. Richards;C. Ross;Y. Segawa;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;N. Stebor;R. Stompor;A. Suzuki;O. Tajima;S. Takakura;S. Takatori;D. Tanabe;G. Teply;T. Tomaru;C. Tucker;N. Whitehorn;A. Zahn
T. C. C. P. Ade-T.-C.-C.-P.-Ade-103029307;M. Aguilar;Y. Akiba;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;F. Bianchini;D. Boettger;J. Borrill;S. Chapman;Y. Chinone;K. Crowley;A. Cukierman;M. Dobbs;A. Ducout;R. Dunner;T. Elleflot;J. Errard;G. Fabbian;S. Feeney;C. Feng;T. Fujino;N. Galitzki;A. Gilbert;N. Goeckner-wald;J. Groh;T. Hamada;G. Hall;N. Halverson;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;Y. Inoue;G. Jaehnig;A. Jaffe;O. Jeong;D. Kaneko;N. Katayama;B. Keating;R. Keskitalo;T. Kisner;N. Krachmalnicoff;A. Kusaka;M. Jeune;A. Lee;E. Leitch;D. Leon;E. Linder;L. Lowry;F. Matsuda;T. Matsumura;Y. Minami;J. Montgomery;M. Navaroli;H. Nishino;H. Paar;J. Peloton;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;P. Richards;C. Ross;Y. Segawa;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;N. Stebor;R. Stompor;A. Suzuki;O. Tajima;S. Takakura;S. Takatori;D. Tanabe;G. Teply;T. Tomaru;C. Tucker;N. Whitehorn;A. Zahn
中科院分区：
其他
文献类型：
--
作者：
T. C. C. P. Ade-T.-C.-C.-P.-Ade-103029307;M. Aguilar;Y. Akiba;K. Arnold;C. Baccigalupi;D. Barron;D. Beck;F. Bianchini;D. Boettger;J. Borrill;S. Chapman;Y. Chinone;K. Crowley;A. Cukierman;M. Dobbs;A. Ducout;R. Dunner;T. Elleflot;J. Errard;G. Fabbian;S. Feeney;C. Feng;T. Fujino;N. Galitzki;A. Gilbert;N. Goeckner-wald;J. Groh;T. Hamada;G. Hall;N. Halverson;M. Hasegawa;M. Hazumi;C. Hill;L. Howe;Y. Inoue;G. Jaehnig;A. Jaffe;O. Jeong;D. Kaneko;N. Katayama;B. Keating;R. Keskitalo;T. Kisner;N. Krachmalnicoff;A. Kusaka;M. Jeune;A. Lee;E. Leitch;D. Leon;E. Linder;L. Lowry;F. Matsuda;T. Matsumura;Y. Minami;J. Montgomery;M. Navaroli;H. Nishino;H. Paar;J. Peloton;A. Pham;D. Poletti;G. Puglisi;C. Reichardt;P. Richards;C. Ross;Y. Segawa;B. Sherwin;M. Silva-Feaver;Praweeen Siritanasak;N. Stebor;R. Stompor;A. Suzuki;O. Tajima;S. Takakura;S. Takatori;D. Tanabe;G. Teply;T. Tomaru;C. Tucker;N. Whitehorn;A. Zahn

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我们报告了一个改进的测量宇宙微波背景B模式偏振功率谱的Polarbear实验在150 GHz。通过将第二季（2013-2014年）收集的新数据添加到第一季（2012-2013年）重新分析的数据中，我们将频带功率不确定性降低了两倍。带功率报告角多极，其中占主导地位的B-模式信号预计是由于E-模式的引力透镜。我们在3.1σ的置信度下拒绝了无B模式偏振的零假设，包括统计和系统不确定性。我们通过拟合相对于普朗克2015年最佳拟合模型预测的单个透镜振幅参数AL来测试测量的B模式与Λ冷暗物质（ΛCDM）框架的一致性。我们获得± 0.14（前景）± 0.04（多），其中是基准ΛCDM值。
We report an improved measurement of the cosmic microwave background B-mode polarization power spectrum with the Polarbear experiment at 150 GHz. By adding new data collected during the second season of observations (2013–2014) to re-analyzed data from the first season (2012–2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles , where the dominant B-mode signal is expected to be due to the gravitational lensing of E-modes. We reject the null hypothesis of no B-mode polarization at a confidence of 3.1σ including both statistical and systematic uncertainties. We test the consistency of the measured B-modes with the Λ Cold Dark Matter (ΛCDM) framework by fitting for a single lensing amplitude parameter AL relative to the Planck 2015 best-fit model prediction. We obtain ± 0.14(foreground) ± 0.04(multi), where is the fiducial ΛCDM value.