Testing the no-hair theorem with black hole ringdowns using TIGER
Testing the no-hair theorem with black hole ringdowns using TIGER
复制标题
使用 TIGER 测试带有黑洞环减的无毛定理
DOI：
10.1103/physrevd.90.064009
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发表时间：
2014
影响因子：
5
通讯作者：
Meidam J
中科院分区：
文献类型：
--
作者：
Meidam J
爱因斯坦望远镜是一个拟议中的第三代引力波天文台，它将通过观察黑洞振铃信号的特征频率和阻尼时间来检验无毛定理。在以前的工作中，它表明，与一个单一的黑洞在距离Gpc（或红移），百分之几的偏差的频率和阻尼时间的主导和次主导模式将在可检测的范围内。考虑到这样的源可能相对稀少，看看无毛定理在更大距离和更小信噪比的事件中的测试效果如何，从而访问更大的空间体积和更多的源是很有意义的。我们采用了一种名为TIGER（通用相对论测试基础设施）的模型选择方案，该方案最初是为了测试广义相对论而开发的，其微弱的二进制合并信号将在第二代探测器（如Advanced LIGO和Advanced Virgo）中看到。TIGER非常适合于低信噪比的情况，并且可以将来自多个源的信息进行组合，以达到更强的测试。通过使用爱因斯坦望远镜的预期噪声功率谱密度进行一系列模拟，我们表明，与TIGER，类似的偏离无毛定理（如在以前的作品中考虑的）将检测到具有很大的信心usingsources均匀分布在一个comoving体积出来。
The Einstein Telescope, a proposed third-generation gravitational-wave observatory, would enable tests of the no-hair theorem by looking at the characteristic frequencies and damping times of black hole ringdown signals. In previous work it was shown that with a singleblack hole at a distanceGpc (or redshift), deviations of a few percent in the frequencies and damping times of dominant and subdominant modes would be within the range of detectability. Given that such sources may be relatively rare, it is of interest to see how well the no-hair theorem can be tested with events at much larger distances and with smaller signal-to-noise ratios, thus accessing a far bigger volume of space and a larger number of sources. We employ a model-selection scheme called TIGER (Test Infrastructure for GEneral Relativity), which was originally developed to test general relativity with weak binary coalescence signals that will be seen in second-generation detectors, such as Advanced LIGO and Advanced Virgo. TIGER is well suited for the regime of low signal-to-noise ratios, and information from a population of sources can be combined so as to arrive at a stronger test. By performing a range of simulations using the expected noise power spectral density of the Einstein Telescope, we show that with TIGER, similar deviations from the no-hair theorem (such as those considered in previous works) will be detectable with great confidence usingsources distributed uniformly in a comoving volume out to.
影响因子：
3.5
作者：
Ueda Akitoshi;T. Akutsu;M. Ando;K. Arai;A. Araya;Pai Archana;Hideki Asada;Y. Aso;L. Baggio;Yoichi Bitou;David R Blair;Junwei Cao;Dan Chen;Sheng-Jui Chen;Yanbei Chen;R. DeSalvo;Sanjeev V. Dhurandhar Satoshi Eguchi;Masataro Fujimoto;M. Fukushima;T. Futamase;Rina Gondo;T. Harada;T. Haruyama;Katsuya Hashizume;K. Hayama;S. Hayashi;Kousuke Higashiura;A. Higuchi;Y. Himemoto;S. Hiramatsu;Shinya Hiratani;E. Hirose;Akira Honma;K. Ioka;H. Ishizaki;H. Ishizuka;Yousuke Ito;Utako Iwasaki;Kiwamu Izumi;Warren Johnson;L. Ju;T. Kajita;M. Kamiizumi;N. Kanda;K. Kashiyama;K. Kawabe;S. Kawamura;Takayoshi Kawara;F. Kawazoe;Agatsuma Kazuhiro;Somiya Kentaro;N. Kimura;Shigeaki Koike;Y. Kojima;K. Kokeyama;W. Kokuyama;K. Kotake;Nakamura Kouji;K. Kuroda;S. Márka;N. Matsumoto;Hsien-Hao Mei;H. Miao;Y. Michimura;V. Milyukov;N. Mio;S. Mitra;O. Miyakawa;S. Miyoki;Takumi Mori;S. Moriwaki;M. Musha;S. Nagano;Ken’ichi Nakagawa;Takashi Nakamura;H. Nakano;K. Nakao;I. Nakatani;W. Ni;E. Nishida;Atsushi Nisizawa;K. Numata;M. Ohashi;N. Ohishi;N. Ohmae;T. Ohmori;Keita Oikawa;Takeshi Okada;Yuta Okada;K. Oohara;S. Pan;Xianyao Ping;S. Reid;N. Sago;Motoyuki Saijo;T. Saito;Y. Saito;Y. Sakakibara;S. Sakata;M. Sasaki;S. Sato;Yuichiro Sekigchi;T. Sekiguchi;N. Seto;K. Shibata;Masaru Shibata;T. Shintomi;Mananori Sumiya;Toshikazu Suzuki;Ayaka Syoda;H. Tagoshi;Shigeki Tajima;H. Takahashi;H. Takahashi;R. Takahashi;A. Takamori;T. Takatsuji;K. Takayama;N. Tanaka;Takahiro Tanaka;A. Taruya;Daisuko Tatsumi;S. Telada;Michael E. Tobar;Y. Torii;Kimio Tsubomo;T. Uchiyama;K. Ueda;Kouji Uryu;T. Ushiba;Kyohei Watanabe;L. Wen;Kent Yagi;Shoichi Yamada;A. Yamamoto;Kazuhiro Yamamoto;Takahiro Yamamoto;Zhang Yang;J. Yokoyama;H. Yoneda;Susa Yuki;H. Yuzurihara;X. Zhai;Chunnong Zhao;Zong-hong Zhu
通讯作者：
Ueda Akitoshi;T. Akutsu;M. Ando;K. Arai;A. Araya;Pai Archana;Hideki Asada;Y. Aso;L. Baggio;Yoichi Bitou;David R Blair;Junwei Cao;Dan Chen;Sheng-Jui Chen;Yanbei Chen;R. DeSalvo;Sanjeev V. Dhurandhar Satoshi Eguchi;Masataro Fujimoto;M. Fukushima;T. Futamase;Rina Gondo;T. Harada;T. Haruyama;Katsuya Hashizume;K. Hayama;S. Hayashi;Kousuke Higashiura;A. Higuchi;Y. Himemoto;S. Hiramatsu;Shinya Hiratani;E. Hirose;Akira Honma;K. Ioka;H. Ishizaki;H. Ishizuka;Yousuke Ito;Utako Iwasaki;Kiwamu Izumi;Warren Johnson;L. Ju;T. Kajita;M. Kamiizumi;N. Kanda;K. Kashiyama;K. Kawabe;S. Kawamura;Takayoshi Kawara;F. Kawazoe;Agatsuma Kazuhiro;Somiya Kentaro;N. Kimura;Shigeaki Koike;Y. Kojima;K. Kokeyama;W. Kokuyama;K. Kotake;Nakamura Kouji;K. Kuroda;S. Márka;N. Matsumoto;Hsien-Hao Mei;H. Miao;Y. Michimura;V. Milyukov;N. Mio;S. Mitra;O. Miyakawa;S. Miyoki;Takumi Mori;S. Moriwaki;M. Musha;S. Nagano;Ken’ichi Nakagawa;Takashi Nakamura;H. Nakano;K. Nakao;I. Nakatani;W. Ni;E. Nishida;Atsushi Nisizawa;K. Numata;M. Ohashi;N. Ohishi;N. Ohmae;T. Ohmori;Keita Oikawa;Takeshi Okada;Yuta Okada;K. Oohara;S. Pan;Xianyao Ping;S. Reid;N. Sago;Motoyuki Saijo;T. Saito;Y. Saito;Y. Sakakibara;S. Sakata;M. Sasaki;S. Sato;Yuichiro Sekigchi;T. Sekiguchi;N. Seto;K. Shibata;Masaru Shibata;T. Shintomi;Mananori Sumiya;Toshikazu Suzuki;Ayaka Syoda;H. Tagoshi;Shigeki Tajima;H. Takahashi;H. Takahashi;R. Takahashi;A. Takamori;T. Takatsuji;K. Takayama;N. Tanaka;Takahiro Tanaka;A. Taruya;Daisuko Tatsumi;S. Telada;Michael E. Tobar;Y. Torii;Kimio Tsubomo;T. Uchiyama;K. Ueda;Kouji Uryu;T. Ushiba;Kyohei Watanabe;L. Wen;Kent Yagi;Shoichi Yamada;A. Yamamoto;Kazuhiro Yamamoto;Takahiro Yamamoto;Zhang Yang;J. Yokoyama;H. Yoneda;Susa Yuki;H. Yuzurihara;X. Zhai;Chunnong Zhao;Zong-hong Zhu
DOI：
10.1007/978-3-642-41992-8_27
发表时间：
2013
期刊：
arXiv: General Relativity and Quantum Cosmology
影响因子：
--
作者：
C. Broeck
通讯作者：
C. Broeck