Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster
Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster
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DOI：
10.3847/2041-8213/aa61fa
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发表时间：
2016-07
期刊：
影响因子：
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通讯作者：
H. C. F. Aharonian;H. Akamatsu;F. Akimoto;S. Allen;L. Angelini;K. Arnaud;M. Audard;H. Awaki;M. Axelsson;A. Bamba;M. Bautz;R. Blandford;L. Brenneman;G. V. Brown;E. Bulbul;E. Cackett;M. Chernyakova;M. Chiao;P. Coppi;E. Costantini;J. Plaa;J. Herder;C. Done;T. Dotani;K. Ebisawa;M. Eckart;T. Enoto;Y. Ezoe;A. Fabian;C. Ferrigno;A. Foster;R. Fujimoto;Y. Fukazawa;A. Furuzawa;M. Galeazzi;L. Gallo;P. Gandhi;M. Giustini;A. Goldwurm;L. Gu;M. Guainazzi;Y. Haba;K. Hagino;K. Hamaguchi;I. Harrus;I. Hatsukade;K. Hayashi;T. Hayashi;K. Hayashida;J. Hiraga;A. Hornschemeier;A. Hoshino;J. Hughes;Y. Ichinohe;R. Iizuka;H. Inoue;S. Inoue;Y. Inoue;K. Ishibashi;M. Ishida;K. Ishikawa;Y. Ishisaki;M. Itoh;M. Iwai;N. Iyomoto;J. Kaastra;T. Kallman;T. Kamae;E. Kara;J. Kataoka;S. Katsuda;J. Katsuta;M. Kawaharada;N. Kawai;R. Kelley;D. Khangulyan;C. Kilbourne;A. King;T. Kitaguchi;S. Kitamoto;T. Kitayama;T. Kohmura;M. Kokubun;S. Koyama;K. Koyama;P. Kretschmar;H. Krimm;A. Kubota;H. Kunieda;P. Laurent;F. Lebrun;Shiu-Hang Lee;M. Leutenegger;O. Limousin;M. Loewenstein;K. Long;D. Lumb;G. Madejski;Y. Maeda;D. Maier;K. Makishima;M. Markevitch;H. Matsumoto;K. Matsushita;D. McCammon;B. McNamara;M. Mehdipour;E. Miller;Jonathan M. Miller;S. Mineshige;K. Mitsuda;I. Mitsuishi;T. Miyazawa;T. Mizuno;H. Mori;K. Mori;H. Moseley;Koji Mukai;H. Murakami;T. Murakami;R. Mushotzky;T. Nakagawa;H. Nakajima;T. Nakamori;T. Nakano;S. Nakashima;K. Nakazawa;K. Nobukawa;M. Nobukawa;H. Noda;M. Nomachi;S. O’Dell;H. Odaka;T. Ohashi;M. Ohno;T. Okajima;N. Ota;M. Ozaki;F. Paerels;S. Paltani;A. Parmar;R. Petre;C. Pinto;M. Pohl;F. Porter;K. Pottschmidt;B. Ramsey;C. Reynolds;H. Russell;S. Safi-Harb;S. Saito;K. Sakai;H. Sameshima;Toru Sasaki;G. Sato;Kosuke Sato;R. Sato;M. Sawada;N. Schartel;P. Serlemitsos;H. Seta;M. Shidatsu;A. Simionescu;Randall K. Smith;Y. Soong;L. Stawarz;Y. Sugawara;S. Sugita;A. Szymkowiak;H. Tajima;H. Takahashi;Tadayuki Takahashi;S. Takeda;Y. Takei;T. Tamagawa;K. Tamura;T. Tamura;Takaaki Tanaka;Yasuo Tanaka;Yasuyuki T. Tanaka;M. Tashiro;Y. Tawara;Y. Terada;Y. Terashima;F. Tombesi;H. Tomida;Y. Tsuboi;M. Tsujimoto;H. Tsunemi;T. Tsuru;H. Uchida;H. Uchiyama;Y. Uchiyama;S. Ueda;Y. Ueda;S. Ueno;S. Uno;C. M. Urry;E. Ursino;C. Vries;S. Watanabe;N. Werner;D. Wik;D. Wilkins;B. Williams;S. Yamada;H. Yamaguchi;K. Yamaoka;N. Yamasaki;M. Yamauchi;S. Yamauchi;T. Yaqoob;Y. Yatsu;D. Yonetoku;A. Yoshida;I. Zhuravleva;A. Zoghbi
中科院分区：
文献类型：
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作者：
H. C. F. Aharonian;H. Akamatsu;F. Akimoto;S. Allen;L. Angelini;K. Arnaud;M. Audard;H. Awaki;M. Axelsson;A. Bamba;M. Bautz;R. Blandford;L. Brenneman;G. V. Brown;E. Bulbul;E. Cackett;M. Chernyakova;M. Chiao;P. Coppi;E. Costantini;J. Plaa;J. Herder;C. Done;T. Dotani;K. Ebisawa;M. Eckart;T. Enoto;Y. Ezoe;A. Fabian;C. Ferrigno;A. Foster;R. Fujimoto;Y. Fukazawa;A. Furuzawa;M. Galeazzi;L. Gallo;P. Gandhi;M. Giustini;A. Goldwurm;L. Gu;M. Guainazzi;Y. Haba;K. Hagino;K. Hamaguchi;I. Harrus;I. Hatsukade;K. Hayashi;T. Hayashi;K. Hayashida;J. Hiraga;A. Hornschemeier;A. Hoshino;J. Hughes;Y. Ichinohe;R. Iizuka;H. Inoue;S. Inoue;Y. Inoue;K. Ishibashi;M. Ishida;K. Ishikawa;Y. Ishisaki;M. Itoh;M. Iwai;N. Iyomoto;J. Kaastra;T. Kallman;T. Kamae;E. Kara;J. Kataoka;S. Katsuda;J. Katsuta;M. Kawaharada;N. Kawai;R. Kelley;D. Khangulyan;C. Kilbourne;A. King;T. Kitaguchi;S. Kitamoto;T. Kitayama;T. Kohmura;M. Kokubun;S. Koyama;K. Koyama;P. Kretschmar;H. Krimm;A. Kubota;H. Kunieda;P. Laurent;F. Lebrun;Shiu-Hang Lee;M. Leutenegger;O. Limousin;M. Loewenstein;K. Long;D. Lumb;G. Madejski;Y. Maeda;D. Maier;K. Makishima;M. Markevitch;H. Matsumoto;K. Matsushita;D. McCammon;B. McNamara;M. Mehdipour;E. Miller;Jonathan M. Miller;S. Mineshige;K. Mitsuda;I. Mitsuishi;T. Miyazawa;T. Mizuno;H. Mori;K. Mori;H. Moseley;Koji Mukai;H. Murakami;T. Murakami;R. Mushotzky;T. Nakagawa;H. Nakajima;T. Nakamori;T. Nakano;S. Nakashima;K. Nakazawa;K. Nobukawa;M. Nobukawa;H. Noda;M. Nomachi;S. O’Dell;H. Odaka;T. Ohashi;M. Ohno;T. Okajima;N. Ota;M. Ozaki;F. Paerels;S. Paltani;A. Parmar;R. Petre;C. Pinto;M. Pohl;F. Porter;K. Pottschmidt;B. Ramsey;C. Reynolds;H. Russell;S. Safi-Harb;S. Saito;K. Sakai;H. Sameshima;Toru Sasaki;G. Sato;Kosuke Sato;R. Sato;M. Sawada;N. Schartel;P. Serlemitsos;H. Seta;M. Shidatsu;A. Simionescu;Randall K. Smith;Y. Soong;L. Stawarz;Y. Sugawara;S. Sugita;A. Szymkowiak;H. Tajima;H. Takahashi;Tadayuki Takahashi;S. Takeda;Y. Takei;T. Tamagawa;K. Tamura;T. Tamura;Takaaki Tanaka;Yasuo Tanaka;Yasuyuki T. Tanaka;M. Tashiro;Y. Tawara;Y. Terada;Y. Terashima;F. Tombesi;H. Tomida;Y. Tsuboi;M. Tsujimoto;H. Tsunemi;T. Tsuru;H. Uchida;H. Uchiyama;Y. Uchiyama;S. Ueda;Y. Ueda;S. Ueno;S. Uno;C. M. Urry;E. Ursino;C. Vries;S. Watanabe;N. Werner;D. Wik;D. Wilkins;B. Williams;S. Yamada;H. Yamaguchi;K. Yamaoka;N. Yamasaki;M. Yamauchi;S. Yamauchi;T. Yaqoob;Y. Yatsu;D. Yonetoku;A. Yoshida;I. Zhuravleva;A. Zoghbi
Hitomi的高分辨率X射线光谱学预计将解决在各种大质量系统的几个低分辨率研究中报告的微弱不明发射线的起源，例如星系和星团，包括英仙座星团。我们已经分析了Hitomi对英仙座星团的第一次观测。在暗物质衰变的情况下，基于来自大型星团样本的XMM-牛顿信号，英仙座的预期发射线太微弱，无法在Hitomi数据中检测到。然而，先前报道的英仙座3.5千电子伏的通量与基于样本的预测相比高得令人不安。我们在报告的高通量水平上没有发现不明谱线。考虑到XMM测量在这一区域的不确定性，与Hitomi的不一致性对于宽的暗物质线是99%的显著性，对于来自气体的窄线是99.7%。我们没有发现附近微弱的K线或Ar卫星线异常高的通量，而这些线是作为早期3.5 keV检测的解释而提出的。我们确实发现了一个暗示，一个广泛的过剩附近的能量高n跃迁的S xvi（休息帧）-一个可能的签名的电荷交换的分子星云和另一个建议的解释不明线。虽然它的能量与XMM pn检测一致，但它不太可能解释MOS信号。这个有趣的特征的确认必须等待未来的量热计实验进行更灵敏的观察。
High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S xvi ( rest-frame)—a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.