Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS
Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS
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DOI：
10.1093/pasj/psx127
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发表时间：
2017-10
影响因子：
2.3
通讯作者：
F. Aharonian;H. Akamatsu;F. Akimoto;S. Allen;S. Allen;L. Angelini;M. Audard;H. Awaki;M. Axelsson;A. Bamba;M. Bautz;R. Blandford;R. Blandford;L. Brenneman;G. V. Brown;E. Bulbul;E. Cackett;M. Chernyakova;M. Chiao;P. Coppi;E. Costantini;J. Plaa;C. Vries;J. Herder;C. Done;T. Dotani;K. Ebisawa;M. Eckart;T. Enoto;Y. Ezoe;A. Fabian;C. Ferrigno;A. Foster;R. Fujimoto;Y. Fukazawa;M. Furukawa;A. Furuzawa;M. Galeazzi;L. Gallo;P. Gandhi;M. Giustini;A. Goldwurm;L. Gu;M. Guainazzi;Y. Haba;K. Hagino;K. Hamaguchi;K. Hamaguchi;I. Harrus;I. Harrus;I. Hatsukade;K. Hayashi;K. Hayashi;T. Hayashi;K. Hayashida;J. Hiraga;A. Hornschemeier;A. Hoshino;J. Hughes;Y. Ichinohe;R. Iizuka;H. Inoue;Y. Inoue;M. Ishida;K. Ishikawa;Y. Ishisaki;M. Iwai;J. Kaastra;J. Kaastra;T. Kallman;T. Kamae;J. Kataoka;S. Katsuda;N. Kawai;R. Kelley;C. Kilbourne;T. Kitaguchi;S. Kitamoto;T. Kitayama;T. Kohmura;M. Kokubun;K. Koyama;S. Koyama;P. Kretschmar;H. Krimm;H. Krimm;A. Kubota;H. Kunieda;P. Laurent;Shiu-Hang Lee;M. Leutenegger;O. Limousin;M. Loewenstein;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;K. Mukai;Koji Mukai;H. Murakami;R. Mushotzky;T. Nakagawa;H. Nakajima;T. Nakamori;S. Nakashima;K. Nakazawa;Kumiko K. Norukawa;M. Nobukawa;H. Noda;H. Odaka;A. Ogorzałek;T. Ohashi;M. Ohno;T. Okajima;N. Ota;M. Ozaki;F. Paerels;S. Paltani;R. Petre;C. Pinto;F. Porter;K. Pottschmidt;K. Pottschmidt;C. Reynolds;S. Safi-Harb;S. Saito;K. Sakai;T. 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;T. Tamura;Takaaki Tanaka;Yasuo Tanaka;Yasuo Tanaka;Yasuyuki T. Tanaka;M. Tashiro;Y. Tawara;Y. Terada;Y. Terashima;F. Tombesi;F. Tombesi;F. Tombesi;H. Tomida;Y. Tsuboi;M. Tsujimoto;H. Tsunemi;T. Tsuru;H. Uchida;H. Uchiyama;Y. Uchiyama;S. Ueda;Y. Ueda;S. Uno;C. M. Urry;E. Ursino;S. Watanabe;N. Werner;N. Werner;N. Werner;D. Wilkins;B. Williams;S. Yamada;H. Yamaguchi;H. Yamaguchi;K. Yamaoka;N. Yamasaki;M. Yamauchi;S. Yamauchi;T. Yaqoob;T. Yaqoob;Y. Yatsu;D. Yonetoku;I. Zhuravleva;A. Zoghbi
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文献类型：
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作者：
F. Aharonian;H. Akamatsu;F. Akimoto;S. Allen;S. Allen;L. Angelini;M. Audard;H. Awaki;M. Axelsson;A. Bamba;M. Bautz;R. Blandford;R. Blandford;L. Brenneman;G. V. Brown;E. Bulbul;E. Cackett;M. Chernyakova;M. Chiao;P. Coppi;E. Costantini;J. Plaa;C. Vries;J. Herder;C. Done;T. Dotani;K. Ebisawa;M. Eckart;T. Enoto;Y. Ezoe;A. Fabian;C. Ferrigno;A. Foster;R. Fujimoto;Y. Fukazawa;M. Furukawa;A. Furuzawa;M. Galeazzi;L. Gallo;P. Gandhi;M. Giustini;A. Goldwurm;L. Gu;M. Guainazzi;Y. Haba;K. Hagino;K. Hamaguchi;K. Hamaguchi;I. Harrus;I. Harrus;I. Hatsukade;K. Hayashi;K. Hayashi;T. Hayashi;K. Hayashida;J. Hiraga;A. Hornschemeier;A. Hoshino;J. Hughes;Y. Ichinohe;R. Iizuka;H. Inoue;Y. Inoue;M. Ishida;K. Ishikawa;Y. Ishisaki;M. Iwai;J. Kaastra;J. Kaastra;T. Kallman;T. Kamae;J. Kataoka;S. Katsuda;N. Kawai;R. Kelley;C. Kilbourne;T. Kitaguchi;S. Kitamoto;T. Kitayama;T. Kohmura;M. Kokubun;K. Koyama;S. Koyama;P. Kretschmar;H. Krimm;H. Krimm;A. Kubota;H. Kunieda;P. Laurent;Shiu-Hang Lee;M. Leutenegger;O. Limousin;M. Loewenstein;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;K. Mukai;Koji Mukai;H. Murakami;R. Mushotzky;T. Nakagawa;H. Nakajima;T. Nakamori;S. Nakashima;K. Nakazawa;Kumiko K. Norukawa;M. Nobukawa;H. Noda;H. Odaka;A. Ogorzałek;T. Ohashi;M. Ohno;T. Okajima;N. Ota;M. Ozaki;F. Paerels;S. Paltani;R. Petre;C. Pinto;F. Porter;K. Pottschmidt;K. Pottschmidt;C. Reynolds;S. Safi-Harb;S. Saito;K. Sakai;T. 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;T. Tamura;Takaaki Tanaka;Yasuo Tanaka;Yasuo Tanaka;Yasuyuki T. Tanaka;M. Tashiro;Y. Tawara;Y. Terada;Y. Terashima;F. Tombesi;F. Tombesi;F. Tombesi;H. Tomida;Y. Tsuboi;M. Tsujimoto;H. Tsunemi;T. Tsuru;H. Uchida;H. Uchiyama;Y. Uchiyama;S. Ueda;Y. Ueda;S. Uno;C. M. Urry;E. Ursino;S. Watanabe;N. Werner;N. Werner;N. Werner;D. Wilkins;B. Williams;S. Yamada;H. Yamaguchi;H. Yamaguchi;K. Yamaoka;N. Yamasaki;M. Yamauchi;S. Yamauchi;T. Yaqoob;T. Yaqoob;Y. Yatsu;D. Yonetoku;I. Zhuravleva;A. Zoghbi
由于其高光谱分辨率（类似于6 keV时的5 eV），Hitomi上的软X射线光谱仪（SXS）使我们能够首次测量星系团中高度电离离子的空间分辨发射线的详细结构。在本系列论文中，我们利用SXS测量了英仙座星系团核心气体的运动速度、金属丰度和气体的多温结构。在这里，我们表明，当推断的物理性质，如英仙座系统的线发射率，共振散射效应应考虑在内。在Hitomi波段，共振散射主要影响Fe XXV He α线（w）-光谱中最强的线。Hitomi在这条线上测量到的通量被抑制了一个类似于1.3的因子，在内部类似于30 kpc，与光学薄等离子体的预测相比;抑制随着离中心的距离而减小。w线也比来自同一离子的其他线稍宽。观测到的w线通量、形状和距离依赖性的扭曲都与英仙座核心共振散射的预期效果一致。通过测量光学厚线（w）和光学薄线（Fe XXV禁戒线、He β线、Ly α线）中的通量比，并将这些比值与蒙特卡罗辐射传输模拟的预测值进行比较，得到了气体运动的速度。结果是一致的气体速度的直接测量线加宽描述在本系列的其他地方，虽然系统和统计的不确定性仍然显着。在等离子体模型中对线发射率的预测的进一步改进，以及对未来X射线任务的更深入观察，提供与Hitomi SXS类似或更好的能力，将使共振散射测量能够对星系团气体运动的振幅和各向异性提供强大的约束。
Thanks to its high spectral resolution (similar to 5 eV at 6 keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus Cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering effect should be taken into account. In the Hitomi waveband, resonant scattering mostly affects the Fe XXV He alpha line (w)-the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor of similar to 1.3 in the inner similar to 30 kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The w line also appears slightly broader than other lines from the same ion. The observed distortions of the w line flux, shape, and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick (w) and thin (Fe XXV forbidden, He beta, Ly alpha) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions offering similar or better capabilities to the Hitomi SXS, will enable resonant scattering measurements to provide powerful constraints on the amplitude and anisotropy of cluster gas motions.