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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Hitomi observation of radio galaxy NGC?1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an active galactic nucleus
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Hitomi observation of radio galaxy NGC?1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an active galactic nucleus

机译：射电星系NGC？1275的瞳孔观察：第一个X射线量热仪，从活动银河核发射Fe-Kα线

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The origin of the narrow Fe-Kα fluorescence line at 6.4?keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In 2016 February–March, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) on board the Hitomi satellite of the Fanaroff–Riley type?I radio galaxy NGC?1275 at the center of the Perseus cluster of galaxies. With the high-energy resolution of ～5?eV at 6?keV achieved by Hitomi/SXS, we detected the Fe-Kα line with ～5.4?σ significance. The velocity width is constrained to be 500–1600?km?s?1 (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC?1275 nucleus up to ～20?keV, giving an equivalent width of ～20?eV for the 6.4?keV line. Because the velocity width is narrower than that of the broad Hα line of ～2750?km?s?1, we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-Kα line comes from a region within ～1.6?kpc of the NGC?1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-Kα line from NGC?1275 is likely a low-covering-fraction molecular torus or a rotating molecular disk which probably extends from a parsec to hundreds of parsecs scale in the active galactic nucleus system.
机译：活跃的银河核在6.4？keV处出现狭窄的Fe-Kα荧光线的起源一直存在争议。一些可能的位置是外部吸积盘，粗线区域，分子环面或星际/星际间介质。 2016年2月至3月，我们在珀尔修斯星团中心的Fanaroff-Riley型“我”射电星系NGC？1275的Hitomi卫星上使用软X射线光谱仪（SXS）进行了首次X射线微热量计光谱分析星系。用Hitomi / SXS在6？keV达到〜5？eV的高能分辨率，我们检测到了〜5.4？σ的Fe-Kα谱线。在90％置信度下，速度宽度限制为500–1600？km？s？1（对于高斯模型，FWHM）。 SXS还限制了从NGC？1275核到〜20？keV的连续谱，对于6.4？keV线，等效宽度为〜20？eV。因为速度宽度比〜2750？km？s？1的宽Hα线的速度宽度窄，所以我们可以从吸积盘和宽线区域排除对线通量的很大贡献。此外，我们对Hitomi / SXS数据进行了像素图分析，并对Chandra档案数据进行了图像分析，结果表明Fe-Kα线来自NGC？1275核心约1.6？kpc范围内的一个活跃银河系。核发射占主导地位，而不是来自集群内介质。因此，我们认为来自NGC？1275的Fe-Kα谱线的来源可能是覆盖率低的分子圆环或旋转的分子盘，在活跃的银河原子核系统中，其旋转可能从视差延伸到数百视差。

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