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arXiv 1804.05652astro-ph.GAastro-ph.HE
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寻找与超快X射线外流对应的H I Lyman $α$

A Search for H I Lyman $α$ Counterparts to Ultra-Fast X-ray Outflows

G. A. Kriss, J. C. Lee, A. Danehkar

备注：
18 pages, 11 figures. Accepted for publication in ApJ, 4/16/18
发表信息：
Astrophys.J.859:94,2018
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摘要：

在类星体PG~1211+143中，H I Ly $α$吸收与X射线在-17，300 $\rm km~s^{-1}$处的超快流出有关，我们在H I Ly $α$吸收的预期位置搜索了存档的紫外光谱，以寻找在XMM-牛顿和朱雀观测中发现的超快流出的大样本。16个X射线流出预测H I Ly $α$波长落入远紫外线光谱探测器或哈勃太空望远镜的光谱带通范围内，尽管没有一个档案观测与发现UFO的X射线观测同时进行。在我们的光谱中，具有1000 $\rm km~s^{-1}$的半峰全宽的宽特征具有通常< $2\times10^{13}~\rm cm^{-2}$的HI柱密度的2- $σ$上限。使用网格的光电离模型覆盖了广泛的光谱能量分布，我们发现，生产Fe XXVI的赖氨酸$α$ X射线吸收与等效宽度$>30$ eV和相关的H I的赖氨酸$α$吸收与$\rm N_{HI}<2\times10^{13}~cm^{-2}$需要总吸收柱密度$\rm N_{H}>5\times10^{22}~cm^{-2}$和电离参数log $ξ$ > 3.7。然而，如果电离参数仅略低于Fe XXV和Fe XXVI的峰值电离分数，则宽范围的SED将预测可观察到的H I Ly $α$吸收。在存档的紫外光谱中缺少Ly $α$特征表明，不明飞行物要么具有非常高的电离参数，非常硬的紫外电离光谱，要么由于可变性，它们在紫外光谱观测时不存在。

英文摘要：

Prompted by the H I Ly$α$ absorption associated with the X-ray ultra-fast outflow at -17,300 $\rm km~s^{-1}$ in the quasar PG~1211+143, we have searched archival UV spectra at the expected locations of H I Ly$α$ absorption for a large sample of ultra-fast outflows identified in XMM-Newton and Suzaku observations. Sixteen of the X-ray outflows have predicted H I Ly$α$ wavelengths falling within the bandpass of spectra from either the Far Ultraviolet Spectroscopic Explorer or the Hubble Space Telescope, although none of the archival observations were simultaneous with the X-ray observations in which UFOs were detected. In our spectra broad features with full-width at half-maximum of 1000 $\rm km~s^{-1}$ have 2-$σ$ upper limits on the H I column density of generally <$2\times10^{13}~\rm cm^{-2}$. Using grids of photoionization models covering a broad range of spectral energy distributions, we find that producing Fe XXVI Ly$α$ X-ray absorption with equivalent widths $>30$ eV and associated H I Ly$α$ absorption with $\rm N_{HI}<2\times10^{13}~cm^{-2}$ requires total absorbing column densities $\rm N_{H}>5\times10^{22}~cm^{-2}$ and ionization parameters log $ξ$ > 3.7. Nevertheless, a wide range of SEDs would predict observable H I Ly$α$ absorption if ionization parameters are only slightly below peak ionization fractions for Fe XXV and Fe XXVI. The lack of Ly$α$ features in the archival UV spectra indicates that either the UFOs have very high ionization parameters, very hard UV-ionizing spectra, or that they were not present at the time of the UV spectral observations due to variability.

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