arXiv 2103.112242021-03-20astro-ph.GA

AGN环面在Circinus星系中位置的X射线约束

X-ray Constraint on Location of AGN Torus in Circinus Galaxy

Ryosuke Uematsu, Yoshihiro Ueda, Atsushi Tanimoto, Taiki Kawamuro, Kenta Setoguchi, Shoji Ogawa, Satoshi Yamada, Hirokazu Odaka

备注：: 20 pages, 10 figures, 8 tables, accepted for publication in ApJ
DOI：: 10.3847/1538-4357/abf0a2

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摘要：

活动星系核（AGN）中的模糊“环面”的位置仍然是一个悬而未决的问题。源自环面，特别是Fe K $α$的X射线荧光线的线宽携带关于线发射区域的半径的关键信息。利用XCLUMPY（Tanimoto et al. 2019），一种X射线cluquetorus模型，我们开发了一个来自AGN环面的发射线轮廓的现实模型，其中我们考虑了由于黑洞周围的开普勒运动而导致的线加宽。然后，我们将更新后的模型应用于朱雀，XMM-牛顿，核光谱望远镜阵列（NuSTAR）和钱德拉，包括0.62 MS钱德拉/HETG数据观察到的最佳宽带光谱（3-100千电子伏）的Circinus星系。我们确认，环是康普顿厚（沿赤道面的氢柱密度为$N_\mathrm{H}^\mathrm{Equ}=2.16^{+0.24}_{-0.16}\times 10^{25}\ \mathrm{cm}^{-2}$），几何薄（环角宽度$σ=10.3^{+0.7}_{-0.3}\ \mathrm{degrees}$），观察边缘（倾角$i=78.3^{+0.4}_{-0.9}\ \mathrm{degrees}$），并具有超太阳丰度（$1.52^{+0.04}_{-0.06}$倍太阳）。同时分析钱德拉/HETG的第一，第二，第三阶光谱与考虑的空间范围的Fe K $α$线发射区域，我们约束的环的内半径为$1.9^{+3.1}_{-0.8}\times 10^5$倍的引力半径，或$1.6^{+1.5}_{-0.9}\times 10^{-2}\ \mathrm{pc}$的黑洞质量的$(1.7\pm 0.3)\times 10^6\ M_{\odot}$。这比根据尘埃升华半径估算的结果小3倍左右，表明环的尘埃区内侧是由无尘气体组成的。

英文摘要：

The location of the obscuring "torus" in an active galactic nucleus (AGN) is still an unresolved issue. The line widths of X-ray fluorescence lines originated from the torus, particularly Fe K$α$, carry key information on the radii of line emitting regions. Utilizing XCLUMPY (Tanimoto et al. 2019), an X-ray clumpy torus model, we develop a realistic model of emission line profiles from an AGN torus where we take into account line broadening due to the Keplerian motion around the black hole. Then, we apply the updated model to the best available broadband spectra (3-100 keV) of the Circinus galaxy observed with Suzaku, XMM-Newton, Nuclear Spectroscopic Telescope Array (NuSTAR), and Chandra, including 0.62 Ms Chandra/HETG data. We confirm that the torus is Compton-thick (hydrogen column-density along the equatorial plane is $N_\mathrm{H}^\mathrm{Equ}=2.16^{+0.24}_{-0.16}\times 10^{25}\ \mathrm{cm}^{-2}$), geometrically thin (torus angular width $σ=10.3^{+0.7}_{-0.3}\ \mathrm{degrees}$), viewed edge-on (inclination $i=78.3^{+0.4}_{-0.9}\ \mathrm{degrees}$), and has super-solar abundance ($1.52^{+0.04}_{-0.06}$ times solar). Simultaneously analyzing the Chandra/HETG first, second, and third order spectra with consideration of the spatial extent of the Fe K$α$ line emitting region, we constrain the inner radius of the torus to be $1.9^{+3.1}_{-0.8}\times 10^5$ times the gravitational radius, or $1.6^{+1.5}_{-0.9}\times 10^{-2}\ \mathrm{pc}$ for a black hole mass of $(1.7\pm 0.3)\times 10^6\ M_{\odot}$. This is about 3 times smaller than that estimated from the dust sublimation radius, suggesting that the inner side of the dusty region of the torus is composed of dust-free gas.

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