arXiv 1606.092652016-06-29astro-ph.HEastro-ph.GA

康普顿厚度活动星系核的增长率指标

A growth-rate indicator for Compton-thick active galactic nuclei

M. Brightman, A. Masini, D. R. Ballantyne, M. Baloković, W. N. Brandt, C. -T. Chen, A. Comastri, D. Farrah, P. Gandhi, F. A. Harrison, C. Ricci, D. Stern, D. J. Walton

备注：: Accepted for publication in ApJ
DOI：: 10.3847/0004-637X/826/1/93

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摘要：

由于其中心引擎被严重遮蔽，康普顿厚度（CT）的活动星系核（AGN）的增长率很难测量。爱丁顿比λ $_{Edd}$和X射线幂律指数Γ之间的统计学显著相关性，在未被遮蔽的活动星系核中观察到，提供了从X射线光谱学（尽管有很大的散射）估计它们的增长率。然而，由于X射线经过康普顿散射和光电吸收的再处理，当到中央引擎的视线被严重遮挡时，恢复固有的Γ是具有挑战性的。在这里，我们研究一个样本的本地，主要是康普顿厚超脉泽AGN，其中的黑洞质量，从而爱丁顿光度，是众所周知的。我们编译的结果与敏感的高能量（E> 10 keV）的NuSTAR数据，其中X射线环面模型，考虑到再处理的影响，已被用来恢复固有的Γ值和X射线光度，L $_X$的这些源的X射线光谱拟合。通过对L $_X$进行简单的热辐射校正来计算λ $_{Edd}$，我们发现Γ和λ $_{Edd}$之间存在统计学显著相关性（p = 0.007）。对数据进行线性拟合得到r =（0.41 $\pm$ 0.18）log $_{10}$ λ $_{Edd}$ +（2.38 $\pm$ 0.20），这与未被遮蔽的活动星系核的结果在统计学上是一致的。这一结果表明，环面模拟成功地恢复了活动星系核的本征参数。由于巨脉泽中有低质量黑洞（M $_{BH}\approx10^6-10^7$ M $_{sol}$）并且高度倾斜，我们的结果将Γ-λ $_{Edd}$关系推广到较低质量，并且反对日冕中的强取向效应，支持活动星系核的统一。最后，这一结果支持使用Γ作为吸积黑洞的增长率指标，即使对于康普顿厚度的活动星系核。

英文摘要：

Due to their heavily obscured central engines, the growth rate of Compton-thick (CT) active galactic nuclei (AGN) is difficult to measure. A statistically significant correlation between the Eddington ratio, λ$_{Edd}$, and the X-ray power-law index, Γ, observed in unobscured AGN offers an estimate of their growth rate from X-ray spectroscopy (albeit with large scatter). However, since X-rays undergo reprocessing by Compton scattering and photoelectric absorption when the line-of-sight to the central engine is heavily obscured, the recovery of the intrinsic Γ is challenging. Here we study a sample of local, predominantly Compton-thick megamaser AGN, where the black hole mass, and thus Eddington luminosity, are well known. We compile results on X-ray spectral fitting of these sources with sensitive high-energy (E> 10 keV) NuSTAR data, where X-ray torus models which take into account the reprocessing effects have been used to recover the intrinsic Γ values and X-ray luminosities, L$_X$. With a simple bolometric correction to L$_X$ to calculate λ$_{Edd}$, we find a statistically significant correlation between Γ and λ$_{Edd}$ (p = 0.007). A linear fit to the data yields Γ = (0.41$\pm$0.18)log$_{10}$λ$_{Edd}$+(2.38$\pm$ 0.20), which is statistically consistent with results for unobscured AGN. This result implies that torus modeling successfully recovers the intrinsic AGN parameters. Since the megamasers have low-mass black holes (M$_{BH}\approx10^6-10^7$ M$_{sol}$) and are highly inclined, our results extend the Γ-λ$_{Edd}$ relationship to lower masses and argue against strong orientation effects in the corona, in support of AGN unification. Finally this result supports the use of Γ as a growth-rate indicator for accreting black holes, even for Compton-thick AGN.

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