Stellar black holes (sBHs) are widely believed to exist in the accretion disks of active galactic nuclei (AGNs). Previous studies often focus on the transient emission produced by embedded sBHs. Here, we explore the possible observational consequences of an AGN accretion disk that contains a population of accreting sBHs. Embedded accreting sBHs change the effective temperature distribution of the AGN accretion disk by heating gas in the outer regions. Two possible observational consequences are presented. First, the spectral energy distribution has a turnover feature at ∼4700 Å when the supermassive black hole mass is ∼10⁸ M _⊙, which can help explain the observed shallow spectral shape at wavelengths >5000 Å for the Sloan Digital Sky Survey quasar composite spectrum. Second, the half-light radius of a given relatively long wavelength is significantly larger than for an AGN disk without sBHs, which can be tested by microlensing observations. With appropriate sBH distributions, the model can be reconciled with quasar microlensing disk sizes. We propose that the half-light radius–wavelength relation can be utilized to investigate the distributions of embedded sBHs in AGN accretion disks.

中文翻译：

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恒星黑洞可以“拉伸”超大质量黑洞吸积盘

人们普遍认为恒星黑洞（sBH）存在于活动星系核（AGN）的吸积盘中。先前的研究通常集中于嵌入式 sBH 产生的瞬态发射。在这里，我们探讨了包含大量吸积 sBH 的 AGN 吸积盘可能的观测后果。嵌入式吸积黑洞通过加热外部区域的气体来改变活动星系核吸积盘的有效温度分布。提出了两种可能的观察结果。首先，当超大质量黑洞质量为~10 ^{8时，光谱能量分布在~4700 Å处具有翻转特征。} 中号 _⊙，这有助于解释斯隆数字巡天类星体复合光谱在波长 >5000 Å 处观察到的浅光谱形状。其次，给定相对较长波长的半光半径明显大于没有 sBH 的 AGN 盘，这可以通过微透镜观测进行测试。通过适当的 sBH 分布，该模型可以与类星体微透镜盘尺寸相协调。我们建议利用半光半径-波长关系来研究活动星系核吸积盘中嵌入的超黑洞的分布。