We compare the microlensing-based continuum emission region size measurements in a sample of 15 gravitationally lensed quasars with estimates of luminosity-based thin disk sizes to constrain the temperature profile of the quasar continuum accretion region. If we adopt the standard thin disk model, we find a significant discrepancy between sizes estimated using the luminosity and those measured by microlensing of $\log(r_{L}/r_{\mu})=-0.57\pm0.08\,\text{dex}$. If quasar continuum sources are simple, optically thick accretion disks with a generalized temperature profile $T(r) \propto r^{-\beta}$, the discrepancy between the microlensing measurements and the luminosity-based size estimates can be resolved by a temperature profile slope $0.37 < \beta < 0.56$ at $1\,\sigma$ confidence. This is shallower than the standard thin disk model ($\beta=0.75$) at $3\,\sigma$ significance. We consider alternate accretion disk models that could produce such a temperature profile and reproduce the empirical continuum size scaling with black hole mass, including disk winds or disks with non-blackbody atmospheres.

中文翻译：

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类星体微透镜变化研究有利于浅吸积盘温度分布

我们将 15 个引力透镜类星体样本中基于微透镜的连续发射区域尺寸测量值与基于光度的薄盘尺寸估计值进行比较，以限制类星体连续吸积区域的温度分布。如果我们采用标准的薄盘模型，我们发现使用光度估计的尺寸与通过微透镜测量的尺寸之间存在显着差异 $\log(r_{L}/r_{\mu})=-0.57\pm0.08\， \text{dex}$。如果类星体连续源是简单的、光学厚的吸积盘，具有广义温度分布 $T(r) \propto r^{-\beta}$，那么微透镜测量和基于光度的尺寸估计之间的差异可以通过温度剖面斜率 $0.37 < \beta < 0.56$ at $1\,\sigma$ 置信度。这比标准的薄磁盘模型 ($\beta=0. 75$) 在 $3\,\sigma$ 意义。我们考虑了替代吸积盘模型，它们可以产生这样的温度分布，并再现经验连续体尺寸随黑洞质量缩放的比例，包括盘风或具有非黑体大气的盘。