自洽X射线光谱与UV/光学/NIR测光拟合得到的吸积盘尺寸：应用于ASASSN-14li和HLX-1
The size of accretion disks from self-consistent X-ray spectra and UV/optical/NIR photometry fitting: applications to ASASSN-14li and HLX-1
AI总结：
本文实现带自由外盘半径的标准薄盘模型，同时拟合X射线光谱与UV/光学/NIR测光，应用于TDE ASASSN-14li和IMBH候选体HLX-1，得到黑洞质量和外盘半径，并讨论简化模型与相对论效应的影响。
摘要：
我们实现了一个标准薄盘模型，将外盘半径（$R_{\rm out}$）作为自由参数，并将其集成到标准X射线拟合包中，以实现X射线光谱和UV/光学/NIR测光的自洽同时拟合。我们将该模型应用于潮汐瓦解事件（TDE）ASASSN-14li的晚期数据（$\Delta t \approx 350-1300$天）。我们表明，在这些晚期，该源的多波段发射可以完全由裸露的紧凑吸积盘来描述。我们得到的黑洞质量（$M_{\rm BH}$）为$7^{+3}_{-2}\times10^{6} M_{\odot}$，与宿主星系标度关系一致；$R_{\rm out}$为$45 \pm 13 \\, R_{\rm g}$，与圆化半径一致，并在最新时刻可能存在膨胀。我们讨论了诸如单温度黑体拟合X射线光谱或UV/光学测光等简化模型如何导致对TDE发射尺度/能量的错误解释。我们还将该模型应用于中等质量黑洞（IMBH）候选体HLX-1的软/高态。该模型拟合了完整的谱能量分布（从X射线到NIR），无需额外的恒星族成分。我们通过实现Kerr度规中具有完整射线追踪计算的模型版本来研究相对论效应如何改进我们的结果。对于HLX-1，我们发现$M_{\rm BH} = 4^{+3}_{-1} \times 10^{4} M_{\odot}$和$R_{\rm out} \approx {\rm few} \times 10^{3} \\, R_{\rm g}$，与先前发现一致。相对论模型可以将HLX-1的倾角（$i$）限制为$10^o \leq i \leq 70^o$。
英文摘要：
We implement a standard thin disk model with the outer disk radius ($R_{\rm out}$) as a free parameter, integrating it into standard X-ray fitting package to enable self-consistent and simultaneous fitting of X-ray spectra and UV/optical/NIR photometry. We apply the model to the late-time data ($Δt \approx 350-1300$ days) of the tidal disruption event (TDE) ASASSN-14li. We show that at these late-times the multi-wavelength emission of the source can be fully described by a bare compact accretion disk. We obtain a black hole mass ($M_{\rm BH}$) of $7^{+3}_{-2}\times10^{6} M_{\odot}$, consistent with host-galaxy scaling relations; and an $R_{\rm out}$ of $45 \pm 13 \, R_{\rm g}$, consistent with the circularization radius, with possible expansion at the latest epoch. We discuss how simplistic models, such as a single-temperature blackbody fitted to either X-ray spectra or UV/optical photometry, lead to erroneous interpretations on the scale/energetics of TDE emission. We also apply the model to the soft/high state of the intermediate-mass black hole (IMBH) candidate HLX-1. The model fits the full spectral energy distribution (from X-rays to NIR) without needing an additional stellar population component. We investigate how relativistic effects improve our results by implementing a version of the model with full ray tracing calculations in the Kerr metric. For HLX-1, we find $M_{\rm BH} = 4^{+3}_{-1} \times 10^{4} M_{\odot}$ and $R_{\rm out} \approx {\rm few} \times 10^{3} \, R_{\rm g}$, in agreement with previous findings. The relativistic model can constrain the inclination ($i$) of HLX-1 to be $10^o \leq i \leq 70^o$.
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