Papers › The size of accretion disks from self-consistent X-ray spectra and UV/optical/NIR...
The size of accretion disks from self-consistent X-ray spectra and UV/optical/NIR photometry fitting: applications to ASASSN-14li and HLX-1
Muryel Guolo, Andrew Mummery
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We implement a standard thin disk model with the outer disk radius (Rₒᵤₜ) 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 ≈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_(BH)) of 7⁺³₋₂×10⁶ M_⊙, consistent with host-galaxy scaling relations; and an Rₒᵤₜ of 45 ±13 R_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_(BH) = 4⁺³₋₁ ×10⁴ M_⊙ and Rₒᵤₜ ≈few ×10³ R_g, in agreement with previous findings. The relativistic model can constrain the inclination (i) of HLX-1 to be 10ᵒ ≤i ≤70ᵒ.
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