Table 4.
Best-fit model parameters from MOSFIT.
| Parameter | Prior | Value | Units |
|---|---|---|---|
| log(Rph0) | [−4, 4] |  |
|
| l | [0, 4] |  |
|
| log(Tviscous) | [−3, 5] |  |
days |
| b (scaled β) | [0, 2] |  |
|
| log(MBH) | [5, 8] |  |
M⊙ |
| log ε | [−2, −0.4] |  |
|
| starmass | [0.01, 10] |  |
M⊙ |
| log σ | [−4, 2] |  |
Notes. The parameter Rph0 and l is the radius normalization and power-law exponent to compute the luminosity-dependent radius of the photosphere in MOSFIT; Tviscous is the viscous time of the gas accretion onto the black hole; b is a proxy for β, β = Rt/Rp, where Rt refers to the tidal disruption radius and Rp refers to the pericenter radius. Full stellar disruption corresponds to b = 1; Mh(M⊙) is the black hole mass; ε is the efficiency parameter that converts the input fallback rate of material to luminosity; starmass is the mass of the disrupted star; σ2 represents the additional variance in the Bayesian analysis to make 
. The errors are only for the fitting statistical uncertainties, and do not include the systematic uncertainties from MOSFIT (Mockler et al. 2019).
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