Broad line region echo from highly accreting intermediate-mass black hole candidate SDSS J144850.08+160803.1 - First probe of intra-night variability and reverberation mapping

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Table E.2.

Black hole mass and BLR radii R_{BLR, Hα}, R_{BLR, Hβ} estimations using single epoch virial calibrations.

SSP Model	FWHM_Hα, km/s	$L_{H α}, \times 10^{40} \frac{erg}{s}$ $L_{H\alpha}, \times10^{40}~\frac{erg}{s}$	R_{Hβ, B13, L_Hα}[lt − days]	M_{BH, R_B13}, ×10⁶ M_⊙	R_{Hα, C23, L_Hα}[lt − days]	M_{BH, R_C23}, ×10⁶ M_⊙	ϵ_D20	ϵ_N19
E-MILES	705.03 ± 24.49	1.27 ± 0.04	$2 . 14_{- 1.07}^{+ 2.12}$ $2.14_{-1.07}^{+2.12}$	$0 . 23_{- 0.14}^{+ 0.36}$ $0.23_{-0.14}^{+0.36}$	$1 . 01_{- 0.49}^{+ 0.96}$ $1.01_{- 0.49}^{+0.96}$	$0 . 10_{- 0.05}^{+ 0.09}$ $0.10_{-0.05}^{+0.09}$	$0 . 38_{- 0.25}^{+ 0.68}$ $0.38^{+0.68}_{-0.25}$	$1 . 07_{- 0.51}^{+ 0.94}$ $1.07_{-0.51}^{+0.94}$
MILES(+MgFe)	709.74 ± 24.49	1.25 ± 0.04	$2 . 12_{- 1.06}^{+ 2.1}$ $2.12_{-1.06}^{+2.1}$	$0 . 23_{- 0.14}^{+ 0.36}$ $0.23_{-0.14}^{+0.36}$	$1 . 00_{- 0.48}^{+ 0.95}$ $1.00_{-0.48}^{+0.95}$	$0 . 10_{- 0.05}^{+ 0.09}$ $0.10_{-0.05}^{+0.09}$	$0 . 38_{- 0.24}^{+ 0.68}$ $0.38^{+0.68}_{-0.24}$	1.07_−0.51^+0.94
MILES	718.22 ± 24.96	1.25 ± 0.04	$2 . 13_{- 1.06}^{+ 2.11}$ $2.13_{-1.06}^{+ 2.11}$	$0 . 24_{- 0.14}^{+ 0.37}$ $0.24_{-0.14}^{+0.37}$	$1 . 00_{- 0.48}^{+ 0.95}$ $1.00_{- 0.48}^{+0.95}$	$0 . 10_{- 0.05}^{+ 0.09}$ $0.10_{-0.05}^{+0.09}$	$0 . 37_{- 0.24}^{+ 0.66}$ $0.37^{+0.66}_{-0.24}$	1.04_−0.50^+0.92
PEGASE	705.03 ± 24.73	1.17 ± 0.03	$2 . 06_{- 1.03}^{+ 2.04}$ $2.06_{-1.03}^{+2.04}$	$0 . 22_{- 0.13}^{+ 0.35}$ $0.22_{-0.13}^{+0.35}$	$0 . 96_{- 0.46}^{+ 0.92}$ $0.96_{-0.46}^{+0.92}$	$0 . 09_{- 0.04}^{+ 0.09}$ $0.09_{-0.04}^{+0.09}$	$0 . 40_{- 0.26}^{+ 0.72}$ $0.40^{+0.72}_{-0.26}$	1.12_−0.54^+1.00
X-Shooter	690.67 ± 24.25	1.27 ± 0.04	$2 . 14_{- 1.0}^{+ 2.12}$ $2.14_{-1.0}^{+2.12}$	$0 . 22_{- 0.13}^{+ 0.34}$ $0.22_{-0.13}^{+0.34}$	$1 . 0_{- 0.48}^{+ 0.96}$ $1.0_{-0.48}^{+0.96}$	$0 . 09_{- 0.05}^{+ 0.09}$ $0.09_{-0.05}^{+0.09}$	$0 . 40_{- 0.26}^{+ 0.71}$ $0.40^{+0.71}_{-0.26}$	1.12_−0.53^+0.99

Notes. M_{BH, Hβ}(FWHM_Hα, L_Hα) is defined as M_{BH, R_B13} (Bentz et al. 2013) and M_{BH, Hα}(FWHM_Hα, L_Hα) id defined as M_{BH, R_C23} (Cho et al. 2023). Accretion rate estimates ϵ_D20 and ϵ_N19 correspond to L_bol/L_Edd, where Eddington luminosity L_Edd calculated assuming M_{BH, R_C23} (Cho et al. 2023) Hα BH mass estimate to use the smallest number of empirical relations altogether, while L_bol calculated using bolometric conversions from L_X[2 − 10keV] from Duras et al. (2020) and Netzer (2019) respectively. Monte Carlo sampling was used for error propagation, incorporating all reported in relation coefficients’ errors and inner scatters. BH mass estimators are calculated as the median, and BH mass error bars are calculated as 68% confidence interval. Luminosity is calculated assuming z = 0.038, H₀ = 70 km s⁻¹ Mpc⁻¹. The Gaussian profile is assumed for broad emission lines in the full-spectrum fit.

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