Evidence of a diffuse, extended continuum source in quasars from the relative sizes of the broad line region and the UV-optical continuum source measured with microlensing

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Volume 695 (March 2025)

A&A, 695 (2025) A10

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Table 2.

BLR to continuum source radius ratios.

Object line date	log₁₀(L_bol)	log₁₀(r_in BLR/r_s Cont)	log₁₀(r_1/2 BLR/r_1/2 Cont)	log₁₀(r_1/2 BLR)	log₁₀(r_1/2 Cont)
J1004 C IV	45.12±0.11	− $0 . 08_{- 0.78}^{+ 0.59}$ $0.08^{+0.59}_{-0.78}$	$0 . 65_{- 0.61}^{+ 0.56}$ $0.65^{+0.56}_{-0.61}$	$0 . 45_{- 0.41}^{+ 0.23}$ $0.45^{+0.23}_{-0.41}$	$- 0 . 20_{- 0.46}^{+ 0.51}$ $-0.20^{+0.51}_{-0.46}$
Q2237 C IV	46.30±0.30	$- 0 . 11_{- 0.57}^{+ 0.87}$ $-0.11^{+0.87}_{-0.57}$	$0 . 36_{- 0.53}^{+ 0.77}$ $0.36^{+0.77}_{-0.53}$	$1 . 59_{- 0.44}^{+ 0.16}$ $1.59^{+0.16}_{-0.44}$	− $1 . 23_{- 0.29}^{+ 0.75}$ $1.23^{+0.75}_{-0.29}$
J1138 C IV	45.40±0.10	− $0 . 13_{- 0.76}^{+ 0.95}$ $0.13^{+0.95}_{-0.76}$	$0 . 59_{- 0.68}^{+ 0.98}$ $0.59^{+0.98}_{-0.68}$	$0 . 69_{- 0.35}^{+ 0.30}$ $0.69^{+0.30}_{-0.35}$	− $0 . 10_{- 0.58}^{+ 0.93}$ $0.10^{+0.93}_{-0.58}$
J1339 C IV 2014	45.88±0.11	− $0 . 24_{- 0.67}^{+ 0.73}$ $0.24^{+0.73}_{-0.67}$	$0 . 99_{- 0.63}^{+ 0.70}$ $0.99^{+0.70}_{-0.63}$	$0 . 71_{- 0.37}^{+ 0.28}$ $0.71^{+0.28}_{-0.37}$	$- 0 . 28_{- 0.51}^{+ 0.64}$ $-0.28^{+0.64}_{-0.51}$
J1339 C IV 2017	46.13±0.11	− $0 . 48_{- 0.73}^{+ 0.65}$ $0.48^{+0.65}_{-0.73}$	$1 . 23_{- 0.69}^{+ 0.65}$ $1.23^{+0.65}_{-0.69}$	$0 . 83_{- 0.26}^{+ 0.28}$ $0.83^{+0.28}_{-0.26}$	$- 0 . 40_{- 0.59}^{+ 0.59}$ $-0.40^{+0.59}_{-0.59}$
J1339 Mg II 2017	46.13±0.11	− $0 . 78_{- 0.95}^{+ 0.76}$ $0.78^{+0.76}_{-0.95}$	$1 . 40_{- 0.82}^{+ 0.76}$ $1.40^{+0.76}_{-0.82}$	$1 . 37_{- 0.45}^{+ 0.34}$ $1.37^{+0.34}_{-0.45}$	$- 0 . 03_{- 0.69}^{+ 0.68}$ $-0.03^{+0.68}_{-0.69}$
J1131 Mg II	45.00±0.10	− $0 . 29_{- 0.78}^{+ 1.05}$ $0.29^{+1.05}_{-0.78}$	$0 . 97_{- 0.56}^{+ 0.73}$ $0.97^{+0.73}_{-0.56}$	$0 . 96_{- 0.32}^{+ 0.40}$ $0.96^{+0.40}_{-0.32}$	$- 0 . 01_{- 0.46}^{+ 0.61}$ $-0.01^{+0.61}_{-0.46}$
J1226 Mg II	45.65±0.15	− $0 . 05_{- 0.59}^{+ 0.64}$ $0.05^{+0.64}_{-0.59}$	$0 . 59_{- 0.46}^{+ 0.60}$ $0.59^{+0.60}_{-0.46}$	$0 . 46_{- 0.26}^{+ 0.31}$ $0.46^{+0.31}_{-0.26}$	$- 0 . 13_{- 0.38}^{+ 0.51}$ $-0.13^{+0.51}_{-0.38}$
J1355 Mg II	46.40±0.10	$- 0 . 33_{- 0.77}^{+ 1.03}$ $-0.33^{+1.03}_{-0.77}$	$0 . 50_{- 0.92}^{+ 0.85}$ $0.50^{+0.85}_{-0.92}$	$0 . 89_{- 0.61}^{+ 0.31}$ $0.89^{+0.31}_{-0.61}$	− $0 . 39_{- 0.69}^{+ 0.79}$ $0.39^{+0.79}_{-0.69}$
J1131 Hα	45.00±0.10	− $0 . 45_{- 0.73}^{+ 0.76}$ $0.45^{+0.76}_{-0.73}$	$1 . 06_{- 0.53}^{+ 0.70}$ $1.06^{+0.70}_{-0.53}$	$1 . 00_{- 0.32}^{+ 0.25}$ $1.00^{+0.25}_{-0.32}$	$- 0 . 06_{- 0.42}^{+ 0.65}$ $-0.06^{+0.65}_{-0.42}$
Q2237 Hα	46.30±0.30	$- 0 . 32_{- 0.63}^{+ 0.91}$ $-0.32^{+0.91}_{-0.63}$	$0 . 23_{- 0.59}^{+ 0.81}$ $0.23^{+0.81}_{-0.59}$	$1 . 57_{- 0.42}^{+ 0.12}$ $1.57^{+0.12}_{-0.42}$	− $1 . 34_{- 0.41}^{+ 0.80}$ $1.34^{+0.80}_{-0.41}$
HE0435 Hα	45.85±0.15	− $0 . 14_{- 1.12}^{+ 1.16}$ $0.14^{+1.16}_{-1.12}$	$0 . 85_{- 0.96}^{+ 1.06}$ $0.85^{+1.06}_{-0.96}$	$1 . 18_{- 0.59}^{+ 0.50}$ $1.18^{+0.50}_{-0.59}$	− $0 . 33_{- 0.76}^{+ 0.93}$ $0.33^{+0.93}_{-0.76}$

Notes. The radius ratios are the median values of the probability densities (see Fig. 1). The half-light radii of the BLR are from Hutsemékers et al. (2023, 2024a,b). They were measured with an average microlens mass of 0.3 M_⊙. For Q2237, the half-light radii are taken from Appendix A of Savić et al. (2024) for consistency with the present work, noting that the time series analysis gives r_1/2 BLR/r_1/2 Cont a factor of four larger, but still within the uncertainties. The continuum source radii were computed from the BLR to continuum radius ratios. All radii are in light-days. The bolometric luminosities (in erg s⁻¹) were computed from the monochromatic luminosities given in Sluse et al. (2012), Shalyapin et al. (2021), and Hutsemékers et al. (2023, 2024a,b), with the bolometric corrections from Sluse et al. (2012).

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