Size and kinematics of the CIV broad emission line region from microlensing-induced line profile distortions in two gravitationally lensed quasars

Abstract

We analyzed the CIV line profile distortions due to microlensing in two quasars, J1339 and J1138. J1339 shows a strong, asymmetric line profile deformation, while J1138 shows a more modest, symmetric deformation. To probe the CIV broad line region (BLR), we compared the observed line profile deformations to simulated ones. The simulations are based on three simple BLR models, a Keplerian disk (KD), an equatorial wind (EW), and a polar wind (PW), of various sizes, inclinations, and emissivities. We find that the line profile deformations can be reproduced with the simple BLR models under consideration, with no need for more complex geometries or kinematics. The models with disk geometries (KD and EW) are preferred, while the PW model is definitely less likely. For J1339, we find the CIV BLR half-light radii to be $r_{1/2}=$ 5.1 ${}_{-2.9}^{+4.6}$ light-days and $r_{1/2}=$ 6.7 ${}_{-3.8}^{+6.0}$ light-days from spectra obtained in 2014 and 2017, respectively. They do agree within uncertainties. For J1138, the amplitude of microlensing is smaller and more dependent on the macro-magnification factor. From spectra obtained in 2005 (single epoch), we find $r_{1/2}=$ 4.9 ${}_{-2.7}^{+4.9}$ light-days and $r_{1/2}=$ 12 ${}_{-8}^{+13}$ light-days for two extreme values of the macro-magnification factor. Combining these new measurements with those previously obtained for the quasars Q2237$+$0305 and J1004$+$4112, we show that the BLR radii estimated from microlensing do follow the CIV radius--luminosity relation obtained from reverberation mapping, although the microlensing radii seem to be systematically smaller, which could indicate either a selection bias or a real offset (abridged).

Accepted for publication in A\&A

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