Microlensing of the broad emission lines in 27 gravitationally lensed quasars. Broad line region structure and kinematics

We thank the anonymous referee for the helpful comments and the constructive remarks on this manuscript. C.F. acknowledges the financial support the Tel Aviv University and University of Haifa through a DFG grant HA3555-14/1. E.M. and J.A.M are supported by the Spanish MINECO with the grants AYA2016- 79104-C3-1-P and AYA2016-79104-C3-3-P. J.A.M. is also supported from the Generalitat Valenciana project of excellence Prometeo/2020/085. J.J.V. is supported by the project AYA2017-84897-P financed by the Spanish Ministerio de Economia y Competividad and by the Fondo Europeo de Desarrollo Regional (FEDER), and by project FQM-108 financed by Junta de Andalucia. V.M. acknowledges partial support from Centro de Astrofisica de Valparaiso. Research by D.C. has been partially supported by an Israeli Science Foundation grant 2398/19.Aims. We aim to study the structure and kinematics of the broad line region (BLR) of a sample of 27 gravitationally lensed quasars with up to five different epochs of observation. This sample is composed of similar to 100 spectra from the literature plus 22 unpublished spectra of 11 systems. Methods. We measure the magnitude differences in the broad emission line (BEL) wings and statistically model the distribution of microlensing magnifications to determine a maximum likelihood estimate for the sizes of the C IV, C III], and Mg II emitting regions. Results. The BELs in lensed quasars are expected to be magnified differently owing to the different sizes of the regions from which they originate. Focusing on the most common BELs in our spectra (C IV, C III], and Mg II), we find that the low-ionization line Mg II is only weakly affected by microlensing. In contrast, the high-ionization line C IV shows strong microlensing in some cases, indicating that its emission region is more compact. Thus, the BEL profiles are deformed differently depending on the geometry and kinematics of the corresponding emitting region. We detect microlensing in either the blue or the red wing (or in both wings with different amplitudes) of C IV in more than 50% of the systems and find outstanding asymmetries in the wings of QSO 0957+561, SDSS J1004+4112, SDSS J1206+4332, and SDSS J1339+1310. This observation indicates that the BLR is, in general, not spherically symmetric and supports the existence of two regions in the BLR, one insensitive to microlensing and another that only shows up when it is magnified by microlensing. Disregarding the existence of these two regions, our estimate for Mg II, R-1/2 = 67.3(-15.7)(+3.8) root M/M-circle dot light-days, is in good agreement with previous results from smaller samples, while we obtain smaller sizes for the C III] and CIV lines, R-1/2 = 31.0(-4.0)(+1.9) root M/M-circle dot light-days and R-1/2 = 15.5(-3.9)(+0.8) root M/M-circle dot light-days, respectively.Tel Aviv UniversityUniversity of Haifa through a DFG HA3555-14/1Spanish MINECO AYA2016- 79104-C3-1-P AYA2016-79104-C3-3-PGeneralitat Valenciana European CommissionGeneral Electric Prometeo/2020/085Spanish Ministerio de Economia y Competividad AYA2017-84897-PEuropean CommissionJunta de Andalucia FQM-108Centro de Astrofisica de ValparaisoIsrael Science Foundation 2398/1