Abstract
Over the past three decades reverberation mapping (RM) has been applied to about 100 AGNs. Their broad line region (BLR) sizes were measured and yielded mass estimates of the black holes in their center. However, very few attempts were carried out for high-luminosity quasars, at luminosities higher than 10$^{46}$ erg/sec in the optical. Most of these attempts failed since RM of such quasars is difficult due to a number of reasons, mostly due to the long time needed to monitor these objects. During the past two decades we carried out a RM campaign on six high-luminosity quasars. This contribution presents some of the final light curves of that RM campaign in which we measured the BLR size in C\,{\sc iv} of three of the objects (S5\,0836+71, SBS\,1116+603, and SBS\,1425+606). We present the C\,{\sc iv} BLR size and luminosity relation over eight orders of magnitude in luminosity, pushing the luminosity limit to its highest point so far.
Highlights
Reverberation Mapping (RM) is a technique to estimate the size of the Broad Line Region (BLR) in Active Galactic Nuclei (AGNs)
In order to estimate the broad line region (BLR) size we use two methods which are commonly used for that purpose
One method is the interpolated cross-correlation function (ICCF: White and Peterson, 1994). In this method one light curve is cross correlated with a linear interpolation of the second light curve, the second light curve is cross correlated with a linear interpolation of the first light curve, and the final cross correlation is the average of these two cross correlation functions
Summary
Reverberation Mapping (RM) is a technique to estimate the size of the Broad Line Region (BLR) in Active Galactic Nuclei (AGNs). Most of the AGNs which were measured with reverberation mapping far were observed using the Hβ emission line and this is the most commonly used line for these studies of lowredshift, low-luminosity AGNs. High-luminosity AGNs are generally at high redshift (order of z ∼ 2–4), observations with optical telescopes are monitoring the UV lines (e.g., Lyα, C IV, C III], and Mg II).
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
