Wavelength-resolved reverberation mapping of quasar CTS C30.10: Dissecting Mg II and Fe II emission regions
| Authors | |
|---|---|
| Year of publication | 2022 |
| Type | Article in Periodical |
| Magazine / Source | Astronomy & Astrophysics |
| MU Faculty or unit | |
| Citation | |
| Web | |
| Doi | http://dx.doi.org/10.1051/0004-6361/202243194 |
| Keywords | accretion; accretion disks; quasars: emission lines; quasars: individual: CTS C30.10; techniques: spectroscopic; techniques: photometric |
| Description | Context. We present the results of the reverberation monitoring of the Mg?II broad line and Fe?II pseudocontinuum for the luminous quasar CTS C30.10 (z = 0.90052) with the Southern African Large Telescope in 2012–2021. Aims. We aimed at disentangling the Mg?II and UV Fe?II variability and the first measurement of UV Fe?II time delay for a distant quasar. Methods. We used several methods for the time-delay measurements and determined the Fe?II and Mg?II time delays. We also performed a wavelength-resolved time delay study for a combination of Mg?II and Fe?II in the 2700–2900 A rest-frame wavelength range. Results. We obtain a time delay for Mg?II of 275.5-19.5+12.4 days in the rest frame, and we have two possible solutions of 270.0-25.3+13.8 days and 180.3-30.0+26.6 in the rest frame for Fe?II. Combining this result with the old measurement of Fe?II UV time delay for NGC 5548, we discuss for first time the radius-luminosity relation for UV Fe?II with the slope consistent with 0.5 within the uncertainties. Conclusions. Because the Fe?II time delay has a shorter time-delay component but the lines are narrower than Mg?II, we propose that the line-delay measurement is biased toward the part of the broad line region (BLR) facing the observer. The bulk of the Fe?II emission may arise from the more distant BLR region, however, the region that is shielded from the observer. |
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