| Issue |
A&A
Volume 667, November 2022
|
|
|---|---|---|
| Article Number | A42 | |
| Number of page(s) | 20 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/202243194 | |
| Published online | 03 November 2022 | |
Wavelength-resolved reverberation mapping of quasar CTS C30.10: Dissecting Mg II and Fe II emission regions
1
Center for Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, Poland
e-mail: raj@cft.edu.pl
2
Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotlářská 2, 61137 Brno, Czech Republic
3
Centre for Astrophysics and Cosmology, University of Nova Gorica, Vipavska 11c, 5270 Ajdovščina, Slovenia
4
Astronomisches Institut Ruhr-Universitat Bochum, Universitatsstrae 150, 44801 Bochum, Germany
5
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
6
Laboratório Nacional de Astrofísica, R. dos Estados Unidos, 154 - Nacões, Itajubá, MG 37504-364, Brazil
7
Departamento de Astronomia, Universidad de Chile, Camino del Observatorio 1515, Santiago, Chile
8
National Centre for Nuclear Research, ul. Pasteura 7, 02-093 Warsaw, Poland
9
Astronomical Institute, Academy of Sciences, Boční II 1401, 14131 Prague, Czech Republic
10
Space Research Center, Polish Academy of Sciences, Bartycka 18A 00-716, Warszawa, Poland
11
Astronomical Observatory of the Jagiellonian University, Orla 171, 30-244 Krakow, Poland
12
Warsaw University Observatory, Al. Ujazdowskie 4, 88-478 Warsaw, Poland
13
outh African Astronomical Observatory, PO Box 9 Observatory, 7935 Cape Town, South Africa
14
University of Cape Town, Rondebosch, 7700 Cape Town, South Africa
Received:
25
January
2022
Accepted:
9
June
2022
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 Å 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.
Key words: accretion, accretion disks / quasars: emission lines / quasars: individual: CTS C30.10 / techniques: spectroscopic / techniques: photometric
© R. Prince et al. 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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