Wavelength-resolved reverberation mapping of quasar CTS C30.10: Dissecting Mg II and Fe II emission regions

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Publikace nespadá pod Fakultu sportovních studií, ale pod Přírodovědeckou fakultu. Oficiální stránka publikace je na webu muni.cz.
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PRINCE Raj ZAJAČEK Michal CZERNY Bozena TRZCIONKOWSKI Piotr BRONIKOWSKI Mateusz FIGAREDO Catalina Sobrino PANDA Swayamtrupta MARTINEZ-ALDAMA Mary Loli HRYNIEWICZ Krzysztof JAISWAL Vikram Kumar SNIEGOWSKA Marzena NADDAF Mohammad-Hassan BILICKI Maciej HAAS Martin SARNA Marek Jacek KARAS Vladimir OLEJAK Aleksandra PRZYLUSKI Robert RALOWSKI Mateusz UDALSKI Andrzej SEFAKO Ramotholo R GENADE Anja WORTERS Hannah L

Rok publikování 2022
Druh Článek v odborném periodiku
Časopis / Zdroj Astronomy & Astrophysics
Fakulta / Pracoviště MU

Přírodovědecká fakulta

Citace
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Doi http://dx.doi.org/10.1051/0004-6361/202243194
Klíčová slova accretion; accretion disks; quasars: emission lines; quasars: individual: CTS C30.10; techniques: spectroscopic; techniques: photometric
Popis 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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