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Title:Wavelength-resolved reverberation mapping of intermediate-redshift quasars HE 0413-4031 and HE 0435-4312 : dissecting Mg II, optical Fe II, and UV Fe II emission regions
Authors:ID Prince, Raj (Author)
ID Zajaček, Michal (Author)
ID Panda, Swayamtrupta (Author)
ID Hryniewicz, Krzysztof (Author)
ID Kumar Jaiswal, Vikram (Author)
ID Czerny, Bożena (Author)
ID Trzcionkowski, Piotr (Author)
ID Bronikowski, Mateusz (Author)
ID Rałowski, Mateusz (Author)
ID Sobrino Figaredo, Catalina (Author), et al.
.pdf aa46738-23.pdf (2,92 MB)
MD5: 54E4BA472F39EBA5A01F58028ACC25B4
Work type:Unknown
Typology:1.01 - Original Scientific Article
Organization:UNG - University of Nova Gorica
Abstract:Context. We present the wavelength-resolved reverberation mapping (RM) of combined Mg II and UV Fe II broad-line emissions for two intermediate-redshift (z ∼ 1), luminous quasars, HE 0413-4031 and HE 0435-4312, monitored by the Southern African Large Telescope (SALT) and 1m class telescopes between 2012 and 2022. Aims. Using a wavelength-resolved technique, we aim to disentangle the Mg II and Fe II emission regions and to build a radius–luminosity (R–L) relation for UV Fe II emission, which has so far remained unconstrained. Methods. We applied several time-delay methodologies to constrain the time delays for total Mg II and Fe II emissions. In addition, wavelength-resolved RM is performed to quantify the inflow or outflow of broad-line region (BLR) gas around the supermassive black hole and to disentangle the emission and the emitting regions based on lines produced in proximity to each other. Results. The mean total FeII time delay is nearly equal to the mean total MgII time delay for HE 0435-4312, suggesting the co-spatiality of their emission regions. However, in HE 0413-4031, the mean FeII time delay is found to be longer than the mean MgII time delay, suggesting that FeII emission is produced at greater distances from the black hole. The UV FeII R–L relation is updated with these two quasars (now four in total) and compared with the optical FeII relation (20 sources), which suggests that the optical FeII emission region is located further than the UV FeII region by a factor of 1.7–1.9, that is, RFeII-opt ∼ (1.7 − 1.9)RFeII-UV. Conclusion. Wavelength-resolved reverberation is an efficient way to constrain the geometry and structure of the BLR. We detected a weak pattern in the time delay versus wavelength relation, suggesting that the MgII broad line originates from a region slightly closer to the SMBH than the UV FeII pseudo continuum, although the difference is not very significant. Comparison of MgII, UV, and optical FeII R–L relations suggests that the difference may be greater for lower-luminosity sources, possibly with the MgII emission originating further from the SMBH. In the future, more RM data will be acquired, allowing better constraints on these trends, in particular the UV FeII R–L relation.
Keywords:accretion, accretion disks, emission lines, photometric, spectroscopic
Publication status:Published
Publication version:Version of Record
Publication date:01.01.2023
Year of publishing:2023
Number of pages:str. 1-22
Numbering:Vol. 678, [article no.] ǂA189
PID:20.500.12556/RUNG-8626-3c6c30b0-4125-cde5-738a-8b670a6b6bf5 New window
COBISS.SI-ID:171872259 New window
ISSN on article:1432-0746
DOI:10.1051/0004-6361/202346738 New window
Publication date in RUNG:13.11.2023
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Record is a part of a journal

Title:Astronomy & astrophysics
Shortened title:Astron. astrophys.
Publisher:EDP Sciences
COBISS.SI-ID:392577 New window

Document is financed by a project

Funder:EC - European Commission
Funding programme:H2020
Project number:951549
Name:Sub-percent calibration of the extragalactic distance scale in the era of big surveys


License:CC BY 4.0, Creative Commons Attribution 4.0 International
Description:This is the standard Creative Commons license that gives others maximum freedom to do what they want with the work as long as they credit the author.