UV FeII emission model of HE 0413-4031 and its relation to
broad-line time delays

ZAJAČEK, Michal, Swayamtrupta PANDA, Ashwani PANDEY, Raj PRINCE, Alberto RODRIGUEZ-ARDILA, Vikram JAISWAL, Bozena CZERNY, Krzysztof HRYNIEWICZ, Maciej URBANOWICZ, Piotr TRZCIONKOWSKI, Marzena SNIEGOWSKA, Zuzanna FALKOWSKA, Mary Loli MARTINEZ-ALDAMA and Norbert WERNER. UV FeII emission model of HE 0413-4031 and its relation to broad-line time delays. Astronomy and Astrophysics. EDP Sciences, 2024, vol. 683, March 2024, p. 1-18. ISSN 0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/202348172.

Other formats: BibTeX LaTeX RIS

TY  - JOUR
ID  - 2396858
AU  - Zajaček, Michal - Panda, Swayamtrupta - Pandey, Ashwani - Prince, Raj - Rodriguez-Ardila, Alberto - Jaiswal, Vikram - Czerny, Bozena - Hryniewicz, Krzysztof - Urbanowicz, Maciej - Trzcionkowski, Piotr - Sniegowska, Marzena - Falkowska, Zuzanna - Martinez-Aldama, Mary Loli - Werner, Norbert
PY  - 2024
TI  - UV FeII emission model of HE 0413-4031 and its relation to broad-line time delays
JF  - Astronomy and Astrophysics
VL  - 683
IS  - March 2024
SP  - 1-18
EP  - 1-18
PB  - EDP Sciences
SN  - 00046361
KW  - accretion
KW  - accretion disks
KW  - techniques: photometric
KW  - techniques: spectroscopic
KW  - quasars: emission lines
KW  - quasars: individual: HE 0413-4031
UR  - https://arxiv.org/abs/2310.03544
N2  - Context. FeII emission is a well-known contributor to the UV spectra of active galactic nuclei and the modeling of this part may affect the results obtained for the MgII λ2800 emission, which is one of the lines used for black hole mass measurements and cosmological applications. Aims. We tested different FeII emission models when modeling the UV emission of the intermediate-redshift quasar HE 0413−4031 to see how the use of a specific template affects the MgII λ2800 line properties and the measurement of the MgII λ2800 and UV FeII time delays with respect to the continuum. Methods. We used the 11-year monitoring of the selected quasar HE 0413−4031 with the South African Large Telescope (SALT), and we supplemented this monitoring with the near-IR spectrum taken with the SOAR telescope, which gave access to the Hβλ4861 and [OIII] λλ4959, 5007 emission lines at the rest frame and allowed for a precise measurement of the redshift. Results. A new redshift determination (z = 1.39117 ± 0.00017) using [OIII] λλ4959, 5007 gave a very different value than the previous determination based only on the UV FeII pseudocontinuum (z = 1.3764). It favors a different decomposition of the spectrum into MgII and UV FeII emissions. The line characteristics and the time delay of the MgII emission (224−23+21 days) are not significantly affected. However, in comparison with the previous analysis, the rest-frame UV FeII time delay (251−7+9 days) is consistent with the inferred UV FeII line full width at half maximum (FWHM) of 4200 km s−1 that is only slightly smaller than the MgII line FWHM. Hence the FeII-emitting material is more distant than the MgII-emitting gas in HE 0413−4031 by ∼0.023 pc (4700 AU). The inferred velocity shift of both MgII and UV FeII lines with respect to the systemic redshift is now rather low, below 300 km s−1. In addition, we constructed an updated MgII radius-luminosity (R − L) relation from 194 sources, which is more than double the previous sample. The MgII R − L relation is flatter than the UV FeII, optical FeII, and HβR − L relations. While the new decomposition of the spectrum is satisfactory, we see a need to create better FeII templates using the newest version of the code CLOUDY.
ER  -

Basic information
Original name	UV FeII emission model of HE 0413-4031 and its relation to broad-line time delays
Authors	ZAJAČEK, Michal (703 Slovakia, belonging to the institution), Swayamtrupta PANDA, Ashwani PANDEY, Raj PRINCE, Alberto RODRIGUEZ-ARDILA, Vikram JAISWAL, Bozena CZERNY, Krzysztof HRYNIEWICZ, Maciej URBANOWICZ, Piotr TRZCIONKOWSKI, Marzena SNIEGOWSKA, Zuzanna FALKOWSKA, Mary Loli MARTINEZ-ALDAMA and Norbert WERNER (703 Slovakia, belonging to the institution).
Edition	Astronomy and Astrophysics, EDP Sciences, 2024, 0004-6361.

Other information
Original language	English
Type of outcome	Article in a journal
Field of Study	10308 Astronomy
Country of publisher	France
Confidentiality degree	is not subject to a state or trade secret
WWW	arXiv URL
Impact factor	Impact factor: 6.500 in 2022
Organization unit	Faculty of Science
Doi	http://dx.doi.org/10.1051/0004-6361/202348172
UT WoS	001185810900029
Keywords in English	accretion; accretion disks; techniques: photometric; techniques: spectroscopic; quasars: emission lines; quasars: individual: HE 0413-4031
Tags	rivok
Tags	International impact, Reviewed
Changed by	Changed by: Mgr. Marie Šípková, DiS., učo 437722. Changed: 3/5/2024 10:13.

Abstract

Context. FeII emission is a well-known contributor to the UV spectra of active galactic nuclei and the modeling of this part may affect the results obtained for the MgII λ2800 emission, which is one of the lines used for black hole mass measurements and cosmological applications. Aims. We tested different FeII emission models when modeling the UV emission of the intermediate-redshift quasar HE 0413−4031 to see how the use of a specific template affects the MgII λ2800 line properties and the measurement of the MgII λ2800 and UV FeII time delays with respect to the continuum. Methods. We used the 11-year monitoring of the selected quasar HE 0413−4031 with the South African Large Telescope (SALT), and we supplemented this monitoring with the near-IR spectrum taken with the SOAR telescope, which gave access to the Hβλ4861 and [OIII] λλ4959, 5007 emission lines at the rest frame and allowed for a precise measurement of the redshift. Results. A new redshift determination (z = 1.39117 ± 0.00017) using [OIII] λλ4959, 5007 gave a very different value than the previous determination based only on the UV FeII pseudocontinuum (z = 1.3764). It favors a different decomposition of the spectrum into MgII and UV FeII emissions. The line characteristics and the time delay of the MgII emission (224−23+21 days) are not significantly affected. However, in comparison with the previous analysis, the rest-frame UV FeII time delay (251−7+9 days) is consistent with the inferred UV FeII line full width at half maximum (FWHM) of 4200 km s−1 that is only slightly smaller than the MgII line FWHM. Hence the FeII-emitting material is more distant than the MgII-emitting gas in HE 0413−4031 by ∼0.023 pc (4700 AU). The inferred velocity shift of both MgII and UV FeII lines with respect to the systemic redshift is now rather low, below 300 km s−1. In addition, we constructed an updated MgII radius-luminosity (R − L) relation from 194 sources, which is more than double the previous sample. The MgII R − L relation is flatter than the UV FeII, optical FeII, and HβR − L relations. While the new decomposition of the spectrum is satisfactory, we see a need to create better FeII templates using the newest version of the code CLOUDY.

Links
GF23-04053L, research and development project	Name: Role mraků při využití zpoždění kontinua v aktivních galaxiích k měření rychlosti rozpínání vesmíru
GF23-04053L, research and development project	Investor: Czech Science Foundation, Partner Agency
GX21-13491X, research and development project	Name: Zkoumání žhavého vesmíru a porozumění kosmické zpětné vazbě (Acronym: EHU)
GX21-13491X, research and development project	Investor: Czech Science Foundation

PrintDisplayed: 25/6/2024 19:50

UV FeII emission model of HE 0413-4031 and its relation to broad-line time delays

Other applications