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

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F24%3A00139415" target="_blank" >RIV/00216224:14310/24:00139415 - isvavai.cz</a>

Result on the web

<a href="https://arxiv.org/abs/2310.03544" target="_blank" >https://arxiv.org/abs/2310.03544</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202348172" target="_blank" >10.1051/0004-6361/202348172</a>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

Result was created during the realization of more than one project. More information in the Projects tab.

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2024

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

683

Issue of the periodical within the volume

March 2024

Country of publishing house

FR - FRANCE

Number of pages

18

Pages from-to

1-18

UT code for WoS article

001185810900029

EID of the result in the Scopus database

2-s2.0-85187979986