UV Fe II emission model of HE 0413-4031 and its relation to broad-line time delays
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2023
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| author | Zajaček, Michal Panda, Swayamtrupta Pandey, Ashwani Prince, Raj Rodríguez-Ardila, Alberto Jaiswal, Vikram Czerny, Bożena Hryniewicz, Krzysztof Urbanowicz, Maciej Trzcionkowski, Piotr Śniegowska, Marzena Fałkowska, Zuzanna Martínez-Aldama, Mary Loli Werner, Norbert |
| author_facet | Zajaček, Michal Panda, Swayamtrupta Pandey, Ashwani Prince, Raj Rodríguez-Ardila, Alberto Jaiswal, Vikram Czerny, Bożena Hryniewicz, Krzysztof Urbanowicz, Maciej Trzcionkowski, Piotr Śniegowska, Marzena Fałkowska, Zuzanna Martínez-Aldama, Mary Loli Werner, Norbert |
| contents | Fe II 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$\lambda2800$ emission, which is one of the lines used for black hole mass measurements and cosmological applications. We use the 11-year monitoring of the selected quasar HE 0413-4031 with the South African Large Telescope (SALT) and we supplement this monitoring with the near-IR spectrum taken with the SOAR telescope. A new redshift determination ($z=1.39117 \pm 0.00017$) 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 Mg II and UV Fe II emissions. The line characteristics and the time delay of the Mg II emission ($224^{+21}_{-23}$ days) are not significantly affected. However, in comparison with the previous analysis, the rest-frame UV FeII time delay ($251^{+9}_{-7}$ days) is consistent with the inferred UV FeII line FWHM of $4200\,{\rm km/s}$ 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 $\sim 0.023$ pc (4700 AU). The inferred velocity shift of both Mg II and UV Fe II lines with respect to the systemic redshift is now rather low, below 300 km s$^{-1}$. In addition, we construct 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 H$β$ $R-L$ relations. While the new decomposition of the spectrum is satisfactory, we see a need to create better Fe II templates using the newest version of the code CLOUDY. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_03544 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | UV Fe II emission model of HE 0413-4031 and its relation to broad-line time delays Zajaček, Michal Panda, Swayamtrupta Pandey, Ashwani Prince, Raj Rodríguez-Ardila, Alberto Jaiswal, Vikram Czerny, Bożena Hryniewicz, Krzysztof Urbanowicz, Maciej Trzcionkowski, Piotr Śniegowska, Marzena Fałkowska, Zuzanna Martínez-Aldama, Mary Loli Werner, Norbert Astrophysics of Galaxies Fe II 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$\lambda2800$ emission, which is one of the lines used for black hole mass measurements and cosmological applications. We use the 11-year monitoring of the selected quasar HE 0413-4031 with the South African Large Telescope (SALT) and we supplement this monitoring with the near-IR spectrum taken with the SOAR telescope. A new redshift determination ($z=1.39117 \pm 0.00017$) 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 Mg II and UV Fe II emissions. The line characteristics and the time delay of the Mg II emission ($224^{+21}_{-23}$ days) are not significantly affected. However, in comparison with the previous analysis, the rest-frame UV FeII time delay ($251^{+9}_{-7}$ days) is consistent with the inferred UV FeII line FWHM of $4200\,{\rm km/s}$ 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 $\sim 0.023$ pc (4700 AU). The inferred velocity shift of both Mg II and UV Fe II lines with respect to the systemic redshift is now rather low, below 300 km s$^{-1}$. In addition, we construct 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 H$β$ $R-L$ relations. While the new decomposition of the spectrum is satisfactory, we see a need to create better Fe II templates using the newest version of the code CLOUDY. |
| title | UV Fe II emission model of HE 0413-4031 and its relation to broad-line time delays |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2310.03544 |