| Name: | Ashwani Pandey |
| Affiliation: | Center for Theoretical Physics Warsaw, Poland |
| Conference ID : | ASI2024_200 |
| Title : | Broad-line region in active galactic nuclei: dusty or dustless? |
| Authors : | Ashwani Pandey1, Bozena Czerny1, Swayamtrupta Panda2, Raj Prince1, Vikram Kumar Jaiswal1, Mary Loli Martinez–Aldama3, Michal Zajaček4, and Marzena Śniegowska5 |
| Authors Affiliation: | 1 Center for Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, Poland
2 Laboratório Nacional de Astrofísica, MCTI, Rua dos Estados Unidos 154, Bairro das Nações. CEP 37504-364, Itajubá, MG, Brazil
3 Astronomy Department, Universidad de Concepción, Casilla 160-C, Concepción, 4030000, Chile
4 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotlářska 2, 611 37 Brno, Czech Republic
5 School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel |
| Mode of Presentation: | Poster |
| Abstract Category : | Galaxies and Cosmology |
| Abstract : | Context. The dust in the active galactic nuclei is clearly present right outside the broad-line region (BLR), in the form of a dusty molecular torus. However, some models of the BLR predict that dust may also exist within the BLR.
Aims. We study the reprocessing of the radiation by the BLR with the aim to see how the presence of the dust affects the reprocessed continuum and the line properties.
Methods. We calculate a range of models with the use of CLOUDY photoionization code for dusty and dustless plasma. We pay particular attention to the well-studied object NGC 5548, and we compare the line equivalent width predictions with the observed data for this object.
Results. We obtain a rough agreement between the expected equivalent widths of the Hβ and Mg II lines with observed values for NGC 5548 for the line distances implied by the time-delay measurement (for Hβ) and by the radius-luminosity relation (for Mg II) when the medium is dusty. The incident radiation is then consistent with the radiation seen by the observer, no shielding between the inner disk and the BLR is required. High ionization lines like He II, however, form clearly in the inner dustless region. When the additional absorber is present, the Hβ emitting region moves closer, to the dustless part of the accretion disk surface. |
