The Warm Absorber constrained by the coronal lines in Seyfert 1 galaxies
| Autor: | Delphine Porquet, Dumont, A. -M, Collin, S., Mouchet, M. |
|---|---|
| Přispěvatelé: | Departement d'Astrophysique Extragalactique et de Cosmologie (DAEC), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Porquet, Delphine |
| Jazyk: | angličtina |
| Rok vydání: | 1998 |
| Předmět: |
[SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
[SDU.ASTR.HE] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] Astrophysics (astro-ph) FOS: Physical sciences GALAXIES: SEYFERT [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph] Astrophysics GALAXIES: ACTIVE [SDU] Sciences of the Universe [physics] X-RAYS: GALAXIES [SDU]Sciences of the Universe [physics] GALAXIES: INDIVIDUAL: MCG -6-30-15 |
| Zdroj: | Astronomy and Astrophysics-A&A Astronomy and Astrophysics-A&A, EDP Sciences, 1999 NASA Astrophysics Data System |
| ISSN: | 0004-6361 |
| Popis: | We present results of the photoionization code IRIS, which calculates the spectrum emitted by the Warm Absorber (WA) in Seyfert 1 galaxies for a large grid of parameters (density, column density, ionization parameter...). We show that in Seyfert 1s, coronal lines Fe X, Fe XI, Fe XIV...), whose emission region shares common characteristics with the WA, could be formed in the WA. Unlike the absorption edges, such as those of O VII and O VIII observed in soft X-rays which are produced by the WA, these lines strongly constrain the physical parameters of the WA, especially the hydrogen density. Indeed, in order to avoid producing coronal line equivalent widths larger than observed, a high density (nH \geq 10^{10} cm-3) is required for the WA in most cases. This result is obtained for the mean observed Seyfert 1 features, as well as for the case study of MCG-6-30-15. It implies that the distance of the WA from the incident radiation source is of the order of that of the Broad Line Region (BLR) 13 pages, 14 figures, version accepted for publication in A&A |
| Databáze: | OpenAIRE |
| Externí odkaz: |
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