Open AccessThe infrared–X‐ray continuum correlation in active galactic nuclei
Author(s) -
Contini M.,
Viegas S. M.,
Campos P. E.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-2966.2003.07059.x
Subject(s) - physics , astrophysics , active galactic nucleus , galaxy , rosat , luminosity , astronomy , infrared , luminous infrared galaxy
The correlation between the soft X‐ray and near‐infrared emission from active galactic nuclei (AGNs) is analysed using composite models. We find new evidence for differences in the ranges of parameters that characterize the narrow‐line region (NLR) of Seyfert galaxies and low‐ionization nuclear emission regions (LINERs). Soft X‐rays show less variability, so they are better fitted for this kind of analysis. In our models, soft X‐rays are emitted in the post‐shock region of clouds with relatively high shock velocities V s > 250 km s −1 . Consequently, dust emission peaks in the mid‐infrared. On the other hand, in the photoionized zone, dust is at lower temperature and usually does not contribute to the mid‐infrared emission. The results are sensible enough to allow the same modelling method to be applied to different types of AGN. We found that shock velocities are between 300 and 1000 km s −1 , with the NLR of low‐luminosity active galactic nuclei (LLAGNs) and type 2 Seyfert galaxies (Sy2s) showing lower velocities than type 1 Seyfert galaxies (Sy1s). The intensity of the ionizing radiation flux at the Lyman limit from the central source is low for LINERs and low‐luminosity AGNs (log F h = 9 to 10) , increasing towards Sy2s (log F h ∼ 11) and Sy1s (11 ≤ F h ≤ 12) . Results obtained by modelling the Einstein and the ROSAT samples of galaxies are in full agreement. Dust‐to‐gas ratios by number are ≥10 −14 in LINERs and LLAGNs, between 10 −15 and 3 × 10 −13 in Sy1s and up to 5 × 10 −13 in Sy2s. In order to fit the infrared and X‐ray continua, an η factor is defined, which accounts for the emitting area of the cloud. If the infrared emission is due to bremsstrahlung and comes from the same cloud that produces the soft X‐rays, the η values obtained from both emissions must be the same. Therefore, if (η) IR < (η) soft X , there must be a strong contribution of soft X‐rays from the active centre. From the η values, we expect to identify the objects that could present strong variability.