Physical Conditions in the Ultraviolet Absorbers of IRAS F22456-5125

Details Physical Conditions in the Ultraviolet Absorbers of IRAS F22456-5125 Physical Conditions in the Ultraviolet Absorbers of IRAS F22456-5125

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...713..900d&link_type=abstract

The Astrophysical Journal, Volume 713, Issue 2, pp. 900-905 (2010).

Astronomy and Astrophysics

Astronomy

2

Galaxies: Seyfert, Ultraviolet: Galaxies

Scientific paper

We present the ultraviolet (UV) and X-ray spectra observed with the Far Ultraviolet Spectroscopic Explorer (FUSE) and the XMM-Newton satellite, respectively, of the low-z Seyfert 1 galaxy IRAS F22456 - 5125. This object shows absorption from five distinct, narrow kinematic components that span a significant range in velocity (~0 to -700 km s-1) and ionization (Lyman series, C III, N III, and O VI). We also show that three of the five kinematic components in these lines appear to be saturated in Lyβ λ1026 and that all five components show evidence of saturation in the O VI doublet lines λλ1032, 1038. Further, all five components show evidence for partial covering due to the absorption seen in the O VI doublet. This object is peculiar because it shows no evidence for corresponding X-ray absorption to the UV absorption in the X-ray spectrum, which violates the 1:1 correlation known for low-z active galactic nuclei (AGNs). We perform photoionization modeling of the UV absorption lines and predict that the O VII column density should be small, which would produce little to no absorption in agreement with the X-ray observation. We also examine the UV variability of the continuum flux for this object (an increase of a factor of 6). As the absorption components lack variability, we find a lower limit of ~20 kpc for the distance for the absorbers from the central AGN.
Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. FUSE is operated for NASA by the Johns Hopkins University under NASA contract NAS5-32985.

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