Emergence of a Broad-Absorption-Line Outflow in the Narrow-line Seyfert 1 Galaxy WPVS 007

Details Emergence of a Broad-Absorption-Line Outflow in the Narrow-line Seyfert 1 Galaxy WPVS 007 Emergence of a Broad-Absorption-Line Outflow in the Narrow-line Seyfert 1 Galaxy WPVS 007

2009-06-11

arxiv.org/abs/0906.2149v1

Astrophys.J.701:176-199,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

Accepted for publication in ApJ, 65 pages, 17 figures

Scientific paper

10.1088/0004-637X/701/1/176

We report results from a 2003 FUSE observation, and reanalysis of a 1996 HST observation of the unusual X-ray transient Narrow-line Seyfert 1 galaxy WPVS 007. The HST FOS spectrum revealed mini-BALs with V_max ~ 900 km s^-1 and FWHM ~ 550 km s^-1. The FUSE spectrum showed that an additional BAL outflow with V_max ~ 6000 km s^-1 and FWHM ~ 3400 km s^-1 had appeared. WPVS 007 is a low-luminosity object in which such a high velocity outflow is not expected; therefore, it is an outlier on the M_V/V_max relationship. Template spectral fitting yielded apparent ionic columns, and a Cloudy analysis showed that the presence of PV requires a high ionization parameter log(U) >= 0 and high column density log(N_H) >= 23 assuming solar abundances and a nominal SED for low-luminosity NLS1s with alpha_ox=-1.28. A recent long Swift observation revealed the first hard X-ray detection and an intrinsic (unabsorbed) alpha_ox ~ -1.9$. Using this SED in our analysis yielded lower column density constraints (log(N_H) >= 22.2 for Z=1, or log(N_H) >= 21.6 if Z=5). The X-ray weak continuum, combined with X-ray absorption consistent with the UV lines, provides the best explanation for the observed Swift X-ray spectrum. The large column densities and velocities implied by the UV data in any of these scenarios could be problematic for radiative acceleration. We also point out that since the observed PV absorption can be explained by lower total column densities using an intrinsically X-ray weak spectrum, we might expect to find PV absorption preferentially more often (or stronger) in quasars that are intrinsically X-ray weak.

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