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Title:
Emergence of a Broad Absorption Line Outflow in the Narrow-line Seyfert 1 Galaxy WPVS 007
Authors:
Leighly, Karen M.; Hamann, Fred; Casebeer, Darrin A.; Grupe, Dirk
Affiliation:
AA(Homer L. Dodge Department of Physics and Astronomy, The University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA ; Visiting Professor, Fall 2006-Spring 2007, The Ohio State University, Department of Astronomy, 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210-1173, USA.; ), AB(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611-2055, USA ), AC(Homer L. Dodge Department of Physics and Astronomy, The University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA ), AD(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA )
Publication:
The Astrophysical Journal, Volume 701, Issue 1, pp. 176-199 (2009). (ApJ Homepage)
Publication Date:
08/2009
Origin:
IOP
ApJ Keywords:
quasars: absorption lines, quasars: individual: [WPV85] 007
DOI:
10.1088/0004-637X/701/1/176
Bibliographic Code:
2009ApJ...701..176L

Abstract

We report results from a 2003 Far Ultraviolet Spectroscopic Explorer (FUSE) observation and reanalysis of a 1996 Hubble Space Telescope (HST) observation of the unusual X-ray transient Narrow-line Seyfert 1 galaxy WPVS 007. The HST Faint Object Spectrograph (FOS) spectrum revealed mini-BALs (broad absorption lines) 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 MV /v max relationship. Template spectral fitting yielded apparent ionic columns, and a Cloudy analysis showed that the presence of P V requires a high-ionization parameter log(U) >= 0 and high-column density log(N H) >= 23 assuming solar abundances and a nominal spectral energy distribution (SED) for low-luminosity NLS1s with α ox = -1.28. A recent long Swift observation revealed the first hard X-ray detection and an intrinsic (unabsorbed) α 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 P V absorption can be explained by lower total column densities using an intrinsically X-ray weak spectrum, we might expect to find P V absorption preferentially more often (or stronger) in quasars that are intrinsically X-ray weak.

Based on observations made with the NASA-CNES-CSA Far-Ultraviolet Spectroscopic Explorer. FUSE is operated for NASA by Johns Hopkins University under NASA contract NAS5-32985.

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