Reference : VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+0...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/19118
VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7
English
Hutsemekers, Damien mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Hall, Patrick [Princeton University > > > >]
Brinkmann, J. [Apache Point Observatory, PO Box 59, Sunspot, NM 88349-0059, USA]
1-Feb-2004
Astronomy and Astrophysics
EDP Sciences
415
77-85
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] quasars: general ; quasars: absorption lines
[en] We analyse high-resolution VLT+UVES spectra of the low-ionization intrinsic absorber observed in the BAL QSO SDSS J001130.56+005550.7. Two narrow absorption systems at velocities -600 km s[SUP]-1[/SUP] and -22 000 km s[SUP]-1[/SUP] are detected. The low-velocity system is part of the broad absorption line (BAL), while the high-velocity one is well detached. While most narrow absorption components are only detected in the high-ionization species, the lowest velocity component is detected in both high- and low-ionization species, including in the excited Si II[SUP]*[/SUP] and C II[SUP]*[/SUP] lines. From the analysis of doublet lines, we find that the narrow absorption lines at the low-velocity end of the BAL trough are completely saturated but do not reach zero flux, their profiles being dominated by a velocity-dependent covering factor. The covering factor is significantly smaller for Mg II than for Si IV and N V , which demonstrates the intrinsic nature of absorber. From the analysis of the excited Si II[SUP]*[/SUP] and C II[SUP]*[/SUP] lines in the lowest velocity component, we find an electron density ~=10[SUP]3[/SUP] cm[SUP]-3[/SUP]. Assuming photoionization equilibrium, we derive a distance ~=20 kpc between the low-ionization region and the quasar core. The correspondence in velocity of the high- and low-ionization features suggests that all these species must be closely associated, hence formed at the same distance of Ë 20 kpc, much higher than the distance usually assumed for BAL absorbers. Based on observations collected at the European Southern Observatory, Cerro Paranal, Chile (ESO 267.A-5698).
http://hdl.handle.net/2268/19118
10.1051/0004-6361:20031688
http://adsabs.harvard.edu/abs/2004A%26A...415...77H
http://de.arxiv.org/abs/astro-ph/0311026

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