Brian A. Keeney et al. 2006 The Astronomical Journal 132 2496 doi:10.1086/508516
Discovery of a Metal-Line Absorber Associated with a Local Dwarf Starburst Galaxy
FREE ISSUEBrian A. Keeney1, John T. Stocke1, Jessica L. Rosenberg2, Jason Tumlinson3 and Donald G. York4,5
Show affiliationsWe present optical and near-infrared images, H I 21 cm emission maps, optical spectroscopy, and Hubble Space Telescope Space Telescope Imaging Spectrograph ultraviolet spectroscopy of the QSO/galaxy pair SBS 1122+594/IC 691. The QSO sight line lies at a position angle of 27° from the minor axis of the nearby dwarf starburst galaxy IC 691 (czgal = 1204 ± 3 km s-1, LB ~ 0.09L*, current star formation rate = 0.08-0.24 h
M
yr-1) and 33 h
kpc (6
6) from its nucleus. We find that IC 691 has an H I mass of M
= (3.6 ± 0.1) × 108 M and a dynamical mass of Mdyn = (3.1 ± 0.5) × 1010 h M. The UV spectrum of SBS 1122+594 shows a metal-line (Lyα+C IV) absorber near the redshift of IC 691 at czabs = 1110 ± 30 km s-1. Since IC 691 is a dwarf starburst and the SBS 1122+594 sight line lies in the expected location for an outflowing wind, we propose that the best model for producing this metal-line absorber is a starburst wind from IC 691. We place consistent metallicity limits on IC 691 ([Z/Z] ~ -0.7) and the metal-line absorber ([Z/Z] < -0.3). We also find that the galaxy's escape velocity at the absorber location is vesc = 80 ± 10 km s-1 and derive a wind velocity of vw = 160 ± 50 km s-1. Thus, the evidence suggests that IC 691 produces an unbound starburst wind that escapes from its gravitational potential to transport metals and energy to the surrounding intergalactic medium.
- Keywords
galaxies: dwarf; galaxies: individual (IC 691); galaxies: starburst; quasars: absorption lines; quasars: individual (SBS 1122+594)
- Dates
-
Issue 6 (2006 December)
Received 2006 June 23, accepted for publication 2006 August 13
Published 2006 November 1
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Discovery of a Metal-Line Absorber Associated with a Local Dwarf Starburst Galaxy
Brian A. Keeney et al. 2006 The Astronomical Journal 132 2496
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