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Stars on Double Duty: Probing Cool Gas in Galaxies at Z ∼ 0.6 with Stellar Light

Published online by Cambridge University Press:  17 September 2012

K.H.R. Rubin ,
J.X. Prochaska ,
D.C. Koo  and
A.C. Phillips
K.H.R. Rubin
Affiliation:
University of California Observatories, University of California, Santa Cruz, CA 95064, USA. e-mail: [email protected]
J.X. Prochaska
Affiliation:
University of California Observatories, University of California, Santa Cruz, CA 95064, USA. e-mail: [email protected]
D.C. Koo
Affiliation:
University of California Observatories, University of California, Santa Cruz, CA 95064, USA. e-mail: [email protected]
A.C. Phillips
Affiliation:
University of California Observatories, University of California, Santa Cruz, CA 95064, USA. e-mail: [email protected]
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Abstract

The luminous components of galaxies can act as powerful probes of halo gas in foreground galaxies along the sightline. We use Keck/LRIS absorption-line spectroscopy of a luminous, blue background galaxy at z = 0.69 to study Mg II halo gas in the outskirts (ρ = 11.1h−1kpc) of a massive, poststarburst galaxy in the foreground at z = 0.47. The foreground absorber shows signs of recent merger activity and is host to a low-luminosity AGN. The halo absorption we observe is extremely strong (Wr(2796) = 4.0 ± 0.1Å) and is indicative of a large Mg II gas velocity width (> 400kms−1). We briefly discuss the possible origins of this absorption, including multiphase cooling of hot halo gas and galactic winds/outflows.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 56: The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall? , 2012 , pp. 101 - 104
Copyright
© EAS, EDP Sciences, 2012

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References

Adelberger, K.L., Shapley, A.E., Steidel, C.C., et al., 2005, ApJ, 629, 636CrossRef
Baldwin, J.A., Phillips, M.M., & Terlevich, R., 1981, PASP, 93, 5CrossRef
Bruzual, G., & Charlot, S., 2003, MNRAS, 344, 1000CrossRef
Bundy, K., Ellis, R.S., & Conselice, C.J., 2005, ApJ, 625, 621CrossRef
Ellison, S.L., 2006, MNRAS, 368, 335CrossRef
Giavalisco, M., et al., 2004, ApJ, 600, L93CrossRef
Ho, L.C., 2008, ARA&A, 46, 475CrossRef
Maller, A.H., & Bullock, J.S., 2004, MNRAS, 355, 694CrossRef
Weiner, B.J., et al., 2009, ApJ, 692, 187CrossRef
Weiner, B.J., et al., 2006, ApJ, 653, 1027CrossRef
Willmer, C.N.A., et al., 2006, ApJ, 647, 853CrossRef
Wirth, G.D., et al., 2004, AJ, 127, 3121CrossRef