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A Gaseous Group with Unusual Remote Star Formation

Published online by Cambridge University Press:  02 January 2013

N. Santiago-Figueroa ,
M. E. Putman ,
J. Werk ,
G. R. Meurer  and
E. Ryan-Weber
N. Santiago-Figueroa*
Affiliation:
Department of Physics, Fisk University, 1000 17th Ave N., Nashville, TN 37208, USA Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN 37235, USA Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA
M. E. Putman
Affiliation:
Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA
J. Werk
Affiliation:
Department of Astronomy and Astrophysics, UCO/Lick Observatory;University of California, 1156 High Street, Santa Cruz, CA 95064, USA
G. R. Meurer
Affiliation:
International Centre for Radio Astronomy Research, The University of Western Australia, M468, 35 Stirling Highway, Crawley, WA 6009, Australia
E. Ryan-Weber
Affiliation:
Centre for Astrophysics and Supercomputer, Swinburne University, PO Box 218, Hawthorn, Victoria 3122, Australia
*
GCorresponding author. Email: [email protected]
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Abstract

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We present VLA 21-cm observations of the spiral galaxy ESO 481-G017 to determine the nature of remote star formation traced by an Hii region found 43 kpc and ∼800 km s−1 from the galaxy center (in projection). ESO 481-G017 is found to have a 120 kpc Hi disk with a mass of 1.2 × 1010M⊙ and UV GALEX images reveal spiral arms extending into the gaseous disk. Two dwarf galaxies with Hi masses close to 108M⊙ are detected at distances of ∼200 kpc from ESO 481-G017 and a Hi cloud with a mass of 6 × 107M⊙ is found near the position and velocity of the remote Hii region. The Hii region is somewhat offset from the Hi cloud spatially and there is no link to ESO 481-G017 or the dwarf galaxies. We consider several scenarios for the origin of the cloud and Hii region and find the most likely is a dwarf galaxy that is undergoing ram pressure stripping. The Hi mass of the cloud and Hi luminosity of the Hii region (1038.1 erg s−1) are consistent with dwarf galaxy properties, and the stripping can trigger the star formation as well as push the gas away from the stars.

Keywords

galaxies: ISMgalaxies: dwarfHii regionsISM: Hi
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 28 , Issue 3 , 2011 , pp. 271 - 279
Copyright
Copyright © Astronomical Society of Australia 2011

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