Intergalactic H II regions discovered in SINGG

Ryan-Weber, E. V., Meurer, G. R., Freeman, K. C., Putman, M. E., Webster, R. L., Drinkwater, M. J., Ferguson, H. C., Hanish, D., Heckman, T. M., Kennicutt, R. C., Kilborn, V. A., Knezek, P. M., Koribalski, B. S., Meyer, M. J., Oey, M. S., Smith, R. C., Staveley-Smith, L. and Zwaan, M. A. (2004) Intergalactic H II regions discovered in SINGG. The Astronomical Journal, 127 3: 1431-1440. doi:10.1086/381905

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Author Ryan-Weber, E. V.
Meurer, G. R.
Freeman, K. C.
Putman, M. E.
Webster, R. L.
Drinkwater, M. J.
Ferguson, H. C.
Hanish, D.
Heckman, T. M.
Kennicutt, R. C.
Kilborn, V. A.
Knezek, P. M.
Koribalski, B. S.
Meyer, M. J.
Oey, M. S.
Smith, R. C.
Staveley-Smith, L.
Zwaan, M. A.
Title Intergalactic H II regions discovered in SINGG
Journal name The Astronomical Journal   Check publisher's open access policy
ISSN 0004-6256
Publication date 2004-03-01
Year available 2004
Sub-type Article (original research)
DOI 10.1086/381905
Open Access Status File (Publisher version)
Volume 127
Issue 3
Start page 1431
End page 1440
Total pages 10
Editor Paul Hodge
Place of publication Madison, WI, United States
Publisher Institute of Physics Publishing
Language eng
Abstract A number of very small isolated H II regions have been discovered at projected distances up to 30 kpc from their nearest galaxy. These H II regions appear as tiny emission-line objects in narrowband images obtained by the NOAO Survey for Ionization in Neutral Gas Galaxies (SINGG). We present spectroscopic confirmation of four isolated H II regions in two systems; both systems have tidal H I features. The results are consistent with stars forming in interactive debris as a result of cloud-cloud collisions. The Halpha luminosities of the isolated H II regions are equivalent to the ionizing flux of only a few O stars each. They are most likely ionized by stars formed in situ and represent atypical star formation in the low-density environment of the outer parts of galaxies. A small but finite intergalactic star formation rate will enrich and ionize the surrounding medium. In one system, NGC 1533, we calculate a star formation rate of 1.5 x 10(-3) M-. yr(-1), resulting in a metal enrichment of similar to 1 x 10(-3) solar for the continuous formation of stars. Such systems may have been more common in the past and a similar enrichment level is measured for the metallicity floor'' in damped Lyalpha absorption systems.
Keyword Galaxies
Intergalactic Medium
Isolated Star-formation
Extreme Outer Regions
Magellanic Stream
Synthesis Models
Virgo Cluster
Disk Galaxies
Hii Region
Atomic Gas
Astronomy & Astrophysics
Galaxies : Halos
Galaxies : Star Clusters
Hii Regions
Stars : Formation
Q-Index Code C1
Institutional Status UQ

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Created: Wed, 15 Aug 2007, 14:44:55 EST