Hostname: page-component-8448b6f56d-gtxcr Total loading time: 0 Render date: 2024-04-24T22:53:37.567Z Has data issue: false hasContentIssue false
  • English
  • Français

Young Stellar Populations in the Collisional Ring Galaxy NGC 922

Published online by Cambridge University Press:  13 April 2010

A. Pellerin ,
G. R. Meurer ,
K. Bekki ,
D. M. Elmegreen ,
O. I. Wong  and
P. Knezek
A. Pellerin
Affiliation:
George P. and Cynthia W. Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics, Texas A&M University, College Station, TX 77843, USA
G. R. Meurer
Affiliation:
Physics & Astronomy Department, Johns Hopkins University, 3400 Charles Street, Baltimore, MD 21218, USA
K. Bekki
Affiliation:
Dept. of Astrophysics & Optics, School of Physics, University of New South Wales, NSW, 2052, Australia
D. M. Elmegreen
Affiliation:
Vassar College, Department of Physics and Astronomy, Box 745, Poughkeepsie, NY 12604, USA
O. I. Wong
Affiliation:
Astronomy Department, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA
P. Knezek
Affiliation:
WIYN Consortium Inc., PO Box 26732, Tucson, AZ 85726, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We studied the star cluster population properties in the nearby collisional ring galaxy NGC 922 using HST/WFPC2 photometry and population synthesis modeling. We found that 69% of the detected clusters are younger than 7 Myr, and that most of them are located in the ring or along the bar, consistent with the strong Hα emission. The images also show a tidal plume pointing toward the companion. Its stellar age is consistent with pre-existing stars that were probably stripped off during the passage of the companion. We compared the star-forming complexes observed in NGC 922 with those of a distant ring galaxy from the GOODS eld. It indicates very similar masses and sizes, suggesting similar origins. Finally, we found clusters that are excellent progenitor candidates for faint fuzzy clusters.

Keywords

galaxies: individual (NGC 922)galaxies: interactionsgalaxies: star clustersgalaxies: stellar contentgalaxies: high-redshift
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 406 - 407
Copyright
Copyright © International Astronomical Union 2010

References

Elmegreen, B. G. 2008, ApJ, 672, 1006CrossRefGoogle Scholar
Elmegreen, B. G. & Elmegreen, D. M. 2005, ApJ, 627, 632CrossRefGoogle Scholar
Hernquist, L. & Weil, M. L. 1993 MNRAS, 261, 804CrossRefGoogle Scholar
Larsen, S. S. & Brodie, J. P.AJ, 120, 2938CrossRefGoogle Scholar
Larsen, S. S. 2002, AJ, 124, 1393CrossRefGoogle Scholar
Leitherer, C. et al. 1999, ApJS, 123, 3CrossRefGoogle Scholar
Whitmore, B. C., Zhang, Q., Leitherer, C., Fall, S. M., Schweizer, F., & Miller, B. W. 1999, ApJ, 118, 1551CrossRefGoogle Scholar
Wolf, C., Meisenheimer, K., Rix, H.-W., Borch, A., Dye, S., & Kleinheinrich, M. 2003, AAP, 401, 73CrossRefGoogle Scholar
Wong, O. I. et al. 2006, MNRAS, 370, 1607CrossRefGoogle Scholar