Determining the Stellar Populations of UGC 2302

Details Determining the Stellar Populations of UGC 2302 Determining the Stellar Populations of UGC 2302

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...20311510b&link_type=abstract

American Astronomical Society Meeting 203, #115.10; Bulletin of the American Astronomical Society, Vol. 35, p.1393

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present ground-based BVRI data on the massive, low surface brightness (LSB) galaxy UGC 2302. UGC 2302 is a typical, disk dominated LSB, that is close enough to resolve its massive stars with HST. The broadband, ground-based data will be combined with the results from HST to begin to deconvolve the stellar populations of this galaxy.
Surface brightness plots and the optical images show evidence of a bar-like concentration at the center of the galaxy. Like many LSBs, UGC 2302 has a disk color that is bluer than the disks of typical high surface brightness disk galaxies. The blue disk color is inconsistent with an old, metal-poor population, indicating the presence of young stars. In the central region of the galaxy the situation is more complicated. While the BV color is consistent with a moderately old/metal-rich population, the VI color is too blue for this scenario, and suggests, instead, a younger/metal-poor population. Determination of the contribution from massive stars to each of the broadband filters using the HST data will help us resolve this puzzle.
Bovill's research was supported by the NOAO/KPNO Research Experience for Undergraduates (REU) Program which is funded by the National Science Foundation (NSF) through Scientific Program Order No.3 (AST-0243875) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF.

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