New Light on the Stellar Populations in IZw18: Deep Near-Infrared Imaging

Details New Light on the Stellar Populations in IZw18: Deep Near-Infrared Imaging New Light on the Stellar Populations in IZw18: Deep Near-Infrared Imaging

2003-01-14

arxiv.org/abs/astro-ph/0301255v1

Astrophys.J. 588 (2003) 281-298

Astronomy and Astrophysics

Astrophysics

29 pages, 9 figures, accepted for publication in ApJ (May, 2003)

Scientific paper

10.1086/368352

We present deep JHK images of IZw18, the most metal-deficient Blue Compact Dwarf galaxy known, and analyze them in conjunction with archival HST/WFPC2 optical images. To investigate the stellar populations, we have divided the main body of IZw18 into eight regions, and fit the optical, near-infrared (NIR), and hybrid optical-NIR colors of these and the C component with evolutionary synthesis models. The composite best fit is obtained for an age for evolved stellar populations of <= 200Myr; fits with an older age of <= 500Myr are less likely but possible. Our data show no evidence for stellar populations in IZw18 older than this, although as much as 22% of the stellar mass in older stars (4% in J light) could remain undetected. The colors of the young and intermediate-age stellar populations are significantly affected by widespread and inhomogeneously distributed ionized gas and dust. Ionized gas emission is important in every region examined except the NW star cluster. Extinction is significant in both the NW and SE clusters. Red H-K, B-H, and V-K colors are not reliable indicators of old stellar populations because ionized gas emission is also red in these colors. V-I, on the other hand, reliably separates stars from gas because the former are red (V-I >= 0.4) while the latter is blue (V-I ~ -0.4).

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