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Stellar Populations in the Pegasus Dwarf Galaxy

Published online by Cambridge University Press:  07 August 2017

Myung Gyoon Lee
Myung Gyoon Lee*
Affiliation:
Department of Astronomy, Seoul National University, Seoul, 151-742, Korea; Email: mglee@astrog.snu.ac.kr

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The Pegasus dwarf galaxy (DDO 216) is a resolved irregular galaxy. We present a study of stars in this galaxy based on BV RI CCD photometry obtained using the Palomar 1.5m telescope. The color-magnitude diagrams show (a) a dominant red giant branch (RGB) population, (b) a small number of asymptotic giant branch (AGB) population above the tip of the RGB (TRGB), and (c) a sparse popultion of massive young stars including the brightest red supergiants. The mean metallicity of the RGB has been estimated from the color of the RGB at MI = −3.5 mag: [Fe/H] = −1.5 ± 0.2 dex. The distance to this galaxy has been measured using the I-magnitude of the TRGB: (m – M)0 = 25.13 ± 0.11 mag (d = 1060 ± 50 kpc) (see Lee et al. 1993). This value is significantly smaller than the Cepheid distance estimate by Hoessel et al. (1990), (m – M)0 = 26.22±0.20 (d = 1750±160 kpc).

Type
Poster Papers
Information
Symposium - International Astronomical Union , Volume 164: Stellar Populations , 1995 , pp. 413
Copyright
Copyright © Kluwer 1995 

References

Hoessel, J. G., Abbot, M. J., Saha, A., Mossman, A. E., and Danielson, G. E. 1990, AJ, 100, 100 CrossRefGoogle Scholar
Lee, M. G., Freedman, W. L., and Madore, B. F. 1993, ApJ, 417, 417 Google Scholar