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Title:
Stellar populations in local group dwarf elliptical galaxies. II - NGC 205
Authors:
Mould, J.; Kristian, J.; Da Costa, G. S.
Affiliation:
AA(Palomar Observatory, Pasadena, CA; Kitt Peak National Observatory, Tucson, AZ)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 15, 1984, p. 575-581. NASA-supported research. (ApJ Homepage)
Publication Date:
03/1984
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Astronomical Photometry, Dwarf Galaxies, Elliptical Galaxies, Local Group (Astronomy), Star Distribution, Andromeda Galaxy, Astronomical Catalogs, Charge Coupled Devices, Globular Clusters, Mass To Light Ratios, Metallicity, Red Giant Stars, Stellar Luminosity
DOI:
10.1086/161824
Bibliographic Code:
1984ApJ...278..575M

Abstract

NGC 205, a dwarf elliptical companion of M31, was studied using deep CCD photometry on the VRI system. Consideration is given to a comparison between the giant branch and the Galactic globular clusters, the degree of chemical enrichment in the outer parts of NGC 204, and the setting of constraints on the stellar population of NGC 205. Should the distance of the galaxy be that of M31, this field's stellar population is extremely old. If star formation in NGC 205 is a recurring phenomenon, it is confined to the interior of the galaxy. Should the stellar population of NGC 205 be as old as Galactic globular clusters, its distance modulus is 24.3 + or - 0.2. The giant branch location corresponds to a mean metallicity greater than or equal to -0.9 + or - 0.2, and a metallicity dispersion is determined to be sigma greater than or equal to 0.5 dex. Also noted is that the color distribution at a given luminosity appears to be positively skewed.

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