Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-10-24
Astronomy and Astrophysics
Astrophysics
To appear in Feb. 1998 AJ. 18 figures, 5 of which are jpg. The jpg's can be incorporated into the main ps file by changing the
Scientific paper
10.1086/300233
We have obtained HST WFPC2 images through the F555W and F814W filters of two M81 group dE's: BK5N and a new system, designated F8D1. The resulting color-magnitude diagrams show the upper two magnitudes of the red giant branch. Surface brightness and total magnitude measurements indicate that BK5N and F8D1 have similar central surface brightness (24.5 and 25.4 mag/arcsec^2 in V, respectively), but F8D1's larger length scale results in it being 3 magnitudes more luminous than BK5N. BK5N lies on the relation between central surface brightness and absolute magnitude defined by Local Group dwarf ellipticals, but F8D1 does not. F8D1 is more luminous for its central surface brightness than the relation predicts, similar to the large low surface brightness dwarf galaxies found in, for example, Virgo. The mean color of the giant branch is used to establish the mean abundance of each galaxy. F8D1, the more luminous galaxy, is significantly more metal rich ([Fe/H] ~ -1.0) than BK5N ([Fe/H] ~ -1.7). Both BK5N and F8D1 lie on the relation between absolute magnitude and metal abundance defined by Local Group dwarf ellipticals. However, as regards the relation between central surface brightness and metal abundance, BK5N again follows the Local Group dwarfs, while F8D1 deviates significantly from this relation. This suggests that the total amount of luminous matter is more fundamental in controlling metal enrichment than the surface density of luminous matter. We also discuss the intermediate age stars, and note 1 globular cluster in F8D1. (edited)
Armandroff Taft E.
Caldwell Nelson
Da Costa Gary S.
Seitzer Patrick
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