DWARF ELLIPTIC GALAXIES IN THE M81 GROUP - THE STRUCTURE AND STELLAR POPULATIONS OF BK5N AND F8D1

those of the Local Group. It has therefore provided a different enviro nment for the evolution of its member galaxies. We have carried out a CCD survey of the M81 Group to search for analogs to Local Group dwarf elliptical (dE) galaxies. All the M81 dwarfs previously identified in photographic surveys were recovered, and we also discovered several n ew systems whose surface brightnesses fall within the range found for Local Group dE's. We have obtained Hubble Space Telescope Wide Field P lanetary Camera 2 images through the F555W and F814W filters of two M8 1 Group dE's, BK5N and a new system, designated F8D1. The resulting co lor-magnitude diagrams show the upper 2 mag of the red giant branch. T he I magnitudes of the red giant branch tip in both galaxies yield dis tances that are consistent with membership in the M81 Group. Surface b rightness and total magnitude measurements indicate that BK5N and F8D1 have similar central surface brightnesses (24.5 and 25.4 mag arcsec(- 2) in V, respectively), but F8D1's larger length scale results in its being 3 mag more luminous than BK5N. BK5N lies on the relation between central surface brightness and absolute magnitude defined by Local Gr oup dwarf elliptical galaxies, but F8D1 does not. F8D1 is more luminou s for its central surface brightness than the relation predicts, simil ar to the large low surface brightness dwarf galaxies found in, for ex ample, 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] approximate to -1.0) than BK5N ( [Fe/H] approximate to -1.7). Both BK5N and F8D1 lie on the relation be tween absolute magnitude and metal abundance defined by Local Group dw arf elliptical galaxies. However, as regards the relation between cent ral surface brightness and metal abundance, BK5N again follows the Loc al Group dwarfs while F8D1 deviates significantly from this relation. This suggests that the total amount of luminous matter is more fundame ntal in controlling metal enrichment than the surface density of lumin ous matter. We have also used the color width of the giant branch comp ared with the photometric errors to establish abundance ranges in both galaxies, the sizes of which are comparable to those in Local Group d E's. From the numbers and luminosities of asymptotic giant branch star s more luminous than the red giant branch tip, we infer that, again li ke many of the Local Group dE's, both BK5N and F8D1 have had extended epochs of star formation. F8D1 contains stars as young as 3-4 Gyr, whi le in BK5N stars as young as similar to 8 GYr are present. The fractio ns of intermediate-age population, at similar to 30%, are similar in b oth galaxies. Further, one globular cluster has been found in F8D1, bu t none are present in BK5N. These numbers of clusters are consistent w ith our expectations from Local Group dwarfs. Overall, we iind that BK 5N is similar in all respects to the Local Group dE's. Thus, despite t he different environments of the M81 Group and the Local Group, dwarf galaxies of very similar properties are present in each. F8D1, on the other hand, has no Local Group counterpart and is indeed rare even in large clusters of galaxies. Our study of its stellar population is the first for a large, low surface brightness dwarf.