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We report the results of a preliminary nova survey of Local Group dwarfellipticals. We used the Tenagra Observatory to observe M32, NGC 205, NGC 147,and NGC 185 in their entirety every clear night over a 4.5 month interval anddiscovered one nova in M32 and a candidate nova in NGC 205. The nova in M32 wasverified spectroscopically. The nova candidate in NGC 205 had an unusually lowpeak luminosity (M_V = -5.1), and we were unable to obtain spectroscopicverification. We report a high bulk nova rate for M32 of 2(+2.4,-1.0) yr^-1and, assuming the candidate nova is correctly identified, for NGC 205 of2(+2.2,-1.0) yr^-1. If the NGC 205 variable is not a nova, we calculate anupper limit on the bulk nova rate for NGC 205 of 1.5 yr^-1. We report upperlimits on the bulk nova rates in NGC 147 of 2 yr^-1 and NGC 185 of 1.8 yr^-1and a combined bulk nova rate for the four galaxies of 4(+4.2,-1.4) yr^-1(2{+3.9,-1.4} yr^-1 without the NGC 205 nova candidate). From the bulk rates,integrated and extinction corrected V-band photometry, and (V-K)_0 colors wederive a luminosity specific nova rate for M32 of 12.0(+14.4,-6.0) yr^-1 [10^10L_Sun,K]^-1 and for NGC 205 of 29.3(+32.3,-14.7) yr^-1 [10^10 L_Sun,K]^-1 andfor the combined 4 galaxies of 14.1(+14.8,-4.9) yr^-1 [10^10 L_Sun,K]^-1(7.0{+13.7,-4.9} yr^-1[10^10 L_Sun,K]^-1 without the NGC 205 nova candidate).If the higher rate is confirmed by surveys in subsequent seasons, it wouldimply that either dwarf ellipticals have a higher interacting binary fractionthan their higher mass counter parts, or that the completeness is higher forthese less complex systems and the nova rates for larger, more distant systemsare systematically underestimated.

A Possible High Nova Rate for Two Local Group Dwarf Galaxies: M32 and NGC 205