Far-Ultraviolet and Visible Imaging of the Nucleus of M32
  We have imaged the nucleus of M32 at 1600 Angstroms (FUV) and 5500 Angstroms (V) using the Wide-Field/Planetary Camera 2 (WFPC2) aboard HST. We detected the nucleus at 1600 Angstroms using the redleak-free Woods filter on WFPC2. The FUV light profile can be fit with a Gaussian of FWHM 0.46" (4.6 pixels), but cannot be resolved into individual stars; no UV-bright nuclear structure was detected. The (FUV-V) color of the nucleus is 4.9 +/- 0.3, consistent with earlier observations. We are unable to confirm any radial variation in (FUV-V) within 0.8" of the nucleus; beyond that radius the FUV surface brightness drops below our detection threshhold. We also performed surface photometry in V and found our results to be in excellent agreement with deconvolved, WFPC1 results. M32's light profile continues to rise in a nuclear cusp even within 0.1" of its center. No intermediate-age stellar population is required by evolutionary population synthesis models to reproduce the (FUV-V) color of the nucleus, although these data and current models are insufficient to resolve this issue. 
A. A. Cole (1), J. S. Gallagher (1), J. R. Mould (2), and the WFPC2   IDT ((1) University of Wisconsin-Madison, (2) Mt. Stro...