paper

Improved evidence for a black hole in M32 from HST/FOS spectra - I. Observations

arXiv:astro-ph/9702147 · doi:10.1086/304690

Abstract

We have obtained spectra through small apertures centered on the nuclear region and major axis of M32, with the HST/FOS. A detailed analysis and reduction of the data is presented, including: (i) new calibrations and modeling of the FOS aperture sizes, PSF and line-spread-functions; (ii) determination of the aperture positioning for each observation; and (iii) accurate wavelength calibration, template matching, and kinematical analysis of the spectra. This yields measurements of the stellar rotation velocities and velocity dispersions with five times higher spatial resolution than the best available ground-based data. The inferred velocities provide the highest angular resolution stellar kinematical data obtained to date for any stellar system. The observations show a steeper rotation curve and higher central velocity dispersion than ground-based data. The rotation velocity is observed to be 30 km/s at 0.1" from the nucleus; roughly twice the value measured from the ground at this distance. The nuclear dispersion measured through the smallest FOS aperture (0.068" square) is 156 +/- 10 km/s. The average of four independent dispersion measurements at various positions inside the central 0.1" is 126 km/s, with a RMS scatter of 21 km/s. The nuclear dispersion measured from the ground is only 85-95 km/s, whereas the dispersion outside the central arcsec is only 45-55 km/s. These results significantly strengthen previous arguments for the presence of a massive nuclear black hole in M32. Detailed dynamical models are presented in a series of companion papers.

35 pages, LaTeX, with 10 PostScript figures; submitted to the Astrophysical Journal; mpeg animation of the stellar motions in M32 available at http://oposite.stsci.edu/pubinfo/Anim.html

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