2000AJ....119.1268G

We have used an Imaging Fabry-Perot Spectrophotometer with the Adaptive Optics Bonnette on the Canada-France-Hawaii Telescope to measure stellar radial velocities in the globular cluster M15 (NGC 7078). An average seeing of 0".15 FWHM, with the best-seeing image having 0".09, allowed us to measure accurately the velocities for five stars within 1" of the center of M15. Our estimate of the second moment of the velocity distribution (i.e., the dispersion, ignoring rotation) inside a radius of 2" is 11.5 km.s^–1, the same value we find out to a radius of about 6". However, the projected net rotation does increase dramatically at small radii, as our previous observations led us to suspect. The rotation amplitude inside a radius of 3".4 is v=10.4±2.7 km.s^–1 and the dispersion after removing the rotation is σ=10.3±1.4 km.s^–1, so v/σ≃1 in this region. In addition, the position angle of the projected rotation axis differs by 100° from that of the net cluster rotation at larger radii. Current theoretical models do not predict either this large an increase in the rotation amplitude or such a change in the position angle. However, a central mass concentration, such as a black hole, could possibly sustain such a configuration. The rotation increase is consistent with the existence of a central dark mass concentration equal to 2500 M_☉. The Strehl ratio is 1% in our worst images and 6% in our best. Despite these low values, the images allow us to resolve the brighter stars with an angular resolution close to the diffraction limit and to perform photometry on these stars accurate to a few percent. Thus, these adaptive optics observations provide us with crucial information on the central kinematics of M15.