Canada-France-Hawaii telescope adaptive optics observations of the centralkinematics in M15

We have used an Imaging Fabry-Perot Spectrophotometer with the Adaptive Opt ics Bonnette on the Canada-France-Hawaii Telescope to measure stellar radia l 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 d ispersion, 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 observ ations led us to suspect. The rotation amplitude inside a radius of 3 ".4 i s upsilon = 10.4 +/- 2.7 km s(-1) and the dispersion after removing the rot ation is sigma = 10.3 +/- 1.4 km s(-1), so upsilon/sigma similar or equal t o 1 in this region. In addition, the position angle of the projected rotati on axis differs by 100 degrees from that of the net cluster rotation at lar ger radii. Current theoretical models do not predict either this large an i ncrease in the rotation amplitude or such a change in the position angle. H owever, 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 Streh l ratio is 1% in our worst images and 6% in our best. Despite these low val ues, the images allow us to resolve the brighter stars with an angular reso lution close to the diffraction limit and to perform photometry on these st ars accurate to a few percent. Thus, these adaptive optics observations pro vide us with crucial information on the central kinematics of M15.