1. Observational Evidence for Black Holes in Globular Clusters
Karl Gebhardt (UT Austin)

2. Results to Date from Dynamical Studies
M15 has been painful for many years
Gerssen et al claim a 2000 Msun BH from radial vels
Baumgardt et al say no evidence
McNamara et al say no evidence from proper motions G1
Gebhardt, Rich, & Ho claim 2e4 Msun BH
NGC 6752
Drukkier et al claim large M/L increase from pm’s
Xie et al claim little M/L increase from radial vels
Colpi et al use pulsars to argue for something massive

3. Current BH/sigma correlation using published results

4. Comparing M15 radial velocities with proper motions (McNamara et al), using distance as measured from Kraft and Ivans 2003 (11.2 kpc)

5. Comparison with Baumgardt et al dispersion profile, including a BH of 1700 Msun.

6. Models with adding a BH to Baumgardt profile
for the 100% and 0% ns population

9. Rotation in Galactic clusters

10. Central Rotation in Galactic clusters

16. Central Surface Brightness Profiles

18. BH/sigma correlation using isotropic models

19. Conclusions
M15 and G1 still have black holes as the best fitting model
central light profiles for clusters show a range of slopes
rotation in clusters is important to consider
many clusters show a statistically significant increase in the central rotation, which has a PA that is not correlated with that of the main body rotation