Black Holes and the Fundamental Correlations

1. Black Holes and the Fundamental Correlations Karl Gebhardt (UT Austin, MPE/USM)

2. HST and Black Holes The superior spatial resolution of HST revolutionized our understanding of black holes. The next step is to understand the effect of black holes on galaxy formation.

3. Evidence for significant influence: • Tight correlations (sigma, mass, light, n, etc.) • BH growth tracks galaxy growth • First stars are likely very massive and produce massive BH • AGN jets clearly have global impact on host If you want to understand how galaxies evolve (and possibly form), you need to understand growth of black holes. How do we figure out what is going on: • establish observational correlations (and scatter) • find most massive BHs; connected to mergers • find seeds (globular clusters?) • watch BH and bulge grow (AGN) • evolutionary observations (hardest, doable with quasars)

4. Measuring Black Hole Mass • Stellar dynamics: can always apply, reliable techniques • Gas dynamics: limited use, concerns about uniqueness • Proper motions: ideal but limited to nearby objects Gemini/GMOS observations of black hole in NGC4472 Measure the velocity, dispersion, higher moments and run dynamical models IFU over a galaxy

5. Stellar Dynamical Models: • Define potential • Integrate orbits that cover available phase-space • Determine orbital weights that best match kinematics • Change potential and determine best fit • These models are now very well-tested, and appear to be quite reliable Orbit models for the 2D kinematic data for N4472 provide a well measured BH

6. Current BH/sigma correlation using published results Black hole appears to correlate with sigma, total mass, light, concentration, etc

7. Theoretical Models for BH correlations Silk & Rees 98 Ostriker 00 Haehnelt & Kauffman 00 Nulsen & Fabian 00 Blandford 99 Adams et al 01, 03 Burkert & Silk 01 Balberg & Shapiro 02 Sellwood 02 MacMillian & Henrickson 02 Ciotti & van Albada 01 Colgate et al 03 King 03 Mathur & Grupe 04 Sirota et al 04 Granato et al 03 Tyler et al 03 Haehnelt 03 Ilvin et al 03 Merritt & Poon 03 Murray et al 04 Bromley et al 04 Springel et al 04 Sommerville et al 05 These differ by slope, normalization, and scatter

8. Theoretical Models fall into a few general camps: • BH feedback (winds, jets): e.g., Silk & Rees, Murray etal • Direct infall: e.g., Adams etal. • Galaxy instabilities: e.g., Sellwood Feedback models also explain galaxy color bi-modality! Large BHs tend to halt star formation (Springel, DiMatteo, Hernquist 04; Sommerville et al. 05; Hopkins et al. 06) • How to improve observational constraints: • slope: probably not that important (easy to adjust in models) • scatter: complicated by messy galaxy processes • extent: very important for most theoretical models • evolution: probably the most important (but the hardest); • look as a function of redshift (time) or, • look as a function of type (young vs. old)

9. The advent of NIR spectrographs with good spatial resolution opens up a new regime for BH studies. Data for CenA was taken with Gemini GNIRS (Silge and KG). NIR IFU behind AO will revolutionize this field.

10. 1D and 2D c2 distribution for Gemini GNIRS data on CenA (Silge et al 05), based on orbit-based models.

11. Adaptive Optics will take over from HST BH studies HST vs KECK/AO N4486A has a 9th mag star 2.5” from nucleus. Keck AO NIR spectroscopy worked extremely well. Nowak et al 06 has same data from VLT/SINFONI.

12. Black hole mass for N4486A is very well measured and lies right on BH/sigma correlation.

13. Need to explore the upper and lower ends! Greene, Barth, Ho make excellent case for 1e5 to 1e6 black holes based on SDSS low-lum AGN spectra (orange points). Next step is pushing to yet lower systems.

14. Results to Date from Globular Clusters • M15 has been painful since 1970s (back and forth for a BH) • G1: latest models support BH interpretation • omega Cen, 47Tuc, NGC6752 appear to be interesting cases

15. New data and models for G1 Flat core of G1 makes it hard to argue for remnants as cause for increase in M/L

16. omega Cen GMOS/IFU observations of the central region (Noyola and KG 06): advantage is that one can choose which light to include.

17. omega Cen dispersion profile from 4 different sources Constant M/L model in the core suggests a central mass of 5e4 (Noyola and KG 06)

18. Preliminary models for 47Tuc using proper motion and radial velocities (McLaughlin et al. 06). The models below have BH masses of 0, 500, 1000, and 2000 solar masses.

19. Central rotation seen in M15 in both proper motions and radial velocities (at the correct PA) from R. van den Bosch et al. 06. This is very hard to explain since 2-body interaction removes it very fast.

20. BH/sigma correlation with both galaxies andglobular clusters (using isotropic models)

21. Evolution of Black Hole Correlations • Spatially-resolved kinematics have limited applications. • Must use integrated light for both BH and host galaxy. • BH mass from Hbeta or MgII, sigma from narrow lines. Calibration is key. • Potentially apply to all QSOs, and get redshift evolution. • SDSS is an excellent database for this study. Offset of black hole mass relative to galaxy will determine which comes first. Shields, KG, Salviander et al. 03

22. Shields et al. (06) using BH masses with CO linewidths

23. About 40 nearby black holes with well measured masses; this will grow to about 100 soon. • We are starting to measure BH evolution. From the most recent studies, it appears that BHs grew first. Evidence is: • massive BHs exist at early times • deviation from BH/sigma at early times • Cen A has 8 times larger BH • theoretical models work well • Future for black studies is very promising. IFU in optical regions will open up studies in largest galaxies and in globular clusters. • IR IFUs behind AO will offer new regime in BH studies. We will be able to measure those galaxies that have significant dust and are actively accreting. Conclusions