=== Milos Milosavljevic - Accretion onto Seed Black Holes in the First Galaxies ===

- IMBHs, missing link between stellar and massive black holes

- z ~ 8-15+ accreting seeds: M_BH = 100 Msun, M_halo = 10^8 Msun
- z ~ 6 quasars, M_halo = 10^12 Msun
- BHs need to grow at Eddington rate 50% of time

=== David Merritt - Dynamics of nuclear star clusters with black holes ===

- nuclei: excess in light w.r.t. what expected at center of galaxy (Sersic's law)
- low-luminosity spheroids (dwarf galaxies) display excesses, nucleus is unresolved
- nuclei hard to see in bright galaxies, although we think they have MBHs
- NCG 205: Hubble model for nucleus
- nuclear star clusters in 50-70% galaxies, sizes similar to GCs; mostly old population
- transition: nuclear star clusters in faint galaxies, MBH in bright ones, transition at M_B ~ -20
- coexistence shown in 11 NSC galaxies; hints that MBH have masses ~ NSC

--> no BH
- core collapse in NSC can be inhibited by outer density profile
- but some models show core collapse or expansion, depending on compactness of nucleus
- with no BHs, most nuclei in core-collapse region, except those with long relaxation times

--> with BH
- additional gravitational potential term; loss term in tidal disruption sphere
	- produce Bahcall-Wolf cusp in t_r (r^-7/4)
	- turn off core collapse
	- increase nucler temperature, reducing inflow of heat from galaxy
- so BHs stabilize nuclei

- observed:
	- nuclei with modest BHs expand more quickly than BH-free nuclei
	- rates of stellar tidal disruption decrease with time and are lower in lighter galaxies
	- small BHs limit core collapse

=== Anil Seth - Black Holes in Nearby Nuclear Star Clusters ===

- HST zoom into NGC4244
- HST can resolve NSCs to 30 Mpc
- complex morphology: in edge-on spirals, bluer disks/rings aligned with galaxy disk
- NSC masses correlated with galaxy masses and bulge velocity dispersions

- study nearest NSCs with Gemini/NIFS
- resolve nuclear cluster kinematics; find lots of rotation (M33, Milky Way, G1, M54)
- formation scenarios: sinking of GC by dynamical friction; formed in situ from gas; young clusters form in inner disk and sink

- NSCs are common, sometimes have BHs
- kinematics, populations, and morphology suggest regular gas accretion into galacy centers
- may host detectable IMBHs

=== Andrea Ghez - present and future adaptive optics studies of BHs at galactic center ===

- initial question: is there SMBH at center of Galaxy? Then:
	- properties, GR tests, dark matter
	- how do young stars come to reside there
- began with speckle imaging
- much better imaging and spectra with adaptive optics
- established lower limit on dark matter density 10^7 better than in pre-diffraction-limited era

- apparent relative motion due to reflex motion or reference-frame instability
- astrometric measurements are limited by source confusion
- will get more stars with future large telescopes, have shorter minimum observing times
- can look for extended mass distribution: stellar remnants and cold dark matter particles
- can measure general relativistic precession

- can get stellar ages from spectroscopy
- "paradox of youth" near BHs (at 0.5 pc, few-million-yr old population)
	- old stars masquerading as youths
	- formed at larger radii, fell in (IMBHs can help)
		- known clusters are not going toward center
	- young stars that formed in situ
		- evidence in stellar dynamics
		- evidence that our galaxy had accretion disk

- old stars: deficit in central 6"

=== Francisco Mueller-Sanchez - The nature of the nuclear black hole in the nearby starburst galaxy NGC253 ===

=== Anca Constantin - Challenges posed by M94, the least luminous AGN-like LINER ===

=== Jenny Greene - Demographics of Low-mass Black Holes at Galaxy Centers ===

=== Misty Bentz - Extending the low-mass end of AGN scaling relationships with reverberation mapping: The Lick AGN Monitoring Project ===

- hard to get black-hole masses in AGNs (too far, too bright)
- use reverberation mapping instead (width of broad emission lines, studied from its response to changes in the continuum)
- get AGN radius from its luminosity (Bentz et al. 2009); few objects and large scatter at low L, small R

=== Joan Wrobel - Local Analogs of the First Active Galactic Nuclei: GH 10 ===

(very nice banner in first slide)

- BH and galaxies coevolve because BHs energize AGNs, AGNs feed back into ISM
- what's the feedback like?
- GH10, broadline emission-line AGN at z ~ 0.08; 8e5 Msun BH, Lbol/Ledd = 2
- suggest outflow-driven radio emission, coronal mass ejection like radio-quiet AGNs

- Boroson & Lauer's BBH candidate: QSO SDSS J153636.22+044127.0
	- 2 broad-line emission systems
	- 2 BHs at z ~ 0.388
	- chance probability of superposition 0.0032
- Wrobel & Laor
	- two broad-line emission regions
	- if they're related they could be energized by 0.1-pc binary BH
	- if independent, energized by 5-kpc binary quasar system