[...ULX session...]

=== Zoltan Haiman - Identifying Decaying Supermassive Black Hole Binaries from their Variable Electromagnetic Emission ===

- Gas/binary evolution
	- Gas cools, settles into circumbinary disk
	- Disk becomes alignes, torques evacuate central cavity
	- Orbit decays, gas follows
	- GW-driven coalescence leaves punctured disk
	- Outer disk falls in with decay
- Counterparts
	- Disk reacts with flare to changing potential (gravitational recoil, mass loss) -> months after merger
	- Gas may fall into BHs before merger -> before and during coalescence
	- Emission is likely variable
- Gravitational recoil
	- Changing disk orbits due to kick in plane result in spiral caustic
	- With perpendicular kick, concentric density enhancements
	- Perhaps 1e-2 L_edd, will harden with time (unlike GRB afterglows)
	- Shaking of disk may also launch sound waves
- Detect decaying binaries as periodically variable quasars

=== Bence Kocsis - Electromagnetic counterparts of black hole mergers ===

- Standard sirens... what are the EM counterparts?
- GW-EM comparisons
	- Match sky coordinates
	- Compare masses to EM luminosity, learn Eddington ratio within %
	- Luminosity/redshifts
	- Spins/masses vs. spectra
	- Learn about theories of gravity: match frequencies
- emission mechanisms
	- circumbinary: periodic accretion
	- final inspiral phase
	- GW dissipation; mass loss -> shocks, GW kick -> shocks, accretion -> X rays
- locating counterparts with LISA
	- look for quasars in LISA error box

=== Simone Callegari - Coalescence of massive black holes in equal and unequal mass galaxy mergers with gas: ultra-high resolution simulations and prospects for LISA ===

- Gas dynamics can drive efficient MBH pairing down to <~ 100 pc scale in LISA-relevant objects

=== Kayhan Gultekin - The SMBH-IMBH Connection ===

=== Michael Bregman - Stars-accretion disk torqueing and applications for massive black hole evolution ===

=== Massimo Dotti - Massive black hole binaries in circumnuclear disks ===

=== Laura Blecha - Effects of Gravitational-Wave Recoil on the Dynamics and Growth of Supermassive Black Holes ===

- GW recoil: asymmetric GW emission, kick speed depends on mass ratio and spins
- phenomenon associated with IMBHs, since more mergers and easier ejections at high redshifts
- few observational constraints:
	- empty galaxies not seen locally
	- 30 offsets seen in AGN narrow lines (DEEP2), probably not recoils (how do you take gas along?)
	- no offsets seen in quasar spectra (SDSS)
	- Komossa et al. SDSS quasar with 2650 km/s offset
- simulations: after kick, accretion episodes, star formation, oscillation to large radii in potential wells
- some recoils suppressed by central gas component
- undermassive BHs may produce scatter/outliers in M_BH-sigma relation

=== Ryan O'Leary - Star Clusters Around Recoiled Black Holes in the Milky Way Halo ===

- even after BH kick, some stars in the nucleus should stay bound
- hierarchical formation of Milky Way led to ejection of 100 IMBHs
- look for such ensembles in SDSS: looks like a galaxy, but has star colors, larger than 3" to a few kpc

=== Alessia Gualandris - Perturbations of Intermediate-mass Black Holes on Stellar Orbits in the Galactic Center ===

- Galactic center: cusp -> disk -> S stars
- S stars, very close to black hole, where star formation is suppressed by shear; but very young, so migration processes must be very efficient
- relaxed, although no time to have done so
- models: in-situ formation, binary capture, cluster infall
- suppose young stars carried to galactic center carried by BH
- IMBH in eccentric orbit can help scatter out stars from initial plane (randomize them, transform eccentricity into thermal distribution)
- long-term interaction can lead to strong perturbations, tidal disruptions and ejections
- a number of constraints on the IMBH parameters; exclude > 2000 Msun and 3-10 mpc separations

=== Linda Strubbe - tidal disruption of stars in optical transients surveys ===

- from ROSAT and GALEX, 1e-5 yr-1 rate
- new optical surveys: Pan-Starrs to m = 23 every few months, LSST to 24.5 every few days
- disruption; bound material -> accretion disk; unbound material -> expanding wedge
- at opt. + IR, unbound material subtends large solid angle, reprocessing hot disk emission; adds significant luminosity, and has lines similar to broadline AGN emission (but no narrowline region)
- for lighter BH, unbound material dominates, allowing for IMBH detections
- Pan-STARRS a few IMBHs/yr, LSST 10s/yr

=== Alberto Sesana - White dwarf inspiralling onto (moderately) massive black holes ===