Jenny E. Greene Princeton University
"Local Galaxies with Radiating Black Holes"

The evolution of supermassive black holes and galaxies are apparently inextricably
linked, and we might hope to gain unique insight into the nature of their connection
by studying galaxies with currently accreting black holes. The study of active host
galaxies has a long history; I focus here on three innovative experiments that exploit
both the recent availability of large spectroscopic surveys such as the SDSS as well
as improved techniques to estimate black hole masses in active galactic nuclei (AGNs).
The first uses HI observations of local AGNs to measure their circular velocities and
disturbance levels. The second focuses on luminous narrow-line AGNs, where we have
a direct view of the host galaxy, to look for direct evidence of large-scale outflows,
possibly driven by the nuclear activity. Finally, I examine the host galaxies of AGNs
selected to have the lowest known black hole masses known, a regime in which the
correlations between black holes and bulges must begin to break down. I discuss
the implications for AGN feedback, and the possibility of observing continuing
evolution in the relations between black hole mass and bulge properties at the
present epoch.

Feb. 26th

Special Colloquium (visit: Feb. 26-27)

Yoram Lithwick Canadian Institute for Theoretical Astrophysics (CITA)
"Dynamics of Protoplanetary Disks: Vortices and Turbulence"

Protoplanetary disks are gaseous accretion disks around young stars. I will show
how, in hydrodynamical accretion disks such as these, vortices form out of a nonlinear
instability. I will also show that a vortex's ultimate fate in 3D depends on whether
it is weak or strong. Weak vortices live essentially forever. Strong vortices decay into
turbulence via a 3D instability. One interesting implication is that in protoplanetary
disks dust can be trapped by weak vortices, triggering planet formation. A second
implication is that strong vortices can be responsible for the turbulence that makes
these accretion disks accrete.

Special Colloquium (visit: Feb. 28-29)

Sarah E. Robinson University of California / Lick Observatory
"Chemistry of Giant Planet Formation: Future Directions in Theory
and Observations"

What role do ices play in giant planet formation? New chemical models of the solar
nebula show that in addition to water ice, Saturn's feeding zone contains solid ammonia,
methane, and hydrogen cyanide. These simulations cann account for both Saturn's large
core (<= 22 Earth masses) and its formation at a large distance from the sun, where
solid core growth is slow. Organic ices incorporated into planetesimals help boost Saturn's
core mass and growth rate so that the planet forms in only 3.4 Myr, similar to the observed
median protostellar disk lifetime.

Models of planet formation in ice-rich regions can be extended to other planets with heavy
cores such as HD 149026 b, Neptune and Uranus. Core accretion simulations based on a
a disk with twice solar metallicity allow HD 149026 b to form in only 1.6 Myr, leaving ample
time for migration into the current short-period, transiting configuration.

Special Event: Beatrice M. Tinsley Visiting Scholar in Astronomy (visit: Apr. 6-18)

Philip F. Hopkins Harvard-Smithsonian Center for Astrophysics
"Quasars and Galaxy Mergers: Fueling, Feedback, and Evolution"

Most models of galaxy formation now invoke (or even require) some form of feedback
and interplay between supermassive black holes and galactic gas, and observations of
quasars increasingly probe their host galaxy properties and fueling mechanisms. But we
know disturbingly little about the details and implications of the 'overlap' between these
areas. I'll discuss work we've done to explore evolutionary models for starbursts, quasars,
and speroidal galaxies in which supermassive black holes play a dominant role. In this
picture, mergers between gas-rich galaxies drive nuclear inflows of gas, producing intense
starbursts and feeding the growth of supermassive black holes. During this phase, the
black hole is heavily obscured, but feedback energy from its growth expels the gas,
rendering the black hole briefly visible as a bright, optical source, and eventually halting
accretion. This class of models provides a natural explanation for correlations between
black hole bass and host galaxy properties, but there arise a number of other interesting,
and in some ways unexpected implications for the nature of quasar lifetimes and lifecurves,
the impact of quasar feedback on the host galaxy, and the interpretation of the quasar
luminosity function. Moreover, this is almost certainly no the only way to make an AGN:
I'll discuss alternative models of quasar fueling, where and when they are expected to
be important, and how observers might be able to tell the difference.

Fred K. Y. Lo Director, National Radio Astronomy Observatory (NRAO)  
"Mega-masers, Dark Energy and the Hubble Constant"

Powerful water maser emission (water mega-masers) can be found in accretion disks in the nuclei
of some galaxies. Besides providing a measure of the mass at the nucleus, such mega-masers can
be used to determine the angular diameter distance to the host galaxy, based on a simple model. We
will explain the importance of determining the Hubble Constant to a high accuracy for constraining the
equation of state of Dark Energy and describe the Mega-maser Cosmology Project that has the goal
of determining the Hubble Constant to ~3%. We will also present the scientific capabilities of the
current and future NRAO facilities: ALMA, EVLA, VLBA and GBT, for addressing key astrophysical
problems.

Special Event: Beatrice M. Tinsley Visiting Scholar in Astronomy (visit: May 14-31)

Rene Goosmann Astronomical Institute, Acadamy of Sciences, Czech Republic
"Using Polarization to Probe Unresolved Structure of AGNs and Other Objects"

The structure of many astrophysical objects (AGNs, supernovae, X-ray binaries, and
gamma-ray bursts) cannot be directly resolved yet. I discuss various mechanisms by
which scattered line and continuum radiation is polarized, and show how polarization
measurements allow profound insights to be gained into the geometrical structure and
the dynamics of AGNs and other objects. Using the Monte Carlo radiative transfer code
STOKES, the polarization signatures of various reprocessing regions around compact
objects can be modeled. The radiative coupling between individual scattering regions
can be complex but is correctle modeled with STOKES because it automatically includes
multiple scattering effects. Recently we introduced the new technique of polarization
reverberation mapping. This method exploits the time-dependence of the polarization
signal and allows us to measure distances between radiation sources and polarizing
mirrors.