// Enter speaker information here. The format is:
//
// ["Date","Name","Affiliation","Title","Abstract","Day","Time"]
//
// In the Abstract field you must escape double quotes (\"). Some HTML
// is possible (like <br>, <b>, etc.).
//
// ** Edited to add color change for special day/time.
// ** If Day or Time field is not empty, special day/time
// ** is/are added in date column in red.
//
January[0]=["29","Paul Wiita","Georgia State University / IAS","High Lorentz Factors and Periodic Components of Variability in Blazars","There is a great deal of evidence that the defining characteristics of blazars, such as extreme variability across the electromagnetic spectrum and high fractional polarization, are produced by shocks in relativistic jets pointing close our line of sight.  Some different techniques that have been employed to estimate the Lorentz factors of these flows will be reviewed before a case for ultrarelativistic flows being present in the subset of blazars known to emit TeV radiation is presented.  We have recently found good evidence for transient periodic components of tens of minutes in the optical emission from S5 0716+714 as well as periodic components in x-ray emission of ~17 days for  AO 0235+164 and of ~420 days for 1ES 2321+419.  The most likely origins of such variability components will be suggested.","",""];

February[0]=["5","Kambiz Fathi","Stockholm Observatory","Two-dimensional ionized gas kinematics in spiral galaxies","","",""];
February[1]=["12","Re'em Sari","Caltech","Updates on Hydrodynamic Self Similar Solutions","","",""];
February[2]=["19","","","","","",""];
February[3]=["26","","","","","",""];

March[0]=["5","David Hogg","NYU","What if the Milky Way isn't integrable and isn't phase-mixed?","","",""];
March[1]=["12","Brice Menard and Masataka Fukugita","CITA, U. of Tokyo","How much dust is there in the universe?","","",""];
March[2]=["19","Nadia Zakamska","IAS","1. Introduction to IR space astronomy: past and future missions. / 2. Molecular hydrogen in infrared galaxies","","",""];
March[3]=["26","Mordecai-Mark Mac Low","AMNH","Planetesimal Formation and Migration","In protostellar accretion disks, magnetorotational turbulence not only transports angular momentum, allowing accretion, but it also strongly influences planet formation.  I will consider the influence of turbulence on the formation of planetesimals from boulders, showing that in its presence streaming instabilities can cause direct gravitational collapse of boulders to objects with the mass of dwarf planets, overcoming the meter-size barrier. I will then show that magnetorotational turbulence also forms density enhancements with mass large enough to cause random walk migration of planetesimals, but that dead zones sufficiently neutral to prevent turbulence reduce this effect, without eliminating it. I then consider whether turbulent density fluctuations can pump the ellipticity or inclination of planetesimal orbits.  Preliminary results suggest that they cannot do so sufficiently to explain the observed range of orbits in planetary systems, supporting the idea that dynamical interactions after loss of the gas disk are primarily responsible.  However, the resulting diffusion of planetesimals outward as well as inward may preserve a significant population from Type I migration into the central star.","",""];

April[0]=["2","Eric Gaidos","U. of Hawaii","The ARCHIPELAGO search for planets","Four centuries ago the son of an Italian lutenist constructed the telescopes with which he would observe the Solar System and forever alter humanity's perception of its place in the Cosmos. Today, that perspective continues to change with the discovery of numerous planets around other Sun-like stars, primarily using the Doppler radial velocity and transit methods. There are numerous surveys to find more planets and I will describe one - ARCHIPELAGO - which is searching the nearest, low mass stars for planets with masses intermediate that of Earth and Neptune. We are screening a new catalog of more than 10,000 late K and early M star candidates within 50 parsecs to verify main sequence status, determine spectral type, estimate heavy element abundance, and assay chromosphere emission. We will identify planet-hosting stars using a multi-stage, hybrid RV-transit scheme that is designed to efficiently detect planets whose mass and radius can both be measured. Among these planets may be some that are very unlike the members of our Solar System. One hypothetical class of planet is composed principally of water, i.e., high-pressure phases of ice underlying a steam atmosphere or liquid ocean. Another will be composed almost entirely of iron; a third may have a mantle of carbides rather than silicates. None may be suitable for life as we know it; all will test theories of planet formation and inform conjecture about the frequency of Earth-like planets and life in the Cosmos.","",""];
April[1]=["9","Freeman Dyson","IAS","Can a single graviton be observed?","","","Location Change: BH Lecture Hall"];
April[2]=["16","Andrew Youdin","CITA","The Early Stages of Planet Formation", "The fast-paced discovery of extrasolar planets has heightened interest in the mechanisms by which planets form. The early stages of planet formation -- growth from dust grains to \"planetesimals\" larger than a kilometer -- is a long-standing problem which sets the stage for subsequent growth phases. Simple growth by collisional sticking stalls as collisions become more violent with increasing particle size. The gravitational collapse of many small solids into a larger planetesimal is a promising mechanism. However stirring of particles by turbulent gas opposes this collapse, and led to the abandonment of the hypothesis. I will describe recent dynamical work which is resurrecting the collapse mechanism for planetesimal formation. A key point is that turbulence not only stirs particles but creates transient clumps, which can act as seeds for gravitational collapse. The streaming instability provides a robust mechanism for drag forces to promote particle clumping (Youdin & Goodman, 2005; Youdin & Johansen, Johansen & Youdin 2007). Simulations by Johansen et al. (2007, Nature) confirm the viability of the collapse hypothesis when initial particle sizes are above tens of centimeters. I will describe ongoing analytic work on gravitational collapse which can be extrapolated across parameter space, including toward smaller particle sizes. A surprising and robust conclusion is that planetesimals can form with initial sizes significantly larger than the canonical value of a few km. I will describe implications both for the detailed properties of our Solar System, and for the formation of planets and exoplanets in general.","",""];
April[3]=["23","Nadia Zakamska","IAS","Molecular hydrogen in ULIRGs","","",""];
April[4]=["30","Bence Kocsis","IAS","Future gravity wave experiments","","",""];

May[0]=["7","Eric Ford","University of Florida","Multi-planet extrasolar planetary systems","","",""];
May[1]=["14","Chi-kwan Chan","CfA/ITC","What do the Spectra Mean in MHD Turbulence?","Magnetohydrodynamic (MHD) turbulence is responsible for many important astrophysics problems.  For example, in the Sun, small scale magnetic fields can self-organize and generate large scale fields; in accreting disks, magnetorotational instability (MRI)-driven turbulence can transport angular momentum outward.  Both of these phenomena can be described in terms of statistical properties of MHD turbulence.  Although one-dimensional energy and helicity spectra are often shown, they could be misleading due to the anisotropic cascade in MHD turbulence.  In this talk, I will first give a brief review of statistical theory of turbulence, which motivates the development a spectral MHD code.  I will discuss some difficulty of applying spectral schemes to shearing systems, and derive a resolution.  I will then propose a few analysis techniques to address the anisotropic cascade, and apply these techniques to study the turbulent solutions from the code.","",""];
May[2]=["21","Zheng Zheng","IAS","Dance of Lyman-alpha Photons -- Modeling Lyman Alpha Emitters Around the End of Reionization","Lyman Alpha Emitters (LAEs) are becoming an important probe of the reionization of the universe. To correctly interpret the observations of LAEs, the effect of resonant scattering of Lyman-alpha photons has to be accounted for.  I will present results from a theoretical study of z>~ 5.7 LAEs, which combines a state-of-the-art cosmological reionization simulations (Trac, Cen, & Loeb 2008) and a Monte Carlo Lyman-alpha radiative transfer code.  The detailed radiative transfer calculation of Lyman-alpha photons shows that the spatial and frequency diffusions of Lyman-alpha photons are important in determining the observability of high-z LAEs and predicts new features in the clustering of LAEs that are observable in future surveys. Based on these results, I will discuss implications in using LAEs for cosmology study.","",""];
May[3]=["26","Jihad Touma","American University Beirut","Self-Organizing Black Hole Nuclei","","Note date change",""];

September[0]=["17","Alexia Schulz","IAS","Refining photometric redshift distributions with cross-correlation","The weak gravitational lensing of source galaxies divided into several redshift slices (tomography) is known to be a powerful cosmological probe that can be used to study the three dimensional distribution of dark matter, the nature of dark energy, potential modifications to General Relativity, and the formation of large scale structure. Key to the programme is the ability to accurately determine the mean redshift and distribution for the source galaxies in each redshift slice.  For photometric galaxy surveys this can be accomplished by calibrating the photometry with a spectroscopic follow-up survey.  However, for very large and deep surveys such as LSST, SNAP and others, obtaining spectra for a fair sub-sample of the data could be cumbersome and expensive. Fortunately, a promising alternative has been proposed; the redshift distribution of photometric galaxies can be determined from cross-correlating them with any overlapping spectroscopic survey whose members trace the same density field.  In my talk I will discuss the applications of weak gravitational lensing tomography.  I will outline the impact of properly calibrating photometric surveys and review the proposed cross-correlation method. I will explain briefly how the method works, highlighting its strengths and discussing potential drawbacks.  I will present the results of using the halo model with N-Body CDM simulations to create mock galaxy catalogs that quantify the properties of this redshift distribution estimator.","",""];

September[1]=["24","Risa Wechsler","Stanford","Connecting Galaxies, Halos, and Star Formation Rates Across Cosmic Time","Recent observational and theoretical studies indicate that galaxy luminosities and stellar masses are tightly correlated with the masses of their dark matter halo hosts. This allows one to infer the connection between galaxies and their associated dark matter halos and provides a powerful approach to understanding galaxy clustering and other statistics of the galaxy distribution.  Based on this connection, I will present a model for understanding how halo masses, galaxy stellar masses, and star formation rates are related, and how these relations evolve with time. I will highlight current uncertainties as well as implications for galaxy formation, including for galaxies at the lowest and highest masses.","",""];


October[0]=["1","Stephen Adler","IAS","Modeling the Flyby Anomalies with Dark Matter Scattering","We continue our exploration of whether the flyby anomalies can be explained by scattering of spacecraft nucleons from dark matter gravitationally bound to the earth. We formulate and analyze a simple model in which inelastic and elastic scatterers populate shells generated by the precession of circular orbits with normals tilted with respect to the earth's axis. Good fits to the data published by Anderson et al. are obtained.","",""];

October[1]=["8","Tobias Heinemann","IAS","The Dynamics of Spiral Density Waves in Turbulent Accretion Disks","Abstract","",""];

October[2]=["19","Boaz Katz","Weizmann Institute","'Fast Radiation Mediated Shocks and SNe Shock Breakouts","Abstract","Note date change",""];

October[3]=["22","Molly Peeples","Ohio State","Balancing Outflows and Gas Dilution: The Mass-Metallicity Relation at z=0","The gas-phase oxygen abundances of star-forming galaxies are tightly correlated with the galaxies' stellar masses such that more massive galaxies are more oxygen-rich.  Because oxygen is produced on relatively short timescales (~10 Myr), this so-called mass-metallicity relation is a sequence of oxygen depletion: low-mass galaxies are metal-depleted relative to the true nucleosynthetic yield rather than massive galaxies being preferentially enriched.  Preferential metal-depletion can be caused by either diluting the gas (e.g., via higher accretion rates of pristine gas or by lower star-formation efficiencies) or by preferentially removing metals from low-mass galaxies via galaxy winds. I will use simple analytic arguments to show how the observed mass-metallicity relation implies the required balance between gas dilution and gas outflow.  In order to reproduce the mass-metallicity relation in cosmological smoothed particle hydrodynamic (SPH) simulations, star formation feedback is required.  The resolution of such simulations, however, demands that this feedback is not directly modeled; I will discuss how I am examining and clarifying the issues surrounding different SPH galaxy wind implementations.","",""];

October[4]=["29","Claude-Andre Faucher-Giguere","ITC, Harvard","Ly-alpha Emission from Galaxy Formation","Astronomers have exquisite observations of both galaxies (by directly imaging their stars) and of the intergalactic medium (in absorption spectra of background sources). While we know that the galactic baryons must have been accreted from the IGM, we currently have virtually no direct observations of the galaxy assembly process itself. Contrary to the classical picture of galaxy formation in which the accreting gas is shock-heated to the virial temperature of the halo before cooling, recent simulations show that most of the gas is instead accreted in cold streams, with temperatures T~10^4-10^5 K. At these temperatures, the accretion streams will radiate primarily in the Ly-alpha line and may be accessible to current observations. I will present new results combining cosmological hydrodynamical simulations with detailed Ly-alpha radiative transfer, including the expected Ly-alpha luminosities, spectra, and morphologies of the accretion streams. I will discuss whether these streams may have already been detected in the form of extended 'Ly-alpha blobs'.","",""];


November[0]=["5","","","","","",""];

November[1]=["12","Mark Hertzberg","MIT","Approaches to Understanding Inflation: Theory, Experiment, and Observation","Although the observational evidence for cosmological inflation is growing, the physical mechanism behind it is still unknown. In part this is because inflation probably occurred at energy scales many orders of magnitude higher than that at man-made or astrophysical particle accelerators. So how can we learn about inflation? How does it constrain microphysical theory? One approach to answering these questions is primarily theoretical: embedding inflation in fundamental theories of quantum gravity, such as string theory. Another approach is primarily experimental: finding correlations between cosmological parameters and experimental observables, such as the Higgs boson at colliders. And another approach is primarily observational: looking for signatures left by light fields that existed during inflation, such as isocurvature fluctuations from the QCD-axion. In this talk I discuss work on all three of these approaches.","",""];

November[2]=["19","Guido D'Amico","SISSA","The Effective Theory of Quintessence and Its Observational Signatures","I will study generic single-field dark energy models, by a parametrization of the most general theory of their perturbations around a given background, including higher derivative terms. In appropriate limits this approach reproduces standard quintessence, k-essence and ghost condensation. There are no general pathologies associated to an equation of state w_Q < -1 or in crossing the phantom divide w_Q = -1. Stability requires that, when w_Q < -1, dark energy behaves, on cosmological scales, as a fluid with a virtually zero speed of sound. Theoretical and stability constraints are summarized on the quintessential plane (1+w_Q) vs. speed of sound squared. Finally, I will discuss the effect of dark energy with a zero speed of sound on non-linear scales, by calculating the cluster mass function.","",""];

November[3]=["26","NO TALK","Thanksgiving","","","",""];


December[0]=["3","Andrew Wetzel","Berkeley","Satellite Galaxies in LCDM: Orbits, Merging & Disruption","Dark matter halos that merge with larger halos persist as subhalos, which host satellite galaxies.  While subhalos are rapidly stripped of their dark mass, the compact luminous material remains intact for some time.  I use a high-resolution, cosmological N-body simulation to explore satellite galaxy merging and tidal disruption.  Using abundance matching to assign stellar mass to subhalos, I compare with observed satellite fractions, galaxy clustering, and cluster luminosity functions. Satellite subhalos must be well-resolved down to ~1% of their mass at infall, and many satellites experience tidal disruption prior to merging with the central galaxy.  I also explore a simple analytic model based on dynamical friction for satellite infall.  Finally, I examine the orbital distribution of infalling satellites and its evolution with halo mass and redshift.","",""];

December[1]=["10","Daisuke Nagai","Yale","Cosmology and Astrophysics with Galaxy Clusters","Clusters of galaxies are unique and powerful probes of cosmology and astrophysics, promising to provide new insights into the nature of dark energy and dark matter to the physics of galaxy formation. The study of galaxy clusters combines the richness of plasma physics with the predictive power of modern cosmological models to explain remarkable new observational results. In this talk, I will describe recent advances in theoretical and intensive numerical modeling of galaxy cluster formation to interpret recent X-ray and Sunyaev-Zel'dovich Effect cluster surveys. I will then discuss outstanding issues and future directions in this area.","",""];

December[2]=["17","","","","","",""];