// Enter speaker information here. The format is:
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// ["Date","Name","Affiliation","Title","Abstract","Day","Time"]
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// is possible (like <br>, <b>, etc.).
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// ** 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.
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// Note: the format is as follows:
//September[0] =["20" ,"Name","Institution","Title","Abstract","",""];

September[0] = ["19","Jeremy Tinker","NYU","The Galaxy-Halo Connection and the Evolution of the Red Sequence","I will review recent advances in the modeling of galaxy bias in the context of galaxy evolution. The connection between galaxies and dark matter halos contains significant information for understanding how galaxies form and evolve. I will focus on the red sequence, using the halo model to constrain the relative importance of different physical mechanisms for quenching star formation and placing galaxies on the red sequence. I will use a combination of SDSS and COSMOS data to show how these mechanisms have evolved over the redshift baseline z=1 to 0.","",""];
September[1] = ["26","Yacine Ali-Haimoud","IAS","21cm fluctuations during the dark ages accounting for the relative velocity of baryons and cdm","Observations of high-redshift 21cm brightness temperature fluctuations are challenging but can potentially provide unprecedented information about the early universe. In particular, they are the only direct probe of large-scale structure during the cosmic dark ages, which follow the last scattering of CMB photons and precede the formation of the first luminous objects. During that epoch, the growth of overdensities is very well described by linear perturbation theory and the power spectrum of 21cm fluctuations can in principle be predicted exactly. Recently, Tseliakhovich & Hirata unveiled a previously overlooked physical effect: the suppression of small-scale density fluctuations due to the large relative velocities between baryons and the cold dark matter after recombination. In this talk I will show that this effect impacts the 21cm power spectrum, not only on small-scales but also on large scales due to fluctuations of the relative velocity field on  100 Mpc scales.","",""];
October[0]   = ["3" ,"Nikku Madhusudhan","Yale","Characterization of Exoplanetary Atmospheres and Interiors","","",""];
October[1]   = ["10","Matt McQuinn","UC Berkeley","The sad story of the cosmic EUV background","After reionization, a largely uniform ~1 Rydberg background pervaded the Universe, keeping the intergalactic hydrogen extremely ionized.  The characteristics of this background depend on the properties of the sources (quasars and galaxies) and the absorbers (Lyman-limit systems).   Modeling the sources is difficult, but I will argue that the absorbers   are likely captured in cosmological simulations, at least at high   redshifts.  Quick evolution (in a time < 0.1 H(z)^-1) in the ionizing   background is observed at z=6, which has (controversially) been   interpreted as indicating the end of reionization.  I will explain why   this evolution must owe to the absorbers and discuss how such quick   evolution could arise.  The only direct probe of the metagalactic   ionizing background comes from comparing the hydrogen Lyman-alpha forest   to the HeII Lyman-alpha forest in the same sightline.  Previous attempts   to measure background fluctuations from this comparison found   order-of-magnitude fluctuations on 1-10 Mpc scales, in conflict with   theoretical expectations.  I will show that these previous analyses were   flawed, and that the data is in fact consistent with the expectation of   an almost uniform background.  This comparison also allows us to infer   the hardness of the EUV background (constraining the quasar versus   stellar contribution) and allows us to constrain quasar lifetimes (via   the transverse proximity effect).  Unfortunately, all does not end well   for the cosmic EUV. ","",""]; October[2]   = ["17","No speaker", "Dark Matter Workshop","","","",""];
October[3]   = ["24","Kohta Murase","IAS","Unveiling the Origin of High-Energy Neutrinos Observed by IceCube","In 2012, the IceCube collaboration reported two PeV neutrino events. Then, 26 more events were found in a follow-up analysis.  Although more statistics are needed to have conclusive evidence, they are likely to include extraterrestrial signals.  In this talk, I will try to demystify the origin of this IceCube excess. The current data suggest that high-energy neutrinos are produced inside astrophysical sources, while it is difficult to explain it with cosmogenic  neutrinos.  I will also demonstrate the power of the multi-messenger approach.  It will be shown that present gamma-ray limits support  extragalactic scenarios and further observations can test Galactic neutrino sources.  Any viable astrophysical scenario relies on pp or pgamma interaction as a neutrino production mechanism, and discriminating them is also relevant to reveal the sources. In particular, pp scenarios can be tested with multi-messenger data in the next several years.  I will discuss future prospects including implications of some specific pgamma scenarios.","",""];
October[4]   = ["31","Brian Lacki","IAS","All Radiation Backgrounds from Star-Forming Galaxies: A Preview","I describe my preliminary results in calculating the extragalactic backgrounds from star-forming galaxies at all energies.  First, I construct very simple models of galaxies using relations like the Schmidt law.  This lets me estimate quantities including the galactic size, gas mass, and metallicity using just the star-formation rate, star-formation mode (normal vs. starburst), and redshift as input.  Then I can use a simple one-zone model of radiative transfer and Starburst99 synthesized spectra to calculate the ultraviolet to infrared spectra of galaxies.  I also calculate the nonthermal emission, including radio and gamma rays, from these galaxies with one-zone models of cosmic ray populations. Finally, I put it all together and calculate the extragalactic background as well as the source counts at different wavelengths.  I discuss the implications of these results. How much of the gamma-ray background do star-forming galaxies make up?  (About half.)  Are previous predictions for microJy radio source counts correct? (Yes.)  And can star-forming galaxies make up the mysterious ARCADE GHz radio background? (No.)","",""];
November[0]  = ["7" ,"Tim Brandt","IAS","A Census of Distant, Giant Exoplanets","I will present an analysis of the SEEDS direct imaging survey for young, self-luminous exoplanets at large separations from their host stars.  I will discuss the survey design and sensitivity, image processing, the selection of imaging targets, and estimates of their ages.  By using several new algorithms, removing the current aggressive Lyot stop, and making small changes to the read-out mode, the SEEDS instrument will gain a factor of ~3-10 in sensitivity. Finally, I will use combine current SEEDS data with imaging from other surveys to suggest that the ~20 currently imaged planet candidates represent the low-mass tail of a substellar population formed by gravitational collapse, rather than the high-mass tail of a population formed by gas accretion onto a rocky core, like the gas giants in our Solar system.  As such, most imaged companions should perhaps not be called massive planets, but rather low-mass brown dwarfs.","",""];
November[1]  = ["14","Surjeet Rajendran","Stanford","Gravitational Wave Detection with Atom Interferometry.","","",""];
November[2]  = ["21","Aaron Parsons","UCB","Building HERA from PAPERclips and Supercomputers","The Precision Array to Probe the Epoch of Reionization (PAPER) is one of several intensity mapping experiments aiming to use redshifted 21cm emission to study our early universe.  PAPER is deployed in South Africa, and combines inexpensive paperclip antennas with signal-processing supercomputers.  In a major breakthrough for the field, we have managed to remove the bulk of our foregrounds, and are now achieving upper limits that constrain the heating and ionization of the intergalactic medium by the first luminous objects.  Building on these successes, the US community is coalescing around a next-generation experiment for exploring cosmic reionization via 21cm emission.  The Hydrogen Epoch of Reionization Array (HERA) is envisioned to be a large array of zenith-pointing parabolic dishes optimized for power spectral measurements.  HERAs considerable collecting area enables it to precisely measure ionization fraction versus redshift, directly imaging larger ionization bubbles, and probe heating in pre-reionization epochs.  HERA is being proposed to the NSF's MSIP program, and if funded, would begin construction in Sept. 2014. ","",""]; 
November[3]  = ["28 (Thanksgiving)","","","","","No Seminar",""];
December[0]  = ["5" ,"Sarbani Basu","Yale","How Asteroseismology is Changing Stellar Astrophysics","","",""];
December[1]  = ["12","Duncan Hanson","McGill","Detection of lensing B-modes in CMB Polarization","","",""];