JULY 7 - 11, 2008

MONDAY, JULY 7

11:00 am: High Energy Astrophysics Division Lunch Talk. "Formation Epochs and Morphologies of Massive Early-Type Galaxies in Cluster and Field Environments at z ~1: Insights from the Rest-Frame UV," Dr. Alessandro Rettura, Johns Hopkins University. Pratt Conference Room.

Abstract: I am presenting a study in which we derive stellar masses, ages and star formation histories of massive early-type galaxies in the z=1.237 RDCS1252.9-2927 cluster and compare them with those measured in a similarly mass-selected sample of field contemporaries drawn from the GOODS South Field. Additionally, I present new, deep U-band photometry of both fields, giving access to the critical FUV rest-frame, in order to constrain empirically the dependence on the environment of the most recent star formation processes. I also analyze the morphological properties of both samples to examine the dependence of their scaling relations on their mass and environment.

THURSDAY, JULY 10

12:30 pm: Optical and Infrared Astronomy Division Lunch Talk. "Possible Cluster Around 3C 270.1," Mr. Frank Heymann, ESO. Pratt Conference Room.

Abstract: We are studying the environment of the complete sample of 60 high-z 3CR sources at 3.6 to 24 microns with the Spitzer Space Telescope. Here we present first cluster signatures obtained for the z=1.5 quasar 3C270.1, when combining the Spitzer maps with ground-based optical/near-infrared images from the 6.5-m MMT and with the Chandra map. Properties of the high-z cluster galaxy candidates and implications for the cluster formation are discussed.

4:00 pm: Summer Colloquium Series. "How to Find a Habitable Exoplanet," Dr. David Charbonneau, CfA. Preceded by refreshments at 3:30 pm. Phillips Auditorium.

Abstract: This tutorial will provide an introduction to the two most successful methods for detecting planets orbiting nearby Sun-like stars. I will review the radial velocity method and the transit technique, focusing on how one deduces the physical parameters of exoplanets from the time-dependent changes in the observable quantities of the star. I will then discuss current techniques for studying the chemistries and dynamics of exoplanet atmospheres. There is great excitement within the exoplanet community over the idea that refinements in the aforementioned methods will soon permit the detection of habitable planets and the spectroscopic study of their atmospheres. I will explain why that excitement is wholly justified.

SAO HUMAN RESOURCES NOTES

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