[Normal Galaxies, Clusters of Galaxies -- Oral ]
Chandra and SZA Observations of Clusters of Galaxies at z>1
Thomas Culverhouse, University of Chicago
Stefano Andreon (OAB Milano), Esra Bulbul (UA Huntsville), Max Bonamente (UA Huntsville), Marshall Joy (NASA Marshall Space Flight Center), John Carlstrom (University of Chicago), Nicole Hasler (UA Huntsville), David Hawkins (Caltech Owens Valley Radio Observatory), Ryan Hennessy (University of Chicago), James Lamb (Caltech Owens Valley Radio Observatory), Erik Leitch (University of Chicago), Daniel Marrone (University of Chicago), Ben Maughan (University of Bristol), Amber Miller (Columbia University), Tony Mroczkowski (University of Penn), Stephen Muchovej (Caltech), Clem Pryke (University of Chicago), Matthew Sharp (University of Chicago), Adam Stanford (UC Davis), David Woody (Caltech Owens Valley Radio Observatory)
I will present Chandra X-ray and Sunyaev-Zeldovich Array (SZA)
observations of a sample of galaxy clusters at high redshift (z>1). This
regime remains relatively unexplored and yet holds the potential to
tightly constrain cosmological models, provided the properties of the
clusterpopulation can be well calibrated. X-ray and Sunyaev-Zeldovich effect
(SZE) measurements offer powerful and complementary probes of the hot
gas in galaxy clusters; X-ray observations with Chandra allow detailed
imaging and spectroscopy, while the SZE enables study of the gas out to
larger radii on account of the weaker dependence of signal on gas
density. Given the redshift independence of the SZE signal, the SZE is
ideal for observing distant clusters.Using data from the SZA, a radio interferometer designed to image the
SZE in galaxy clusters, constraints will be presented on the integrated
Compton-y parameter, a measure of the total thermal energy in clusters.
These new SZA measurements have produced high significance images of the
SZE in several z>1 systems, including a cluster at z=1.39, the most
distant system for which an SZE has been observed.Mass measurements calculated from Chandra observations, in conjunction
with the SZA data, are used to compare the properties of our high
redshift sample to scaling relations derived at lower redshift, to test
for evidence of evolution.