NOAO >   Observing Info >   Approved Programs >   2011A-0034

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Program Information for 2011A-0034


PI: Christopher Stubbs, Harvard U., stubbs@physics.harvard.edu
Address: Department of Physics, 17 Oxford St., Cambridge, MA 02138 USA

CoI: Matthew Ashby, Harvard-Smithsonian Center for Astrophysics
CoI: K Anderson, Max Planck Institut fuer extraterrestrische Physik
CoI: Gurvan Bazin, Max Planck Institut fuer extraterrestrische Physik
CoI: Bradford Benson, U. of Chicago
CoI: Lindsey Bleem, U. of Chicago
CoI: Mark Brodwin, Harvard-Smithsonian Center for Astrophysics
CoI: John E Carlstrom, U. of Chicago
CoI: Alejandro Clocchiatti, Pontificia Universidad Catolica de Chile
CoI: Thomas Crawford, U. of Chicago
CoI: Tijmen De Haan, McGill University
CoI: Matt A Dobbs, McGill University
CoI: J P Dudley, McGill University
CoI: Ryan Foley, Harvard-Smithsonian Center for Astrophysics
CoI: Michael D Gladders, U. of Chicago
CoI: Fredrick W. High, U. of Chicago
CoI: Gil Holder, McGill University
CoI: William Holzapfel, UC Berkeley
CoI: Ryan Keisler, U. of Chicago
CoI: Daniel Marrone, U. of Chicago
CoI: Joseph Mohr, Universitaets-Sternwarte Munchen
CoI: Thomas Montroy, Case Western Reserve U.
CoI: C L Reichardt, UC Berkeley
CoI: Armin Rest, STScI
CoI: Jonathan Ruel, Harvard U.
CoI: John Ruhl, Case Western Reserve U.
CoI: B Saliwanchik, Case Western Reserve U.
CoI: Laurie Shaw, Yale U.
CoI: Jeeseon Song, U. of Illinois Urbana-Champaign
CoI: Brian Stalder, Harvard U.
CoI: Adam Stanford, UC Davis
CoI: Antony Stark, Harvard-Smithsonian Center for Astrophysics
CoI: K Story, Harvard U.
CoI: K Vanderlinde, McGill University
CoI: R Williamson, STScI

Title: Spectroscopy of Galaxies in Massive Clusters: Galaxy Properties and Dynamical Cluster Mass Calibration

Abstract: We propose to acquire GMOS spectroscopy of $ clusters of galaxies selected via the Sunyaev-Zel'dovich (SZ) effect from the South Pole Telescope (SPT) microwave background survey. This will bring our total to 100 SPT clusters with velocity dispersions. The SPT survey is delivering a uniformly-selected high-mass cluster sample that is essentially volume-complete beyond $z>.3. We will target a subset (.3 < z < 0.8$) of the SPT cluster catalog, extracted from 00 \,\mathrm^2$. This data set will establish competitive, independent constraints on cosmological parameters, including the nature of the dark energy. Achieving this goal requires a precise understanding of the relationship between the cluster's SZ signature and the cluster mass, and this mass normalization is currently the largest systematic error in SPT's cosmological constraints. One promising method of determining galaxy cluster masses is to probe the dark matter potential with galaxy velocities. Using data from a large cluster sample will average over random projection effects, and will enable the calibration of the SZ-mass scaling relation, in conjunction with X-ray and lensing data on a smaller sample. The cluster galaxy spectroscopy we obtain will also equip the community to address a wide range of questions in galaxy evolution and cluster astrophysics.

Program Type: Survey

Scheduled Nights:
Run 1 (2011A):  GEM-S/GMOSS -- 3n on Jul 27 - Jul 31 2011
Run 1 (2011B):  GEM-S/GMOSS -- 4n on Sep 27 - Sep 30 2011
Run 1 (2012A):  GEM-SQ/GMOSS -- 23.7hrs band 1 (GS-2012A-Q-4)
Run 1 (2012B):  GEM-SQ/GMOSS -- 32hrs band 1 (GS-2012B-Q-29)
Run 1 (2013A):  GEM-SQ/GMOSS -- 9hrs band 1 (GS-2013A-Q-5)
Run 1 (2013B):  GEM-SQ/GMOSS -- 32hrs band 1 (GS-2013B-Q-25)
Run 1 (2014B):  GEM-SQ/GMOSS -- 20hrs band 1 (GS-2014B-Q-31)
Run 2 (2011A):  GEM-SQ/GMOSS -- 5.5hrs band 1 (GS-2011A-Q-4)
Run 2 (2011B):  GEM-SQ/GMOSS -- 5.5hrs band 1 (GS-2011B-Q-33)
Run 3 (2012A):  GEM-SQ/GMOSS -- 14.6hrs band 2 (GS-2012A-Q-37)
Run 3 (2012B):  GEM-SQ/GMOSS -- 20hrs band 2 (GS-2012B-Q-59)
Run 3 (2013A):  GEM-SQ/GMOSS -- 5hrs band 2 (GS-2013A-Q-45)
Run 3 (2013B):  GEM-SQ/GMOSS -- 20hrs band 2 (GS-2013B-Q-72)
Run 3 (2014B):  GEM-SQ/GMOSS -- 20hrs band 2 (GS-2014B-Q-64)


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NOAO >   Observing Info >   Approved Programs >   2011A-0034

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