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Large Scale Structure in Dark Matter and Galaxies

Scoville, Nick (2009) Large Scale Structure in Dark Matter and Galaxies. In: Sources and detection of dark matter and dark energy in the universe. AIP Conference Proceedings. No.1166. American Institute of Physics , Melville, NY, pp. 10-15. ISBN 978-0-7354-0703-9 http://resolver.caltech.edu/CaltechAUTHORS:20100805-111401779

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Abstract

Galaxy evolution and AGN growth in the early universe are believed to be strongly driven by merging (hierarchical growth) and galaxy dynamical interactions. Thus, a fall exploration of the environmental influences is absolutely essential to understanding this early evolution. The Cosmic Evolution Survey (COSMOS, [Scoville et al. 2007a]) is specifically designed to probe the correlated coevolution of galaxies, star formation, active galactic nuclei (AGN) and dark matter (DM) largescale structures (LSS) over the redshift range z > 0.5 to 6. The survey includes midti-wavelength imaging and spectroscopy from X-ray to radio wavelengths covering a 2 square degree equatorial field. Photometric redshifts are derived using 34 photometric UV-IR bands for 800,000 galaxies with accuracy reaching σ_z/(l +z) = 0.7 — 1.6% for bright galaxies (I_(AB) = 22 —24mag). Large scale structures have been traced in COSMOS from z = 0.2 to 2.5 in the baryons (from the galaxy density distribution) and in the dark matter to z = 1.1 (from weak tensing analysis of HST ACS images). These LSS extend over 20 Mpc with total mass up to ~10^(15)_ ⊙. The overall distribution of galaxy overdensities is similar with those predicted from the Millennium simulation. A trend for an increasing high overdensities at low z is clearly apparent in these data. At higher redshifts of z ~ 1, there appears to be a significant discrepancy between the observations and the simulations - with the simidations exhibiting earUer development of high density structores than is seen in the observed galaxy distributions. The observed galaxy spectral energy distributions (SEDs) and star formation rates (SFRs) clearly depend systematically on both redshift and environmental density - early SED types and lower SFRs in denser regions and at lower redshift. This evolution is probably driven by the exhaustion of the ISM and by galaxy interactions, the latter being strongly correlated with regions of highest dark matter density. Strong evolution is seen the frequency of close pairs of galaxies - particidarly for lower mass companions at projected separations 10 - 20 kpc.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1063/1.3232166 DOIUNSPECIFIED
http://link.aip.org/link/?APCPCS/1166/10/1PublisherUNSPECIFIED
ORCID:
AuthorORCID
Scoville, Nick0000-0002-0438-3323
Additional Information:© 2009 American Institute of Physics. Issue Date: 8 September 2009. I gratefully acknowledge the contributions of the entire COSMOS colaboration consisting of more than 100 scientists. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822 and Spitzer PID 20070 & 30143. The status of these observational programs is continuously updated on the COSMOS web-site : http://www.astro.caltech.edu/~cosmos/. The major COSMOS datasets become publicly available in staged releases (following calibration and validation) through the web site for IPAC/IRSA : http://irsa.ipac.caltech.edu/data/COSMOS/
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASAHST-GO-09822
Spitzer PID 20070
Spitzer PID 30143
Subject Keywords:cosmology; galaxy evolution
Classification Code:PACS: 95.35.+d; 98.80.-k; 98.35.Jk
Record Number:CaltechAUTHORS:20100805-111401779
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100805-111401779
Official Citation:Large Scale Structure in Dark Matter and Galaxies Nick Scoville, AIP Conf. Proc. 1166, 10 (2009), DOI:10.1063/1.3232166
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:19295
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:05 Aug 2010 21:02
Last Modified:19 Apr 2016 21:50

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