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A halo mass—concentration relation from weak lensing

Mandelbaum, Rachel and Seljak, Uroš and Hirata, Christopher M. (2008) A halo mass—concentration relation from weak lensing. Journal of Cosmology and Astroparticle Physics, 2008 (08). Art. No. 006. ISSN 1475-7516. http://resolver.caltech.edu/CaltechAUTHORS:MANjcap08

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Abstract

We perform a statistical weak lensing analysis of dark matter profiles around tracers of halo mass from galaxy-size to cluster-size halos. In this analysis we use 170 640 isolated ∼L∗ galaxies split into ellipticals and spirals, 38 236 groups traced via isolated spectroscopic luminous red galaxies and 13 823 maxBCG clusters from the Sloan Digital Sky Survey covering a wide range of richness. Together these three samples allow a determination of the density profiles of dark matter halos over three orders of magnitude in mass, from 10^12M☉ to 10^15M☉. The resulting lensing signal is consistent with a Navarro–Frenk–White (NFW) or Einasto profile on scales outside the central region. In the inner regions, uncertainty in modeling of the proper identification of the halo center and inclusion of baryonic effects from the central galaxy make the comparison less reliable. We find that the NFW concentration parameter c200b decreases with halo mass, from around 10 for galactic halos to 4 for cluster halos. Assuming its dependence on halo mass in the form of c200b = c0(M/10^14h^−1 M☉)−β we find c0 = 4.6 ± 0.7 (at z = 0.22) and β = 0.13 ± 0.07, with very similar results for the Einasto profile. The slope (β) is in agreement with theoretical predictions, while the amplitude is about two standard deviations below the predictions for this mass and redshift, but we note that the published values in the literature differ at a level of 10–20% and that for a proper comparison our analysis should be repeated in simulations. We compare our results to other recent determinations, some of which find significantly higher concentrations. We discuss the implications of our results for the baryonic effects on the shear power spectrum: since these are expected to increase the halo concentration, the fact that we see no evidence of high concentrations on scales above 20% of the virial radius suggests that baryonic effects are limited to small scales, and are not a significant source of uncertainty for the current weak lensing measurements of the dark matter power spectrum.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/1475-7516/2008/08/006DOIUNSPECIFIED
http://stacks.iop.org/JCAP/2008/i=08/a=006PublisherUNSPECIFIED
http://www.iop.org/EJ/abstract/1475-7516/2008/08/006PublisherUNSPECIFIED
http://arxiv.org/abs/0805.2552arXivUNSPECIFIED
Additional Information:Copyright © 2008 IOP Publishing Ltd and SISSA. Received 16 May 2008, accepted for publication 7 July 2008. Published 6 August 2008. We thank the anonymous referee for useful comments on the submitted version of this paper. RM is supported by NASA through Hubble Fellowship grant No. HST-HF-01199.02-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. US is supported by the Packard Foundation, NSF CAREER-0132953 and Swiss National Foundation (grant number 200021-116696/1). CH is supported by DoE DE-FG03-92-ER40701. Funding for the SDSS and SDSS-II has been provided by the Alfred P Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max Planck Institute for Astronomy (MPIA), the Max Planck Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NASAHST-HF-01199.02-A
NASANAS 5-26555
David and Lucille Packard FoundationUNSPECIFIED
National Science FoundationCAREER-0132953
Swiss National Foundation200021-116696/1
Department of EnergyDE-FG03-92-ER40701
Alfred P. Sloan FoundationUNSPECIFIED
Participating InstitutionsUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:dark matter; structure of galaxies; gravitational lensing
Record Number:CaltechAUTHORS:MANjcap08
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:MANjcap08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:11617
Collection:CaltechAUTHORS
Deposited By: Archive Administrator
Deposited On:12 Sep 2008 06:15
Last Modified:26 Dec 2012 10:17

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