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Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7

Mandelbaum, Rachel and Slosar, Anže and Baldauf, Tobias and Seljak, Uroš and Hirata, Christopher M. and Nakajima, Reiko and Reyes, Reinabelle and Smith, Robert E. (2013) Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7. Monthly Notices of the Royal Astronomical Society, 432 (2). pp. 1544-1575. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20130828-154954270

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Abstract

Recent studies have shown that the cross-correlation coefficient between galaxies and dark matter is very close to unity on scales outside a few virial radii of galaxy haloes, independent of the details of how galaxies populate dark matter haloes. This finding makes it possible to determine the dark matter clustering from measurements of galaxy–galaxy weak lensing and galaxy clustering. We present new cosmological parameter constraints based on large-scale measurements of spectroscopic galaxy samples from the Sloan Digital Sky Survey (SDSS) data release 7. We generalize the approach of Baldauf et al. to remove small-scale information (below 2 and 4 h^(−1) Mpc for lensing and clustering measurements, respectively), where the cross-correlation coefficient differs from unity. We derive constraints for three galaxy samples covering 7131 deg^2, containing 69 150, 62 150 and 35 088 galaxies with mean redshifts of 0.11, 0.28 and 0.40. We clearly detect scale-dependent galaxy bias for the more luminous galaxy samples, at a level consistent with theoretical expectations. When we vary both σ_8 and Ω_m (and marginalize over non-linear galaxy bias) in a flat Λ cold dark matter model, the best-constrained quantity is σ_8(Ω_m/0.25)^(0.57) = 0.80 ± 0.05 (1σ, stat. + sys.), where statistical and systematic errors (photometric redshift and shear calibration) have comparable contributions, and we have fixed n_s = 0.96 and h = 0.7. These strong constraints on the matter clustering suggest that this method is competitive with cosmic shear in current data, while having very complementary and in some ways less serious systematics. We therefore expect that this method will play a prominent role in future weak lensing surveys. When we combine these data with Wilkinson Microwave Anisotropy Probe 7-year (WMAP7) cosmic microwave background (CMB) data, constraints on σ_8, Ω_m, H_0, w_(de) and ∑m_ν become 30–80 per cent tighter than with CMB data alone, since our data break several parameter degeneracies.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1207.1120arXivDiscussion Paper
http://dx.doi.org/10.1093/mnras/stt572 DOIArticle
http://mnras.oxfordjournals.org/content/432/2/1544PublisherArticle
ORCID:
AuthorORCID
Hirata, Christopher M.0000-0002-2951-4932
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 March 30. Received 2013 March 8; in original form 2012 July 5. First published online: April 28, 2013. We thank the anonymous referee for providing numerous comments that improved the presentation of this work. We thank Jim Gunn, Robert Lupton, Benjamin Joachimi and David Spergel for useful discussions related to this work, and we also thank Eyal Kazin for helpful discussions on selection of the LRG sample. RM was supported for part of the duration of this project by the US Department of Energy Early Career Program. During this project, US was supported in part by the US Department of Energy under Contract No. DE-AC02-98CH10886, the Swiss National Foundation under contract 200021-116696/1 and the WCU grant R32-10130. During this project, CH has been supported by the US Department of Energy (DOE-FG03-92-ER40701 and DOE.DE-SC0006624), the National Science Foundation (NST AST-0807337) and the David & Lucile Packard Foundation. RES acknowledges support from a Marie Curie Reintegration Grant and an award for Experienced Researchers from the Alexander von Humboldt Foundation. We thank V. Springel for making public GADGET-2 and for providing his B-FoF halo finder, and R. Scoccimarro for making public his 2LPT code. 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, and the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) 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, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The 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.
Funders:
Funding AgencyGrant Number
Department of Energy (DOE)DE-AC02-98CH10886
Swiss National Foundation (SNF)200021-116696/1
WCUR32-10130
Department of Energy (DOE)DE-FG03-92-ER40701
Department of Energy (DOE)DE-SC0006624
NSFAST-0807337
David and Lucile Packard FoundationUNSPECIFIED
Marie Curie FellowshipUNSPECIFIED
Alexander von Humboldt FoundationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Participating InstitutionsUNSPECIFIED
NASAUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:gravitational lensing: weak; cosmological parameters; cosmology: observations; large-scale structure of Universe
Issue or Number:2
Record Number:CaltechAUTHORS:20130828-154954270
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130828-154954270
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:40983
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:30 Aug 2013 18:28
Last Modified:03 Oct 2019 05:44

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