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Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications

Ho, Shirley and Hirata, Christopher and Padmanabhan, Nikhil and Seljak, Uroš and Bahcall, Neta (2008) Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications. Physical Review D, 78 (4). Art. No. 043519. ISSN 2470-0010. doi:10.1103/PhysRevD.78.043519.

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We cross correlate large-scale structure (LSS) observations from a number of surveys with cosmic microwave background (CMB) anisotropies from the Wilkinson Microwave Anisotropy Probe (WMAP) to investigate the integrated Sachs-Wolfe (ISW) effect as a function of redshift, covering z~0.1–2.5. Our main goal is to go beyond reporting detections towards developing a reliable likelihood analysis that allows one to determine cosmological constraints from ISW observations. With this in mind we spend a considerable amount of effort in determining the redshift-dependent bias and redshift distribution (b(z)×dN/dz) of these samples by matching with spectroscopic observations where available, and analyzing autopower spectra and cross-power spectra between the samples. Because of wide redshift distributions of some of the data sets we do not assume a constant-bias model, in contrast to previous work on this subject. We only use the LSS data sets for which we can extract such information reliably and as a result the data sets we use are 2-Micron All Sky Survey (2MASS) samples, Sloan Digital Sky Survey (SDSS) photometric Luminous Red Galaxies, SDSS photometric quasars, and NRAO VLA Sky Survey (NVSS) radio sources. We make a joint analysis of all samples constructing a full covariance matrix, which we subsequently use for cosmological parameter fitting. We report a 3.7sigma detection of ISW combining all the data sets. We do not find significant evidence for an ISW signal at z>1, in agreement with theoretical expectation in the LambdaCDM model. We combine the ISW likelihood function with weak lensing of CMB (hereafter Paper II [C. M. Hirata, S. Ho, N. Padmanabhan, U. Seljak, and N. A. Bahcall, arXiv:0801.0644.]) and CMB power spectrum to constrain the equation of state of dark energy and the curvature of the Universe. While ISW does not significantly improve the constraints in the simplest six-parameter flat LambdaCDM model, it improves constraints on seven-parameter models with curvature by a factor of 3.2 (relative to WMAP alone) to OmegaK=-0.004-0.020+0.014, and with dark energy equation of state by 15% to w=-1.01-0.40+0.30 [posterior median with “1sigma” (16th–84th percentile) range]. A software package for calculating the ISW likelihood function can be downloaded at

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Hirata, Christopher0000-0002-2951-4932
Additional Information:© 2008 The American Physical Society. (Received 16 February 2008; revised 29 July 2008; published 13 August 2008) We would like to thank Joanna Dunkley for her extensive help on the discussion of chain convergences, and Lucas Lombriser and Anže Slosar for bringing an error in an earlier version of this paper to our attention. We would also like to thank David Spergel, Kendrick Smith, and Jim Gunn for helpful conversations. N.P. is supported by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS 5-26555. Part of this work was supported by the Director, Office of Science, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. U.S. is supported by the Packard Foundation and NSF CAREER-0132953. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, the U.S. 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 website is 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, the University of Basel, the University of Cambridge, Case Western Reserve University, the 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, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The 2dF QSO Redshift Survey (2QZ) was compiled by the 2QZ survey team from observations made with the two-degree field on the Anglo-Australian Telescope. The 2dF-SDSS LRG and QSO (2SLAQ) Survey was compiled by the 2SLAQ team from SDSS data and observations made with the two-degree field on the Anglo-Australian Telescope. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
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Space Telescope Science InstituteUNSPECIFIED
Association of Universities for Research in Astronomy, Inc.UNSPECIFIED
NASANAS 5-26555
Department of Energy (DOE)DE-AC02-05CH11231
David and Lucile Packard FoundationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Astrophysical Research ConsortiumUNSPECIFIED
Participating InstitutionsUNSPECIFIED
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Record Number:CaltechAUTHORS:HOSprd08
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:11462
Deposited By: Marie Noren
Deposited On:28 Aug 2008 04:27
Last Modified:08 Nov 2021 21:59

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