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

Abstract

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{approx}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)xdN/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 cosmologicalmore » parameter fitting. We report a 3.7{sigma} 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 {lambda}CDM 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 {lambda}CDM model, it improves constraints on seven-parameter models with curvature by a factor of 3.2 (relative to WMAP alone) to {omega}{sub K}=-0.004{sub -0.020}{sup +0.014}, and with dark energy equation of state by 15% to w=-1.01{sub -0.40}{sup +0.30} [posterior median with ''1{sigma}'' (16th-84th percentile) range]. A software package for calculating the ISW likelihood function can be downloaded at http://www.astro.princeton.edu/{approx}shirley/ISW{sub W}L.html.« less

Authors:
;  [1];  [2];  [3];  [4]
  1. Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544 (United States)
  2. California Institute of Technology M/C 130-33, Pasadena, California 91125 (United States)
  3. Lawrence Berkeley National Laboratory, Berkeley, California 94720 (United States)
  4. Institute for Theoretical Physics, Zurich University, Zurich 8057 (Switzerland)
Publication Date:
OSTI Identifier:
21250467
Resource Type:
Journal Article
Journal Name:
Physical Review. D, Particles Fields
Additional Journal Information:
Journal Volume: 78; Journal Issue: 4; Other Information: DOI: 10.1103/PhysRevD.78.043519; (c) 2008 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0556-2821
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; 99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE; ANISOTROPY; CORRELATIONS; DETECTION; DISTRIBUTION; EQUATIONS OF STATE; GALAXIES; NONLUMINOUS MATTER; PROBES; QUASARS; RED SHIFT; RELICT RADIATION; SPECTRA; TOMOGRAPHY; UNIVERSE

Citation Formats

Ho, Shirley, Bahcall, Neta, Hirata, Christopher, Padmanabhan, Nikhil, Seljak, Uros, and Department of Physics, University of California at Berkeley, Berkeley, California 94704. Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications. United States: N. p., 2008. Web. doi:10.1103/PHYSREVD.78.043519.
Ho, Shirley, Bahcall, Neta, Hirata, Christopher, Padmanabhan, Nikhil, Seljak, Uros, & Department of Physics, University of California at Berkeley, Berkeley, California 94704. Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications. United States. doi:10.1103/PHYSREVD.78.043519.
Ho, Shirley, Bahcall, Neta, Hirata, Christopher, Padmanabhan, Nikhil, Seljak, Uros, and Department of Physics, University of California at Berkeley, Berkeley, California 94704. Fri . "Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications". United States. doi:10.1103/PHYSREVD.78.043519.
@article{osti_21250467,
title = {Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications},
author = {Ho, Shirley and Bahcall, Neta and Hirata, Christopher and Padmanabhan, Nikhil and Seljak, Uros and Department of Physics, University of California at Berkeley, Berkeley, California 94704},
abstractNote = {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{approx}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)xdN/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 3.7{sigma} 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 {lambda}CDM 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 {lambda}CDM model, it improves constraints on seven-parameter models with curvature by a factor of 3.2 (relative to WMAP alone) to {omega}{sub K}=-0.004{sub -0.020}{sup +0.014}, and with dark energy equation of state by 15% to w=-1.01{sub -0.40}{sup +0.30} [posterior median with ''1{sigma}'' (16th-84th percentile) range]. A software package for calculating the ISW likelihood function can be downloaded at http://www.astro.princeton.edu/{approx}shirley/ISW{sub W}L.html.},
doi = {10.1103/PHYSREVD.78.043519},
journal = {Physical Review. D, Particles Fields},
issn = {0556-2821},
number = 4,
volume = 78,
place = {United States},
year = {2008},
month = {8}
}