TITLE:
Correlation of CMB with large-scale structure: I. ISW Tomography and Cosmological Implications.
AUTHOR(S):
Shirley Ho (Princeton); Christopher Hirata (Caltech); Nikhil Padmanabhan (LBL); Uros Seljak (Zurich); Neta Bahcall (Princeton).
DATE:
2008 Jan 04 (arXiv, posted, v1);
2008 Feb 16 (Phys. Rev. D, submitted);
2008 May 29 (Phys. Rev. D, accepted);
2008 Jul 29 (revised);
2008 Aug 08 (arXiv, posted, v2);
2008 Aug 13 (Phys. Rev. D, published).
AVAILABILITY:
arXiv 0801.0642 (free);
APS (requires subscription).
PUBLICATION INFORMATION:
Phys. Rev. D, 78, 043519, 2008.
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~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
auto-power spectra and cross-power spectra between the samples.
Due to 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 datasets.
We do not find significant evidence for an ISW signal at z>1, in agreement with theoretical
expectation in Lambda CDM model.
We combine the ISW likelihood function with weak lensing of CMB (hereafter Paper II) 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 6-parameter flat Lambda CDM model,
it improves constraints on 7-parameter models with curvature by a factor of 3.2 (relative to WMAP alone)
to Omega_K=-0.004^{+0.014}_{-0.020},
and with dark energy equation of state by 15% to w=-1.01^{+0.30}_{-0.40}
[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/~shirley/ISW_WL.html.
ADS BIBLIOGRAPHIC CODE: N/A.
COMMENTS: SDSS Publication #851. Paper II is here.