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Non-detection of a statistically anisotropic power spectrum in large-scale structure

Pullen, Anthony R. and Hirata, Christopher M. (2010) Non-detection of a statistically anisotropic power spectrum in large-scale structure. Journal of Cosmology and Astroparticle Physics, 2010 (5). Art. No. 027 . ISSN 1475-7516.

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We search a sample of photometric luminous red galaxies (LRGs) measured by the Sloan Digital Sky Survey (SDSS) for a quadrupolar anisotropy in the primordial power spectrum, in which P(k) is an isotropic power spectrum P[overbar](k) multiplied by a quadrupolar modulation pattern. We first place limits on the 5 coefficients of a general quadrupole anisotropy. We also consider axisymmetric quadrupoles of the form P(k) = P[overbar](k){1+g_*[k[circuflex] ∙ n[circumflex]^2 − (1/3)]} where n[circumflex] is the axis of the anisotropy. When we force the symmetry axis n[circumflex] to be in the direction (l,b) = (94°,26°) identified in the recent Groeneboom et al. analysis of the cosmic microwave background, we find g* = 0.006±0.036 (1σ). With uniform priors on n[circumflex] and g_* we find that −0.41 < g_* < +0.38 with 95% probability, with the wide range due mainly to the large uncertainty of asymmetries aligned with the Galactic Plane. In none of these three analyses do we detect evidence for quadrupolar power anisotropy in large scale structure.

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Additional Information:© 2010 IOP Publishing Ltd and SISSA. Received March 5, 2010; Revised March 30, 2010; Accepted April 22, 2010; Published May 21, 2010. We thank N Padmanabhan and S Ho for providing the LRG sample and for their useful feedback. We also thank M Kamionkowski for helpful comments. AP acknowledges the support of the NSF. This work was supported by DOE DE-FG03- 92-ER40701, NASA NNG05GF69G, the Gordon and Betty Moore Foundation, and a NASA Einstein Probe mission study grant, “The Experimental Probe of Inflationary Cosmology.” CH is supported by the US Department of Energy under contract DE-FG03-02-ER40701, the National Science Foundation under contract AST-0807337, and the Alfred P Sloan Foundation. Funding for the Sloan Digital Sky Survey (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 Web site is 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.
Funding AgencyGrant Number
Department of Energy (DOE)DE-FG03-92-ER40701
Gordon and Betty Moore FoundationEinstein Probe mission study grant
Department of Energy (DOE)DE-FG03-02-ER40701
Alfred P. Sloan FoundationUNSPECIFIED
Subject Keywords:power spectrum; galaxy surveys
Classification Code:PACS: 95.80.+p; 98.62.Ve; 98.70.Vc; 98.62.Ck; 98.62.Qz
Record Number:CaltechAUTHORS:20100720-115900943
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Official Citation:Anthony R. Pullen and Christopher M. Hirata JCAP05(2010)027 doi: 10.1088/1475-7516/2010/05/027
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:19129
Deposited By: Jason Perez
Deposited On:21 Jul 2010 18:24
Last Modified:26 Dec 2012 12:15

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