TY - JOUR
T1 - Cosmological parameters from galaxy clustering in the SDSS
AU - Pope, Adrian
AU - Szalay, Alexander
AU - Matsubara, Takahiko
AU - Blanton, Michael R.
AU - Eisenstein, Daniel J.
AU - Gray, Jim
AU - Jain, Bhuvnesh
N1 - Funding Information:
Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbuka-gakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.
Funding Information:
tions used for this project. We would like to thank Licia Verde for providing us with the WMAP MCMC points. This material is based upon work supported under a National Science Foundation Graduate Research Fellowship and by NSF AST-9802980 at Johns Hopkins University.
Publisher Copyright:
© 2004 Sissa Medialab Srl.
PY - 2004
Y1 - 2004
N2 - We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the 3D power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use {equation presented} to describe the shape of the power spectrum, σL 8g for the (linearly extrapolated) normalization, and β to parametrize linear theory redshift space distortions. On scales {equation presented}, our maximum likelihood values are Wmh {equation presented}. When we take a prior on ωb from WMAP , we find ωm h = 0.207 ± 0.030, which is in excellent agreement with WMAP and 2dF. This indicates that we have reasonably measured the gross shape of the power spectrum but we have difficulty breaking the degeneracy between ωmh and fb because the baryon oscillations are not resolved in the current spectroscopic survey window function.
AB - We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the 3D power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use {equation presented} to describe the shape of the power spectrum, σL 8g for the (linearly extrapolated) normalization, and β to parametrize linear theory redshift space distortions. On scales {equation presented}, our maximum likelihood values are Wmh {equation presented}. When we take a prior on ωb from WMAP , we find ωm h = 0.207 ± 0.030, which is in excellent agreement with WMAP and 2dF. This indicates that we have reasonably measured the gross shape of the power spectrum but we have difficulty breaking the degeneracy between ωmh and fb because the baryon oscillations are not resolved in the current spectroscopic survey window function.
UR - https://www.scopus.com/pages/publications/85056835515
UR - https://www.scopus.com/pages/publications/85056835515#tab=citedBy
M3 - Conference article
AN - SCOPUS:85056835515
SN - 1824-8039
VL - 16
JO - Proceedings of Science
JF - Proceedings of Science
M1 - 007
T2 - 28th Johns Hopkins Workshop on Current Problems in Particle Theory, JHW 2004
Y2 - 5 June 2004 through 8 June 2004
ER -