The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z=0.57 from anisotropic clustering

Дата и время публикации : 2012-03-29T19:41:01Z

Авторы публикации и институты :
Beth A. Reid
Lado Samushia
Martin White
Will J. Percival
Marc Manera
Nikhil Padmanabhan
Ashley J. Ross
Ariel G. Sánchez
Stephen Bailey
Dmitry Bizyaev
Adam S. Bolton
Howard Brewington
J. Brinkmann
Joel R. Brownstein
Antonio J. Cuesta
Daniel J. Eisenstein
James E. Gunn
Klaus Honscheid
Elena Malanushenko
Viktor Malanushenko
Claudia Maraston
Cameron K. McBride
Demitri Muna
Robert C. Nichol
Daniel Oravetz
Kaike Pan
Roland de Putter
N. A. Roe
Nicholas P. Ross
David J. Schlegel
Donald P. Schneider
Hee-Jong Seo
Alaina Shelden
Erin S. Sheldon
Audrey Simmons
Ramin A. Skibba
Stephanie Snedden
Molly E. C. Swanson
Daniel Thomas
Jeremy Tinker
Rita Tojeiro
Licia Verde
David A. Wake
Benjamin A. Weaver
David H. Weinberg
Idit Zehavi
Gong-Bo Zhao

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 19 pages, 11 figures, submitted to MNRAS, comments welcome
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: We analyze the anisotropic clustering of massive galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) sample, which consists of 264,283 galaxies in the redshift range 0.43 < z < 0.7 spanning 3,275 square degrees. Both peculiar velocities and errors in the assumed redshift-distance relation ("Alcock-Paczynski effect") generate correlations between clustering amplitude and orientation with respect to the line-of-sight. Together with the sharp baryon acoustic oscillation (BAO) standard ruler, our measurements of the broadband shape of the monopole and quadrupole correlation functions simultaneously constrain the comoving angular diameter distance (2190 +/- 61 Mpc) to z=0.57, the Hubble expansion rate at z=0.57 (92.4 +/- 4.5 km/s/Mpc), and the growth rate of structure at that same redshift (d sigma8/d ln a = 0.43 +/- 0.069). Our analysis provides the best current direct determination of both DA and H in galaxy clustering data using this technique. If we further assume a LCDM expansion history, our growth constraint tightens to d sigma8/d ln a = 0.415 +/- 0.034. In combination with the cosmic microwave background, our measurements of DA, H, and growth all separately require dark energy at z > 0.57, and when combined imply Omega_{Lambda} = 0.74 +/- 0.016, independent of the Universe’s evolution at z<0.57. In our companion paper (Samushia et al. prep), we explore further cosmological implications of these observations.

Category: Physics