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Detection of the Baryon Acoustic Peak in the Large‐Scale Correlation Function of SDSS Luminous Red Galaxies

  • Authors: Daniel J. Eisenstein, Idit Zehavi, David W. Hogg, Roman Scoccimarro, Michael R. Blanton, Robert C. Nichol, Ryan Scranton, Hee-Jong Seo, Max Tegmark, Zheng Zheng, Scott F. Anderson, Jim Annis, Neta Bahcall, Jon Brinkmann, Scott Burles, Francisco J. Castander, Andrew Connolly, Istvan Csabai, Mamoru Doi, Masataka Fukugita, Joshua A. Frieman, Karl Glazebrook, James E. Gunn, John S. Hendry, Gregory Hennessy, Zeljko Ivezić, Stephen Kent, Gillian R. Knapp, Huan Lin, Yeong-Shang Loh, Robert H. Lupton, Bruce Margon, Timothy A. McKay, Avery Meiksin, Jeffery A. Munn, Adrian Pope, Michael W. Richmond, David Schlegel, Donald P. Schneider, Kazuhiro Shimasaku, Christopher Stoughton, Michael A. Strauss, Mark SubbaRao, Alexander S. Szalay, István Szapudi, Douglas L. Tucker, Brian Yanny, and Donald G. York

Eisenstein et al. 2005 The Astrophysical Journal 633 560.

  • Provider: AAS Journals

Caption: Fig. 2.

Large‐scale redshift‐space correlation function of the SDSS LRG sample. The error bars are from the diagonal elements of the mock‐catalog covariance matrix; however, the points are correlated. Note that the vertical axis mixes logarithmic and linear scalings. The inset shows an expanded view with a linear vertical axis. The models are ﹩\Omega _{m}h^{2}=0.12﹩ (green line), 0.13 (red line), and 0.14 (blue line), all with ﹩\Omega _{b}h^{2}=0.024﹩ and ﹩n=0.98﹩ and with a mild nonlinear prescription folded in. The magenta line shows a pure CDM model (﹩\Omega _{m}h^{2}=0.105﹩), which lacks the acoustic peak. It is interesting to note that although the data appear higher than the models, the covariance between the points is soft as regards overall shifts in ξ(s). Subtracting 0.002 from ξ(s) at all scales makes the plot look cosmetically perfect but changes the best‐fit χ2 by only 1.3. The bump at 100 h−1 Mpc scale, on the other hand, is statistically significant.

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