The clustering of luminous red galaxies in the Sloan Digital Sky Survey imaging data
The clustering of luminous red galaxies in the Sloan Digital Sky Survey imaging data
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DOI：
10.1111/j.1365-2966.2007.11593.x
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发表时间：
2006-05
影响因子：
4.8
通讯作者：
N. Padmanabhan;D. Schlegel;U. Seljak;U. Seljak;A. Makarov;N. Bahcall;M. Blanton;J. Brinkmann;D. Eisenstein;D. Finkbeiner;J. Gunn;D. Hogg;Ž. Ivezić;G. Knapp;J. Loveday;R. Lupton;R. Nichol;D. Schneider;M. Strauss;M. Tegmark;D. York
中科院分区：
文献类型：
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作者：
N. Padmanabhan;D. Schlegel;U. Seljak;U. Seljak;A. Makarov;N. Bahcall;M. Blanton;J. Brinkmann;D. Eisenstein;D. Finkbeiner;J. Gunn;D. Hogg;Ž. Ivezić;G. Knapp;J. Loveday;R. Lupton;R. Nichol;D. Schneider;M. Strauss;M. Tegmark;D. York
我们展示了由斯隆数字巡天测量的约60万个发光红星系样本的三维实空间聚类功率谱，使用光度红移。这些星系是古老的椭圆系统，具有强烈的4000-A断裂，具有精确的光度红移，平均误差为Δz= 0.03。这个星系样本的红移范围从z= 0.2到0.6，覆盖了3528°2的天空，探测的体积为1.5 h - 3 Gpc3，使其成为有史以来用于星系团测量的最大体积。我们测量了8个红移切片中的角聚类功率谱，并使用校准良好的红移分布将它们组合成k= 0.005至k= 1 h Mpc−1的高精度3D实空间功率谱。我们在千兆秒差距尺度上检测到的功率，超出了物质功率谱的转换，当k < 0.01 h Mpc - 1时，显著性为~ 2σ，当k < 0.02 h Mpc - 1时，显著性增加到5.5σ。这种功率探测的尺度明显大于当前光谱红移测量所能达到的尺度。我们还发现了重子振荡的证据，无论是在功率谱中，还是在与重子密度的拟合中，在2.5 σ置信水平上。大体积和由此产生的功率谱上的小统计误差使我们能够约束宇宙学拟合中星系偏差的幅度和尺度依赖。这些数据约束宇宙学的统计能力比以前的聚类分析好1.7倍。改变物质密度和重子分数，我们发现对于固定的哈勃常数70 km s−1 Mpc−1和初始扰动的尺度不变谱，ΩM= 0.30±0.03，Ωb/ΩM= 0.18±0.04。重子振荡的检测也使我们能够测量到z= 0.5的移动距离；我们发现最佳拟合距离为1.73±0.12 Gpc，对应于距离上6.5%的误差。这些结果证明了利用光度测量进行精确聚类测量的能力。
We present the 3D real-space clustering power spectrum of a sample of ∼600 000 luminous red galaxies measured by the Sloan Digital Sky Survey, using photometric redshifts. These galaxies are old, elliptical systems with strong 4000-A breaks, and have accurate photometric redshifts with an average error of Δz= 0.03. This sample of galaxies ranges from redshift z= 0.2 to 0.6 over 3528 deg2 of the sky, probing a volume of 1.5 h−3 Gpc3, making it the largest volume ever used for galaxy clustering measurements. We measure the angular clustering power spectrum in eight redshift slices and use well-calibrated redshift distributions to combine these into a high-precision 3D real-space power spectrum from k= 0.005 to k= 1 h Mpc−1. We detect power on gigaparsec scales, beyond the turnover in the matter power spectrum, at a ∼2σ significance for k < 0.01 h Mpc−1, increasing to 5.5σ for k < 0.02 h Mpc−1. This detection of power is on scales significantly larger than those accessible to current spectroscopic redshift surveys. We also find evidence for baryonic oscillations, both in the power spectrum, as well as in fits to the baryon density, at a 2.5 σ confidence level. The large volume and resulting small statistical errors on the power spectrum allow us to constrain both the amplitude and the scale dependence of the galaxy bias in cosmological fits. The statistical power of these data to constrain cosmology is ∼1.7 times better than previous clustering analyses. Varying the matter density and baryon fraction, we find ΩM= 0.30 ± 0.03, and Ωb/ΩM= 0.18 ± 0.04, for a fixed Hubble constant of 70 km s−1 Mpc−1 and a scale-invariant spectrum of initial perturbations. The detection of baryonic oscillations also allows us to measure the comoving distance to z= 0.5; we find a best-fitting distance of 1.73 ± 0.12 Gpc, corresponding to a 6.5 per cent error on the distance. These results demonstrate the ability to make precise clustering measurements with photometric surveys.