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首页> 外文期刊>The Astrophysical journal >DETECTION OF THE INTEGRATED SACHS-WOLFE AND SUNYAEV-ZELDOVICH EFFECTS FROM THE COSMIC MICROWAVE BACKGROUND-GALAXY CORRELATION
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DETECTION OF THE INTEGRATED SACHS-WOLFE AND SUNYAEV-ZELDOVICH EFFECTS FROM THE COSMIC MICROWAVE BACKGROUND-GALAXY CORRELATION

机译：从宇宙微波背景-银杏相关性检测萨克斯-沃尔夫和萨尼亚耶夫-泽维奇奇效应

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摘要

We present a cross-correlation analysis of the W ilkinson Microwave Anisotropy Probe cosmic microwave background (CMB) temperature anisotropies and the Sloan Digital Sky Survey galaxy density fluctuations. We find significant detections of the angular CMB-galaxy correlation for both a flux-limited galaxy sample (z ～0.3) and a high-redshift (z ～0.5) color-selected sample. The signal is compatible with that expected from the integrated Sachs-Wolfe (ISW) effect at large angles (θ> 4°) and the Sunyaev-Zeldovich (SZ) effect at small scales (θ< 1°). The detected correlation at low z is in good agreement with a previous analysis using the Automated Plate Measuring survey (z ～ 0.15). The combined analysis of all three samples yields a total significance of better than 3 σ for the ISW effect and of about 2.7 σ for the SZ effect, with a Compton parameter y approx= 10~(-6). For a given flat A cold dark matter model, the ISW effect depends on both the value of Ω_Λ and the galaxy bias b. To break this degeneracy, we estimate the bias using the ratio between the galaxy and mass autocorrelation functions in each sample. With our bias estimation, all samples consistently favor a best-fit dark-energy-dominated model: Ω_Λ approx= 0.8, with a 2 σ error Ω_Λ = 0.69-0.86.
机译：我们提出了Wilkinson微波各向异性探测器宇宙微波背景（CMB）温度各向异性和Sloan Digital Sky Survey星系密度波动的互相关分析。我们发现对通量受限星系样本（z〜0.3）和高红移（z〜0.5）选色样本的角CMB-星系相关性都有显着检测。该信号与大角度（θ> 4°）的集成Sachs-Wolfe（ISW）效果和小尺度（θ<1°）的Sunyaev-Zeldovich（SZ）效果预期的信号兼容。在低z处检测到的相关性与先前使用自动板测量调查（z〜0.15）进行的分析非常吻合。对这三个样品的综合分析得出，对于ISW效应，总显着性优于3σ;对于SZ效应，总显着性约为2.7σ，康普顿参数y大约为10〜（-6）。对于给定的平面A冷暗物质模型，ISW效应取决于Ω_Λ的值和星系偏差b。为了打破这种退化，我们使用每个样本中星系和质量自相关函数之间的比率来估计偏差。利用我们的偏差估计，所有样本始终都支持最适合暗能量控制的模型：Ω_Λ近似= 0.8，具有2σ误差Ω_Λ= 0.69-0.86。

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