Structure Formation in the Universe
Structure Formation in the Universe
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DOI：
10.1007/978-94-017-1778-6_19
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发表时间：
2003
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通讯作者：
E. Gaztañaga
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作者：
E. Gaztañaga
我们报告了一次星系-类星体互相关ω的探测，这是斯隆数字天文测量早期数据发布的结果。我们将不同平均深度r‘=19−22(G=0.15−0.35)的星系样本与Q≃为1.6时的主要类星体群(I’Q<；19.2)进行了交叉关联。该信号在弧分尺度上的幅度约为10-20%。这比目前结构形成ACDM模型在弧分尺度上的预期大几倍，但更重要的是证实了几个小组之前的测量结果。这些观测结果可以与具有σ8≃1的平坦A宇宙相一致，只要在小(星团)尺度上的线性谱比在ACDM模型中更陡峭(n≃1)。星系分布在小尺度上呈反偏分布，b=0.1，在10Mpc/h时随尺度tb=1增大而增大。
We report a detection of galaxy-QSO cross-correlationωGQin the Sloan Digital Sky Survey (SDSS) Early Data Release (EDR). We cross-correlate galaxy samples of different mean depths r’ = 19−22 (G= 0.15−0.35) with the main QSO population (i’Q< 19.2) atQ≃ 1.6. The amplitude of the signal on arc-minute scales is about 10–20%. This is a few times larger than currently expected from structure formation ACDM models on arc-minute scales, but confirms, at a higher significance, previous measurements by several groups. The observations can be reconciled with flat A universe with σ8≃ 1 provided the linear spectrum is steeper (n≃ 1) than in the ACDM model on small (cluster) scales. The galaxy distribution are anti-bias withb =0.1 on small scales, increasing with scale tob =1 at 10 Mpc/h.