QSO-LRG两点交叉关联函数与红移空间畸变
QSO-LRG 2-Point Cross-Correlation Function and Redshift-Space Distorions
摘要：
在固定的红移（z<1）下，通过将类星体与LRGs互相关，我们测量了类星体的偏差随类星体光度的变化，从而打破了类星体光度与红移之间的简并性。我们使用了来自2SLAQ、2 QZ和SDSS的三个类星体样本，覆盖了类星体绝对星等范围：-24.5< M_{b_J} <-21.5，并将它们与同样红移范围内的2SLAQ（z~0.5）和AAOmega（z~0.7）测光和分光LRG进行了互相关。2-D和3-D交叉聚类测量通常是一致的。我们的（2SLAQ）类星体LRG成簇幅度从半投影交叉关联函数测量的（r_0=6.8_{-0.3}^{+0.1}h^{-1}Mpc）看起来类似于（2SLAQ）LRG-LRG自关联幅度（r_0=7.45 \pm 0.35 h ^{-1}Mpc），均高于（2 QZ +2SLAQ）类星体-类星体振幅（r_0 \simeq 5.0 h ^{-1}Mpc）。我们的测量结果表明，非常小的类星体LRG交叉聚类依赖于类星体光度。如果有的话，结果意味着较亮的类星体可能比微弱的类星体的偏置程度低，这与简单的高峰值偏置模型所预期的方向相反。假设标准LCDM模型和从LRG自相关分析测量的b_{LRG}值，我们发现在M_{b_J} \approx-24时b_Q=1.45 \pm 0.11，在M_{b_J}-22时b_Q=1.90 \pm 0.16。我们还发现一致的结果，类星体偏差从z空间失真分析的类星体LRG交叉聚类在z~0.55。动力学计算结果给出β_Q=0.55 \pm 0.10，即b_Q=1.4 \pm 0.2。因此，z空间失真和振幅分析均在M_{b_J} ~-23处产生b_Q~1.5。在z~0.55处，类星体所居住的DM晕质量为\sim 10^{13}h^{-1} M_{\sun}，同样近似与类星体的光度无关。
英文摘要：
We have measured the bias of QSOs as a function of QSO luminosity at fixed redshift (z<1) by cross-correlating them with LRGs in the same spatial volume, hence breaking the degeneracy between QSO luminosity and redshift. We use three QSO samples from 2SLAQ, 2QZ and SDSS covering a QSO absolute magnitude range, -24.5<M_{b_J}<-21.5, and cross-correlate them with 2SLAQ (z~0.5) and AAOmega (z~0.7) photometric and spectroscopic LRGs in the same redshift ranges. The 2-D and 3-D cross-clustering measurements are generally in good agreement. Our (2SLAQ) QSO-LRG clustering amplitude (r_0=6.8_{-0.3}^{+0.1}h^{-1}Mpc) as measured from the semi-projected cross-correlation function appears similar to the (2SLAQ) LRG-LRG auto-correlation amplitude (r_0=7.45\pm0.35h^{-1}Mpc) and both are higher than the (2QZ+2SLAQ) QSO-QSO amplitude (r_0\simeq5.0h^{-1}Mpc). Our measurements show remarkably little QSO-LRG cross-clustering dependence on QSO luminosity. If anything, the results imply that brighter QSOs may be less highly biased than faint QSOs, the opposite direction expected from simple high peaks biasing models. Assuming a standard LCDM model and values for b_{LRG} measured from LRG autocorrelation analyses, we find b_Q=1.45\pm0.11 at M_{b_J}\approx-24 and b_Q=1.90\pm0.16 at M_{b_J}~-22. We also find consistent results for the QSO bias from a z-space distortion analysis of the QSO-LRG cross-clustering at z~0.55. The dynamical infall results give β_Q=0.55\pm0.10, implying b_Q=1.4\pm0.2. Thus both the z-space distortion and the amplitude analyses yield b_Q~1.5 at M_{b_J}~-23. The implied DM halo mass inhabited by QSOs at z~0.55 is \sim10^{13}h^{-1}M_{\sun}, again approximately independent of QSO luminosity.
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