如何最佳地约束星系集合偏差：用细胞计数统计补充投影关联函数
How to Optimally Constrain Galaxy Assembly Bias: Supplement Projected Correlation Functions with Count-in-cells Statistics
摘要：
大多数关于星系及其晕之间联系的模型都忽略了星系性质可能与质量以外的晕性质相关的可能性，这种现象称为星系聚集偏差。然而，已知的是，这种相关性可能导致勘测数据的解释中的系统误差。目前，在真实的宇宙中，星系聚集偏差的程度可能存在，以及限制它的最佳策略仍然不确定。我们研究的能力，几个观测约束星系装配偏差的红移调查数据使用装饰晕占领分布（dHOD），经验模型的星系-晕连接，包括装配偏差。我们涵盖了广泛的一组观测，包括投影的两点关联函数$w_{\mathrm{p}}(r_{\mathrm{p}})$，星系-星系透镜信号$ΔΣ(r_{\mathrm{p}})$，空概率函数$\mathrm{VPF}(r)$，计数在圆柱$P(N_{\mathrm{CIC}})$的分布，和计数在环$P(N_{\mathrm{CIA}})$，和不同大小的圆柱$P(N_2/N_5)$的计数比的分布。我们发现，尽管经常使用的组合$w_{\mathrm{p}}(r_{\mathrm{p}})+ΔΣ(r_{\mathrm{p}})$在解释星系数据，计数统计，$P(N_{\mathrm{CIC}})$和$P(N_{\mathrm{CIA}})$，一般更有效地约束星系组装偏差时，结合$w_{\mathrm{p}}(r_{\mathrm{p}})$。基于$w_{\mathrm{p}}(r_{\mathrm{p}})$和$ΔΣ(r_{\mathrm{p}})$的约束在参数空间中共享共同的简并方向，而$w_{\mathrm{p}}(r_{\mathrm{p}})$与计数统计的组合更具互补性。因此，我们强烈建议在今后的星系晕联系研究中，应采用计数统计来补充正则观测量。
英文摘要：
Most models for the connection between galaxies and their haloes ignore the possibility that galaxy properties may be correlated with halo properties other than mass, a phenomenon known as galaxy assembly bias. Yet, it is known that such correlations can lead to systematic errors in the interpretation of survey data. At present, the degree to which galaxy assembly bias may be present in the real Universe, and the best strategies for constraining it remain uncertain. We study the ability of several observables to constrain galaxy assembly bias from redshift survey data using the decorated halo occupation distribution (dHOD), an empirical model of the galaxy--halo connection that incorporates assembly bias. We cover an expansive set of observables, including the projected two-point correlation function $w_{\mathrm{p}}(r_{\mathrm{p}})$, the galaxy--galaxy lensing signal $ΔΣ(r_{\mathrm{p}})$, the void probability function $\mathrm{VPF}(r)$, the distributions of counts-in-cylinders $P(N_{\mathrm{CIC}})$, and counts-in-annuli $P(N_{\mathrm{CIA}})$, and the distribution of the ratio of counts in cylinders of different sizes $P(N_2/N_5)$. We find that despite the frequent use of the combination $w_{\mathrm{p}}(r_{\mathrm{p}})+ΔΣ(r_{\mathrm{p}})$ in interpreting galaxy data, the count statistics, $P(N_{\mathrm{CIC}})$ and $P(N_{\mathrm{CIA}})$, are generally more efficient in constraining galaxy assembly bias when combined with $w_{\mathrm{p}}(r_{\mathrm{p}})$. Constraints based upon $w_{\mathrm{p}}(r_{\mathrm{p}})$ and $ΔΣ(r_{\mathrm{p}})$ share common degeneracy directions in the parameter space, while combinations of $w_{\mathrm{p}}(r_{\mathrm{p}})$ with the count statistics are more complementary. Therefore, we strongly suggest that count statistics should be used to complement the canonical observables in future studies of the galaxy--halo connection.
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