AI 中文总结
研究星系聚集偏差，通过将淬火邻域统计写成关联函数形式，测试其尺度依赖性，分离晕质量偏差和聚集偏差贡献，发现聚集偏差决定双晕星系一致性幅度，统计结构抑制非线性残差。
AI 中文摘要
双晕星系一致性常被视为星系聚集偏差的表现，但其统计结构和物理起源不明。本文旨在将淬火邻域统计写成关联函数形式，测试其尺度依赖性，分离晕质量偏差和聚集偏差贡献。利用IllustrisTNG300 - 1中z = 0的星系进行测量和分析，得出相关结论。
英文摘要
Two-halo galactic conformity is commonly interpreted as a manifestation of galaxy assembly bias, but its statistical structure and physical origin remain unclear. We aim to write the quenched-neighbour statistic in correlation-function form, test whether its scale dependence follows the linear matter correlation function $ξ_{\rm mm}^{\rm lin}(r)$, and separate the contributions of halo-mass bias and assembly bias to its amplitude. Using galaxies in IllustrisTNG300-1 at $z=0$, we measure the two-halo galactic conformity statistic of quenched neighbours at distance $r$, $Δf_{Q}(r)$, and related quantities in real space, compute the required correlations, perform shuffling tests at fixed halo mass, compare several $Δf$ observables, and explore the transformed family $G_n$. We show explicitly that $Δf_{Q}(r)$ can be written directly in terms of correlation functions and that, over $\sim 2$--$40\,h^{-1}\,\mathrm{Mpc}$, it is well described by $A_{\rm fit}\,ξ_{\rm mm}^{\rm lin}(r)$. Thus nonlinear and baryonic terms do not dominate the residual scale dependence isolated by this statistic. Halo-mass bias alone predicts lower amplitudes than measured, while fixed-mass shuffling strongly suppresses the signal; in TNG300 the amplitude is therefore dominated by galaxy assembly bias at fixed halo mass. Quenching, colour, and concentration share a common rescaled shape, whereas stellar-mass and halo-mass splits do not. These results suggest that galaxy assembly bias sets the amplitude of two-halo conformity, while the double-difference structure of the statistic suppresses nonlinear residuals when the compared populations have similar halo-mass and transition-scale structure.
CommentsLetter to the Editor -- Accepted for publication in A&A
