星系团质量估计的Caustic技术的IllustrisTNG视角
An IllustrisTNG View of the Caustic Technique for Galaxy Cluster Mass Estimation
AI总结：
本文基于IllustrisTNG模拟数据，应用caustic技术估计星系团质量剖面，发现填充因子在宽径向范围内恒定且不受红移影响，校准后质量估计无偏，为大样本星系团质量测量提供了可靠的统计平台。
摘要：
IllustrisTNG模拟的TNG300-1运行包含1697个星系团，其$M_{200c}>10^{14}$M$_\odot$，红移范围为$0.01-1.04$。我们为这些星系团内的模拟星系构建了模拟光谱红移目录，并应用caustic技术来估计累积星系团质量剖面。我们从3D模拟数据中计算了真实的累积质量剖面，并计算了caustic质量与3D总质量的比率$\mathcal{F}_β$作为星系团中心距离的函数，从而确定了$\mathcal{F}_β$大致保持不变的径向范围。填充因子$\mathcal{F}_β=0.41\pm 0.08$在一个覆盖较宽星系团中心距离范围的平台上保持恒定，即$(0.6-4.2)R_{200c}$。该校准对红移不敏感。校准后的caustic质量剖面是无偏的，平均不确定度为$23\\%$。在$R_{200c}$处，平均$M^C/M^{3D}=1.03\pm 0.22$；在$2R_{200c}$处，平均$M^C/M^{3D}=1.02\pm 0.23$。模拟星系是质量分布的无偏示踪体。IllustrisTNG是一个广泛的统计平台，可将caustic技术应用于每个系统包含$\gtrsim 200$个成员星系的光谱红移大样本星系团。这些观测将允许与弱透镜质量进行广泛比较，并将补充其他测量宇宙结构增长率的技术。
英文摘要：
The TNG300-1 run of the IllustrisTNG simulations includes 1697 clusters of galaxies with $M_{200c}>10^{14}$M$_\odot$ covering the redshift range $0.01-1.04$. We build mock spectroscopic redshift catalogues of simulated galaxies within these clusters and apply the caustic technique to estimate the cumulative cluster mass profiles. We compute the total true cumulative mass profile from the 3D simulation data and calculate the ratio of caustic mass to total 3D mass, $\mathcal{F}_β$, as a function of cluster-centric distance and identify the radial range where $\mathcal{F}_β$ is roughly constant. The filling factor, $\mathcal{F}_β=0.41\pm 0.08$, is constant on a plateau that covers a wide cluster-centric distance range, $(0.6-4.2)R_{200c}$. This calibration is insensitive to redshift. The calibrated caustic mass profiles are unbiased, with an average uncertainty of $23\%$. At $R_{200c}$, the average $M^C/M^{3D}=1.03\pm 0.22$; at $2R_{200c}$, the average $M^C/M^{3D}=1.02\pm 0.23$. Simulated galaxies are unbiased tracers of the mass distribution. IllustrisTNG is a broad statistical platform for application of the caustic technique to large samples of clusters with spectroscopic redshifts for $\gtrsim 200$ members in each system. These observations will allow extensive comparisons with weak lensing masses and will complement other techniques for measuring the growth rate of structure in the universe.
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