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arXiv 2305.00992astro-ph.CO
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利用MillenniumTNG解释Sunyaev-Zel'dovich观测：质量与环境标度关系

Interpreting Sunyaev-Zel'dovich observations with MillenniumTNG: Mass and environment scaling relations

Boryana Hadzhiyska, Simone Ferraro, Rüdiger Pakmor, Sownak Bose, Ana Maria Delgado, César Hernández-Aguayo, Rahul Kannan, Volker Springel, Simon D. M. White, Lars Hernquist

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14 pages, 6 figures
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AI总结：

本研究利用MillenniumTNG流体模拟解释SZ观测，分析CAP滤波器去视线贡献、kSZτ信号分布特征，拟合Y-M与τ-M标度关系并量化亚网格物理、环境及星系示踪的偏差影响。

摘要：

未来几年，Sunyaev-Zel'dovich（SZ）测量可极大提升我们对星系际介质（IGM）及反馈过程在星系形成中作用的理解，使我们能够校准弱引力透镜星系成团巡天宇宙学限制中的重要天体物理系统误差。然而，该信号仅能通过二维投影测量，其正确解读除了需要理解气体与底层物质分布的关系外，还依赖于对可观测物理量与气体内在固有属性之间关联的认知。应对这些挑战的一种方法是使用流体动力学模拟，例如高分辨率、大体积的MillenniumTNG模拟套件。我们发现，光学深度$τ$和康普顿y参数$Y$的测量存在显著的视线方向贡献，可通过应用补偿孔径光度测量（CAP）滤波器有效去除。与其他$τ$探测手段（如X射线和快速射电暴）相比，由运动学SZ效应（kSZ）推断的$τ$的信号主要来自暗晕周围的受限圆柱区域，这是由沿视线方向的速度去相关效应导致的。此外，我们对$Y-M$和$τ-M$标度关系进行了拟合，并采用平滑折断幂律（SBPL）形式给出了最佳拟合参数。我们注意到，对于中等质量暗晕（约$10^{13} \rm M_{\rm \bigodot}$），亚网格物理建模可使这些参数的误差范围扩大30%。标度关系的弥散可通过对浓度的内在依赖，以及对潮汐剪切的外在依赖来解释。最后，我们讨论了实际观测中使用星系而非暗晕的影响，这可能使$L_\rm \bigast$星系的推断SZ轮廓产生约20%的偏差。

英文摘要：

In the coming years, Sunyaev-Zel'dovich (SZ) measurements can dramatically improve our understanding of the Intergalactic Medium (IGM) and the role of feedback processes on galaxy formation, allowing us to calibrate important astrophysical systematics in cosmological constraints from weak lensing galaxy clustering surveys. However, the signal is only measured in a two-dimensional projection, and its correct interpretation relies on understanding the connection between observable quantities and the underlying intrinsic properties of the gas, in addition to the relation between the gas and the underlying matter distribution. One way to address these challenges is through the use of hydrodynamical simulations such as the high-resolution, large-volume MillenniumTNG suite. We find that measurements of the optical depth, $τ$, and the Compton-y parameter, $Y$, receive large line-of-sight contributions which can be removed effectively by applying a Compensated Aperture Photometry (CAP) filter. In contrast with other $τ$ probes (e.g., X-rays and Fast Radio Bursts), the kSZ-inferred $τ$ receives most of its signal from a confined cylindrical region around the halo due to the velocity decorrelation along the line-of-sight. Additionally, we perform fits to the $Y-M$ and $τ-M$ scaling relations and report best-fit parameters adopting the smoothly broken power law (SBPL) formalism. We note that subgrid physics modeling can broaden the error bar on these by 30\% for intermediate-mass halos ($\sim$$10^{13} \, {\rm M}_{\odot}$). The scatter of the scaling relations can be captured by an intrinsic dependence on concentration, and an extrinsic dependence on tidal shear. Finally, we comment on the effect of using galaxies rather than halos in real observations, which can bias the inferred SZ profiles by $\sim$20\% for $L_\ast$-galaxies.

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