The SZ flux-mass ( Y – M ) relation at low-halo masses: improvements with symbolic regression and strong constraints on baryonic feedback
The SZ flux-mass ( Y – M ) relation at low-halo masses: improvements with symbolic regression and strong constraints on baryonic feedback
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低晕质量下的 SZ 通量-质量 ( Y – M ) 关系：符号回归的改进和重子反馈的强约束
DOI：
10.1093/mnras/stad1128
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发表时间：
2023
影响因子：
4.8
通讯作者：
Ho, Shirley
中科院分区：
文献类型：
--
作者：
Wadekar, Digvijay;Thiele, Leander;Hill, J. Colin;Pandey, Shivam;Villaescusa-Navarro, Francisco;Spergel, David N.;Cranmer, Miles;Nagai, Daisuke;Anglés-Alcázar, Daniel;Ho, Shirley
来自活动星系核和超新星的反馈会影响宇宙微波背景辐射测量中的晕积分Sunyaev-Zeldovich通量（YSZ），使其与晕质量（YSZ-M）的关系偏离维里定理的自相似幂律预测。我们使用CAMELS，一套流体动力学模拟与反馈处方的广泛变化，这样的偏差进行了全面的研究。我们使用两种机器学习工具（随机森林和符号回归）的组合来搜索Y-M关系的类似物，这些类似物对低质量的反馈过程更鲁棒（）;我们发现简单地在关系中添加Y →Y（1 +M*/Mgas）使其具有显著的自相似性。这可以作为一个强大的多波长质量代理低质量的集群和星系群。我们的方法也可以普遍有用，以提高其他天体物理标度关系的有效性域。我们还预测，测量theY-Mrelation可以提供百分之水平的约束反馈参数的某些组合和/或排除了当前最先进的流体动力学模拟中使用的超新星和活动星系核反馈模型的参数空间的主要部分。我们的结果可以使用即将到来的SZ调查（如SO，CMB-S4）和星系调查（如DESI和鲁宾）约束重子反馈的性质是有用的。最后，我们发现替代关系Y-M* 比Y-M提供了反馈的补充信息。
Feedback from active galactic nuclei (AGNs) and supernovae can affect measurements of integrated Sunyaev–Zeldovich (SZ) flux of haloes (YSZ) from cosmic microwave background (CMB) surveys, and cause its relation with the halo mass (YSZ–M) to deviate from the self-similar power-law prediction of the virial theorem. We perform a comprehensive study of such deviations using CAMELS, a suite of hydrodynamic simulations with extensive variations in feedback prescriptions. We use a combination of two machine learning tools (random forest and symbolic regression) to search for analogues of theY–Mrelation which are more robust to feedback processes for low masses (); we find that simply replacingY→Y(1 +M*/Mgas) in the relation makes it remarkably self-similar. This could serve as a robust multiwavelength mass proxy for low-mass clusters and galaxy groups. Our methodology can also be generally useful to improve the domain of validity of other astrophysical scaling relations. We also forecast that measurements of theY–Mrelation could provide per cent level constraints on certain combinations of feedback parameters and/or rule out a major part of the parameter space of supernova and AGN feedback models used in current state-of-the-art hydrodynamic simulations. Our results can be useful for using upcoming SZ surveys (e.g. SO, CMB-S4) and galaxy surveys (e.g. DESI and Rubin) to constrain the nature of baryonic feedback. Finally, we find that the alternative relation,Y–M*, provides complementary information on feedback thanY–M.