论文标题
低光晕质量的SZ Flux-Mass（$ y $ -M $）关系：符号回归和重大限制的改进，对重的反馈
The SZ flux-mass ($Y$-$M$) relation at low halo masses: improvements with symbolic regression and strong constraints on baryonic feedback
论文作者
论文摘要
Feedback from active galactic nuclei (AGN) and supernovae can affect measurements of integrated SZ flux of halos ($Y_\mathrm{SZ}$) from CMB surveys, and cause its relation with the halo mass ($Y_\mathrm{SZ}-M$) to deviate from the self-similar power-law prediction of the virial theorem.我们对使用骆驼，一套流体动力模拟的套件进行了全面的研究，这些偏差的反馈处方有很大差异。我们使用两个机器学习工具（随机森林和符号回归）的组合来搜索$ y-m $关系的类似物，这对低质量的反馈过程（$ m \ sillesim 10^{14} \，h^{ - h^{ - 1}} \，m_ \ odot $）;我们发现，仅替换$ y \ rightarrow y（1+m _*/m_ \ mathrm {gas}）$在关系中使其非常相似。这可以用作低质量簇和星系组的强大多波长质量代理。我们的方法通常对于提高其他天体分级关系的有效性领域通常也很有用。 我们还预测，$ y-m $关系的测量结果可以在反馈参数的某些组合和/或排除超新星参数空间的主要部分和AGN反馈模型中，以提供百分比级别的约束。我们的结果对于使用即将进行的SZ调查（例如，CMB-S4）和Galaxy Surveys（例如Desi和Rubin）来限制Baryonic反馈的性质。最后，我们发现一种替代关系$ y-m _*$提供了有关反馈的补充信息，而不是$ y-m $
Feedback from active galactic nuclei (AGN) and supernovae can affect measurements of integrated SZ flux of halos ($Y_\mathrm{SZ}$) from CMB surveys, and cause its relation with the halo mass ($Y_\mathrm{SZ}-M$) 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 the $Y-M$ relation which are more robust to feedback processes for low masses ($M\lesssim 10^{14}\, h^{-1} \, M_\odot$); we find that simply replacing $Y\rightarrow Y(1+M_*/M_\mathrm{gas})$ 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 the $Y-M$ relation could provide percent-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 an alternative relation, $Y-M_*$, provides complementary information on feedback than $Y-M$
