论文标题
与3D光晕质量相比，星系簇孔径对重型效应更强大
Galaxy cluster aperture masses are more robust to baryonic effects than 3D halo masses
论文作者
论文摘要
星系簇的质量测量中的系统不确定性限制了未来调查的宇宙学限制能力，该调查将检测到$ 10^5 $簇。以前，我们认为可以比3D质量更准确，更精确地推断出孔径，而不会损失宇宙学约束功率。在这里，我们使用大型系统（巴哈马）宇宙学，流体动力学模拟的重子和光环，以表明光圈质量对星系形成过程引起的质量变化也不太敏感。对于带有$ M_ \ MATHRM {200M，DMO}> 10^{14} \，H^{ - 1} \，\ Mathrm {M Mathrm {M} _ \ odot $的光环，由其3D晕质量质量影响量的halo sapers and ape rabor ape radia，haro sape and to aper sap rado s ape ragion sap rado s ape radius a ap ape ragion ape ragion， $ \ 3 \，\％$。对于低质量光环，$ 10^{13.5} <m_ \ mathrm {200m，dmo} /（h^{ - 1} \，\ Mathrm {m} _ \ odot）<10^{14} $在弱透镜观测值中，孔径质量始终降低（$ \ lyssim 5 \，\％$），而不是3D halo质量（$ \ sillsim 10 \，\％$ for $ m_ \ mathrm {200m {200m} $）。光晕质量减少仅略微演变，最高$ 2 $百分比，在孔径质量和$ m_ \ mathrm {200m} $的红移0.25和1之间。 Varying the strength of the simulated feedback so the mean simulated hot gas fraction covers the observed scatter inferred from X-ray observations, we find that the aperture mass is consistently less biased than the 3D halo mass, by up to $2 \, $ percentage points at $m_\mathrm{200m,dmo} = 10^{14} \, h^{-1} \, \ Mathrm {M} _ \ odot $。因此，簇孔径的质量校准为将来的集群调查提供了一条富有成果的途径，以降低其对系统不确定性的敏感性。
Systematic uncertainties in the mass measurement of galaxy clusters limit the cosmological constraining power of future surveys that will detect more than $10^5$ clusters. Previously, we argued that aperture masses can be inferred more accurately and precisely than 3D masses without loss of cosmological constraining power. Here, we use the Baryons and Haloes of Massive Systems (BAHAMAS) cosmological, hydrodynamical simulations to show that aperture masses are also less sensitive to changes in mass caused by galaxy formation processes. For haloes with $m_\mathrm{200m,dmo} > 10^{14} \, h^{-1} \, \mathrm{M}_\odot$, binned by their 3D halo mass, baryonic physics affects aperture masses and 3D halo masses similarly when measured within apertures similar to the halo virial radius, reaching a maximum reduction of $\approx 3 \, \%$. For lower-mass haloes, $10^{13.5} < m_\mathrm{200m,dmo} / (h^{-1} \, \mathrm{M}_\odot) < 10^{14}$, and aperture sizes $\sim 1 \, h^{-1} \, \mathrm{cMpc}$, representative of weak lensing observations, the aperture mass is consistently reduced less ($\lesssim 5 \, \%$) than the 3D halo mass ($\lesssim 10 \, \%$ for $m_\mathrm{200m}$). The halo mass reduction evolves only slightly, by up to $2$ percentage points, between redshift 0.25 and 1 for both the aperture mass and $m_\mathrm{200m}$. Varying the strength of the simulated feedback so the mean simulated hot gas fraction covers the observed scatter inferred from X-ray observations, we find that the aperture mass is consistently less biased than the 3D halo mass, by up to $2 \, $ percentage points at $m_\mathrm{200m,dmo} = 10^{14} \, h^{-1} \, \mathrm{M}_\odot$. Therefore, cluster aperture mass calibrations provide a fruitful path forward for future cluster surveys to reduce their sensitivity to systematic uncertainties.
