Preparing for low surface brightness science with the Vera C. Rubin Observatory: a comparison of observable and simulated intracluster light fractions
Preparing for low surface brightness science with the Vera C. Rubin Observatory: a comparison of observable and simulated intracluster light fractions
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与 Vera C. Rubin 天文台一起为低表面亮度科学做准备：可观测和模拟的星团内光分数的比较
DOI：
10.1093/mnras/stad3810
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发表时间：
2024
影响因子：
4.8
通讯作者：
Brough S
中科院分区：
文献类型：
--
作者：
Brough S
星系团内光（ICL）提供了星系团相互作用的重要记录。然而，我们的理解受限于我们的测量方法。为了解决这个问题，我们使用观测方法（表面亮度阈值- sb、非参数测量- np、复合模型- cm和多星系拟合- mgf）和正在开发的新方法（小波分解- wd）测量了最亮星团星系和ICL （BCG+ICL分数）和ICL单独（ICL分数）中包含的星团光的比例，这些方法应用于来自四个宇宙流体动力学模拟的61个星团（14 <log10M200c/M⊙< 14.5）的模拟图像。我们比较了观测测量的BCG+ICL和ICL分数与使用模拟测量（孔径和运动分离）的分数。运动分离测得的ICL分数明显大于观察到的分数。我们发现测量是相关的，并提供了从观察到的分数估计运动ICL分数的方程。不同的观测技术给出了一致的BCG+ICL和ICL分数，但与孔径模拟测量相比，有低估BCG+ICL和ICL分数的倾向。比较不同的方法和算法，我们发现MGF算法与模拟结果最一致，CM和SB方法分别对BCG+ICL和ICL分数的投影效果最小。Ahad (CM)， MGF和WD算法最好设置为处理较大的样本；然而，当前形式的WD算法容易受到投影效应的影响。我们建议探索使用这些方法的新算法来分析鲁宾天文台的空间和时间遗产调查将提供的大量样本。
Intracluster light (ICL) provides an important record of the interactions galaxy clusters have undergone. However, we are limited in our understanding by our measurement methods. To address this, we measure the fraction of cluster light that is held in the Brightest Cluster Galaxy and ICL (BCG+ICL fraction) and the ICL alone (ICL fraction) using observational methods (surface brightness threshold-SB, non-parametric measure-NP, composite models-CM, and multi-galaxy fitting-MGF) and new approaches under development (wavelet decomposition-WD) applied to mock images of 61 galaxy clusters (14 <log10M200c/M⊙< 14.5) from four cosmological hydrodynamical simulations. We compare the BCG+ICL and ICL fractions from observational measures with those using simulated measures (aperture and kinematic separations). The ICL fractions measured by kinematic separation are significantly larger than observed fractions. We find the measurements are related and provide equations to estimate kinematic ICL fractions from observed fractions. The different observational techniques give consistent BCG+ICL and ICL fractions but are biased to underestimating the BCG+ICL and ICL fractions when compared with aperture simulation measures. Comparing the different methods and algorithms, we find that the MGF algorithm is most consistent with the simulations, and CM and SB methods show the smallest projection effects for the BCG+ICL and ICL fractions, respectively. The Ahad (CM), MGF, and WD algorithms are best set up to process larger samples; however, the WD algorithm in its current form is susceptible to projection effects. We recommend that new algorithms using these methods are explored to analyse the massive samples that Rubin Observatory’s Legacy Survey of Space and Time will provide.