Preparing for low surface brightness science with the Vera C. Rubin Observatory: a comparison of observable and simulated intracluster light fractions

ABSTRACT 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 (...

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Published in:Monthly notices of the Royal Astronomical Society 2024-01, Vol.528 (1), p.771-795
Main Authors: Brough, Sarah, Ahad, Syeda Lammim, Bahé, Yannick M, Ellien, Amaël, Gonzalez, Anthony H, Jiménez-Teja, Yolanda, Kimmig, Lucas C, Martin, Garreth, Martínez-Lombilla, Cristina, Montes, Mireia, Pillepich, Annalisa, Ragusa, Rossella, Remus, Rhea-Silvia, Collins, Chris A, Knapen, Johan H, Mihos, J Christopher
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container_title Monthly notices of the Royal Astronomical Society
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creator Brough, Sarah
Ahad, Syeda Lammim
Bahé, Yannick M
Ellien, Amaël
Gonzalez, Anthony H
Jiménez-Teja, Yolanda
Kimmig, Lucas C
Martin, Garreth
Martínez-Lombilla, Cristina
Montes, Mireia
Pillepich, Annalisa
Ragusa, Rossella
Remus, Rhea-Silvia
Collins, Chris A
Knapen, Johan H
Mihos, J Christopher
description ABSTRACT 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
doi_str_mv 10.1093/mnras/stad3810
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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 &lt;log10M200c/M⊙ &lt; 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. 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title 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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