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Brightest Cluster Galaxies and the Intracluster Light
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In this chapter, we delve into the formation and primary characteristics of two significant components within galaxy clusters: the brightest cluster galaxies (BCGs) and the intracluster light (ICL). Drawing upon recent and pertinent studies in the field, we explore the mechanisms driving their growth from high redshift to the present day, i.e., mergers and stellar stripping. Mergers between satellite galaxies and the BCGs account for a significant amount of ICL, as well as stellar stripping which is responsible for the formation of the bulk of it. We also examine how these formation mechanisms are intertwined with the dynamical state of their host clusters, suggesting their potential utility as luminous tracers of dark matter.
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Cited by 4 Pith papers
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On the Separation Between the Brightest Cluster Galaxy and the Intracluster Light
The optimal BCG–ICL separation aperture is about 4.5% of the virial radius, with only a weak dependence on halo mass and redshift.
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The Role of Cluster Environments in Quiescent Galaxy Stellar Halo Assembly
High-mass quiescent galaxies in clusters assemble more luminous stellar halos than field galaxies while low-mass cluster galaxies assemble less luminous ones over 0.1 < z < 1.
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On the Origin of Intracluster Light based on the High-resolution Simulation, NewCluster
In a high-resolution cluster simulation, most intracluster-light stars come from satellite galaxies, and stars stripped before cluster infall are old, metal-poor, alpha-enhanced and trace dark matter.
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Deep view of the intracluster light in the Coma cluster of galaxies
A deep image of Coma's intracluster light traces it to roughly 1.5 Mpc, measures ICL fractions near 20 percent in the g and r bands, and reveals a faint stellar bridge to the galaxy NGC 4839.
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