wiki:notes
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wiki:notes [2024/09/10 23:35] Cheng Li |
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| * The radial surface brightness profile of the BCG+ICL is best described by a double Sérsic model, with 68±4% of the H_E-band light contained in the extended, outer component. The transition between these components occurs at ≈50 kpc, beyond which the isophotes become increasingly elliptical and off-centered.The BCG+ICL colour becomes increasingly blue with radius, consistent with the stellar populations in the ICL having subsolar metallicities [Fe/H] ∼ −0.6. The colour of the ICL, and the specific frequency and luminosity function of the ICGCs suggest that the ICL+ICGCs were tidally stripped from the outskirts of massive satellites with masses of a few ×10^10 M⊙, with an increasing contribution from dwarf galaxies at large radii. | * The radial surface brightness profile of the BCG+ICL is best described by a double Sérsic model, with 68±4% of the H_E-band light contained in the extended, outer component. The transition between these components occurs at ≈50 kpc, beyond which the isophotes become increasingly elliptical and off-centered.The BCG+ICL colour becomes increasingly blue with radius, consistent with the stellar populations in the ICL having subsolar metallicities [Fe/H] ∼ −0.6. The colour of the ICL, and the specific frequency and luminosity function of the ICGCs suggest that the ICL+ICGCs were tidally stripped from the outskirts of massive satellites with masses of a few ×10^10 M⊙, with an increasing contribution from dwarf galaxies at large radii. | ||
| + | === Simulations === | ||
| + | * Horizon-AGN simulation: https://arxiv.org/abs/2409.10607 | ||
| + | * Satellite stripping, mergers, and pre-processing are all found to make significant contributions to the ICL, but any contribution from in-situ star-formation directly into the ICL appears negligible. | ||
| + | * ~90% of the stacked ICL that is not pre-processed should come from galaxies infalling with stellar masses above 10^9 M_⊙, with roughly half coming from infalling galaxies with stellar masses within half a dex of 10^11 M_⊙. The fact that the ICL appears largely sourced from such massive objects suggests that the ICL assembly of any individual cluster may be principally stochastic. | ||
| + | * | ||
| ==== Globular Clusters ==== | ==== Globular Clusters ==== | ||
wiki/notes.1726011314.txt.gz · Last modified: 2024/09/10 23:35 by Cheng Li
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