Distribution of Merging and Post-merger Galaxies in Nearby Galaxy Clusters

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dc.contributor.authorKim, Duho
dc.contributor.authorSheen, Yun-Kyeong
dc.contributor.authorJaffe, Yara L.
dc.contributor.authorKelkar, Kshitija
dc.contributor.authorRanjan, Adarsh
dc.contributor.authorPiraino-Cerda, Franco
dc.contributor.authorCrossett, Jacob P.
dc.contributor.authorLourenco, Ana Carolina Costa
dc.contributor.authorMartin, Garreth
dc.contributor.authorNantais, Julie B.
dc.contributor.authorDemarco, Ricardo
dc.contributor.authorTreister, Ezequiel
dc.contributor.authorYi, Sukyoung K.
dc.date.accessioned2025-01-20T17:05:29Z
dc.date.available2025-01-20T17:05:29Z
dc.date.issued2024
dc.description.abstractWe study the incidence and spatial distribution of galaxies that are currently undergoing gravitational merging (M) or that have signs of being post-merger (PM) in six galaxy clusters (A754, A2399, A2670, A3558, A3562, and A3716) within the redshift range of 0.05 less than or similar to z less than or similar to 0.08. To this aim, we obtained Dark Energy Camera mosaics in the u ' , g ' , and r ' bands covering up to 3 x R 200 of the clusters, reaching 28 mag arcsec-2 surface brightness limits. We visually inspect u ' g ' r ' color-composite images of volume-limited (M r < -20) cluster member galaxies to identify whether galaxies are of M or PM type. We find 4% M-type and 7% PM-type galaxies in the galaxy clusters studied. By adding spectroscopic data and studying the projected phase-space diagram (PPSD) of the projected clustocentric radius and the line-of-sight velocity, we find that PM-type galaxies are more virialized than M-type galaxies, having a 1%-5% higher fraction within the escape-velocity region, while the fraction of M-type was similar to 10% higher than the PM type in the intermediate environment. Similarly, on a substructure analysis, M types were found in groups in the outskirts, while PM-type populated groups were found in ubiquitous regions of the PPSD. Adopting literature-derived dynamical state indicator values, we observed a higher abundance of M types in dynamically relaxed clusters. This finding suggests that galaxies displaying post-merger features within clusters likely merged in low-velocity environments, including clusters outskirts and dynamically relaxed clusters.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ad32ce
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ad32ce
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90711
dc.identifier.wosidWOS:001211488700001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleDistribution of Merging and Post-merger Galaxies in Nearby Galaxy Clusters
dc.typeartículo
dc.volumen966
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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