The Next Generation Virgo Cluster Survey. XXXIII. Stellar Population Gradients in the Virgo Cluster Core Globular Cluster System

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dc.contributor.authorKo, Youkyung
dc.contributor.authorPeng, Eric W.
dc.contributor.authorCote, Patrick
dc.contributor.authorFerrarese, Laura
dc.contributor.authorLiu, Chengze
dc.contributor.authorLongobardi, Alessia
dc.contributor.authorLancon, Ariane
dc.contributor.authorMunoz, Roberto P.
dc.contributor.authorPuzia, Thomas H.
dc.contributor.authorAlamo-Martinez, Karla A.
dc.contributor.authorSales, Laura, V
dc.contributor.authorRamos-Almendares, Felipe
dc.contributor.authorAbadi, Mario G.
dc.contributor.authorLee, Myung Gyoon
dc.contributor.authorHwang, Ho Seong
dc.contributor.authorCaldwell, Nelson
dc.contributor.authorBlakeslee, John P.
dc.contributor.authorBoselli, Alessandro
dc.contributor.authorCuillandre, Jean-Charles
dc.contributor.authorDuc, Pierre-Alain
dc.contributor.authorEyheramendy, Susana
dc.contributor.authorGuhathakurta, Puragra
dc.contributor.authorGwyn, Stephen
dc.contributor.authorJordan, Andres
dc.contributor.authorLim, Sungsoon
dc.contributor.authorSanchez-Janssen, Ruben
dc.contributor.authorToloba, Elisa
dc.date.accessioned2025-01-20T21:06:43Z
dc.date.available2025-01-20T21:06:43Z
dc.date.issued2022
dc.description.abstractWe present a study of the stellar populations of globular clusters (GCs) in the Virgo Cluster core with a homogeneous spectroscopic catalog of 692 GCs within a major-axis distance R (maj) = 840 kpc from M87. We investigate radial and azimuthal variations in the mean age, total metallicity, [Fe/H], and alpha-element abundance of blue (metal-poor) and red (metal-rich) GCs using their co-added spectra. We find that the blue GCs have a steep radial gradient in [Z/H] within R (maj) = 165 kpc, with roughly equal contributions from [Fe/H] and [alpha/Fe], and flat gradients beyond. By contrast, the red GCs show a much shallower gradient in [Z/H], which is entirely driven by [Fe/H]. We use GC-tagged Illustris simulations to demonstrate an accretion scenario where more massive satellites (with more metal- and alpha-rich GCs) sink further into the central galaxy than less massive ones, and where the gradient flattening occurs because of the low GC occupation fraction of low-mass dwarfs disrupted at larger distances. The dense environment around M87 may also cause the steep [alpha/Fe] gradient of the blue GCs, mirroring what is seen in the dwarf galaxy population. The progenitors of red GCs have a narrower mass range than those of blue GCs, which makes their gradients shallower. We also explore spatial inhomogeneity in GC abundances, finding that the red GCs to the northwest of M87 are slightly more metal-rich. Future observations of GC stellar population gradients will be useful diagnostics of halo merger histories.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ac63cf
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ac63cf
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93366
dc.identifier.wosidWOS:000804426000001
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleThe Next Generation Virgo Cluster Survey. XXXIII. Stellar Population Gradients in the Virgo Cluster Core Globular Cluster System
dc.typeartículo
dc.volumen931
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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