The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the <i>M</i>.-<i>M</i> <sub>*</sub> Correlation

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dc.contributor.authorGonzalez-Lopezlira, Rosa A.
dc.contributor.authorLomeli-Nunez, Luis
dc.contributor.authorOrdenes-Briceno, Yasna
dc.contributor.authorLoinard, Laurent
dc.contributor.authorGwyn, Stephen
dc.contributor.authorAlamo-Martinez, Karla
dc.contributor.authorBruzual, Gustavo
dc.contributor.authorLancon, Ariane
dc.contributor.authorPuzia, Thomas H.
dc.date.accessioned2025-01-20T21:01:02Z
dc.date.available2025-01-20T21:01:02Z
dc.date.issued2022
dc.description.abstractD We continue to explore the relationship between the total number of globular clusters (GCs), NGC, and the central black hole mass, M alpha, in spiral galaxies. We present here results for the Sab galaxies NGC 3368, NGC 4736 (M94), and NGC 4826 (M64), and the Sm galaxy NGC 4395. The GC candidate selection is based on the (u* - i cent) versus (i cent - Ks) color-color diagram, and i cent-band shape parameters. We determine the M alpha versus NGC correlation for these spirals, plus NGC 4258, NGC 253, M104, M81, M31, and the Milky Way. We also redetermine the correlation for the elliptical sample in Harris et al., with updated galaxy types from Sahu et al. Additionally, we derive the total stellar galaxy mass, M*, from its two-slope correlation with NGC, and fit M _ versus M* for both spirals and ellipticals. We obtain log M alpha. (1.01 +/- 0.13) log NGC for ellipticals, and log M alpha. (1.64 +/- 0.24) log NGC for latetype galaxies (LTGs). The linear M alpha versus NGC correlation in ellipticals could be due to statistical convergence through mergers, unlike the much steeper correlation for LTGs. However, in the M alpha versus total stellar mass (M*) parameter space, with M* derived from its correlation with NGC, M alpha. (1.48 +/- 0.18) log M* for ellipticals, and M alpha. (1.21 +/- 0.16) log M* for LTGs. The observed agreement between ellipticals and LTGs in this parameter space may imply that black holes and galaxies coevolve through calm accretion, active galactic nuclei feedback, and other secular processes.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ac982e
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ac982e
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/92808
dc.identifier.wosidWOS:000898256400001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleThe Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the <i>M</i>.-<i>M</i> <sub>*</sub> Correlation
dc.typeartículo
dc.volumen941
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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