BUDDI-MaNGA II: the star-formation histories of bulges and discs of S0s

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dc.contributor.authorJohnston, Evelyn J.
dc.contributor.authorHaussler, Boris
dc.contributor.authorJegatheesan, Keerthana
dc.contributor.authorFraser-McKelvie, Amelia
dc.contributor.authorCoccato, Lodovico
dc.contributor.authorCortesi, Arianna
dc.contributor.authorJaffe, Yara
dc.contributor.authorGalaz, Gaspar
dc.contributor.authorMora, Marcelo
dc.contributor.authorOrdenes-Briceno, Yasna
dc.date.accessioned2024-01-10T13:10:39Z
dc.date.available2024-01-10T13:10:39Z
dc.date.issued2022
dc.description.abstractMany processes have been proposed to explain the quenching of star formation in spiral galaxies and their transformation into S0s. These processes affect the bulge and disc in different ways, and so by isolating the bulge and disc spectra, we can look for these characteristic signatures. In this work, we used BUDDI to cleanly extract the spectra of the bulges and discs of 78 S0 galaxies in the MaNGA Survey. We compared the luminosity and mass weighted stellar populations of the bulges and discs, finding that bulges are generally older and more metal rich than their discs. When considering the mass and environment of each galaxy, we found that the galaxy stellar mass plays a more significant role on the formation of the bulges. Bulges in galaxies with masses >= 10(10) M-circle dot built up the majority of their mass rapidly early in their lifetimes, while those in lower mass galaxies formed over more extended time-scales and more recently. No clear difference was found in the formation or quenching processes of the discs as a function of galaxy environment. We conclude that more massive S0 galaxies formed through an inside-out scenario, where the bulge formed first and evolved passively while the disc underwent a more extended period of star formation. In lower mass S0s, the bulges and discs either formed together from the same material, or through an outside-in scenario. Our results therefore imply multiple formation mechanisms for S0 galaxies, the pathway of which is chiefly determined by a galaxy's current stellar mass.
dc.fechaingreso.objetodigital2024-05-02
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stac1447
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stac1447
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77904
dc.identifier.wosidWOS:000825725300016
dc.information.autorucFacultad de Física; Galaz Lladser, Gaspar; S/I; 1000955
dc.issue.numero4
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final6156
dc.pagina.inicio6141
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectgalaxies: bulges
dc.subjectgalaxies: disc
dc.subjectgalaxies: elliptical and lenticular, cD
dc.subjectgalaxies: evolution
dc.titleBUDDI-MaNGA II: the star-formation histories of bulges and discs of S0s
dc.typeartículo
dc.volumen514
sipa.codpersvinculados1000955
sipa.indexWOS
sipa.trazabilidadCarga SIPA;09-01-2024
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