The stellar content of the bulge of M31

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dc.contributor.authorStephens, AW
dc.contributor.authorFrogel, JA
dc.contributor.authorDePoy, DL
dc.contributor.authorFreedman, W
dc.contributor.authorGallart, C
dc.contributor.authorJablonka, P
dc.contributor.authorRenzini, A
dc.contributor.authorRich, RM
dc.contributor.authorDavies, R
dc.date.accessioned2025-01-21T01:09:29Z
dc.date.available2025-01-21T01:09:29Z
dc.date.issued2003
dc.description.abstractWe analyze the stellar populations present in M31 by using nine sets of adjacent Hubble Space Telescope NICMOS camera 1 and 2 fields with galactocentric distances ranging from 2' to 20'. These infrared observations provide some of the highest spatial resolution measurements of M31 to date; our data place tight constraints on the maximum luminosities of stars in the bulge of M31. The tip of the red giant branch is clearly visible at M-bol similar to -3.8, and the tip of the asymptotic giant branch (AGB) extends to M-bol similar to -5. This AGB peak luminosity is significantly fainter than previously claimed; through direct comparisons and simulations we show that previous measurements were affected by image blending. We do observe field-to-field variations in the luminosity functions, but simulations show that these differences can be produced by blending in the higher surface brightness fields. We conclude that the red giant branch of the bulge of M31 is not measurably different from that of the bulge of the Milky Way. We also find an unusually high number of bright bluish stars (7.3 arcmin(-2)), which appear to be Galactic foreground stars.
dc.fuente.origenWOS
dc.identifier.issn0004-6256
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/96588
dc.identifier.wosidWOS:000182371800014
dc.issue.numero5
dc.language.isoen
dc.pagina.final2493
dc.pagina.inicio2473
dc.revistaAstronomical journal
dc.rightsacceso restringido
dc.subjectgalaxies : individual (M31=NGC 224)
dc.titleThe stellar content of the bulge of M31
dc.typeartículo
dc.volumen125
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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