The Central Regions of M31 in the 3 - 5 micron Wavelength Region

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dc.creatorDavidge, T. J.
dc.creatorJensen, Joseph B.
dc.creatorOlsen, K. A. G.
dc.date2006-04-28
dc.date.accessioned2026-07-07T11:25:33Z
dc.date.available2026-07-07T11:25:33Z
dc.descriptionImages obtained with NIRI on the Gemini North telescope are used to investigate the photometric properties of the central regions of M31 in the 3 - 5 micron wavelength range. The light distribution in the central arcsecond differs from what is seen in the near-infrared in the sense that the difference in peak brigh tness between P1 and P2 is larger in M' than in K'; no obvious signature of P3 is dete cted in M'. These results can be explained if there is a source of emission that contributes ~ 20% of the peak M' light of P1 and has an effective temperature of no more than a few hundred K that is located between P1 and P2. Based on the red K-M' color of this source, it is suggested that the emission originates in a circumstellar dust shell surrounding a single bright AGB star. A similar bright source that is ~ 8 arcsec from the center of the galaxy is also detected in M'. Finally, the (L', K-L') color-magnitude diagram of unblended stars shows a domin ant AGB population with photometric characteristics that are similar to those of the most luminous M giants in the Galactic bulge.
dc.descriptionTo appear in the Astronomical Journal
dc.identifierhttps://arxiv.org/abs/astro-ph/0605006
dc.identifierhttp://arxiv.org/abs/astro-ph/0605006
dc.identifierAstron.J.132:521-530,2006
dc.identifierdoi:10.1086/505463
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195541
dc.subjectAstrophysics
dc.titleThe Central Regions of M31 in the 3 - 5 micron Wavelength Region
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