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

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

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.1416d&link_type=abstract

American Astronomical Society Meeting 208, #14.16; Bulletin of the American Astronomical Society, Vol. 38, p.95

Physics

Optics

Scientific paper

Images in L' (3.8µm) and M' (4.7µm), obtained with NIRI on the Gemini North telescope, are used to investigate the stellar content near the center of M31. The light distribution in the central arcsec differs from what is seen at 1 - 2.5µm in that P2 appears to have a bluer K-M' color than P1; no obvious signature of P3 is detected. It is demonstrated that these results can be explained if there is a source of thermal emission that contributes 20% of the peak M' light of P1, that is located between P1 and P2, and has a characteristic temperature of a few hundred K. The source of this emission is proposed to be a circumstellar dust shell surrounding a bright AGB star. A similar isolated source is also detected in M' roughly 8 arcsec from the center of the galaxy. Finally, a sample of unblended AGB stars outside of the nuclear region is defined using high angular resolution adaptive optics images. The (L', K-L') color-magnitude diagram of these sources shows a dominant AGB population with a peak L' brightness and a range of K-L' colors that are similar to those of the most luminous M giants in the Galactic bulge. Stars as bright as IRS 7 would easily be detected, and none are seen.

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