Asymptotic giant branch stars in the central regions of M32

Details Asymptotic giant branch stars in the central regions of M32 Asymptotic giant branch stars in the central regions of M32

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...391l..13d&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 391, no. 1, May 20, 1992, p. L13-L16.

Astronomy and Astrophysics

Astrophysics

20

Asymptotic Giant Branch Stars, Elliptical Galaxies, Galactic Evolution, Infrared Imagery, Astronomical Photometry, Galactic Structure, Stellar Luminosity

Scientific paper

The paper discusses high-resolution (FWHM about 0.4 arcsec) near-infrared images of the central regions of the Local Group compact elliptical galaxy M32. The data are used to study the photometric properties of bright asymptotic giant branch stars in three annuli located within 30 arcsec of the galaxy center. The brightest AGB stars in each annulus occur near I about 19, and hence are roughly a magnitude brighter than the brightest stars in a field 2 arcmin from the galaxy center. The brightness of the AGB tip is similar to what is seen in galaxies which contain intermediate-age populations, strongly suggesting that an intermediate-age component is also present in the central regions of M32. The I luminosity function in each annulus follows a power law with logarithmic slope Delta log (n)/Delta I about 1.6 in the interval I between 19 and 20. There is also a tendency for the color of the ridge line of luminous giants to become bluer with increasing distance from the center of M32, suggesting that a metallicity gradient is present. Finally, it is noted that the presence of an intermediate-age population in the center of M32 suggests that the substructures which have been detected in the central regions of many galaxies may have formed during relatively recent epochs.

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