Structure of the M33 nucleus

Details Structure of the M33 nucleus Structure of the M33 nucleus

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..101g&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 101-107. Research supported by the University of Illinois

Astronomy and Astrophysics

Astronomy

29

Astronomical Spectroscopy, Galactic Nuclei, Galactic Structure, Star Distribution, Absorption Spectra, Globular Clusters, Infrared Astronomy, Line Spectra, Mass To Light Ratios, Quantitative Analysis, Spatial Resolution, Spectral Resolution, Stellar Evolution, Visible Spectrum

Scientific paper

New optical and infrared observations of the M33 nucleus provide the basis for a quantitative structural analysis. The nucleus has been spatially resolved on a direct CCD image and is found to have FWHM approximately 0.8 in. (approximately 2 pc for D equals 900 kpc) and thus is similar in size to a typical globular cluster or the M31 nucleus. Sharp absorption lines are seen on a high resolution echelle spectrogram which indicates that the velocity dispersion is approximately equal to or less than 30 km/s. This value, in combination with the size and luminosity, leads to a low mass-to-light ratio of approximately 2-3. The M33 nucleus is therefore a very different type of object than high M/L, high mass density nuclei found in M31 and many luminous spirals. Spectroscopic and photometric evidence for a composite-age stellar population is presented, and it is suggested that growth of the M33 nucleus may be continuing as gas is fed in from the surrounding galactic disk.

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