The bulge/halo luminosity of M33 and its globular cluster population

Details The bulge/halo luminosity of M33 and its globular cluster population The bulge/halo luminosity of M33 and its globular cluster population

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....103..104b&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 103, Jan. 1992, p. 104-109.

Astronomy and Astrophysics

Astronomy

35

Galactic Bulge, Galactic Structure, Globular Clusters, Halos, Luminosity, Spiral Galaxies, Astronomical Photometry, Brightness Distribution, Charge Coupled Devices, Disk Galaxies

Scientific paper

The method of surface photometry using blue and 12-micron images was used to constrain the luminosity of the bulge component in M33. In both bondpasses, the bulge was constrained to be not brighter than Mv = -15.0, assuming a distance to M33 of 800 kpc. However, the observed blue colors and the high CO intensity in the interior regions of M33 argue against the existence of any bulge in the classical sense. In view of the report of Schommer et al. (1991), who have shown that M33 has a significant population of old globular clusters that are distributed in a kinematic halo, it is suggested that M33 is an example of disk galaxy formation which can produce globular clusters without the requisite bulge population.

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