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CFHT Wide-Field Deep Imaging of M33

Published online by Cambridge University Press:  25 May 2016

J.-C. Cuillandre ,
J. Lequeux  and
L. Loinard
J.-C. Cuillandre
Affiliation:
Canada-France-Hawaii Telescope Corporation, PO Box 1597, Kamuela, HI 96743, USA
J. Lequeux
Affiliation:
Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France
L. Loinard
Affiliation:
IRAM, 300 Rue de la Piscine, Domaine Universitaire, 38406 St Martin d'Hères Cedex, France

Abstract

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28′ x 28′ deep V- and I-band images of the center and of the SE field of M33 have been obtained at the prime focus of the Canada-France-Hawaii 3.6m telescope. They allowed to map separately the young blue stars, the red supergiants, the red giants and the extreme AGB stars. The disk as traced by red giants has a surprisingly sharp edge. The young blue stars trace the spiral structure very well, but the detailed comparison with H I and CO maps does not show a very good correspondence. The simple spiral-shock model of star formation proposed for the South arm of M33 is not confirmed. On the edge of the galaxy, star formation starts at a column density of H I of about 3 x 1020 atom cm−2. The colour-magnitude diagram for the halo stars shows a broadened red giant branch with a mean metallicity [Fe/H] ≃ −1.0. The shape of the red giant branch confirms the distance modulus of 24.82±0.20 for M33.

Type
Part 2: The Database
Information
Symposium - International Astronomical Union , Volume 192: The Stellar Content of Local Group Galaxies , 1999 , pp. 185 - 194
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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