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Paper: A Journey across the M 33 Disk
Volume: 396, Formation and Evolution of Galaxy Disks
Page: 19
Authors: Corbelli, E.; Magrini, L.; Verley, S.
Abstract: The Local Group member M 33 is a pure disk galaxy bearing no prominent bulge or stellar halo. It constitutes a challenge for any hierarchical galaxy formation theory and an ideal laboratory for studying quiescent star formation. Using multiwavelength observations of the gas and stellar component in this nearby galaxy we are able to constrain the gas accretion and star formation history. In the centermost region we find kinematic evidence of a weak bar, which explains the central light excess and the enhanced metallicity. In the more extended disk the lack of strong gradients of metal and dust abundances supports the picture that the slow radial decline of the star formation rate is due to a change in the large scale disk perturbations: bright H II regions and giant molecular clouds being born only in the inner disk. The analysis of the infrared Spitzer maps has however revealed hundreds of low luminosity star forming sites in places with a variety of dust content. These are essential ingredients for understanding the overall gas to star formation process in M 33 and in more distant late type galaxies.
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