Other
Scientific paper
Jul 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9479s&link_type=abstract
HST Proposal ID #9479
Other
Hst Proposal Id #9479
Scientific paper
In cycle 5, we observed 10 globular clusters in the halo of M33 with HST/WFPC2. For each cluster, we have constructed VI color-magnitude diagrams {CMDs} that reach some 2 magnitudes below the horizontal branch {HB}. Although their mean metallicity is < ngleFe/H angle= -1.27 +/- 0.11, 80 possess completely red HB morphologies, much redder than comparable globular clusters in the halo of the Milky Way. Furthermore, these M33 halo globulars therefore suffer from the `second parameter effect' where another parameter in addition to metallicity is influencing the HB morphology. If interpreted in terms of age, this leads us to the surprising conclusion that the epoch of halo formation in M33 was significantly more extended as compared with the Milky Way. Of course, this conclusion is based only on the properties of the halo clusters in M33. As a result, we propose to investigate the properties of the halo field stars in M33. Our approach involves the construction of VI color-magnitude diagrams for 3 fields located at projected distances of 7 kpc, 8 kpc, and 9 kpc from the center of M33. From the color-magnitude diagrams, we will measure the mean metallicity, metallicity dispersion, and horizontal branch morphology of the field halo stars in M33. These properties will be compared with those of the M33 halo globular clusters as well as the halo populations of the Milky Way and M31.
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