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SMART is a model to derive both star formation history and chemical evolution simultaneously from color-magnitude diagrams of resolved stars in a galaxy. We present current progress and discuss the prospects of SMART for the next decade.
We present a new numerical model of star formation history and chemical evolution using the color-magnitude diagrams of resolved stars in galaxies. Our model differs from previous models in that it generates the simulated color-magnitude diagrams with the metal enrichment law calculated from the galactic chemical evolution model. We present a case of applying our model to a resolved galaxy in the Local Group: the Sextans dwarf spheroidal galaxy. It is found the the primary origin of the radial gradient of stellar population in this galaxy is star formation followed by metallicity.
We report the discovery of three new star clusters in the halo of the Local Group dwarf irregular galaxy NGC 6822. These clusters were found in the deep images taken with the MegaPrime at the CFHT covering a total field of 2 deg $\times$ 2 deg. The most remote cluster is found to be located as far as 79 arcmin away from the center of NGC 6822. This distance is several times larger than the size of the region in NGC 6822 where star clusters were previously found. Morphological structures of the clusters and color-magnitude diagrams of the resolved stars in the clusters show that at least two of these clusters are proabably old globular clusters.
The Far-ultraviolet IMaging Spectrograph (FIMS) is a small spectrograph optimized for the observations of diffuse hot interstellar medium in far-ultraviolet wavebands (900–1150Å and 1335–1750Å). The instrument is expected to be sensitive to emission line fluxes an order of magnitude fainter than any previous missions. FIMS is currently under development and is scheduled for launch in 2002.
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