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Narrow-band classification photometry, on a six-color system that measures near-infrared bands of TiO and CN, has been obtained for a set of red supergiants in the Small Magellanic Cloud. To investigate the effects of metallicity on the band-strength indices, comparisons are made to supergiants in the LMC and the Galaxy. Two new variable stars are reported.
We describe a program of determining proper motions from digitized scans of Palomar Oschin Schmidt telescope plates at the Space Telescope Science Institute. Our method is most useful over 11 ≲ V ≲ 18 and .
We describe a long term project to find faint, heavily-reddened, cool supergiants and carbon stars and to classify IRAS Point Sources within 6° of the southern galactic plane. Many new supergiants and carbon stars have been found, and thousands of IRAS Point Sources have had their spectral types determined.
The combination of the excellent large-field imaging capabilities of Schmidt telescopes and of prisms covering the full aperture has made an impact on stellar, galactic, and extragalactic astronomy far out of proportion to the numbers of such telescopes. I discuss some of the milestones in the continuing development of this combination with a view to signposts of the future.
We are acquiring a large-area sample of faint, high-latitude carbon star candidates for the study of halo dynamics by using an intermediate-band color system with CCDs in efficient survey modes. Except for one odd dwarf carbon (C) star, G77-61, it has long been assumed that these faint C stars are distant giants. However, we recently demonstrated that three more faint C stars are high proper motion objects, and therefore dwarfs. Now we are completing a proper motion survey of known faint high-latitude C stars to search for additional C dwarfs. The CCD and proper motion surveys together will place significant limits on the space density of C stars, be they dwarfs or giants.
Of the more than 100 symbiotic stars now known in our Galaxy, only two have previously been reported to contain carbon stars as their cool components. We here present observations of a third such object, which we wish to call Weaver’s star since Weaver (1972) first identified it as a symbiotic.
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