On the Classification of V3798 Sgr

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V3798 Sgr was first classified as an RV Tau variable (Hoffleit 1972). However Springob et al. (1998) suggested that it could be an UXOR - a star with sporadic drops of brightness. We studied the past brightness of the star using the Harvard plates from 1895 to 1949. In addition, the star was monitored in BVRI with a CCD camera on the MMO's 24” telescope in 2007. Sporadic drops of brightness were confirmed, up to 1.3 magnitudes, within a broad range of time scales - from a month to an hour. No periodicity was detected. Observations with the FOSC spectrometer on the 1-m telescope of the Tel-Aviv U. Wise Observatory in 1999 and with the FAST spectrometer on the Tillinghast 1.5-m telescope at Whipple Observatory in 2007 showed a typical early A absorption line spectrum with variable narrow emission in the cores of Hα and other absorption lines. A dramatic emission line flare was observed on September 19, 2007, with an increase of Hα equivalent width by a factor of 4 relative to the previous observation, five nights before. No continuum photometry is available for September 19 but the brightness in R two days before and one day after that date differ by only 0.07 magnitude. A closer synchronism of spectroscopy and photometry is needed to verify the lack of correlation between the variations of the emission lines and continuum. So far, the lack of periodicity and an early spectral type seem to disprove the classification of V3798 Sgr as an RV Tau star and support the hypothesis that it is an UXOR. We thank A. Doane for help with measuring the plates and P. Berlind, M. Calkins and O. Shemmer for taking the spectra. This project was supported by the NSF/REU grant AST-0354056 and the Nantucket Maria Mitchell Association.

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