ar X iv : a st ro - p h / 96 08 12 0 v 1 1 9 A ug 1 99 6 Photometry of GX 349 + 2 : Evidence for a 22 - hour Period

The intense galactic X-ray source GX 349+2 (Sco X-2) belongs to the class of persistently bright low-mass X-ray binaries called Z-sources. GX 349+2, although observed in X-rays for more than 30 years, has only recently been optically identified with a 19th mag star. Of the six known Z-sources, only two (Sco X-1 and Cyg X-2) have been studied in the optical. It has been suggested that Z-sources as a group are characterized by evolved companions and correspondingly long orbital periods (Sco X-1, P = 0.8 d; Cyg X-2, P = 9.8 d). Recently Southwell et al. (1996) have presented spectroscopic observations of GX 349+2 suggesting a 14 d orbital period. We have obtained broadband photometry of the system on six consecutive nights, and find a statistically significant 21.85 ± 0.4 h (3σ) period of 0.14 mag half-amplitude, superposed on erratic flickering typical of Sco X-1 type objects. As with other Z-sources, caution will be needed to insure that the variations are truly periodic, and not simply due to chaotic variability observed over a relatively short time span. Depending on the origin of the brightness variations, our proposed period could be either the orbital or half the orbital period. If our period is confirmed, then the nature of the 14 d spectroscopic variation found by Southwell et al. (1996) is unclear. There is evidence that the mass function of GX 349+2 is similar to that of Sco X-1. operated by AURA, Inc. under cooperative agreement with the NSF.