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R. M. Wagner (OSU and LBTO), J. Steinfadt (UCSB), H. E. Bond (STScI), E. Hooper (U. Texas), A. Karam (U. Arizona), J. Rohrbach (ASU), G. Schwarz (West Chester U.), S. Starrfield (ASU)
We report the results of optical photometry and spectroscopy of the bright classical nova and super-soft X-ray source V4743 Sgr during its outburst in 2003 and 2004. Time resolved photometric observations were obtained with a variety of telescopes including the SMARTS 1.3 m (2003 Apr and Jul), McDonald 2.7 m (2003 Aug and Sep), Bok 2.3 m (2003 Sep), and the Kuiper 1.6 m (2004 Jul). The data also include several nights of photometry obtained by members of VSNET during 2003 Jul as part of a coordinated campaign with the Chandra X-ray Observatory. Substantial changes in the light curves are evident during the decline phase. Timing analysis reveals the presence of a 0.2782 d period which is probably the orbital period of the binary system. A shorter period of 1419 s is also evident and might be related to the spin period of the white dwarf. Optical spectroscopy was obtained at the 6.5 m MMT, Bok, and 1.5 m SMARTS telescopes. The spectra are typical of a classical nova in decline but variations in the later spectra correlated with the photometric variations might also be present. RMW and SS acknowledge partial support from NSF and NASA grants to OSU and ASU respectively.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.