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C. C. Venturini, R. J. Rudy, D. K. Lynch, S. Mazuk (The Aerospace Corporation), R. C. Puetter (UC San Diego), R. B. Perry (NASA Langley)
We present 0.4 - 2.5 micron spectrophotometry of the fast Nova Sagittarii 2004 (V5114 Sgr) observed on June 22, 2004 UT approximately 3 months after initial discovery. The data was taken on the 3-meter Shane Telescope at Lick Observatory using The Aerospace Corporation's Enhanced Near-Infrared and Visible Imaging Spectrograph. At this time, the nova was into its coronal phase exhibiting a broad range of excitation including a number of coronal lines. Lines present included: Balmer, Paschen, and Bracket lines with He I at 1.0830 microns being the strongest line in the whole spectrum, fluorescently excited O I lines, and coronal lines such as [S VIII] at 0.9911 microns, [Si IX] at 1.2517 microns, and [Si VI] at 1.9641 microns. The coronal line [S III] at 0.9069 and 0.9532 microns was present which is not typically seen in a fast nova. The line FWHM was approximately 2200 km/s and exhibited a unique combination of flat, double-peaked profiles for the lower excited lines and more round line profiles for the coronal lines.
The authors acknowledge the assistance of the Aerospace Corporation's Independent Research and Development program.
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.