AAS 205th Meeting, 9-13 January 2005
Session 19 Cataclysmic Variable Stars
Poster, Monday, January 10, 2005, 9:20am-6:30pm, Exhibit Hall

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[19.20] 0.4-2.5 Micron Spectrophotometry of the Fe II Novae V5113 Sagittarii and V2574 Ophiuchi

R. J. Rudy, D. K. Lynch, S. M. Mazuk, C. C. Venturini (Aerospace Corp.), R. C. Puetter (UCSD), R. B. Perry (NASA Langley)

We present simultaneous optical and IR spectrophotometry of two Fe II type novae at different stages of their developments. Measurements of V2574 Oph (Nova Oph 2004) and V5113 Sgr (Nova Sgr 2003 No. 2) were acquired 2004 June 23 and June 24 UT, respectively, using The Aerospace Corporation's Near-Infrared and Visible Imaging Spectrograph on the 3-meter Shane Telescope at Lick Observatory. V2574 Oph was observed approximately 73 days after outburst but was still in an "Oxygen I" phase where the O I lines at 0.8446 and 1.1287 microns that are fluorescently excited by Lyman Beta have strengths comparable to H alpha. The optical region showed the numerous multiplets of Fe II that characterize this class. Fe II lines were also present in the infrared but were not prominent and were mainly confined to the "1 micron" group. In place of Fe II, there are several permitted lines of C I and N I, species that have few features in the optical.

In contrast to V2574 Oph, V5113 Sgr was observed 9 months after outburst and was in a much later state of development. The neutral permitted lines of C, N, and O had all disappeared and coronal lines of [Si VI], [S VIII], and possibly [Ca VIII], had emerged. He II lines were also present and He I 1.0830 microns was the strongest line in the infrared. In addition, the continuum displayed a pronounced rise beyond 1.5 microns indicative of thermal emission from dust.

The authors thank NASA, the NSF, and the Aerospace Corporation's Independent Research and Development program for support.

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© 2004. The American Astronomical Society.