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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[19.23] Spitzer Space Telescope and Coordinated Optical Spectrophotometry of V1187 Scorpii (Nova Scorpii 2004 #2)

C.E. Woodward, G. Ruch, R.D. Gehrz, R.M. Humphreys, E. Polomski (U. Minnesota), R.M. Wagner (LBT Obs.), M. Barlow (U. College London), M.F. Bode (Liverpool John Moores U.), S. Eyres (U. Central Lancaster), A. Evans (Keele U.), T.R. Geballe (Gemini Obs.), M.A. Greenhouse (NASA Goddard), P. Hauschildt (U. Hamburg), J. Krautter (U. Heidleberg), W. Liller (U. Chile), J.E. Lyke (Keck Obs.), R. Rudy (Aerospace Corp.), A. Salama (ISO Vilspa), G. Schwarz (U. Arizona), S.N. Shore (U. Pisa, INFN/Pisa), S. Starrfield (Arizona State U.), M.F. Strutskie (U. Virginia), J. Truran (U. Chicago), R.E. Williams (STScI)

Classical nova (CN) explosions are thermonuclear runaway (TNR) in the accreted H-rich envelope on the white dwarf (WD) in a cataclysmic variable system. Infrared and optical observations of CN have established their importance for understanding the formation of astrophysical grains, and as contributors to abundance anomalies in the ISM on local scales. Abundance studies of nova ejecta also provide information about nucleosynthesis in the WD progenitor and in the TNR. Here, we present Spitzer Space Telescope IRS spectra of the Galactic Classical nova V1187 Scorpii (Nova Scorpii 2004 #2) as well as coordinated optical spectroscopy and photometry obtained on the MMT 6.5-m and the 2.0-m robotic Liverpool telescopes.

The Spitzer spectra, obtained on 28.40 September 2004 UT as part of our Cycle 1 ToO nova program, exhibit broad (~4800 km/s) H-recombination line emission (e.g., HI 6-5, HI 7-6, HI 9-8) as well as forbidden line emission including [Mg VII]5.50 micron, [Mg V]5.61 micron, [Ne II]12.81 micron, and [Ne III]15.55 micron. Of note, the [O IV]25.89 micron line is present in the spectra of V1187 Sco. The high resolution optical spectra, obtained on 2004 September 23.01 UT, show double peaked emission lines with velocity components separated by ~1200 km/s, suggesting that the ejecta of V1187 Sco is distributed in clumps of varying ionization states exhibiting a range of ejection velocities (frequently found in CN). We present a preliminary discussion of line identification, reddening, abundances, as well as a comparison of V1187 Sco to other ONeMg nova. Our Spitzer observations are also supported by complementary ground-based infrared spectra obtain as part of a large collaborative study of this nova (see posters by Lynch et al. and Russell et al.).

This work is supported in part by NASA (JPL/SSC) and the NSF (AST02-05814).

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© 2004. The American Astronomical Society.