Previous | Session 19 | Next
D.K. Lynch, R.W. Russell, R.J. Rudy (The Aerospace Corp.), S.J. Bus (U. Hawaii), R.D. Gehrz, N. Smith, C.E. Woodward (U. Minnesota), T.E. Harrison (New Mexico State University), T.R. Geballe, S. Fisher (Gemini Observatory), S. Eyres (U. Central Lancaster), A. Evans (U. Keele), J. Lyke (W. M. Keck Observatory)
We present a time-series of 0.8 - 5 micron spectra of V1187 Scorpii (Nova Scorpii 1004 #2) during the period Aug 8 to Sept 30 UT, 2004. Our spectra show the appearance, evolution and development of a wide range of lines that are diagnostic of the nova shell. On Aug 8th, we used CGS4/UKIRT to obtain a 1- 5 micron spectrum that revealed low excitation emission and broad hydrogen lines with structured profiles. On Aug 13, we began a series of observations with SpeX/IRTF that revealed a gradual and well-defined evolution of lines beginning with low excitation (essentially all H I lines) in mid August to a wealth of more highly excited lines including the coronal lines in mid Sept. Additional data were obtained with NIRSPEC/Keck. Concurrent with the H I lines, the spectra showed strong Lyman beta-fluoresced O I lines at 0.8446 and 1.1287 microns, and these lines remained strong throughout the period. At the end of August, the He I 1.0830 micron and 2.0581 micron lines strengthened and became the strongest lines in the spectrum. By Sept 16 the He II lines appeared quickly followed by [Ca IV] at 3.2058 microns. On Sept 22, the unidentified novae lines at 1.1900, 1.5545, 2.0996 microns) had increased significantly, and the coronal lines [S VIII] and [S IX] first appeared. On Sept 30th, the [Si VI] at 1.9641 microns and [Ca VIII] at 2.3205 microns appeared. At no time during this observation period was there any evidence of thermal emission from dust.
The observations show classical nova development in the infrared with unprecedented time and spectral coverage. The unique time series began serendipitously using BASS at the IRTF (See poster by Russell et al.) and included collaborative observations with the IRTF, UKIRT, Gemini and Keck. The series was crowned by a Spitzer spectrum (See poster by Woodward et al.) on Sept 28th accompanied by near-simultaneous observations from the IRTF and Gemini. We are grateful to Alan Tokunaga of the IRTF for granting us telescope time on short notice and to Jean Rene Roy for granting us time on Gemini.
If you would like more information about this abstract, please follow the link to http://www.aero.org/remote-sensing/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
Previous | Session 19 | Next
Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.