Very Early 3-13 micron Spectral Development of V1187 Sco (Nova Scorpii 2004 #2)

Details Very Early 3-13 micron Spectral Development of V1187 Sco (Nova Scorpii 2004 #2) Very Early 3-13 micron Spectral Development of V1187 Sco (Nova Scorpii 2004 #2)

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.1924r&link_type=abstract

American Astronomical Society Meeting 205, #19.24; Bulletin of the American Astronomical Society, Vol. 36, p.1374

Astronomy and Astrophysics

Astronomy

Scientific paper

Moderate spectral resolution (30-200) data were obtained with the Aerospace Broadband Array Spectrograph System (BASS) on the NASA IRTF 3 m and with Michelle on Gemini North of V1187 Scorpii during the week following maximum light ( Aug. 3UT, 2004). We present a time-series of 3-13 micron spectra from Aug. 5 to Aug. 11 UT, 2004. The spectra initially exhibited the expected gray body continuum at about 1500 K, which cooled from night to night, followed by the appearance of numerous hydrogen lines, of which Humphreys alpha was one of the most prominent. The hydrogen lines increased in intensity until about Aug 8 UT, and then began a gradual decline. The higher spectral resolution Michelle data on Aug. 11 UT showed that essentially all of the features seen were hydrogen lines. The dependence with time of the line intensities will be shown and discussed. These data complement the spectroscopy presented in poster sessions by Lynch et al. (.8-5 microns with a variety of instruments and telescopes) and Woodward et al. (Spitzer data from Sept 28 UT, 2004) at this meeting.
Thus, the observations show classical nova development typical of a very fast nova (t2 about 8 or 9 days) in the infrared with unprecedented thermal spectral coverage this close to maximum light. The unique time series began serendipitously using BASS at the IRTF, and included collaborative observations by the IRTF, UKIRT, Gemini and Keck. The series was crowned by the Spitzer spectrum cited above, 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 to extend our BASS coverage and to Jean Rene Roy for granting us time on Gemini. This work was supported at The Aerospace Corporation by the Independent Research and Development program.

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