0.8 - 2.5 micron Spectroscopy of V4633 Sagittarii (Nova Sagittarii 1998)

Details 0.8 - 2.5 micron Spectroscopy of V4633 Sagittarii (Nova Sagittarii 1998) 0.8 - 2.5 micron Spectroscopy of V4633 Sagittarii (Nova Sagittarii 1998)

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.0906v&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #09.06; Bulletin of the American Astronomical Society, Vol. 32, p.1411

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present near IR spectroscopy of V4633 Sagittarii taken on August 29.5 1999 UT and again on July 21.36 2000 UT. The spectra from these two dates provides us an opportunity to study not only the many processes of the nova's outburst but also its evolution over time. V4633 Sgr is a moderately fast nova with no evidence of dust formation. On August 1999, the nova was in the early stages of its coronal phase with the He I λ 10830 being the strongest line. Eleven months later on July 2000, the nova had faded by more then a magnitude in the JHK region and its spectrum was dominated by coronal lines and features of He II. On both dates the lines appeared symmetric and unstructured with the hydrogen lines being relatively weak compared to the heavier elements. A number of lines remain unidentified and we have seen some of these lines in previous nova. The estimated distance, uncorrected for reddening, is approximately 11 Kpc. Support for this research provided by The Aerospace Corporation's Independent Research and Development Program. Also see posters by Rudy et al. and Lynch et al.

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