The 0.5 13 µm Spectrum of V4332 Sagittarii in 2006

Details The 0.5 13 µm Spectrum of V4332 Sagittarii in 2006 The 0.5 13 µm Spectrum of V4332 Sagittarii in 2006

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.0905l&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #09.05; Bulletin of the American Astronomical Society, V

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V4334 Sgr is one of three strange stars that suddenly brightened and cooled dramatically (V838 Mon and M31 RV are the others). The outburst mechanism(s) are not understood but judging from the enormous energy release (more than a nova and less than a supernova), it must involve a new mechanism or be an extremely rare (or brief) stage in stellar evolution.
During spring and summer 2006, we observed V4332 Sgr using VNIRIS on the Lick 3 meter telescope, SpeX on the IRTF and BASS on the IRTF. Owing to the star's slow changes, we view the combined spectrum as a common-epoch observation, i.e. essentially simultaneous.
At short wacelengths, the spectrum is dominated by emission lines of aluminum oxide (AlO). Also present are the anomalously bright KI resonance lines at 0.7667 and 0.7701 µm, and the deep ice absorption feature at 3.05 µm reported earlier by Banerjee et al. (2003 ApJL 598, L31 and 2004 ApJL 615 L53). At longer wavelengths the spectrum and spectral energy distribution are consistent with a 900 K black body with a strong absorption between 8 and 13 µm. This feature cannot be fit by absorption by gaseous silicon monoxide (SiO) or water ice absorption. It can be reasonably fit by a profile derived from the interstellar amorphous silicate feature. Whether this absorption is interstellar or circumstellar is still under investigation.

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