Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.3704g&link_type=abstract
American Astronomical Society, 186th AAS Meeting, #37.04; Bulletin of the American Astronomical Society, Vol. 27, p.864
Astronomy and Astrophysics
Astronomy
Scientific paper
The infrared spectral region of supernovae is relatively unexplored. Here, I present spectra of five supernovae in the wavelength range of 1.2microns to 2.4microns. The data were obtained in March 1995 with the Rieke `F-Spec' IR spectrometer mounted on the MMT. The most spectacular spectrum is that of 1994Y, a peculiar SN II with narrow optical emission lines. In the infrared, Brgamma and Pbeta emission is very strong and higher level Brackett series lines are also visible. The Brgamma line has a width of 2000 kms(-1) FWHM, while the Balmer lines are broader with a FWHM of 3400 kms(-1) . A strong line at a rest wavelength of 2.206microns is tentatively identified as NaI emission and, along with the permitted FeII lines seen in the optical, suggest the presence of cool and rather dense gas. Late-time optical spectra of 1993J show broad Hα emission thought to be due to an ongoing interaction with its circumstellar environment. The K band spectrum contains no evidence of Brgamma , but an intense HeI line at 2.058microns implies emission from a thin shell expanding at nearly 10000 kms(-1) . The progenitor's hydrogen layer was severely depleted in this `SN IIb', and the strength of the HeI relative to Brgamma is consistant with interaction models which predict that most of the emission comes from the SN ejecta behind the reverse shock. The type Ia supernovae 1995D and 1995E were observed about 30 days past maximicrons light. The mysterious `1.2microns' feature is seen to extend well into the H band. The IR flux from 1995E confirms that it is highly obscured at optical wavelengths by dust in its host galaxy. Supernova 1994AE (Ia) reached a maximicrons of V=13.0, but was only marginally detected in the H band spectra four months after peak brightness.
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