0.8-2.5 micron spectrum of the Wolf-Rayet Star WR 134

The 0.8-2.5 micron spectrum of the Wolf-Rayet star WR 134 (WN6) obtained with SpeX using the 0.3"x15" slit (R=2000). Wolf-Rayet stars are the evolved descendants of the most massive O stars, and their spectra are remarkable for the presence of strong, broad emission lines from He, C, and N which result from the tremendous mass loss rates and powerful, fast stellar winds. A blow-up of the region between 1 and 1.2 microns in the spectrum of WR 134 shows the P-Cygni profile of the He I 10830 line. The hatched regions denote wavelengths affected by absorption due to water in the Earth's atmosphere. The different colors in the spectrum denote the different spectral orders.

The 2-d image of the spectrum is also available.

The observations were taken by Bill Vacca and John Rayner. The spectra were processed by Bill Vacca, using the spectral reduction code Spextool written by Mike Cushing and Bill Vacca.