Figure 14. Spectral profiles captured with the 100 grooves/mm Jeulin grating near the focal plane of a 190mm telescope. The camera is an Audine with a KAF-0400 CCD. The spectrum in green is that of Delta Cassiopeae, of type A5. The hydrogen Balmer lines are readily visible. The spectrum in red is Gamma Cassiopeae's, whose type is B0e. The Ha hydrogen emission line is spectacular. Exposure times of 30 seconds.
Figure 15. Our homemade spectrograph can give access to galaxy spectra. On this image obtained on a 190 mm Lichtenknecker flat-field telescope by compositing 19 exposures of 2 minutes each one can see elliptic galaxies NGC 2258 (right) and NGC 2256 (left, the galaxies images are included in a blue rectangle). Corresponding spectra are surrounded by an orange rectangle. They are pretty much similar to that of most stars. The grating with 100 grooves/mm is located 19.5 mm from the KAF-0400 surface and dispersion is 45A/pixel. North is to the right.
Figure 16. Spectrum of the dual system NGC 3690 (ARP 299) obtained with the same instrument configuration as above. Thirty seven images of 120 seconds exposure have been composited, which is equivalent to an integrated exposure of 1 hour and 10 minutes. The spectrum for those active galactic centers clearly shows an emission line (note that at the time the image was obtained, on 1999/01/28, a supernova of magnitude 16.5 was located to the right of NGC 3690's center, but being too weak it was not within reach of this spectrograph). The wavelength measured for the emission line is 0.6740 micron. It is most probably the Haline normaly seen at 0.6563 micron, however it has been displaced towards the red because of the galaxy's recession velocity, that has be measured to be 8000 km/s.
Figure 17. In order to obtain this image showing spectra for the main Pleiades stars, the 100 grooves/mm Jeulin grating has been located between a simple photographic lens of 80 mm focal length at F/5.6 and an Audine camera. Atmospheric atomic oxygen's line at 0.76 microns is readily visible in the spectra for most stars. The emission Haline is visible for some stars (of Be type).
Figure 18. Spectrum for 77 Cygni, of type A0V, captured with a 190 mm telescope and an Audine camera (CCD KAF-0401E). The Balmer lines are clearly visible in the blue part of the spectrum. Resolution has been significantly increased by use of a GRISM-type system built around a Rainbow Optics grating and a prism with a 3°57' angle.
Figure 19. Comparison of a spectrum for 77 Cygni (after photometric scaling) with an A0V star's reference spectrum.
