4.Spectrographs
4.1. The wide field spectrograph (2000-2002)
During the Autumn 1999 we designed an instrument capable of obtaining GRB spectra for our rapid response system. When placed on the Cassegrain focus of the 0.3m telescope it is capable of of acquiring slitless spectra of all the objects in a field of 43'x28'. This instrument allows us to have a rapid pointin and fast switching from image to spectroscopic mode. It received first light on November 2000.
Technical information:
| Field of View (0.3 f/10 telescope): | 43' x 28' |
| Dispersing element | Direct vision prism |
| Dispersion : | ~4Å/pixel at 4000Å
~30Å/pixel at 5500Å ~100Å/pixel at 8000Å |
| Limiting magnitude: | 13.5 in 30s (spectrographic mode) |
Pictures of the instrument mounted on the Cassegrain focus of the 0.3m telescope:
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Images obtained through the instrument:
| Direct image | Same field with the dispersing element in the optical path |
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In these images we can see the field surrounding the planetary nebula M57 (ring nebula) in Lyra.
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The nebula has two emissions due to ionized hidrogenof which its composed. |
We can also see some absorption lines in the stellar objects of the field. |
4.2. The COLORES long-slit spectrograph (2011)
A long-slit spectrograph (COLORES) was developed at IAA-CSIC in collaboration with ASU-CAS and got first light in 2011).
