In its standard configuration CASPEC uses a a 31.6 lines/mm echelle grating together with a 300 lines/mm grating cross disperser. A short focal length camera (f/1.46) focuses the beam into a thinned, back illuminated CCD consisting of pixels. One pixel on the detector corresponds to an entrance aperture or seconds of arc on the sky, the first dimension being in the dispersion direction. The table D.1 shows the change in resolution with the order number.
| Order | Resolution | Central Wavelength |
|---|---|---|
| (Å/pixel) | (Å) | |
| 140 | 0.125 0.01 | 4062.21 |
| 130 | 0.133 | 4374.95 |
| 120 | 0.143 | 4739.34 |
| 110 | 0.157 | 5170.49 |
| 100 | 0.174 | 5687.50 |
| 90 | 0.194 | 6319.20 |
| 80 | 0.217 | 7109.60 |
| 70 | 0.244 | 8120.00 |
In this configuration, the spectrograph records in a single CCD frame an Å wide portion of the spectrum of objects with with a resolving power of and a signal-to-noise ratio . This magnitude limit is set primarily by the readout noise of the chip (50 electrons rms) and by the maximum exposure time of min before contamination by cosmic rays becomes a problem. Fainter objects can be observe at lower resolution by binning the CCD data.
Scattered light.
Assuming a plane grating, used in near-Littrow mode, the blaze function R at wavelength is approximated by
| (16) |