The previous line lists and plots were generated in an iterative manner. Night sky lines were first used to identify the bright lines in the HgCdZn and Ne spectra independently. The HgCdZn and Ne plots were then added and the previously identified lines were used to make further identifications. A comparison with Keck LRIS line lists was then performed to improve confidence in the identifications.
Feedback is always welcome.
Though basically a standard polynomial it is rumored that the Chebyshev form, in the presence of noise, fits the underlying function more precisely. Though most spectrographs do not show the red turn over we observe, we believe that this is a consequence of the unusually large range of angles of light exiting the grating. Finally, all data represented below was acquired with the LRS set to observe the highest resolution possible with a given grism. We used the 0.5 arc-second pinholes illuminated by the comparison lamps. This should give the user and idea of which lines are likely to be blended.