Last Updated on May 17 2013 at 08:36:30 by Julien Spronck.

This page was automatically generated by /tous/mir7/jspronck/chiron.py based on data found in the python file /tous/mir7/jspronck/structs/CHIRON_st_py.dat.

Power on the CCD (in the iodine region) and spectrograph efficiency for Alpha Cen A observations (using the narrow slit).

All observations were taken with iodine and with the narrow slit. The spectrograph efficiency is calculated using the narrow slit and iodine throughputs (measured in the next figure) and comparing to the 3.8 nW that we should get for a 0th magnitude star above atmosphere for a 1.5m telescope with a 76cm central obstruction.

Power on the CCD (in the iodine region) and spectrograph efficiency for Alpha Cen A observations (using the slit).

All observations were taken with iodine and with the narrow slit. The spectrograph efficiency is calculated using the slit and iodine throughputs (measured in the next figure) and comparing to the 3.8 nW that we should get for a 0th magnitude star above atmosphere for a 1.5m telescope with a 76cm central obstruction.

Power on the CCD (in the iodine region) for quartz observations.

Different curves correspond to different modes (fiber: blue squares, slicer: red diamonds, slit: green asterisks, narrow slit: black pluses) without iodine. The dotted black line is the power obtained with the narrow slit and iodine. The efficiencies given in the figure legend are calculated based on a median of the last 25 observations for each mode.

Average exposure meter count rate for Alpha Cen A observations

Total EM counts as a function of CCD counts for Alpha Cen A (blue squares) and B (red diamonds)

Total EM counts as a function of CCD counts for Quartz observations

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