awhoward
commented
1 year ago Here’s a suggested implementation:
To start, use the tutorials on Readthedocs to familiarize oneself with the EM data product and the L1 files. Then, determine the peak-of-blaze wavelengths for the spectral orders in the L1 file. Convert the L1 flux (summing SCI1+SCI2+SCI3) into units of e-/nm/sec. Convert the EM spectra into similar flux units (see the tutorials). Take a ratio of the L1 / EM flux at the peak-of-blaze wavelengths, perhaps doing some local averaging to make sure that the flux values are good estimates in each spectrum. Report this ratio as a function of wavelength with numbers and a plot.
Do a similar procedure for the EM sky and the L1 SKY.
This is needed so that we can set one of the exposure meter channels to a particular threshold in counts and know that that will correspond to some signal level (and SNR) at peak-of-blaze in certain orders. This can probably be done with data in hand.
These two issues are related: https://github.com/California-Planet-Search/KPF-Pipeline/issues/514 https://github.com/California-Planet-Search/KPF-Pipeline/issues/535