https://packaging-guide.openastronomy.org/en/latest/

Probably good practice.

Create a tutorial for APF data that shows the progression of 1D data products, starting from the reduced 1D spectra.

Zoe
Wavelength solution in constant RV space.
Shifted to rest frame.

SM-emp plots showing the offsets that need to be applied.

After deblazing each order of an APF stellar spectrum, two more steps must be taken before the spectrum can be input into SpecMatch-Emp: combining the spectral orders, and resampling onto the reference/library wavelength scale. In the original method of resampling a deblazed APF spectrum onto the SpecMatch-Emp library wavelength scale, these are done simultaneously by looping over each library wavelength value, finding all elements of the spectrum that are within +/- 0.17 A of that value, and averaging those values. Because the orders overlap, this often means averaging not only adjacent values within one order but also between orders. This is done by calling the script called resample.py.
However, this method results in a much 'noisier' spectrum in the region of overlap between orders.
In addition, there are some issues at the ends of each order: 1) an 8 pixel wide dip in flux which comes from the blaze functions containing 8 zero-valued pixels at the end of each order, and 2) a 100 pixel wide section at each end of each order where the deblazed order is gradually set equal to the undeblazed order. These issues could both be fixed in the deblazing step or in the resampling step.

All three of these issues are evident in the example segment of HIP111169 (note that the step-like offsets between orders is a different issue from the deblazing which must be resolved separately).

Create a tutorial for APF data that shows the progression of 1D data products, starting from the reduced 1D spectra.

Malik
Normalized
Deblazed

Use this link:https://github.com/yngvem/python-project-structure
to setup the right file structure for ReadTheDocs.

Modify the script which runs SM-emp to output stellar property plots.

Once the detrend values for Teff, R_star and [Fe/H] are determined, let's hardwire them into the code so that future observations have the corrected values as their default.