Notes from meeting 2016.12.21

• Can CCD Reduction Pipeline be used for imaging mode? And how does it work with different ROI?
• What about SAMI? And SOI?
• What about Spectroscopic MOS?
• Single Object vs Multiple Object longslit.
• Understand the software limits and explain them to the user (astronomer).
• Explain the interpolation for the wavelength solution for the users. "Median filters" was not mentioned but it is know to cause losses in resolution. Is that the case with the interpolation? Why?
• Will we have flux calibration?
• In the current version, can we extract the radial velocities?

• The software only touch the science data to apply the wavelength solution found with the comparison lamp

• Provide and install bin files.
• Test on Mac Os.
• What about software installation (setup.py / pip / environments / anaconda).
• Test compatibility between Python 2.7 and Python 3.
• Separate between different configurations - the reduced configuration can be an user input.
• Guidelines for observations in order to use the Pipeline.
• Use known parameters as trace inputs (and maybe other calculations).
• Target is 3 SNR unbinned (e.g., does this work with a 16 mag object?).
• Calculate and provide unbinned SNR to the astronomer.
• How useful will the pipeline be? That is, in how many case it is expected to be used?
• How does sky subtraction work if more than one object is found? Document better.
• What is the type of extraction done? It should be "Optimal Extraction", from IRAF, specially on fainter objects.

• Definitely optimal extraction has to be implemented

• Too many rejected points - Maybe exclude the lines that are problematic.

• Difference data is now clipped to 2 sigmas

• Help.
• Wiki.
• Documentation.
• Add configuration.
• Test with other users.