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Ok I guess my main question now is, what kind of plots should I be making now?

Jul 31

As far as I understand, my tasks now are the following:

1. Use stacked images from photpipe to build a catalogue of stars with low error in all bands, no close neighbors and are close to the stellar locus.
2. Check how (airmass corrected) stellar color in that catalogue change with time, and if so if that change is dependent on median stellar color.

So currently I am very close to attaining the first goal. The second goal is a bit tricky because of the mass of data I have to churn through, but hopefully I'll be able to get the code right soon.

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Data access on Odyssey:

1. Run JAuth.jar to get login key
2. ssh -Y into to odyssey.fas.harvard.edu, or herophysics.fas.harvard.edu, using the electronic key. 
3. run tcsh
4. source .myrcstubbs
5. data are at /n/panlfs/data/MIRROR/ps1-md/gpc1/
6. nightly science uses individually warped images, nightly stacks run on stacked frames
7. image types: wrp is warped. 
8. see available modules with "module avail"
9. load a module with "module load hpc/ds9-5.6"
10. photometry is in .cmf files, as FITS tables. 
11. in python: 
    1. import pyfits as p
    2. p.open('filename')
    3. print a[0].header
12. or, imhead on command line
13. a[1].data.AP_MAG for aperture magnitudes
14. PSF_RA and PSF_DEC are in the skycell files. 
15. make a scratch directory for data in /n/panlfs

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