To do

Expand GUI to h-a Filter name.

• Data reduction techniques
  1. BUGS and other problems with the data reduction pipeline! (NGD has updated this list and corrected most of the bugs) -- only major problems are listed in this todo file!
  2. - DONE by ND
  3. Xstartrails could be placing seeing and weight estimates in the image header, this could assist in paper-writing, OR (better?) generate a table DATE, EXP, SEEING
  4. Discuss a MAJOR PROBLEM: With present strategy (aligning via star spectra) the alignment can fail when the filter profile changes, and we think we see this happening from night to night. It can be corrected for IF we have a arc+mask and tungsten+mask image for each night. The problem can be corrected in xstartrails but an extra routine is required to fine-tune the alignment of the images automatically: WHO? ND has incorporated an arbitrary shift into xstartrails so the errors, if present, can be corrected without degrading the data.
     Nigel suggests "dithering" the stack of images (in X only) to optimise signal at (say) four locations.
  5. Update website to ensure that certain tasks (eg arc+mask and tungsten+mask) are done each night. I.e "Night checklist" required! Make sure one image is braketted by a stable mask pair
  6. Check which holes can/must be used in a given mask. NOTE THE FOLLOWING POINT!!
  7. Use a summed mask for each night to provide a wavelength solution to Calctrans - this will have higher S/N and will allow more wavelengths to be used. Use the individual masks, as before, to align images (AJR has produced stackmasks.cl to do this) but it does not seem to enhance the visibility of the spots enough (NGD will experiment and report)
  8. Possible bug: codes 501728 and 501725 have been used for the same wavelength. UNTIL FURTHER NOTICE WE IGNORE BLEND ISSUE AND DESIGNATE ALL 5017 BLENDED LINES 5017 (ABOVE CODES ARE CANCELLED)
  9. Check vignetting/shutter function using the obs of stars/galactic PNe and implement the shutter correction procedure
  10. Other gaps in reduction pipeline?
  11. Iterate within team and write up findings on source extraction; Look for ways to discriminate background galaxies from PNe: line width, etc, check for known catalogued sources in field (KK,NRN).
      Think about PHOTOMETRY and CENTROIDING; is PSF fitting of interest?
  12. more Monte Carlo image simulations to estimate completeness limits, contamination fraction, etc; also differing effects over field (PSF and vignetting at edges, brightness nearer centre, star trails obscuring) (NRN)
  13. PSF fit to M31 data? (HRM polynomial solution-> AJR, NRN)
      Establish quantitatively what our rejection limit is: look for rotation curve in galaxies (OII emission from bkg galaxy at z=0.35) - resolve doublet?; objective comparison of object shape with PSF from other nearby objects; compare predictions from large scale structure simulations or observations (Steidel) -- compare density, luminosity function, clustering (AJR/NRN)
  14. derive empirical S/N relation with time, etc. and check predictions (AJR)
  15. measure bandpass over the field for different filter angles, using TUNGSTEN maks: issues are
      1. filter cutoff for planning observations: use master mask? - (currently done for B-6°, B-0°;)
      2. post-hoc analysis of completeness: use master mask?
      3. photometry: preferably use run masks?