To do

Red items need to be done by next observing run

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. 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.
3. Update website to ensure that certain tasks (eg arc+mask and tungsten+mask) are done each night. I.e "Night checklist" required!
4. Figure out the small problem raised by AJR (too many flats discared due to screening possible non-linear pixels in fpixels.cl)
5. Check which holes can/must be used in a given mask. NOTE THE FOLLOWING POINT!!
6. 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)
7. Make test images by seeding real images with an artificial PNe and running them through the pipeline; this could be done with the identical script in a "parallel" directory; the PNe/velocity could be based on a mask hole image/wavelength.
8. Provide an optimum alignment routine which includes a weighting scheme for the outer and inner parts of the galaxy
9. CHECK LA_COS AGAIN... does it leave many residuals??
10. Check vignetting/shutter function using the obs of stars/galactic PNe and implement the shutter correction procedure
11. Other gaps in reduction pipeline?
12. 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.
  Think about PHOTOMETRY and CENTROIDING; is PSF fitting of interest?
13. 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) 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?

(AJR -> NGD)
B-6: bandpass is characterised, but not yet checked for changes with time; high-quality arc is available
B-3, etc: observe at beginning of next run, to plan better
B-0: bandpass is characterised, but not yet checked for changes with time; high-quality arc is available
A-0: bandpass needs characterisation; high-quality arc available??
C: never used??
D: to be delivered

verify best wavelength to use for 5017 arc line blend by looking at ISIS data (currently we use 5017.25 from PN.S data) (KK)

photometric calibration: use standard stars, Galactic PNe, local group PNe, PNe from NGC 1023, M51 and M101; check against published values; make sure to use the empirical pixel dispersion when adding columns (AJR)

astrometry of PNe: use USNO-B and utilise proper motion data (NGD)

Data sets to reduce (primary)

NGC 3379 (AJR)
NGC 4494
NGC 5866 (NGD) compare to ISIS, SAURON, Ciardullo data
NGC 821 (NRN
NGC 7457
NGC 7332/7339 (KK)
NGC 4339

Group-wide discussion on Data analysis

methods for comparing x-y distribution of PNe with galaxy isophotes
methods for reconstructing velocity field
dynamical modelling methods for non-spherical cases
methods for reconstructing velocity field of extended nebula: local cross-correlation? or a deconvolution method like Kankelborg's?
reduce JKT imaging data (NGC 5866 + NGC 7013) (NGD/AJR UK student, NGD/NRN NL student?)

Miscellaneous

plan filter tilts/offsets for 04A, incl ellipticity effects
write 04B proposal? 03B had bad weather
calculate bolometric correction for target galaxies
surface photometry from Saglia et al.?
stellar kinematics data for Virgo galaxies from ACS Virgo survey?
acquire deep imaging data for NGC 821, etc. ?
acquire stellar kinematics data for NGC 3379: SAURON, ?
acquire stellar kinematics data for NGC 4494: ?
acquire stellar kinematics data for NGC 5866: SAURON (R. Peletier)
acquire stellar kinematics data for NGC 821: SAURON (Verolme/Cappellari/McDermott?); long-slit (Rix: KPNO, Bergmann: HET, Gebhardt: STIS, ?)
acquire stellar kinematics data for NGC 7457: SAURON; long-slit (Bergmann: HET, Gebhardt?: STIS?)
acquire stellar kinematics data for NGC 7332: SAURON (J. Falcón-Barroso), STIS?
acquire stellar kinematics data for NGC 7339: ?
acquire stellar kinematics data for NGC 4339: ?
derive probability of intrinsic galaxy ellipticity given observed ellipticity: P(q_3D|q_2D)

Instrument

improve filter holder (AOD Groningen)
check from time-to-time on nitrogen flushing of instrument) Kevin Dee 6/3/02)
upgrading of motor drive box (for H-alpha camera)
investigate clunk again (problem in run 09/01, try using the same telescope angles)
speed up shutter by changing gearbox? (see email J Hart 31.10.01 for notes, also on testing of mask stability!)
check rigidity of mask after power is off
Post minutes from ING debriefing 8/10/03 (AJR)
Write down instructions for start/stop/reboot DAS and startobssys
Script for tilt/focus adjustment
PC! The "focus" script should read: PA=0 step east

DONE!

second weighting scheme added to Xstartrails (NGD 1/04)

last modified by NGD, 1/2004