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As described in section 1 these are essential to calibrate the gains of the individual pixels, and in so doing, many if not most of the apparent defects in raw CCD frames can be red away. They need doing for each filter, and good flat field exposures should have a mean level of between 20,000 and 40,000 counts/pixel. Although flat fields (i.e. pixel gains) appear very stable (they have been used from run to run), it is recommended that a complete set of flat fields (i.e. at least one per filter) is obtained each night. This is best done from the twilight sky when exposures of at least one second can be used to give the required levels. For the broad-band set of filters this happens during a short window of about 15 minutes duration in evening and morning twilight. The morning window starts 30 min. (winter) to 40 min. (summer) after Astronomical Twilight and the evening window ends 30 to 40 min. before Astronomical Twilight. For the narrow-band emission line interference filters this window is much larger with some filters giving the correct level more than 4 hours before sunset. See Appendix H for blank areas of sky more free of stars than most. The GLANCE command is used to check the levels through the various filters. This obtains and displays the frame without writing it to disk/tape - (section 2.3.1).
Adam:> GLANCE 2.0 (sec.)
Try setting DIPARM 2 0 65535 with the default LUT and use DISP to re-display - you can tell from the colour if the level is correct. To be more quantitative, use the PHOTOM routine with the STATS option:
Adam:> PHOTOM (select ``STATS'' with the joystick box mode switch. section2.4.3)
then save the frame with the KEEP command:
Adam:> KEEP (section 2.5.4)
Proceed through the filter set in this way ( REDDEST FIRST AT
THE END OF THE NIGHT, LAST AT THE BEGINNING). If the flat
fields appear statistically similar each night, they can be
added together to produce master flat-fields of very high
s/n. It is worth comparing beginning to end of night flat-fields
to check for problems.
For the procedure for taking flat field frames, see subsection 2.3.16.
To combine or average flat fields the following commands can be used:
Adam:> DEFINE OFF COMBINE/WORKSPACE = 50
Adam:> OFF
Then answer prompts. Do NOT try and handle more than 5 files at a time. When you have finished, end the process with:
Adam:> FORGET/DICT OFF
The sky flat fields are preferable because of colour
resemblance to the night
sky. But dome flat fields are very convenient in
that they can be done during the day. They can serve as backup
to the sky flat fields - in general they remove pixel-to-pixel variations very
effectively, but because of poor colour
matching, particularly at the extreme blue and red ends, large
scale gain variations remain. Dome flat fields can further
provide a quick check that the system is operating normally
and that gain and noise are expected. They are thus a
recommended afternoon/early evening occupation. To carry them
out, illuminate evenly (but dimly) a clear patch of dome
in front of the telescope using a single free-standing tungsten
lamp. (Note that the fluorescent lighting is far too
bright and has lines in its spectrum whilst
floor lighting is too faint and does not have a high enough
colour temperature. Use the GLANCE technique described above
unless you know from the previous day just what exposures
are right.