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- IMage
- (file) Name of image for input. This should be a file
containing an arc spectrum.
- ARC_OPTS
- (char) Enter arc fit option:
- NEW (N)
- set up a new wavelength calibration
- REPEAT (R)
- Iterate on previous calibration
- CLONE (C)
- CLone a previous calibration
- OLD (O)
- Correct using previous results
- OUtput
- (file) Name of output file
File to contain corrected data.
- YStart
- (int) analysis lower limit
The data between the limits ystart and yend is extracted
and the resultant spectrum is used to locate the lines.
- YEnd
- (int) analysis upper limit
The data between the limits ystart and yend is extracted
and the resultant spectrum is used to locate the lines.
- YBlock
- (int) Enter analysis x-sect width
Each window is of this width (except perhaps the final one).
- ITeration
- (short) New value of iteration
- ORder
- (int) order for polynomial fitting
This is for the continuity correction of the data. Ideally the
arc should have been pre-processed with ARCSDI, so a low
order e.g. 2 should be used.
- MAXLines
- (int) Maximum number of lines to allow room for
This must be greater than or equal to the number of lines
fitted, so room should be allowed in case any more are
to be added later.
- CLfile
- (file) Name of image for cloning from
This should be a file containing an arc spectrum.
- TOls
- (char) For use in batch only
- KEEP_ITT
- (key) keep iteration files
- PRFits
- (key) Print out details of fitting
- PLOtcorr
- (key) Plot correction?
This is used with the OLD option.
Next: Display Programs
Up: ARCSDI Correction for Line Curvature
Previous: ARCSDI Correction for Line Curvature
FIGARO A general data reduction system
Starlink User Note 86
Keith Shortridge, Horst Meyerdierks,
Malcolm Currie, Martin Clayton, Jon Lockley,
Anne Charles, Clive Davenhall,
Mark Taylor, Tim Ash, Tim Wilkins, Dave Axon,
John Palmer, Anthony Holloway and
Vito Graffagnino
2004 February 17
E-mail:starlink@jiscmail.ac.uk
Copyright © 2013 Science and Technology Facilities Council