ISOCAM Interactive Analysis User's Manual Version 5.0 - ISO - ESA

B.3. DATA VISUALIZATION 315
stabilize Stabilize IMAGEs in .CUBE using the method s90.
CIA> stabilize, pds_scd, method=’s90’
corr jitter Compute the jitter in the IMAGEs in .CUBE. The arrays .DU and .DV are filled
with the jitter offsets.
CIA> corr_jitter, pds_scd
reduce Reduce the IMAGEs in .CUBE to EXPOSUREs in .IMAGE.
CIA> reduce, pds_scd
corr flat Perform flat-field correction on the EXPOSUREs in .IMAGE.
CIA> corr_flat, pds_scd
raster scan Useful only with a raster PDS. It creates the raster MOSAIC and places it in
.RASTER. In the example here a projection method is used.
CIA> raster_scan, raster_pds, method=’project’
reduce bs Useful only with a BS PDS. It creates the beam-switch MOSAIC and places it in
.RASTER.
CIA> reduce_bs, bs_pds
conv flux Converts data from ADU/gain/sec to janskys.
CIA> conv_flux, pds
B.3 Data visualization
This section summarizes some of the visualization routines that appear in Chapter 14.
tviso The simplest display routine. Accepts any 2D numeric array, e.g. a raster MOSAIC.
CIA> tviso, raster_pds.raster
x3d Examine a 3D numeric array, i.e. a cube of images. To display .CUBE with the option of
indicating masked pixels:
CIA> x3d, pds
isocont Displays an image and overlays with contours from another image. Screen output can
be directed to a postscript file. Useful for multi-wavelength comparison. Requires that
images are accompanied by astrometry. It will take FITS files and raster PDSs and BS
PDSs as input. Supposing that you have a DSS FITS image, and a CAM raster of the
same field-of-view, then to overlay the optical and IR data: