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

28 CHAPTER 3. RASTER OBSERVATION (CAM01)
CIA> corr_dark, raster_pds
CIA> deglitch, raster_pds
CIA> stabilize, raster_pds
After some time, and many messages printed to the screen, you will have a fully calibrated
raster PDS. Now take a look at the cube of IMAGEs again.
CIA> x3d, raster_pds
Cube(1,9,106) = 4.03450
You will see that the IMAGE displayed by x3d (Figure 3.2) has been greatly transformed.
The dark current bright and dark lines have gone and so has the glitch. In fact a previously
obscured source is now visible in the top half of the IMAGE. You may notice also that
the data values of the pixel have decreased. This is because before dark correction all the
IMAGEs are normalised to ADUs/gain/second.
We can complete the calibration be reducing the IMAGEs to EXPOSUREs and flat-fielding
the EXPOSUREs.
CIA> reduce, raster_pds
CIA> corr_flat, raster_pds
You can use x3d to take a look at the EXPOSUREs.
CIA> x3d, raster_pds.image
Finally we can create the raster MOSAIC. All the EXPOSUREs will be projected on to
the raster field of view.
CIA> raster_scan, raster_pds
You can view this MOSAIC with tviso (a convenient modified version of IDL’s TVSCL).
CIA> tviso, raster_pds.raster
The window in Figure 3.3 will appear. It contains the raster MOSAIC that is stored in
raster pds.raster.
6. You may wish to save the results of the data analysis. You can do this with IDL’s SAVE.
CIA> save, file=’raster_pds.xdr’, raster_pds
Alternatively you can export the data to a FITS file. This is more useful if you intend to
perform further analyses with other analysis packages. The following will export raster pds
to an IRAF FITS file (see also Section 18.2).