Instructions for AIPS++ continuum data processing
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Stage 1 - use the aips++ GUIs to load, image and view the data
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1. login to a Sun using synwork account
2. rsh to nelle
3. cd /data/NELLE_1/synwork/aips++/data
4. type ls to list the data files, then type aips++ an wait for the 
   toolmanager to appear
5. Select the atnf package, atca module, create an atcafiller tool
6. Specify the data in this directory
  ( the 94-*.C284) files, using options birdie and reweight, call the output
   c284.uv. You'll need to run 'fill' to actually load the data.
7. Just for fun, let's make an image of our source (without flagging or
   calibration)
   Fire up the imager tool, in the synthesis/imager section
   Specify the file we just created as the input.
8. Run summary to get some details about the data
9. Goto the setup group, first select what data to use with setdata
   then specify the image you want to make with setimage
10. Goto the image group and select makeimage, specify an output image name,
    press go.
11. Press tools in use, click on viewer, then show, find your image in
    the datamanager that pops up, select it and choose a raster image.
    Your image should appear in the viewer display panel. 
    Press 'contrast' and move the mouse around with button 1 pressed to
    change the lookup table. Adjust lets you change colors and put coordinates
    on the plot.
   
    

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Stage 2 - use the command line to do calibration & imaging
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1. Fire up netscape (on the Sun) and point it at 
   http://nelle.atnf.csiro.au/aips++s/aips++.html
   (it's in the toolbar)
2. Navigate to documentation, then to Telescope Specific processing and find
   the ATCA chapter, follow this guide to calibrate the data.
Notes: - you will need to flag the data on CA01 after 23:19
       - also flag the data after 00:15 on the 15th Feb 94
       (due to telescope problems)
       
      
       
calibrate:
primary cal
set flux with imager
cal:=calibrater('c284.ms')
cal.setdata(msselect='FIELD_ID==3 && DATA_DESC_ID==0') #1934
cal.setapply(type='P', t=10.0);                 # Correct for parallactic angle
cal.setsolve(type='G', t=30.0, table='cal.G')   # Solve for G Jones
cal.setsolve(type='B', t=1.e6, table='cal.B')   # Solve for B Jones 
cal.setsolve(type='D', t=1.e6, table='cal.D')   # Solve for D Jones
cal.solve();                                    # Do the actual solution
cal.plotcal(tablename='cal.G');                 # Plot the calibration solution obtained
cal.done()                                      # Destroy the calibrater tool

secondary cal
cal:=calibrater('c284.ms')
cal.setdata(msselect='FIELD_ID==1 && DATA_DESC_ID==0') #1934
cal.setapply(type='P', t=10.0)                         # Correct for paral
cal.setapply(type='B', table='cal.B')                  # Apply B Jones 
cal.setapply(type='D', table='cal.D')                  # Apply D Jones 
cal.setsolve(type='G', t=60.0, table='cal.G',append=T) # Solve for G Jones 
cal.solve()                                            # Do the actual solution
cal.plotcal(tablename='cal.G',plottype='PHASE',fields=2);  # Plot the solution 
cal.linpolcor(tablein='cal.G', fields='1756-663');
cal.fluxscale(tablein='cal.G', reference='1934-638',transfer='1756-663')
cal.done();

apply cal
cal:= calibrater('c284.ms')
cal.setapply(type='P', t=10.0)            # Apply parallactic angle 
cal.setapply(type='G', table='cal.G')     # Apply the G Jones solutions
cal.setapply(type='D', table='cal.D')     # Apply the D Jones solutions
cal.setapply(type='B', table='cal.B')     # Apply the B Jones solutions
cal.correct()                             # Correct the data
cal.done()

image
# make a quick first look image
include 'imager.g';
imgr:=imager(filename="c284.ms");
imgr.summary();
imgr.setdata(mode="channel" , nchan=12, start=2, step=1,
  spwid=1, fieldid=2);
imgr.setimage(nx=1024, ny=1024, cellx="2arcsec", celly="2arcsec", 
  stokes="I" , mode="mfs" , nchan=12, start=2, step=1, spwid=1, fieldid=2);
#imgr.makeimage(type="observed" , image="ngc6300.image");
# Image, and deconvolve using the Clark CLEAN.
imgr.clean(algorithm='clark', niter=500, gain=0.1, 
            threshold='0.0Jy', 
            model='ngc6300.model',                  # Save model
            image='ngc6300.restored',               # Save restored
            residual='ngc6300.residual')            # Save residual
imgr.done();
#
im:= image('ngc6300.restored')                      # View restored image
im.view()