CARMA test data and shell scripts

For this chapter there are 3 shell scripts available for study that with their comments go into more depth and show plotting example of a simple continuum observation. You will always be able to find these scripts, and their accompanying data, in ftp://ftp.astro.umd.edu/pub/carma/data

1. simple0.csh: A very short 1 minute observation called ``fringetest'', used to show how the various calibration schemes can even dillute the signal of a strong quasar.

2. simple1a.csh: a simple calibration pipeline, as we discussed before. The advantage of keeping all sources together in a single file is fewer files (and thus I/O, saving time) is needed and it is easier to check how well the calibration worked on any source in your track.

   
   

      1 #! /bin/csh -f
      2 #
      3 # extracted from c0319.1D_86GCRing.5.mir, originally observed at CARMA on 20 March 2009.
      4 # PI: Marc Pound and Farhad Yusef-Zadeh.
      5 #
      6 #
      7 # this script works mostly with one visibility file, and uses select= to work on selected data
      8 #
      9 # sources: 
     10 # --------
     11 # MWC349     flux (ignored here)
     12 # 3C345      passband
     13 # 1733-130   phase
     14 # GCRING     source
     15 
     16 
     17 # administration: getting the data
     18 
     19 set tar=../SgrA.mir.tar.gz
     20 tar -zxf $tar
     21 # set vis=$tar:t:r:r
     22 set vis=SgrA.mir
     23 
     24 # set an antpos file for baseline correction: two are available 090225 and 090331
     25 set antpos=$MIRCAT/baselines/carma/antpos.090331 
     26 
     27 # source names (we use the PURPOSE code from listobs: S, B, G)
     28 set sname=GCRING
     29 set bname=3C345
     30 set gname=1733-130
     31 
     32 # reference ants
     33 set bref=2
     34 set pref=2
     35 
     36 # work can start -------------------------------------------------------------------------
     37 
     38 # get a listing of what happened
     39 listobs vis=$vis log=listobs.log
     40 
     41 # select out only the useful astronomical data 
     42 rm -rf all.vis
     43 uvcat vis=$vis  select='-source(NOISE),-auto' out=all.vis
     44 
     45 # notice ant 1 has some issue
     46 # smauvplt vis=all.vis device=/xs axis=time,phase options=nocal,nopass
     47 uvflag vis=all.vis flagval=flag select="ant(1)"
     48 
     49 # baseline calibration
     50 rm -rf all_1.vis
     51 uvedit vis=all.vis    out=all_1.vis apfile=$antpos
     52 
     53 # linelength calibration
     54 rm -rf all_2.vis
     55 linecal vis=all_1.vis 
     56 #gpplt vis=all_1.vis yaxis=phase nxy=5,3 device=/xs options=wrap
     57 uvcat   vis=all_1.vis out=all_2.vis
     58 
     59 # smauvplt vis=all_2.vis device=/xs axis=time,phase options=nocal,nopass
     60 
     61 # bandpass calibration
     62 rm -rf all_3.vis 
     63 mfcal vis=all_2.vis refant=$bref select="source($bname)" interval=999
     64 #gpplt vis=all_2.vis yaxis=phase nxy=5,3 device=/xs options=bandpass
     65 #gpplt vis=all_2.vis yaxis=amp   nxy=5,3 device=/xs options=bandpass
     66 uvcat vis=all_2.vis out=all_3.vis options=nocal
     67 
     68 
     69 # gain calibration, looking quite nice now
     70 rm -rf all_4.vis 
     71 mselfcal vis=all_3.vis refant=$pref select="source($gname)" options=amp,apriori,noscale interval=5
     72 
     73 #gpplt vis=all_3.vis yaxis=phase nxy=5,3 device=/xs options=gains
     74 #gpplt vis=all_3.vis yaxis=amp   nxy=5,3 device=/xs options=gains
     75 
     76 puthd in=all_3.vis/interval value=0.1
     77 uvcat vis=all_3.vis out=all_4.vis 
     78 
     79 # should check flagged values in all_3 and all_4 and they should be the same
     80 # if the new interval is long enough to catch all inter- and extra-polations
     81 
     82 # map the calibrator
     83 
     84 rm -rf beam0 map0  model0 clean0
     85 invert vis=all_4.vis map=map0 beam=beam0 imsize=128 line=wide,1,1,2,2 select="source($gname)"
     86 clean map=map0 beam=beam0 out=model0
     87 restor map=map0 beam=beam0 model=model0 out=clean0
     88 
     89 # map the source
     90 
     91 rm -rf beam1 map1 model1 clean1
     92 invert vis=all_4.vis map=map1 beam=beam1 line=wide,1,1,2,2 "select=source($sname)" options=mosaic,double,systemp imsize=129
     93 mossdi map=map1 beam=beam1 out=model1
     94 restor map=map1 beam=beam1 model=model1 out=clean1
   

3. simple1b.csh: breaking it up in different source files. This is the way the more complex calibration routines work. You will wind up with a lot more files this way.

   
   

      1 #! /bin/csh -f
      2 #
      3 # extracted from c0319.1D_86GCRing.5.mir, originally observed at CARMA on 20 March 2009.
      4 # PI: Marc Pound and Farhad Yusef-Zadeh.
      5 #
      6 #
      7 # this script works by copying over gain tables and applying them, not the simplest
      8 # of ways, but flexible in terms of the more complex calibration schemes that can occur.
      9 #
     10 # sources: 
     11 # --------
     12 # MWC349     flux (ignored here)
     13 # 3C345      passband
     14 # 1733-130   phase
     15 # GCRING     source
     16 
     17 
     18 # administration: getting the data
     19 
     20 set tar=../SgrA.mir.tar.gz
     21 tar -zxf $tar
     22 # set vis=$tar:t:r:r
     23 set vis=SgrA.mir
     24 
     25 # set an antpos file for baseline correction: two are available 090225 and 090331
     26 set antpos=$MIRCAT/baselines/carma/antpos.090331 
     27 
     28 # source names (we use the PURPOSE code from listobs: S, B, G)
     29 set sname=GCRING
     30 set bname=3C345
     31 set gname=1733-130
     32 
     33 # reference ants
     34 set bref=2
     35 set pref=2
     36 
     37 # work can start -------------------------------------------------------------------------
     38 
     39 # get a listing of what happened
     40 listobs vis=$vis log=listobs.log
     41 
     42 # select out only the useful astronomical data 
     43 rm -rf all.vis
     44 uvcat vis=$vis  select='-source(NOISE),-auto' out=all.vis
     45 
     46 # notice ant 1 has some issue
     47 # smauvplt vis=all.vis device=/xs axis=time,phase options=nocal,nopass
     48 uvflag vis=all.vis flagval=flag select="ant(1)"
     49 
     50 # baseline calibration
     51 rm -rf all_1.vis
     52 uvedit vis=all.vis    out=all_1.vis apfile=$antpos
     53 
     54 # linelength calibration
     55 rm -rf all_2.vis
     56 linecal vis=all_1.vis 
     57 #gpplt vis=all_1.vis yaxis=phase nxy=5,3 device=/xs options=wrap
     58 uvcat   vis=all_1.vis out=all_2.vis
     59 
     60 # now we split the full source (B,G,S) in pieces
     61 rm -rf b_1.vis g_1.vis s_1.vis
     62 uvcat vis=all_2.vis out=b_1.vis select="source($bname)"
     63 uvcat vis=all_2.vis out=g_1.vis select="source($gname)"
     64 uvcat vis=all_2.vis out=s_1.vis select="source($sname)"
     65 
     66 # bandpass calibration
     67 mfcal vis=b_1.vis refant=$bref interval=999
     68 #gpplt vis=b_1.vis yaxis=phase nxy=5,3 device=/xs options=bandpass
     69 #gpplt vis=b_1.vis yaxis=amp   nxy=5,3 device=/xs options=bandpass
     70 
     71 # and copy gains into G and S, and apply them
     72 rm -rf g_2.vis
     73 gpcopy vis=b_1.vis out=g_1.vis options=nocal,nopol
     74 uvcat  vis=g_1.vis out=g_2.vis
     75 
     76 rm -rf s_2.vis
     77 gpcopy vis=b_1.vis out=s_1.vis options=nocal,nopol
     78 uvcat  vis=s_1.vis out=s_2.vis
     79 
     80 
     81 # gain calibration, looking quite nice now
     82 mselfcal vis=g_2.vis refant=$pref options=amp,apriori,noscale interval=5
     83 
     84 #gpplt vis=g_2.vis yaxis=phase nxy=5,3 device=/xs options=gains
     85 #gpplt vis=g_2.vis yaxis=amp   nxy=5,3 device=/xs options=gains
     86 
     87 puthd in=g_2.vis/interval value=0.1
     88 
     89 rm -rf s_3.vis
     90 gpcopy vis=g_2.vis out=s_2.vis options=nopass,nopol
     91 uvcat  vis=s_2.vis out=s_3.vis
     92 
     93 # should check flagged values in s_2 and s_3 and they should be the same
     94 # if the new interval is long enough to catch all inter- and extra-polations
     95 
     96 # map the calibrator
     97 
     98 rm -rf beam0 map0  model0 clean0
     99 invert vis=g_2.vis map=map0 beam=beam0 imsize=128 line=wide,1,1,2,2 
    100 clean map=map0 beam=beam0 out=model0
    101 restor map=map0 beam=beam0 model=model0 out=clean0
    102 
    103 # map the source
    104 
    105 rm -rf beam1 map1 model1 clean1
    106 invert vis=s_3.vis map=map1 beam=beam1 line=wide,1,1,2,2 options=mosaic,double,systemp imsize=129
    107 mossdi map=map1 beam=beam1 out=model1
    108 restor map=map1 beam=beam1 model=model1 out=clean1
   

Figure 2.1: Flow diagram simple1a