Here are the notes I made, Megan Jackson, on the imaging using the multi-scale cleaning algorithm for NGC 1569.  I started with the THINGS .UVLIN data (continuum subtracted).  So, skip down to step 6, part C to see where I started.  There are some notes just before part C where I noted the trimming of the 10 beginning and ending channels.  These notes are for the NATURAL WEIGHTED cube ONLY!  Robust weighting is going to be done separately so not to confuse things, in my mind anyway!


Combining data sets of different array configurations and different observation dates 
=====================================================================================

data combining recipe v. 1.0 : Dana Ficut-Vicas   22Dec08
data combining recipe v. 2.0 : Dana Ficut-Vicas    5Jan09
data combining recipe v. 2.1: Dana Ficut-Vicas   2Mar09
data combining recipe v. 4: Dana Ficut-Vicas 20Jul09
data combining recipe v. 5: Dana Ficut-Vicas 23Jul09


Data reduced by Dana Ficut Vicas, Hertfordshire 16th of December 2008


1. Newly observed data

   A.If in the calibration recipe one has taken out only 10 channels from the begining and end channels for the new data (5 channels from both sides for the old data)then a new UVCOP is necessary here for the new data which will take out another ten channels on both sides.

executed on

DEFAULT UVCOP  
    outcla 'LINCOP';bchan 10;echan 231;
    uvcopprm 0; uvcopprm(4) 1;

    getn *.LINCOP


----> *.LINCOP.2

###Note: One should take the same even number of channels from both sides of the band and in such a way that one remains with a data set with an odd number of channels.THIS preserves the convention that (n+1)/2 is the central channel


   B.Spliting the data and applying the calibration and the flags.

###Note: Check values for GAINUSE and FLAGVER in case of non-standard reduction.

executed on

DEFAULT SPLIT
Sources 'ddo133',''; Qual -1; Calcode ''; Timerang 0;
Stokes ' '; Selband -1; Selfreq -1; Freqid 1; Bif 0; Eif 0; Bchan 1;
Echan 0; Subarray 0; Docalib 1; Gainuse 3; Dopol -1; Blver -1;
Flagver 2; Doband 1; Bpver 1; Smooth 0; Douvcomp -1; Aparm 0; Nchav 1;
Chinc 1; Ichansel 0; Baddisk 0


   C.Cliping the hot pixels

Either check calibration recipe UVPLT or run a quick WIPER to select the CLIP level

executed on

DEFAULT CLIP
aparm 0
aparm(1) 6 $ clip any parallel hand visibilities amplitude greater than 6Jy; 
           $the clipping level should be set according to the previous UVPLT
           $or WIPER checks 

getn *.SPLIT


   D.1  Shifting the data without Hanning smoothing to a common central velocity

D.1.1 

executed on

DEFAULT CVEL
outname 'ddo133.b1-nh'; outcl 'cvel'; outdi 1;
aparm 0, 111, 1, 0, 1420E6, 405752, 1, 0, 0;  $aparm(2)=the reference pixel which can be found in
                                              $the header;aparm(5) and aparm(6)set the Hydrogen 
                                              $rest frequency;aparm(3)to choose heliocentric as
                                              $velocity type;aparm(7)=1 for VLA data;
                     
aparm(1)=331e3;                $the velocity you want in the central channel
aparm(9)=0                     $don't smooth
sources ''; qual -1; timerang 0; selband -1; selfreq -1;
freqid 1; subarray 0; 
flagver 1;                     $apply the flag table which we created when clipping 
doband -1; bpver -1;
gainuse 0;

getn *.SPLIT

###CVEL should print in the messenger window something like this:

CVEL 1: CVELIN: using flag table version    1 on the data
uhppc5> CVEL 1: NOT USING FFT: I WILL BE SLOWWWW
uhppc5> CVEL 1: CONSIDER CHANGING THE NUMBER OF CHANNELS
uhppc5> CVEL 1: Will use velocity and frequency information from APARMS
uhppc5> CVEL 1: Velocity type is heliocentric
uhppc5> CVEL 1: Velocity definition is OPTICAL
uhppc5> CVEL 1: Rest frequency =      1420.405762 MHz
uhppc5> CVEL 1: Ref. pixel for new velocity is   111.00
uhppc5> CVEL 1: New velocity at given pixel is   331.0000 km/s
uhppc5> CVEL 1:      Ant:   1 IF#:  1 Average shift =      3.52560
uhppc5> CVEL 1:      Ant:   2 IF#:  1 Average shift =      3.52555
uhppc5> CVEL 1:      Ant:   3 IF#:  1 Average shift =      3.52573
uhppc5> CVEL 1:      Ant:   6 IF#:  1 Average shift =      3.52562
uhppc5> CVEL 1:      Ant:   7 IF#:  1 Average shift =      3.52547
uhppc5> CVEL 1:      Ant:   8 IF#:  1 Average shift =      3.52560
uhppc5> CVEL 1:      Ant:   9 IF#:  1 Average shift =      3.52559
uhppc5> CVEL 1: Flag table applied - not copied to output
uhppc5> CVEL 1: If spectral flagging requested, spectra will have
uhppc5> CVEL 1: been interpolated before shifting
uhppc5> CVEL 1: Copied NX file from vol/cno/vers  1  103   1 to  1  179   1
uhppc5> CVEL 1: Copied OF file from vol/cno/vers  1  103   1 to  1  179   1
uhppc5> CVEL 1: Copied AN file from vol/cno/vers  1  103   1 to  1  179   1
uhppc5> CVEL 1: Copied WX file from vol/cno/vers  1  103   1 to  1  179   1
uhppc5> CVEL 1: Appears to have ended successfully
uhppc5> CVEL 1: uhppc51 31DEC08 TST: Cpu=    192.3  Real=    320  IO=      155



  D.1.2. Checks:
     
### Spectrum is shifted, but there is no change in the header frequency, 
so you need to run a few checks.

 
  D.1.2.1. CVEL shifts the spectum so some channels, either at the begining , or at the end will end up without valid information. To identify those we use possm to look at the beginning and end channels. You will recognize them by having very low values compared with the rest. The number of these kind of channels depends on how much the spectrum has been shifted.

executed on

    DEFAULT POSSM
    docal -1 ; 
    doband -1;    
    freqid 1             
    flagver -1;
    aparm 0    $ Plot data 
    solint 0   $ average all time
    nplots 0   $ average all baselines
    aparm 0
      aparm(1) 0 $ scalar average
    source='DDO133',''     $ your galaxy
    bchan 1;echan 20;      $ choose the beginning 20 channels to make more obvious 
                           $ the channels with invalid information

    dotv 1

    tvinit
    getn *.CVEL 

    
    DEFAULT POSSM
    docal -1 ; 
    doband -1;    
    freqid 1            
    flagver -1;
    aparm 0    $ Plot data 
    solint 0   $ average all time
    nplots 0   $ average all baselines
    aparm 0
      aparm(1) 0 $ scalar average
    source='DDO133',''     $ your galaxy
    bchan 195;echan 215;   $ choose the last 20 channels to make more obvious 
                           $ the channels with invalid information

    dotv 1

    tvinit
    getn *.CVEL


The number of beginning channels with invalid information: 4
The number of end channels with invalid information: 0

###Note: For the moment we just take a note of this channels. We can get rid of these channels at a later stage, when we are triming in preparation for DBCON, which requires all data sets to have the same number of channels.If for any particular reason we decide not to get rid of these invalid channels at that stage, then they should be excluded from the continuum subtraction.

   

D.2  Shifting the data with Hanning smoothing
     This step is needed if data are to be combined with archive data observed with Hanning smoothing.

D.2.1

executed on

DEFAULT CVEL
outname 'ddo133.b1-h'; outcl 'cvel'; outdi 1;
aparm 0, 111, 1, 0, 1420E6, 405752, 1, 0, 0;  $aparm(2)=the reference pixel which can be found in
                                              $the header;aparm(5) and aparm(6)set the Hydrogen 
                                              $rest frequency;aparm(3)to choose heliocentric as
                                              $velocity type;aparm(7)=1 for VLA data;
                     
aparm(1)=331e3;                $the velocity you want in the central channel
aparm(9)=2                     $smooth crosscorrelation spectra by Hanning
sources ''; qual -1; timerang 0; selband -1; selfreq -1;
freqid 1; subarray 0; 
flagver 1;                     $apply the flag table which we created when clipping 
doband -1; bpver -1;
gainuse 0;

getn *.SPLIT

  D.2.2. Checks:
   ### Spectrum is shifted, but there is no change in the header frequency, 
so you need to run a few checks.
   
  D.2.2.1. Has CVEL done anything?   executed on
    DEFAULT POSSM
    docal -1 ; 
    doband -1;    
    freqid 1             $ set this to match the calibrator
    flagver 1;
    aparm 0    $ Plot data 
    solint 0   $ average all time
    nplots 0   $ average all baselines
    aparm 0
      aparm(1) 0 $ scalar average
    source='DDO133',''     $ your galaxy

    dotv 1

    tvinit

    grchan 1;
    getn *.SPLIT

    flagver -1;grchan 2;
    getn *.CVEL

###You should see the SPLIT and the CVEL do not overlap perfectly

  D.2.2.2. CVEL shifts the spectum so some channels, either at the begining , either at the end will end up without real, valid information. To identify those we use possm to look at the begining and ending channels. You will recognize them by having very low values compared with the rest. The number of these kind of channels depends on how much the spectrum has been shifted.

executed on

    DEFAULT POSSM
    docal -1 ; 
    doband -1;    
    freqid 1             
    flagver -1;
    aparm 0    $ Plot data 
    solint 0   $ average all time
    nplots 0   $ average all baselines
    aparm 0
      aparm(1) 0 $ scalar average
    source='DDO133',''     $ your galaxy
    bchan 1;echan 20;      $ choose the beginning 20 channels to make more obvious 
                           $ the channels with invalid information

    dotv 1

    tvinit
    getn *.CVEL 

    
    DEFAULT POSSM
    docal -1 ; 
    doband -1;    
    freqid 1            
    flagver -1;
    aparm 0    $ Plot data 
    solint 0   $ average all time
    nplots 0   $ average all baselines
    aparm 0
      aparm(1) 0 $ scalar average
    source='DDO133',''     $ your galaxy
    bchan 210;echan 231;   $ choose the last 20 channels to make more obvious 
                           $ the channels with invalid information

    dotv 1

    tvinit
    getn *.CVEL

The number of beginning channels with invalid information: 2
The number of end channels with invalid information: 0

   ###Note: For the moment we just take a note of this channels. We can get rid of this channels at a later stage, when we are triming in preparation for DBCON, which requires all data sets to have the same number of channels.If for any paritcular reason we decide not to get rid of these invalid channels at that stage, then they should be excluded from the continuum subtraction.

   D.2.3.1 CVEL will shift and smooth for you, however it will not get you rid of the every second channel which will be the case in a Hanning smoothed data set in the archive.To do that we use UVDEC.
 
executed on
  
    DEFAULT UVDEC
chinc 2;            $to take every second channel 
outn 'D133.B1H';outcl 'UVDEC'
bchan 1;echan 0;

getn *.CVEL

## In UVDEC is necessary to ensure that among the channels you are taking is the reference pixel.If before CVEL you had an odd number of channels than the reference pixel will be in an odd channel number so in UVDEC you want to take chnnels 1, 3, 5 etc. (see above).

  D.2.4.2 UVDEC has been found not to update the header properly(This should have been fixed by Eric in the mean time). However if it still happens, then the header has to be updated by hand. The problem is with the ALTRPIX which is not updated. This should be the same as the REFPIX.
  
   inp gethead

getn *.UVDEC

keyword 'ALTRPIX'

gethead


inp puthead
keyval 56,0
inp puthead

puthead

imh $ to check if it worked
    

### Recently I worked with UVDEC and it updated the header properly. Please always check!!!


2. Archival data

  
   A.Spliting the data and applying the calibration and the flags.

executed on

DEFAULT SPLIT
Sources 'ddo133',''; Qual -1; Calcode ''; Timerang 0;
Stokes ' '; Selband -1; Selfreq -1; Freqid 1; Bif 0; Eif 0; Bchan 1;
Echan 0; Subarray 0; Docalib 1; Gainuse 3; Dopol -1; Blver -1;
Flagver 2; Doband 1; Bpver 1; Smooth 0; Douvcomp -1; Aparm 0; Nchav 1;
Chinc 1; Ichansel 0; Baddisk 0

getn *.LINCOP.1; 

   B.Cliping the hot pixels

Either check calibration recipe UVPLT or run a quick WIPER to select the CLIP level

executed on

DEFAULT CLIP
aparm 0
aparm(1) 6 $ $ clip any parallel hand visibilities amplitude greater than 6Jy; 
           $the clipping level should be set according to the previous UVPLT
           $or WIPER checks

getn *.SPLIT

  C. Applying the flag table created in CLIP

###We need to apply the flag table here as we do not run CVEL on archival data.

executed on

DEFAULT SPLIT
Sources 'ddo133',''; Qual -1; Calcode ''; Timerang 0;
Stokes ' '; Selband -1; Selfreq -1; Freqid 1; Bif 0; Eif 0; Bchan 1;
Echan 0; Subarray 0; Docalib -1; Gainuse 3; Dopol -1; Blver -1;
Flagver 1; Doband -1; Bpver 1; Smooth 0; Douvcomp -1; Aparm 0; Nchav 1;
Chinc 1; Ichansel 0; Baddisk 0

getn *.SPLIT.1;

  D. If the data was observed in B1950 coordinates then precess the data from B1950 to B2000 coordinates.

executed on

To correct the u,v,w's to the original (J2000) position:

DEFAULT UVFIX
getn *.SPLIT


To shift the phases and the u,v,w's to the new position:

DEFAULT UVFIX
getn *.UVFIX


4. Repeat 1 or 2 for all the data sets that you have on one particular galaxy


5. Now we glue the three array configurations together in one dataset.

  A. We trim the data sets where necessary to ensure same number of channels in all data sets and the same velocity in the central channel.At this stage one might consider trimming away the channels with invalid information created by CVEL, or alternatively if one is trimming the archival data to the number of channels of the new data, it might be more time efficient to trim the beginning or end channels of invalid information created by CVEL after the glueing stage of DBCON.

executed on

    DEFAULT UVCOP
    outcla 'TRIMCOP';
    bchan 4;echan 110;              $the decision is taken comparing all imheaders
    uvcopprm 0; uvcopprm(4) 1;

    getn *.CVEL

 B. Glueing.

###Unfortunately DBCON is glueing only two data sets at a time.

executed on

   DEFAULT DBCON
   Reweight 0 0; Outname 'Dummy'; Dopos 0; Doarray 0; 
   Fqtol 0

   getn ddo133.D1.CP
   get2n ddo133.D2.CP

----> dummy.dbcon


   outname 'dummy1'
   getn dummy.dbcon
   get2n ddo133.C2H.UVDEC

----> dummy1.dbcon



   outname 'dummy2'
   getn dummy1.dbcon
   get2n ddo133.C1H.UVDEC 

----> dummy2.dbcon



   outname 'dummy3'
   getn dummy2.dbcon
   get2n ddo133.B3H.UVDEC

----> dummy3.dbcon


   outname 'dummy4'
   getn dummy3.dbcon
   get2n ddo133.B2H.UVDEC

----> dummy4.dbcon


   outn 'ddo133.BCD'
   getn dummy4.dbcon
   get2n ddo133.B1H.UVDEC

----> dummy4.dbcon



*******  I made a "dirty" naturally weighted cube using these parameters.
  C. Checks:  executed on 5 November 2009
  
  DEFAULT IMAGR
sources 'NGC1569',''; docalib -1;doband -1;outseq 0;
outname 'NGC1569.dirt'; cellsize 1.5; imsize 2048; niter 1000; 
uvwtfn 'na'; dotv -1; calcode '-cal';

getn DDO47_BCD.DBCON
>getn 2
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

*******  I made another "dirty" naturally weighted cube using these parameters.
  C. Checks:  executed on 6 November 2009
  
  DEFAULT IMAGR
sources 'NGC1569',''; docalib -1;doband -1;outseq 0;
outname 'NGC1569.drt1'; cellsize 1.5; imsize 2048; niter 1e6; 
uvwtfn 'na'; dotv -1; calcode '-cal'; flux .0017

getn DDO47_BCD.DBCON
>getn 2
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1


##Also inspect the data with TVMOVIE and find which are the Line channels

The line channels are: 35 - 75

6. Continuum subtraction

  A. Subtracting the continuum:    executed on

###Before subtracting the continuum make sure that the channels with invalid information created by CVEL when shifting were trimmed away using UVCOP. Those channels should not be used in the continuum subtraction. If they were not removed, their input can be avoided by setting ICHANSEL in UVLSF and AVSPC.

  DEFAULT UVLSF
Shift 0 0; Flux 0; Dooutput -1; 
Ichansel 1,30,1,0,77,107,1,0;
Order 1; infil '' 

getn *.DBCON

  B. Creating the continuum map:    executed on
  
  DEFAULT AVSPC
avoption ''; flagver -1;
bif 0;eif 0; channel 0; outcl 'UVCONT'
Ichansel 1,30,1,0,77,107,1,0; $the line free channels

getn *.DBCON

###To make a continuum map we thus need a proper cleaning down to a flux level which depends on how many line free channels we have. A quick and dirty IMAGR is necessary here to establish the flux level to clean down to.

DEFAULT IMAGR
sources '',''; docalib -1;doband -1;outseq 0;
outname 'continuum'; cellsize 1; imsize 2048; niter 1000; 
uvwtfn '';dotv -1; calcode '';robust 0.5;

getn *.UVCONT:
>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.UVLIN.1

Rms noise is: 0.074mJy


  DEFAULT IMAGR
sources '',''; docalib -1;doband -1;outseq 0;
outname 'continuum'; cellsize 1; 
imsize 1024; $in a complex field one might need 2048 
niter 10000; 
uvwtfn ''; dotv -1; calcode '';robust 0.5;
flux 0.00015   $it should be set to a 2 sigma level

getn *.UVCONT








*****  I used the THINGS NGC1569-BCD.UVLIN.1.FITS file from Elias, so, I started from here:
*****  But first, I loaded the images from Elias into AIPS using UVLOD as follows:

DEFAULT UVLOD
Datain '/tb/mjackson/NGC1569-BCD.UVLIN.1.FITS'; outname 'NGC1569-BCD'; outclass 'UVLIN';
outseq 0; outdisk 1; dotable 1; nfiles 0; intape 1; doall 0; object ''; qual -1; band ''; bcount 1; ncount 1;

*****  The line free channels are: Ichansel 12,26,1,0,100,112,1,0; as copied from the THINGS notes.

*****  I used 'UVCOP' from the calibration recipe to cut-off the 10 beginning and ending channels:
From LT Calibration recipe:
3. UVCOP -> LINCOP.1    30 October 2009
  ***Discard the first and last channels: 
    1st and last 10 channels if 127 channels total --> I did this.
    1st and last 20 channels if 255 channels total
  ***We discard these Evil Channels because (1) they're pretty much useless;
    (2) they seem to confuse BPASS (which takes the solution from
    channel N as the initial guess for channel N+1); (3) their noise
    characteristics are quite different from the rest of the channels, which
    can be confusing e.g. in clipping and imaging.

  default UVCOP
  outcla 'LINCOP'
  bchan 11; echan 127-10; uvcopprm 0; sources '';
    uvcopprm(4) 1 $ report progress

  getn *.LINE
>getn 1
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.UVLIN.1


    ***From now on we operate on LINCOP data unless otherwise specified.  The line-free channels are now 2,16,1,0,90,102,1,0.
  
   C. Checks           19 August 2009
Making a dirty cube of the continuum subtracted data

*****  	I didn't make a dirty cube.  Instead, I imaged a single line-free channel (getn 7) to get noise (with 		TVLOD then IMSTAT) and used the THINGS moment 0 (getn 11) map to get coordinates of box (with TVLOD, then 	TVWIN).  I used FLUX = 0.0017 from the THINGS notes file 'ngc1569_com.aips.notes.'  I also changed IMSIZE to 2048; BCHAN = 5; ECHAN = 5.

  DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569_test'; cellsize 1.5; imsize 2048; niter 1e6; 
uvwtfn ''; dotv -1; calcode '-cal';imagrprm 0; imagrprm(10) 1
bchan 5; echan 5;robust 0.5;
flux 0.0017   $set this to 3 times the sigma of the B array dirty cube ---> instead I used flux = 0.0017 from THINGS notes.

getn *.UVLSF
>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

###Having a whole dirty cube at this stage will enable you to decide what the MSCLEAN IMAGR window should be.Use TVWIN to get coordinates of the window you mark yourself on the TVscreen.

*****  I found box parameters of BLC = 500, 671 and TRC = 1510, 1451 for a 2048 image size.

###Some close by galaxies might need a 2048 imsize in IMAGR;this necessity will become obvious when looking at the D array data.


##Inspect the cube and note down the noise level. 

In this particular case it was: 0.47 mJy robust 0

*****  For NGC 1569 the rms = 0.62 mJy.

7. Imaging

   A.  Noise TESTS:
We need the rms noise in a line free channel as given by MSCLEAn with no cleaning.The rms noise is measured by setting a window with TVWIN and than running an IMSTAT.It is this noise level that we will further use with MSCLEAN.

*****  I used SOURCES 'NGC1569',''; BCHAN = 7; ECHAN = 7; CLBOX = 500.00 671.00 1510.00 1451.00; 
*****  IMSIZE = 2048

DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5;
ngauss 4;wgauss 0,15,45,135;
fgaus  0          $ no fgauss levels are necessary as we are not cleaning
niter 0        $no cleaning, we just want to quantify the rms noise
nbox 1
clbox 500.00 671.00 1510.00 1451.00      $enough to hold all the signal in every channel
                                         $its size should have been decided at step 6C
bchan 7;echan 7;             $select one or more line free channels
outn 'noise'
imagrprm 0;
imagrprm(10) 1;    $multiplier of max image size to set beam size
imagrprm(11) 0.2;  $the alpha parameter, which steers MSCLEAN towards certain scale components

>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

 The rms noise measured in a line free channel for NGC 1569 is:
Field 1(5asec resolution): 0.64 mJy (getn 16)
Field 2(15 asec resolution):0.74 mjy (getn 17)
Field 3(45 asec resolution):1.02 mJy (getn 18)
Field 4(135 asec resolution):1.90 mJy (getn 19)
  


   B. Tuning our multi-resolution clean parameters        30 October 2009
 
    DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.64e-3 2*0.74e-3  2*1.02e-3 2*1.90e-3        $ fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 500.00 671.00 1510.00 1451.00       $enough to hold all the signal in every channel
                                         $its size should have been decided at step 6C
bchan 50;echan 55;outn 'test1'
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components

getn *.UVLSF
>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1


Noise level: 0.39 - 0.49 millyJy ----> for NGC 1569 rms noise = 0.65 mJy

#### Look at the maps, see if there are any indicatives of calibration problems or imaging problems
########Monitor the AIPS_MSGRV for any warning messeages especiallly ones like : "SOMETHING IS GOING WRONG.ABANDON CLEAN" or "Clean has begun to diverge.Stopping". IMAGR is running too fast to be able to make a true statistics of these messages, that is why the easiest way to go is after running IMAGR, run a PRTMSG and write the messages in a text file where you can easily scroll through and even use a query-replace to replace the text of the offending messages with more obvious lines of text to be able to see them faster.

default prtmsg
prtask 'IMAGR' $ the task for which you want the aips messages
prtime 1       $ all IMAGRS younger than 1 day
outprint '/tb/mjackson/n1569msg1'    $ the name of the file to write to
docrt -1

prtmsg         &prtmsg is a verb not a task
AIPS 1: ZTXOP2: using translated file name =
AIPS 1: ZTXOP2: /TB/MJACKSON/N1569MSG1
AIPS 1: User    3:  4684 messages, oldest written 30-OCT-2009  13:38:30
AIPS 1: Printed   3883 messages
   
   C. If satisfied with the above than put the whole cube through this imaging recipe

executed on	30 October 2009

DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0; echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.64e-3 2*0.74e-3  2*1.02e-3 2*1.90e-3  $fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 500.00 671.00 1510.00 1451.00
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components

getn *.UVLSF
>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

###Some close by galaxies might need a 2048 imsize in IMAGR;this necessity will become obvious when looking at the D array data.

#### Look at the maps, see if there are any indicatives of calibration problems or imaging problems
########Monitor the AIPS_MSGRV for any warning messeages especiallly ones like : "SOMETHING IS GOING WRONG.ABANDON CLEAN" or "Clean has begun to diverge.Stopping". IMAGR is running too fast to be able to make a true statistics of these messages, that is why the easiest way to go is after running IMAGR, run a PRTMSG and write the messages in a text file where you can easily scroll through and even use a query-replace to replace the text of the offending messages with more obvious lines of text to be able to see them faster.See above, at step 7B for how to set PRTMSG.
###########Limit your cleaning if your science project allows it to the channels with line emission. In this sense worry if you see the above mentioned offending messages in line emission channels. Also it is possible that IMAGR scoops in one field, shoots out the message, gets out of the major cycle, restores components in all fields and by doing so also corrects the negativity of the problematic field.In the message file, where you see IMAGR after having given the warning message, return to that same field it means that MSCLEAN was able to correct itself. The big worry comes in when MSCLEAN stops cleaning alltogether, especially when that happens in a line emission channel.
##################Report any galaxies that do not comply to the above set of parameters.When you find that cleaning leaves behind a negative bowl, or when you find repeated offending messages with no indication of MSCLEAN correcting itself, let Elias or Dana know.Thanks!

cleaned image:
AIPS 2: Mean= 5.7848E-05 rms= 9.7190E-04 JY/BEAM   over 6790182. pixels
AIPS 2: Maximum= 7.3619E-02 at   921  1099    1    1    1    1    1
AIPS 2: Skypos: RA 04 26 30.163  DEC 64 46 08.88
AIPS 2: Skypos: 1420.115 MHZ  IPOL
AIPS 2: Minimum=-7.1308E-02 at  902 1023    1    1    1    1    1
AIPS 2: Skypos: RA 04 26 34.587  DEC 64 44 14.83
AIPS 2: Skypos: 1420.115 MHZ  IPOL
AIPS 2: Flux density =  2.2472E+01 Jy.   Beam area =  17.48 pixels

*****Cleaned NGC 1569 image: (I used channel 5 for my line free channel. I used TVLOD (with TBLC(3)=5 and TTRC(3)=5), then IMSTAT for just channel 5.)
AIPS 1: Mean= 9.3284E-07 rms= 6.2381E-04 JY/BEAM   over  211841. pixels
AIPS 1: Maximum= 2.7056E-03 at   390   982    5    1    1    1    1
AIPS 1: Skypos: RA 04 28 34.461  DEC 64 43 08.86
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-3.1966E-03 at  625 1111    5    1    1    1    1
AIPS 1: Skypos: RA 04 27 39.620  DEC 64 46 25.16
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density =  1.2951E-02 Jy.   Beam area =  15.26 pixels

test image:
AIPS 2: Mean= 1.9816E-04 rms= 7.6901E-04 JY/BEAM   over  320796. pixels
AIPS 2: Maximum= 5.5889E-03 at  1051  1042    6    1    1    1    1
AIPS 2: Skypos: RA 04 25 59.671  DEC 64 44 43.49
AIPS 2: Skypos: 1420.774 MHZ  IPOL
AIPS 2: Minimum=-3.3195E-03 at  925 1066    1    1    1    1    1
AIPS 2: Skypos: RA 04 26 29.213  DEC 64 45 19.39
AIPS 2: Skypos: 1420.713 MHZ  IPOL
AIPS 2: Flux density =  4.1622E+00 Jy.   Beam area =  15.27 pixels

*****Test NGC 1569 image: (I used TVLOD, then IMSTAT with TBLC = 0, TTRC = 0.) 
AIPS 1: Mean= 5.4954E-06 rms= 6.5694E-04 JY/BEAM   over  211841. pixels
AIPS 1: Maximum= 3.1253E-03 at   439  1134    3    1    1    1    1
AIPS 1: Skypos: RA 04 28 23.309  DEC 64 46 57.54
AIPS 1: Skypos: 1420.860 MHZ  IPOL
AIPS 1: Minimum=-3.0984E-03 at  640 1020    3    1    1    1    1
AIPS 1: Skypos: RA 04 27 35.974  DEC 64 44 08.80
AIPS 1: Skypos: 1420.860 MHZ  IPOL
AIPS 1: Flux density =  7.6233E-02 Jy.   Beam area =  15.27 pixels


Computing the noise levels for the natural weigthing setting:
**** I changed sources 'ngc1569',''; imsize 2048; clbox 500.00 671.00 1510.00 1451.00
DEFAULT IMAGR 
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5;
ngauss 4;wgauss 0,15,45,135;
fgaus  0          $ no fgauss levels are necessary as we are not cleaning
niter 0        $no cleaning, we just want to quantify the rms noise
nbox 1
clbox 500.00 671.00 1510.00 1451.00       $enough to hold all the signal in every channel
                                         $its size should have been decided at step 6C
bchan 3;echan 8;             $select one or more line free channels
outn 'noiseNA'
imagrprm 0;
imagrprm(10) 1;    $multiplier of max image size to set beam size
imagrprm(11) 0.2;  $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'na'

>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

 The rms noise measured in a line free channel is:
>getn 40
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NOISENA.IIM001.1
>trc(3)=3;blc(3)=3
>tvlod
>imstat
AIPS 1: Mean=-7.9189E-07 rms= 5.7081E-04 JY/BEAM   over 4194304. pixels
AIPS 1: Maximum= 2.9224E-03 at  1828  2046    3    1    1    1    1
AIPS 1: Skypos: RA 04 22 54.592  DEC 65 09 41.92
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-2.9790E-03 at    1 2023    3    1    1    1    1
AIPS 1: Skypos: RA 04 30 09.450  DEC 65 09 02.73
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density = -1.2152E-01 Jy.   Beam area =  27.33 pixels
>tvinit
Field 1(5asec resolution): 0.57 mJy

>getn 41
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NOISENA.IIM002.1
>tvinit
>trc(3)=3;blc(3)=3
>tvlod
>imstat
AIPS 1: Mean=-2.5047E-06 rms= 7.4631E-04 JY/BEAM   over 4194304. pixels
AIPS 1: Maximum= 3.7056E-03 at  2039   997    3    1    1    1    1
AIPS 1: Skypos: RA 04 22 08.277  DEC 64 43 24.10
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-3.2717E-03 at  647  106    3    1    1    1    1
AIPS 1: Skypos: RA 04 27 33.109  DEC 64 21 17.87
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density = -3.2605E-02 Jy.   Beam area = 322.20 pixels
Field 2(15 asec resolution):0.75 mjy

>getn 42
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NOISENA.IIM003.1
>tvinit
>tvlod
>imstat
AIPS 1: Mean=-7.1267E-06 rms= 1.0313E-03 JY/BEAM   over 4194304. pixels
AIPS 1: Maximum= 4.4332E-03 at  2048   351    3    1    1    1    1
AIPS 1: Skypos: RA 04 22 08.530  DEC 64 27 15.00
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-4.5950E-03 at 2048 2024    3    1    1    1    1
AIPS 1: Skypos: RA 04 22 02.309  DEC 65 09 04.20
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density = -1.6640E-02 Jy.   Beam area =1796.35 pixels
Field 3(45 asec resolution):1.03 mJy

>getn 43
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NOISENA.IIM004.1
>tvinit
>tvlod
>imstat
AIPS 1: Mean=-2.7980E-05 rms= 1.6173E-03 JY/BEAM   over 4194304. pixels
AIPS 1: Maximum= 6.3855E-03 at  2048  1466    3    1    1    1    1
AIPS 1: Skypos: RA 04 22 04.423  DEC 64 55 07.30
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-7.3552E-03 at 1033 1030    3    1    1    1    1
AIPS 1: Skypos: RA 04 26 03.891  DEC 64 44 25.50
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density = -1.0458E-02 Jy.   Beam area =******* pixels
Field 4(135 asec resolution):1.62 mJy



Making a natural weighted data cube:  02 November 2009

****I changed: sources 'ngc1569',''; outname 'ngc1569NA';imsize 2048; fgaus 2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3; clbox 500.00 671.00 1510.00 1451.00;bchan 0;echan 0;
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569NA'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3   $fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 500.00 671.00 1510.00 1451.00 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'NA'  $this will override the robust setting

getn *.UVLSF
>getn 2
AIPS 1: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

*******Here, I made a cube using a small box around NGC 1569.
****I changed: sources 'ngc1569',''; outname 'ngc1569NA';imsize 2048; fgaus 2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3; clbox 807 806 1293 1166;bchan 0;echan 0;
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569NA_SB'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3   $fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 807 806 1293 1166 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'NA'  $this will override the robust setting

>getn 2
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1


*******Here, I made a cube using a medium box around NGC 1569 with an imsize of 2048.
****I changed: sources 'ngc1569',''; outname 'ngc1569NA_MB';imsize 2048; fgaus 2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3; clbox 537 763 1457 1350;bchan 0;echan 0;
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569NA_MB'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3   $fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 537 763 1457 1350; 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'NA'  $this will override the robust setting

>getn 2 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

*******Here, I made a cube using a medium box around NGC 1569 with an imsize of 1024.
****I changed: sources 'ngc1569',''; outname 'ngc1569_MB10';imsize 1024; fgaus 2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3; clbox 25 251 945 838;bchan 0;echan 0;
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569_MB10'; cellsize 1.5; imsize 1024; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2*0.57e-3 2*0.75e-3  2*1.03e-3 2*1.62e-3   $fgaus 2sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 25 251 945 838; 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'NA'  $this will override the robust setting

>getn 2 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

=============================================================================================================================
This is the Natural Weighted cube posted on the NRAO website.  It is the FINAL NATURAL WEIGHTED CUBE:
*******Here, I made a cube using no box around NGC 1569 with an imsize of 2048 and a 2.5 sigma noise level.
****I changed: sources 'ngc1569',''; outname 'ngc1569_MB10';imsize 2048; fgaus 2.5*0.57e-3 2.5*0.75e-3  2.5*1.03e-3 2.5*1.62e-3; clbox 0;bchan 0;echan 0;
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569R_NOB'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2.5*0.57e-3 2.5*0.75e-3  2.5*1.03e-3 2.5*1.62e-3   $fgaus **2.5**sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 0; 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2;   $the alpha parameter, which steers MSCLEAN towards certain scale components
uvwtfn 'NA'  $this will override the robust setting

>getn 2 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1

=============================================================================================================================
ROBUST CUBE at 2.5sigma. ---> 2sigma cleaned too deep, so, I remade the cube at 2.5sigma.:
DEFAULT IMAGR
sources 'ngc1569',''; docalib -1;doband -1;outseq 0;
outname 'ngc1569R_NOB'; cellsize 1.5; imsize 2048; 
uvwtfn ''; dotv -1; calcode '-cal';
robust 0.5; bchan 0;echan 0;
ngauss 4;wgauss 0,15,45,135;
fgaus  2.5*0.57e-3 2.5*0.75e-3  2.5*1.03e-3 2.5*1.62e-3   $fgaus **2.5**sigma in all fields
niter 1e6        $just to ensure we reach the Fgauss limits
nbox 1
clbox 0; 
imagrprm 0;
imagrprm(10) 1;     $multiplier of max image size to set beam size
imagrprm(11) 0.2; 

>getn 2 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=UV   NGC1569-BCD.LINCOP.1
OUTPUT in RANA = 183 - 186


8. Convolution and Blanking  executed on 	03 November 2009

  A. Convolution
    DEFAULT CONVL
blc 0; trc 0; outname ''; opcode ''; bmaj 25; bmin 25
outclass 'CVL25'

  getn *NA.ICL001
>  getn 48
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.ICL001.1

****For small box cube:
>getn 62 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA_SB.ICL001.1


****For no box, 2048^2 cube:
In Tortuga:
>getn 60
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CUBE.1


###We are going to use the NAtural weighted cube to create the master blanking cube. 
 ### Get rms in convolved cube: 0.44e-3 
For NGC 1569: *** IMSTAT results for channel 5 - line-free channel. For large box
AIPS 2: Mean=-1.0526E-06 rms= 1.6986E-03 JY/BEAM   over  789591. pixels
AIPS 2: Maximum= 5.4296E-03 at  1301  1168    5    1    1    1    1
AIPS 2: Skypos: RA 04 25 00.948  DEC 64 47 51.61
AIPS 2: Skypos: 1420.286 MHZ  IPOL
AIPS 2: Minimum=-5.2095E-03 at 1047 1054    5    1    1    1    1
AIPS 2: Skypos: RA 04 26 00.608  DEC 64 45 01.49
AIPS 2: Skypos: 1420.286 MHZ  IPOL
AIPS 2: Flux density = -2.6405E-03 Jy.   Beam area = 314.75 pixels
*** rms = 1.70e-3

***For small box cube:
>tblc 807 806 5;ttrc 1293 1166 5
>tvlod
>tvstat
AIPS 2: Begin setting region number  1
AIPS 2: Press button A to set intermediate vertex
AIPS 2: Press buttons B, C, or D to set final vertex
AIPS 2: C => then reset a vertex,  D => then exit
AIPS 2: Mean=-3.6972E-06 rms= 1.2614E-03 JY/BEAM   over  116191. pixels
AIPS 2: Maximum= 4.1048E-03 at   972  1098    5    1    1    1    1
AIPS 2: Skypos: RA 04 26 18.199  DEC 64 46 07.47
AIPS 2: Skypos: 1420.286 MHZ  IPOL
AIPS 2: Minimum=-3.7157E-03 at 1002  850    5    1    1    1    1
AIPS 2: Skypos: RA 04 26 11.141  DEC 64 39 55.49
AIPS 2: Skypos: 1420.286 MHZ  IPOL
AIPS 2: Flux density = -1.3648E-03 Jy.   Beam area = 314.75 pixels
***rms = 1.2614e-3

****For no box, 2048^2 cube:
>getn 61 (in Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL25.1
>tvlod
>imstat
AIPS 1: Mean=-6.6487E-06 rms= 1.3987E-03 JY/BEAM   over 4194304. pixels
AIPS 1: Maximum= 5.5362E-03 at  1302  1168    5    1    1    1    1
AIPS 1: Skypos: RA 04 25 00.713  DEC 64 47 51.60
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Minimum=-5.2778E-03 at  492   63    5    1    1    1    1
AIPS 1: Skypos: RA 04 28 08.842  DEC 64 20 11.76
AIPS 1: Skypos: 1420.286 MHZ  IPOL
AIPS 1: Flux density = -8.8600E-02 Jy.   Beam area = 314.75 pixels
***rms = 1.3987E-03 

  B. Blanking
  
  B.1 Blank the cube at 2 sigma

DEFAULT BLANK
opcode 'SELC'; dparm 1, 0, 10000, 0.0034, 0  $dparm(4) is the 2 sigma value (1.70E-3 * 2)
outclass 'CVL_BL'; trc 0; blc 0; bchan 0; echan 0

getn *NA.CVL25
>getn 53 (in RANA)       
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.CVL25.1

**** Correct sigma for small box:
DEFAULT BLANK
opcode 'SELC'; dparm 1, 0, 10000, 0.00252, 0  $dparm(4) is the 2 sigma value (1.2614E-3 * 2)
outclass 'CVL_BL'; trc 0; blc 0; bchan 0; echan 0

>getn 66 (in RANA)
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA_SB.CVL25.1

***For no box, 2048^2 cube:
DEFAULT BLANK
opcode 'SELC'; dparm 1, 0, 10000, 0.002797, 0  $dparm(4) is the 2 sigma value (1.3987E-3 * 2)
outclass 'CVL_BL'; trc 0; blc 0; bchan 0; echan 0
>getn 61 (in Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL25.1

***For no box, 2048^2 cube:
DEFAULT BLANK
opcode 'SELC'; dparm 1, 0, 10000, 0.00349675, 0  $dparm(4) is the 2.5 sigma value (1.3987E-3 * 2.5)
outclass 'CVL_BL'; trc 0; blc 0; bchan 0; echan 0
>getn 61 (in Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL25.1


  B.2 Blank cube by hand - output is the master cube
 
    B.2.1 Making contour plots to identify the true line from the noise.


DEFAULT KNTR
docont 1; dogrey -1;dovect -1; ny 3; ltype 6; clev 0.001;  $ clev gives the units of levs param. So, clev=.001 converts all levs to millijanskies.;  
levs 3.4, 5.1,7, 10, 20, 40, 80; $ the lowest level is at 2.5sigma;
                               	$ always between 2-2.5sigma);
dotv 1; pixra -0.0034, 0.0136;   $ pixrange=(-2sigma to +8sigma);
docircle -1;
blc 500.00 671.00      $ I used the same size as the window in IMAGR 
trc 1510.00 1451.00 

getn *NA.CVL_BL
>getn 54
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.CVL_BL.1 ---> Blanked with dparm(4) = .0009 (from DDO133)
>getn 72
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.CVL_BL.3 ---> Blanked at the correct 2sigma level, dparm(4) = 0.0034

***For small box cube: RMS = 1.2614e-3
DEFAULT KNTR
docont 1; dogrey -1;dovect -1; ny 3; ltype 6; clev 0.001;
levs 3.15, 5, 10, 20, 40, 80  $the lowest level is at 2.5sigma, I used 2sigma as the first level and 2.5sigma as the second level and left the rest of the levels the same;
                               $always between 2-2.5sigma);
dotv 1; pixra -0.00252, 0.010    $ pixrange=(-2sigma to +8sigma);
docircle -1;
blc 807 806      $ I used the same size as the window in IMAGR 
trc 1293 1166

>getn 70
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA_SB.CVL_BL.2

****For no box, 2048^2 cube:
DEFAULT KNTR
docont 1; dogrey -1;dovect -1; ny 3; ltype 6; clev 0.001;
levs 3.4, 5, 10, 20, 40, 80  $the lowest level is at 2.5sigma, I used 2.5sigma as the first level and left the rest of the levels the same;
                               $always between 2-2.5sigma);
dotv 1; pixra -0.0028, 0.011    $ pixrange=(-2sigma to +8sigma);
docircle -1;
blc 0      $ I used the same size as the window in IMAGR 
trc 0

blanked at 2 sigma:
>getn 62
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL_BL.1

blanked at 2.5 sigma:
>getn 66
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL_BL.2

****For no box, 2048^2 cube:
DEFAULT KNTR
docont 1; dogrey -1;dovect -1; ny 3; ltype 6; clev 0.001;
levs 4.2, 5, 10, 20, 40, 80  $the lowest level is at 3sigma, I used 3sigma as the first level and left the rest of the levels the same;
                               $always between 2-2.5sigma);
dotv 1; pixra -0.0028, 0.011    $ pixrange=(-2sigma to +8sigma);
docircle -1;
blc 0      $ I used the same size as the window in IMAGR 
trc 0

>getn 62
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL_BL.1

**** blc(3) and trc(3) are the channels to be put on one page.
to get all interesting channels into PL files:
for i=1 to 12;dotv -1; blc(3)= 1+(i-1)*9;trc(3)=i*9;go kntr;wait kntr; end


*****TO MAKE CHANNEL MAPS: use task 'KNTR' with dogrey 1 and docont -1 and ltype 3:
DEFAULT KNTR
docont -1; dogrey 1;dovect -1; ny 3; ltype 3; 
dotv -1; pixra -0.0028, 0.011    $ pixrange=(-2sigma to +8sigma);
docircle -1;
blc 0      $ I used the same size as the window in IMAGR 
trc 0

>getn 60
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CUBE.1

for i=1 to 12;dotv -1; blc(3)= 1+(i-1)*9;trc(3)=i*9;go kntr;wait kntr; end
filename ' /USERS/MJACKSON/N1569HIDATA/N1569_CHAN_MAPS.PA'
for i=1 to 12; plver =i; go lwpla; wait lwpla; end

to print all created PL files **** I left out the 'print i' in order to print to file rather than a printer and added outfile '/tb/mjackson/N1569_CONTOURS.PS' ---> this file is the messy contours with wrong sigma, '/tb/mjackson/N1569_*CONT*.PS' ---> has correct sigma.
for i=1 to 12; plver =i; go lwpla; wait lwpla; end

**** To delete extensions: I reset the 'PL' extension back to zero by deleting all using the following loop.
>getn 54
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.CVL_BL.1
>in
AIPS 1: EXTDEST:  Verb to delete an image or uv extension file
AIPS 1: Adverbs     Values                 Comments
AIPS 1: ----------------------------------------------------------------
AIPS 1: INNAME     'NGC1569NA'             Image name(name). SPECIFY
AIPS 1: INCLASS    'CVL_BL'                Image name(class).
AIPS 1: INSEQ         1                    Image name(seq. #).
AIPS 1: INDISK        1                    Disk drive #.
AIPS 1: INEXT      ' '                     Extension file type. SPECIFY
AIPS 1: INVERS        0                    Extension file version #.
AIPS 1:                                    0 => highest, -1 => all.
>inext 'pl'
>for i=1 to 12; invers = i; extde;end


   B.2.2 Blank cube by hand

DEFAULT BLANK
opcode 'TVCU'; doinvers -1; outclass 'master'
txinc 2; tyinc 2

*****These were done but not used in the final version:
getn *NA.CVL_BL
>getn 72 (14 - Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.CVL_BL.3

***For no box, 2048^2 cube, blanked at 2sigma in Tortuga:
>getn 62
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL_BL.1

=========================================================================================================
I used this as the FINAL Natural Weighted version:
***For no box, 2048^2 cube, blanked at 2.5sigma in Tortuga:
>getn 66
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CVL_BL.2

   B.2.3 use the master cube to blank the full resolution cube and the robust=0.5 cube

DEFAULT BLANK
opcode 'IN2C';outclass 'LMV';

****This was done but not used in the final version:
getn *NA.ICL001  $the full resolution cube, the one created at step 7B
>getn 48 (16 - Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.ICL001.1
get2n *.MASTER
>get2n 79 (15 - Tortuga) (128 - Rana; blanked areas in blue pen)
AIPS 1: Got(2)   disk= 1  user=   3   type=MA   NGC1569NA.MASTER.1

==========================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted version:
*****For 2048^2 cube, 2.5sigma blanked.
>getn 60
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.CUBE.1
>get2n 67
AIPS 1: Got(2)   disk= 1  user=   3   type=MA   NGC1569_NOBX.MASTER.2

==========================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted version:

getn *.ICL001  $the full resolution cube, the one created at step 7B
>getn 116 (Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.CUBE.1
get2n *.MASTER
>get2n 67 (Tortuga)
AIPS 1: Got(2)   disk= 1  user=   3   type=MA   NGC1569_NOBX.MASTER.2


### It blanks the full resolution cube using the MASTER cube as a blanking model.

DEFAULT PBCOR
doinvers -1; coord 0; bparm 0; outclass 'X0_PBC'

*****For 2048^2 cube, 2.5sigma blanked.
==========================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted version:

>getn 68
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.LMV.1

==========================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted version:
>getn 117
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.LMV.1


9. Transposing the cube                          executed on  November 24, 2009
							      December 4, 2009
 DEFAULT TRANS
outclass ''; blc 0; trc 0; transcod '312'

****These were done but not used in the final version:
>getn 76
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   N1569_NA_NC.X0_PBC.1
>getn 77
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   N1569_RO_NC.X0_PBC.1

>getn 131
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569NA.X0_PBC.1
>getn 132
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569.X0_PBC.1

==========================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted version:
*****For 2048^2 cube, 2.5sigma blanked.
>getn 69 (Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_PBC.1

==========================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted version:
>getn 118 (Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.X0_PBC.1

10. Switching the header from frequency description to spectral-line velocity description

getn *. TRANS
==========================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted version:
*****For 2048^2 cube, 2.5sigma blanked.
>getn 70 (Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.TRANS.1
>altswtch

==========================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted version:
>getn 119
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.TRANS.1
>altswtch

11. Final products                               executed on  November 24, 2009

A. Moment maps:

DEFAULT XMOM
flux -10000; icut -10000; blc 0; trc 0

==========================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted version:
*****For 2048^2 cube, 2.5sigma blanked.
>getn 70
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.TRANS.1

==========================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted version:
>getn 119
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.TRANS.1


13.  Replacing blanks with 0
**** Do REMAG to each moment map:
DEFAULT REMAG 
pixval 0; blc 0; trc 0; outclass 'X0_P_R'

getn *.X0_PBC
>getn 22
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569_NA.TRANS.1
>getn 23
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569_RO.TRANS.1

==============================================================================================
I used this for the FINAL Natural Weighted cube:
*****For 2048^2 cube, 2.5sigma blanked.
>getn 75 ----> output #80 (in Tortuga)
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOMNC.1
>getn 76 ----> output #81
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM0.1
>getn 77 ----> output #82
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM1.1
>getn 78 ----> output #83
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM2.1
>getn 79 ----> output #84
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM3.1

*****For the 2048^2 cube, 2.5sigma blanked, with beginning channel=26.
>getn 85 ----> output #90 (in Tortuga)mcat
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOMNC.2
>getn 86 ----> output #91
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM0.2
>getn 87 ----> output #92
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM1.2
>getn 88 ----> output #93
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM2.2
>getn 89 ----> output #94
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.XMOM3.2

==============================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted cube:
>getn 121 ----> output #125
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM0.1
>getn 122 ----> output #126
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM1.1
>getn 123 ----> output #127
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM2.1
>getn 124 ----> output #128
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM3.1


###Note: The Primary beam correction(PBCOR) has not been applied. Something to think about would be which final products we want and which ones among those should be primary beam corrected####


12. Primary Beam Corrections

***Corrects an image for the primary beam attenuation of the 25-meter antennas used at the VLA.

altsw $PBCOR needs the FREQ axis rather than the velocity one 
      $ use this verb to switch between the two

DEFAULT PBCOR
doinvers -1; coord 0; bparm 0; outclass 'X0_PBC'

REMARK:  If one wants to take a spectrum and needs the correct value of the flux in that spectrum, than the whole cube should be primary beam corrected. For more details contact Elias or Dana.



13.  Replacing blanks with 0

DEFAULT REMAG 
pixval 0; blc 0; trc 0; outclass 'X0_P_R'

getn *.X0_PBC



14. Convolutions

DEFAULT CONVL
bmaj 10; bmin 10; blc 0; trc 0; opcode ''; 
outclass 'CVL10'; doblank 0; factor 0; outse 0; outname 'N1569_mscl'

getn *.X0_P_R 

=================================================================================================
I used this for the FINAL Natural (2.5sigma) Weighted cube:
>getn 80
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.1

------> AIPS 1:  131    3 N1569_MSCL  .CVL10 .    3 MA 27-SEP-2010 18:18:20

*****For the 2048^2 cube, 2.5sigma blanked, with beginning channel=26.
>getn 90
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.6

------> AIPS 1:  130    3 N1569_MSCL  .CVL10 .    2 MA 27-SEP-2010 18:15:27

=================================================================================================
I used this for the FINAL Robust (2.5sigma) Weighted cube:

>getn 125
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.X0_P_R.1

------> AIPS 1:  129    3 N1569_MSCL  .CVL10 .    1 MA 27-SEP-2010 18:11:08

15. Writing out the moment maps:

DEFAULT FITTP

===============================================================================================
For FINAL Robust (2.5sigma) Weighted Cube:

DEFAULT FITTP

>dataout '/users/mjackson/NGC1569R_ICL.FITS'
>getn 116
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.CUBE.1

>dataout '/users/mjackson/NGC1569R_LMV.FITs'
>getn 117
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.LMV.1

>dataout '/users/mjackson/NGC1569R_XMOMNC.fits'
>getn 120
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOMNC.1

>dataout '/users/mjackson/NGC1569R_XMOM0.fits'
>getn 121
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM0.1

>dataout '/users/mjackson/NGC1569R_XMOM1.fits'
>getn 122
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM1.1

>dataout '/users/mjackson/NGC1569R_XMOM2.fits'
>getn 123
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM2.1

>dataout '/users/mjackson/NGC1569R_XMOM3.fits'
>getn 124
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   N1569R2.5.XMOM3.1

===============================================================================================
For FINAL Natural (2.5sigma) Weighted Cube:

>dataout '/users/mjackson/N1569_NOBOX_MOMNC.FITS 
>getn 80
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.1

>dataout '/users/mjackson/N1569_NOBOX_MOM0.FITS
>getn 81
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.2

>dataout '/users/mjackson/N1569_NOBOX_MOM1.FITS
>getn 82
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.3

>dataout '/users/mjackson/N1569_NOBOX_MOM2.FITS
>getn 83
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.4

>dataout '/users/mjackson/N1569_NOBOX_MOM3.FITS
>getn 84
AIPS 1: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.5

>dataout '/users/mjackson/N1569_NA_CH26_NOBOX_MOMNC.FITS
>getn 90
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.6

>dataout '/users/mjackson/N1569_NA_CH26_NOBOX_MOM0.FITS
>getn 91
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.7

>dataout '/users/mjackson/N1569_NA_CH26_NOBOX_MOM1.FITS
>getn 92
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.8

>dataout '/users/mjackson/N1569_NA_CH26_NOBOX_MOM2.FITS
>getn 93
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.9

>dataout '/users/mjackson/N1569_NA_CH26_NOBOX_MOM3.FITS
>getn 94
AIPS 2: Got(1)   disk= 1  user=   3   type=MA   NGC1569_NOBX.X0_P_R.10

++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
DAH --- fixing a few things up:

28 July 2011:

PROBLEM: NA & ROB X0_PBC are cubes and not maps

Start with NGC1569_NA_XMOM0.FITS and NGC1569_R_XMOM0.FITS obtained from NRAO data site.

NA---

getn 1
altsw
>default pbcor
>doinvers -1; coord 0; bparm 0; outclass 'X0_PBC'
>getn 1
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569NA.MOM0.1
>go
=====> AIPS 1:    2    2 N1569NA     .X0_PBC.    1 MA 28-JUL-2011 19:22:58 
altsw

>default remag
>pixval 0; blc 0; trc 0; outclass 'X0_P_R'
>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569NA.X0_PBC.1
>go
=====> AIPS 1:    2    2 N1569NA     .X0_PBC.    1 MA 28-JUL-2011 19:22:58
altsw

=====> 
>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569NA.X0_PBC.1
>dataout '/ta/n1569/NGC1569_NA_X0_PBC.FITS
>getn 3
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569NA.X0_P_R.1
>dataout '/ta/n1569/NGC1569_NA_X0_P_R.FITS

R--

datain '/ta/n1569/NGC1569_R_XMOM0.FITS
>outna 'n1569r'
>getn 1
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569R.MOM0.1
>altsw
>tget pbcor
>getn 1
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569R.MOM0.1
=====> AIPS 1:    2    2 N1569R      .X0_PBC.    1 MA 28-JUL-2011 19:30:05
altsw

>tget remag
>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569R.X0_PBC.1
=====> AIPS 1:    3    2 N1569R      .X0_P_R.    1 MA 28-JUL-2011 19:30:27
altsw

>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569R.X0_PBC.1
>dataout '/ta/n1569/NGC1569_R_X0_PBC.FITS

>getn 3
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569R.X0_P_R.1
>dataout '/ta/n1569/NGC1569_R_X0_P_R.FITS

-------------------------------------------------------------------------------------------
28 July 2011:

PROBLEM: no CVL data at all

Obtain NGC1569_NA_ICL001.FITS and NGC1569_NA_MASTER.FITS from NRAO data site

11. Convolutions
REMARK: If the beam size allows it is better to produce the convolved cube from the natural weight
ed cube which has a better signal to noise.

-----> NA cube has beam size 7.71 x 7.04

DEFAULT CONVL
bmaj 10; bmin 10; blc 0; trc 0; opcode '';
outna 'n1569CVL10'; outclass ''; doblank 0; factor 0; outse 0;

getn *NA.ICL001
>getn 1
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569NA.ICL001.1

=====> AIPS 1:    2    2 N1569CVL10  .CONVL .    1 MA 28-JUL-2011 20:12:08

>tget imlod
>datain '/ta/n1569/NGC1569_NA_MASTER.FITS
>outcl 'master'
>outna 'n1569na'
>go

=====> AIPS 1:    3    2 N1569NA     .MASTER.    1 MA 28-JUL-2011 20:14:28


DEFAULT BLANK
opcode 'IN2C';outclass 'LMV';

getn *.CONVL
get2n *.MASTER

=====>
>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.CONVL.1
>get2n 3
AIPS 1: Got(2)   disk= 1  user=   2   type=MA   N1569NA.MASTER.1

=====> AIPS 1:    4    2 N1569CVL10  .LMV   .    1 MA 28-JUL-2011 20:15:54

ON THE CONVOLVED CUBE
11.1   Transposing the cube                          executed on 28 Jul 2011

 DEFAULT TRANS
outclass ''; blc 0; trc 0; transcod '312'

>getn 4
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.LMV.1

=====> AIPS 1:    5    2 N1569CVL10  .TRANS .    1 MA 28-JUL-2011 20:17:50

11.2 Switching the header from frequency description to spectral-line velocity description

getn *. TRANS
ALTSWCH

>getn 5
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.TRANS.1
>altsw


11.3  Final products                               executed on 28 Jul 2011

A. Moment maps:

DEFAULT XMOM
flux -10000; icut -10000; blc 0; trc 0

getn *.TRANS
>getn 5
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.TRANS.1

=====>
AIPS 1:    6    2 N1569CVL10  .XMOMNC.    1 MA 28-JUL-2011 20:21:33
AIPS 1:    7    2 N1569CVL10  .XMOM0 .    1 MA 28-JUL-2011 20:21:33
AIPS 1:    8    2 N1569CVL10  .XMOM1 .    1 MA 28-JUL-2011 20:21:33
AIPS 1:    9    2 N1569CVL10  .XMOM2 .    1 MA 28-JUL-2011 20:21:34
AIPS 1:   10    2 N1569CVL10  .XMOM3 .    1 MA 28-JUL-2011 20:21:34

###Note: The Primary beam correction(PBCOR) has not been applied. Something to think about would be which final products we want and which ones among those should be primary beam corrected####


11.4  Primary Beam Corrections

***Corrects an image for the primary beam attenuation of the 25-meter antennas used at the VLA.

altsw $PBCOR needs the FREQ axis rather than the velocity one
      $ use this verb to switch between the two

>getn 7
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM0.1
>altsw


DEFAULT PBCOR
doinvers -1; coord 0; bparm 0; outclass 'X0_PBC'

getn *.XMOM0
>getn 7
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM0.1

=====> AIPS 1:   11    2 N1569CVL10  .X0_PBC.    1 MA 28-JUL-2011 20:27:32
altsw

11.5  Replacing blanks with 0
DEFAULT REMAG
pixval 0; blc 0; trc 0; outclass 'X0_P_R'

getn *.X0_PBC
>getn 11
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.X0_PBC.1

=====> AIPS 1:   12    2 N1569CVL10  .X0_P_R.    1 MA 28-JUL-2011 20:33:25

REMARK: The REMAG task is useful not only for moment0 maps but for any map in which you would like the magic values of AIPS to be replaced with zeroes, for better data handling when outside AIPS(In programs like KARMA the magic values will disturb your histogram, in programs like IDL the magic values can lead to calculation errors).

=====>
>getn 2
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.CONVL.1
>dataout '/ta/n1569/NGC1569_CVL10_ICL001.FITS

>getn 4
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.LMV.1
>dataout '/ta/n1569/NGC1569_CVL10_LMV.FITS

>getn 6
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOMNC.1
>dataout '/ta/n1569/NGC1569_CVL10_XMOMNC.FITS

>getn 7
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM0.1
>dataout '/ta/n1569/NGC1569_CVL10_XMOM0.FITS

>getn 8
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM1.1
>dataout '/ta/n1569/NGC1569_CVL10_XMOM1.FITS

>getn 9
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM2.1
>dataout '/ta/n1569/NGC1569_CVL10_XMOM2.FITS

>getn 10
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.XMOM3.1
>dataout '/ta/n1569/NGC1569_CVL10_XMOM3.FITS

>getn 11
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.X0_PBC.1
>dataout '/ta/n1569/NGC1569_CVL10_X0_PBC.FITS

>getn 12
AIPS 1: Got(1)   disk= 1  user=   2   type=MA   N1569CVL10.X0_P_R.1
>dataout '/ta/n1569/NGC1569_CVL10_X0_P_R.FITS