SMA CO Line Data 3.1: Difference between revisions
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== Continuum imaging and subtraction == | == Continuum imaging and subtraction == | ||
Next we want to make a continuum-free line dataset. We use field 0 to pick the line free spw. You need to make a clean mask. The strongest source is in the upper NE of the mosaic and there is a much weaker source to the SW corner. | |||
<source lang="python"> | <source lang="python"> | ||
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The line is confined to spws 13~15. | The line is confined to spws 13~15. | ||
Copy original ms in case something goes wrong | Copy the original ms in case something goes wrong. Currently [[uvcontsub2]] will change the input model and corrected columns, so it's best to make a back up. This behavior will change in future. | ||
<source lang="python"> | <source lang="python"> | ||
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</source> | </source> | ||
Now use new task [[uvcontsub2]] to subtract the continuum. Unlike [[uvcontsub]], this task will subtract the continuum estimate for spw that are ''not'' in the fitspw list. In future releases [[uvcontsub2]] will likely replace [[uvcontsub]]. | Now use new task [[uvcontsub2]] to subtract the continuum. Unlike [[uvcontsub]], this task will subtract the continuum estimate for spw that are ''not'' in the fitspw list. In future releases [[uvcontsub2]] will likely replace [[uvcontsub]]. Setting '''fitspw='0~12,16~23'''' tells [[uvcontsub2]] where to fit the continuum emission. | ||
<source lang="python"> | <source lang="python"> | ||
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</source> | </source> | ||
The directory g19_d2usb_targets_line.ms.cont/ contains the estimated continuum, while g19_d2usb_targets_line.ms.contsub/ contains the continuum subtracted line data | The directory g19_d2usb_targets_line.ms.cont/ contains the estimated continuum, while g19_d2usb_targets_line.ms.contsub/ contains the continuum-subtracted line data. | ||
Next we image the continuum data: | |||
<div style="background-color: #dddddd;"> | <div style="background-color: #dddddd;"> | ||
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Here you can see one stronger continuum source to the NE (18:25:58.5 -12:03:58.9) and one weak one to the SW (18:25:52, -12:04:53). The weak one is only visible after one round of cleaning. Because the mosaic is sparse you should make a clean mask to get the best cleaned image. | Here you can see one stronger continuum source to the NE (18:25:58.5 -12:03:58.9) and one weak one to the SW (18:25:52, -12:04:53). The weak one is only visible after one round of cleaning. Because the mosaic is sparse you should make a clean mask to get the best cleaned image. | ||
Make a dirty image of the continuum subtracted data, excluding the line | Make a dirty image of the continuum subtracted data, excluding the spws which contain line emission. You should see nothing but noise. | ||
<source lang="python"> | <source lang="python"> | ||
Revision as of 19:11, 10 May 2010
This script describes the data reduction of an SMA six-pointing mosaic of 12CO 2-1 emission in the infrared dark cloud G19.3+0.07. The CO line was placed in the USB. These data are from Brogan et al. in prep.; please do not use them for scientific purposes. This tutorial is based on the SMA CO Line Data script found in the CASA Scripts and Data page here.
The data were previously filled in Miriad. A Tsys correction was applied, and the data were then written out in uvfits format. In this tutorial, CASA is used to read the uvfits files, and flag, calibrate, continuum subtract and image the data. Plotting for datasets with many spw such as SMA data (plotxy) can be slow. Where possible the new plotter plotms has been used.
You will need the tarball of the uvfits data, which can be downloaded here.
Creating the measurement set from uvfits data
First, remove any files from previous run-throughs and unpack the tarball:
# In CASA
# Remove any files from previous run-throughs
os.system('rm -rf spw_fits.files')
os.system('tar xvf spw_fits_files.tar')
os.system('rm -rf g19_d2usb*')
Read in each uvfits file using the importuvfits filler (need to put upper range to one more than have, to satisfy ipython peculiarity). We create a list of the filenames in 'myfiles' that can be used in a later call.
os.system('rm -rf spw_ms_files')
os.system('mkdir spw_ms_files')
myfiles = []
for i in range(1,25):
msfile = "spw_ms_files/g19_d2usb.spw"+str(i)+".ms"
importuvfits(fitsfile="spw_fits_files/g19_d2usb.spw"+str(i),
vis=msfile)
myfiles.append(msfile)
Using concat, create a single measurement set (ms) from the filenames listed in 'myfiles':
concat(vis=myfiles,concatvis='g19_d2usb.ms',timesort=True)
Finally, initialize the scratch columns using clearcal and use listobs to look at the contents of the measurement set:
clearcal(vis='g19_d2usb.ms')
listobs(vis='g19_d2usb.ms',verbose=False)
0 jupiter 13:01:25.48 -05.18.53.00 J2000
1 1743-038 17:43:58.85 -03.50.04.62 J2000
2 g19.3a 18:25:58.70 -12.03.57.80 J2000
3 g19.3b 18:25:57.40 -12.04.18.50 J2000
4 g19.3c 18:25:56.09 -12.04.28.20 J2000
5 g19.3d 18:25:54.60 -12.04.23.10 J2000
6 1908-201 19:11:09.65 -20.06.55.11 J2000
7 g19.3e 18:25:54.80 -12.04.43.80 J2000
8 g19.3f 18:25:53.30 -12.04.51.00 J2000
9 3c454.3 22:53:57.74 +16.08.53.56 J2000
10 0359+509 03:59:29.75 +50.57.50.15 J2000
11 hip19167 04:06:35.04 +50.21.04.54 J2000
12 polaris 02:31:48.70 +89.15.50.72 J2000
13 uranus 22:44:40.51 -08.50.23.77 J2000
Spectral Windows:(24 unique spectral windows and 1 unique polarization setups)
SpwID #Chans Frame Ch1(MHz) ChanWid(kHz)TotBW(kHz) Ref(MHz) Corrs
0 128 LSRK 229347.598 812.5 104000 229347.598 XX
1 128 LSRK 229429.601 812.5 104000 229429.601 XX
2 128 LSRK 229504.79 812.5 104000 229504.79 XX
3 128 LSRK 229586.792 812.5 104000 229586.792 XX
4 128 LSRK 229675.607 812.5 104000 229675.607 XX
5 128 LSRK 229757.609 812.5 104000 229757.609 XX
6 128 LSRK 229832.798 812.5 104000 229832.798 XX
7 128 LSRK 229914.8 812.5 104000 229914.8 XX
8 128 LSRK 230003.615 812.5 104000 230003.615 XX
9 128 LSRK 230085.617 812.5 104000 230085.617 XX
10 128 LSRK 230160.806 812.5 104000 230160.806 XX
11 128 LSRK 230242.808 812.5 104000 230242.808 XX
12 128 LSRK 230331.623 812.5 104000 230331.623 XX
13 128 LSRK 230413.625 812.5 104000 230413.625 XX
14 128 LSRK 230488.814 812.5 104000 230488.814 XX
15 128 LSRK 230570.817 812.5 104000 230570.817 XX
16 128 LSRK 230659.631 812.5 104000 230659.631 XX
17 128 LSRK 230741.634 812.5 104000 230741.634 XX
18 128 LSRK 230816.823 812.5 104000 230816.823 XX
19 128 LSRK 230898.825 812.5 104000 230898.825 XX
20 128 LSRK 230987.639 812.5 104000 230987.639 XX
21 128 LSRK 231069.641 812.5 104000 231069.641 XX
22 128 LSRK 231144.831 812.5 104000 231144.831 XX
23 128 LSRK 231226.833 812.5 104000 231226.833 XX
The sources contained in this measurement set are:
Source Name Description ID ==================================================================== 3c454.3 Bandpass and flux calibrator 9 1743-038 Gain calibrator 1 1908-201 Gain calibrator 6 Uranus Flux calibrator 13 g19.7 Science target (6-pointing mosaic) 2,3,4,5,7,8 ====================================================================
Other sources in the ms were not part of this program.
Initial inspection and flagging
Use plotms to inspect the data.
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='1~9,13',
avgchannel='3072')
There are a few bad data points in this ms. You can use the locate features in plotms to find the bad data points on field 8 and antenna ids 1-2 and 0-2. Flagging can be done in plotms, or in a script using the flagdata command. Here we will do all flagging within the script.
Tip: locate gives antenna ids, but flagdata looks first at the name column. Since SMA antenna names are numbers, this can be confusing. The corresponding names are antennas 2-3 and 1-3, which you can check with listobs.
flagdata(vis='g19_d2usb.ms',mode='manualflag',field='8',spw='20~23',
timerange='07:52:45~07:52:47',antenna='2&3;1&3')
Plotting again shows that the bad data are gone:
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='8',
avgchannel='3072')
Tip: to confirm the data were flagged in plotms, you need to change selection in plot (for example change field and then change back), and then change back to original to clear the cache and force a re-read of the data.
Make an inital amplitude vs. channel plot of the bandpass calibrator 3c454.3, averaging all the data together in time. Here, we are using plotxy because we would like to have multiple subplots (not yet functional in plotms). We set the plotxy parameter crossscan=T because there are two scans on 3c454.3. Note the rolloff of 24 individual spw. Try zooming to see better.
Tip: after you run plotxy, run clearstat() before trying to run plotms or you will get a table lock.
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="amp",datacolumn="data",
iteration="baseline",
antenna="",spw="",field="9",
averagemode="vector",width="1",timebin="all",
crossscans=T,crossbls=False,stackspw=F,
subplot=331,plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
As you can see in this plot, SMA spw overlap by a fair amount. Here we will flag the first seven channels on either side of each spw to aid calibration:
default('flagdata')
flagdata(vis='g19_d2usb.ms', mode='manualflag',spw='0~23:0~6;121~127')
On many baselines the first integration of every scan is low. These can also be flagged with flagdata. The integration time of these data is 30.9s. Note that more recent SMA data rarely show this problem.
flagdata(vis="g19_d2usb.ms",mode="quack",field='',
spw="0~23",quackinterval=40.0)
[Plotxy [plotxy]] can be used to plot the antenna positions. For these observations, antenna 8 was in the barn for repair.
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="x")
Bandpass Calibration
Next plot phase vs. channel. Note the large discrepancy in phase for spw=4-7 on some baselines - this will be important later.
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="phase",datacolumn="data",
iteration="baseline",
antenna="",spw="",field="9",
averagemode="vector",width="1",timebin="all",
crossscans=T,crossbls=False,stackspw=F,
subplot=331,plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
Now plot amplitude and phase as a function of time.
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='9',
avgchannel='3072')
The gap in the 3C454.3 observation is due to a pause to determine pointing solutions. The flags below catch times just before and after when the amplitudes and phase are off. This flagging could also have been accomplished interactively in plotms.
default('flagdata')
flagdata(vis="g19_d2usb.ms",field="9",timerange='12:16:58~12:19:00')
flagdata(vis="g19_d2usb.ms",field="9",timerange='12:08:00~12:09:30')
Here because plotms cannot do multipanel iteration yet we use the slower plotxy.
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="time",yaxis="phase",datacolumn="data",
iteration="baseline", antenna="",spw="0~23",field="9",
averagemode="vector",width="allspw",timebin="0",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
Start by determining an initial phase only solution for 3c454.3 using gaincal to take out major phase variations with time. For maximum sensitivity, we average all the spw together, with the exception of spw 4-7 which show large phase offsets from the other spw in phase vs. channel.
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.pcal',
field='9', spw='0~3,8~23', gaintype='G', minsnr=2.0,
refant='3', calmode='p',solint='int', combine='spw')
clearstat()
plotcal(caltable="g19_d2usb.ms.pcal",xaxis="time",yaxis="phase",
field="9",antenna="",spw="",timerange="",subplot=331,
overplot=False,clearpanel="Auto",iteration="antennas",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Next we do a bandpass calibration. There are several possible solution types. A regular 'B' type solution can work well if you have lots of S/N on your bandpass calibrator. You may wish to make this table and compare to 'BPOLY' solution further down. elaborate
bandpass(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.bpcal',
field='9', spw='0~23', bandtype='B', solint='inf', combine='scan',
refant='3', gaincurve=False, opacity=0.0,
gaintable='g19_d2usb.ms.pcal',spwmap=[0])
plotcal(caltable="g19_d2usb.ms.bpcal",xaxis="freq",yaxis="amp",
field="9",antenna="",spw="",timerange="",subplot=311,
overplot=False,clearpanel="Auto",iteration="antenna",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
A polynomial bandpass solution is more sensitive than simply fitting a polynomial to the channel based solutions 'B' after the fact. For the mm/submm, where the S/N is often low on the bandpass calibrator, 'BPOLY' is often the best choice, but every dataset is different. You may especially need to play with the degamp and degphase parameters in bandpass. The parameter combine='scan' is needed to average together the two 3c454.3 scans. The spwmap=[0] is telling it to apply the phase solution that was found from the average of all spw to each spw before determining the bandpass solution.
bandpass(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.bpoly7',
field='9', spw='0~23', bandtype='BPOLY',
solint='inf', combine='scan',
refant='3', degamp=7, degphase=7,
gaintable='g19_d2usb.ms.pcal',spwmap=[0])
clearstat()
plotcal(caltable="g19_d2usb.ms.bpoly7",xaxis="freq",yaxis="amp",
field="9",antenna="",spw="",timerange="",subplot=311,
overplot=False,clearpanel="Auto",iteration="antenna",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Unfortunately, this kind of plot with many spw and colors takes a long time. Be patient for now, as it's being worked on. You can safely ignore where the solution gets large at edges of spw. This is showing where we flagged channels - this is also being worked on. Zoom in if necessary to see that inner portions are nice and flat.
The next step is to apply the bandpass solution while re-calculating with gaincal the phase only solution for 3c454.3 on a short time interval (here, we use the integration time), but now including all spw (including 4~7 since antenna based solutions will have taken out phase vs.spw differences).
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.pcal2',
field='9', spw='0~23', gaintype='G', minsnr=2.0,
refant='3', calmode='p',solint='int', combine='spw',
gaintable=['g19_d2usb.ms.bpoly7'])
clearstat()
plotcal(caltable="g19_d2usb.ms.pcal2",xaxis="time",yaxis="phase",
field="9",antenna="",spw="",timerange="",subplot=331,
overplot=False,clearpanel="Auto",iteration="antennas",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Next we apply the antenna based bandpass, and phase only solution to solve for amplitude solutions over a longer solint to increase the S/N. The spwmap=[[0],[]] tells gaincal that the pcal solution is independent of spw while the bpoly7 solution is per spw. spwmap order must be in the same order as the tables in gaintable.
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.apcal',
field='9', spw='0~23', gaintype='G', minsnr=2.0,
refant='3', calmode='a',solint='300s', combine='spw',
gaintable=['g19_d2usb.ms.pcal2','g19_d2usb.ms.bpoly7'],
spwmap=[[0],[]])
clearstat()
plotcal(caltable="g19_d2usb.ms.apcal",xaxis="time",yaxis="amp",
field="9",antenna="",spw="",timerange="",subplot=331,
overplot=False,clearpanel="Auto",iteration="antennas",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Although in previous steps solutions were applied "on-the-fly", the data were not actually changed. Running applycal will fill the corrected data column in the ms. Again be careful with specification of gaintable, and keeping the same order in spwmap and gainfield. This applycal is not necessary for later steps, but allows plotting of data calibration to this point.
applycal(vis='g19_d2usb.ms',spw='0~23', field='9',
gaintable=['g19_d2usb.ms.pcal2','g19_d2usb.ms.apcal',
'g19_d2usb.ms.bpoly7'],
spwmap=[[0],[0],[]],gainfield=['9','9','9'])
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="amp",
datacolumn="corrected",iteration="baseline",
antenna='',spw="0~23",field="9",
averagemode="vector",width="1",timebin="all",crossscans=T,
crossbls=False,stackspw=False,extendflag=F,
extendchan="",extendspw="",extendant="",extendtime="",
plotcolor='darkcyan',subplot=331,
multicolor="none",figfile="")
As this plotxy shows, after antenna based bandpass, SMA data often show residual baseline based problems as a function of spw (i.e. a few abnormally low amplitudes for a few spw on a few baselines). To fix this problem we need to do a baseline based amplitude only solution per spw, but we'll need to remove an overall normalization factor first by combining all spw (this option will be incorporated into blcal one day so that only one run is necessary).
blcal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.blcal1',
field='9', spw='0~23',solint='inf', combine='spw,scan',
gaintable=['g19_d2usb.ms.pcal2','g19_d2usb.ms.apcal',
'g19_d2usb.ms.bpoly7'],
calmode='a',spwmap=[[0],[0],[]])
blcal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.blcal2',
field='9', spw='0~23',solint='inf', combine='scan',
gaintable=['g19_d2usb.ms.pcal2','g19_d2usb.ms.apcal',
'g19_d2usb.ms.blcal1','g19_d2usb.ms.bpoly7',],
calmode='a',spwmap=[[0],[0],[0],[]])
clearstat()
plotcal(caltable="g19_d2usb.ms.blcal1",xaxis="freq",yaxis="amp",
field="9",antenna="",spw="",timerange="",subplot=511,
overplot=False,clearpanel="Auto",iteration="antenna",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Now we can do a new applycal including only the second blcal2 solution. Note that applycal overwrites the corrected column, so there is no need to clearcal. Like the antenna based bandpass the blcal solution is independent for each spw, so we set spwmap = [].
applycal(vis='g19_d2usb.ms',spw='0~23', field='9',
gaintable=['g19_d2usb.ms.pcal2','g19_d2usb.ms.apcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],
spwmap=[[0],[0],[],[]],gainfield=['9','9','9','9'])
Note how flat the full bandpass is after all this calibration:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="amp",
datacolumn="corrected",iteration="baseline",
antenna='',spw="0~23",field="9",
averagemode="vector",width="1",timebin="all",crossscans=T,
crossbls=False,stackspw=False,extendflag=F,
extendchan="",extendspw="",extendant="",extendtime="",
plotcolor='darkcyan',subplot=331,
multicolor="none",figfile="")
Inspection of gain calibrators and setting the flux scale
Apply antenna and baseline based bandpass solutions to the gain calibrators with applycal:
clearstat()
applycal(vis='g19_d2usb.ms',spw='0~23', field='1,6',
gaintable=['g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],
spwmap=[[],[]],gainfield=['9','9'])
Have a look at the corrected data for both calibrators with channel vs. amplitude:
# First field 1:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="amp",datacolumn="corrected",
iteration="baseline", antenna="",spw="",field="1",
averagemode="vector",width="1",timebin="all",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
# Next field 6:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="channel",yaxis="amp",datacolumn="corrected",
iteration="baseline", antenna="",spw="",field="6",
averagemode="vector",width="1",timebin="all",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
Have a look at the corrected data for both calibrators in phase and amplitude vs. time. For the moment, unfortunately, multicolor='field' doesn't work, so this is easiest to do separately.
# First, amplitude vs. time for field 1:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",datacolumn="corrected",
iteration="baseline", antenna="",spw="0~23",field="1",
averagemode="vector",width="allspw",timebin="0",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
# Second, amplitude vs. time for field 6:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",datacolumn="corrected",
iteration="baseline", antenna="",spw="0~23",field="6",
averagemode="vector",width="allspw",timebin="0",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="red",
overplot=F,showflags=False,interactive=True,figfile="")
# Third, phase vs. time for field 1:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="time",yaxis="phase",datacolumn="corrected",
iteration="baseline", antenna="",spw="0~23",field="1",
averagemode="vector",width="allspw",timebin="0",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
# Last, phase vs. time for field 6:
clearstat()
plotxy(vis="g19_d2usb.ms",xaxis="time",yaxis="phase",datacolumn="corrected",
iteration="baseline", antenna="",spw="0~23",field="6",
averagemode="vector",width="allspw",timebin="0",
subplot=331,plotsymbol=".",
multicolor="none",plotcolor="darkcyan",
overplot=False,showflags=False,interactive=True,figfile="")
At the time of these observations, the calibrator J1911 had the most recent and relatively stable monitor data (SMA website), so we will use it for absolute flux calibration. In future tools for using resolved planets will be implemented.
1911-201 1mm 17 Jul 2005 11:38 SMA 274.5 1.88 +/- 0.13 mgurwell 1mm 05 Sep 2005 08:10 SMA 221.4 1.99 +/- 0.12 mgurwell
setjy(vis='g19_d2usb.ms', field='6', spw='0~23', fluxdensity=[2.0,0.,0.,0.])
Final gain and flux calibration for all calibrators
Next, we calculate two separate phase solutions from the data. To avoid decorrelation of the amplitude, the phase solutions fed to the amplitude calibration step should be at the shortest solint your S/N can support. Typically this will be the integration time.
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.allpcal',
field='1,6,9', spw='0~23', gaintype='G', minsnr=2.0,
refant='3', calmode='p',solint='int', combine='spw',
gaintable=['g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],
spwmap=[[],[]])
Unless you chose to do some more sophisticated smoothing, the phase solutions applied to your target might as well be on the scan time of your phase calibrator(s). Without combine='scan', the solution will not cross scan boundaries even though solint='inf'. This is an easy way to "manually" interpolate.
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.allpcalscan',
field='1,6,9', spw='0~23', gaintype='G', minsnr=2.0,
refant='3', calmode='p',solint='inf', combine='spw',
gaintable=['g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],
spwmap=[[],[]])
Plot the phase solutions of the phase calibrators. Can repeat for both short and long solution intervals.
clearstat()
plotcal(caltable="g19_d2usb.ms.allpcalscan",xaxis="time",yaxis="phase",
field="1,6",antenna="",spw="",timerange="",subplot=331,
overplot=False,clearpanel="Auto",iteration="antennas",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Amplitude calibration with longer solint and applying short solint phase solution.
gaincal(vis='g19_d2usb.ms', caltable='g19_d2usb.ms.allapcal',
field='1,6,9', spw='0~23', gaintype='G', minsnr=2.0,
refant='3', calmode='ap',solint='300s', combine='spw',
gaintable=['g19_d2usb.ms.allpcal','g19_d2usb.ms.bpoly7',
'g19_d2usb.ms.blcal2'],spwmap=[[0],[],[]])
Plot the amplitude solutions:
clearstat()
plotcal(caltable="g19_d2usb.ms.allapcal",xaxis="time",yaxis="amp",
field="1,6",antenna="",spw="",timerange="",subplot=331,
overplot=False,clearpanel="Auto",iteration="antennas",
plotsymbol="o",plotcolor="blue",showgui=True,figfile="")
Derive the absolute flux calibration using fluxscale (based on setjy above):
fluxscale(vis='g19_d2usb.ms',caltable='g19_d2usb.ms.allapcal',
fluxtable='g19_d2usb.ms.fluxcal',reference='6')
Apply final calibrations
The final application of calibration for each source is done independently below. Flux densities from SMA flux monitoring are provided as checks of the absolute flux calibration.
applycal(vis='g19_d2usb.ms',spw='0~23', field='9',
gaintable=['g19_d2usb.ms.allpcal','g19_d2usb.ms.fluxcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],spwmap=[[0],[0],[],[]],
gainfield=['9','9','9','9'])
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='9',
avgchannel='3072',ydatacolumn='corrected')
3C454.3 1mm 19 Aug 2005 16:01 SMA 225.3 27.36 +/- 1.37 mgurwell
applycal(vis='g19_d2usb.ms',spw='0~23', field='1',
gaintable=['g19_d2usb.ms.allpcal','g19_d2usb.ms.fluxcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],spwmap=[[0],[0],[],[]],
gainfield=['1','1','9','9'])
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='1',
avgchannel='3072',ydatacolumn='corrected')
J1743-038 1mm 26 Aug 2005 06:05 SMA 225.6 1.71 +/- 0.09 mgurwell
applycal(vis='g19_d2usb.ms',spw='0~23', field='6',
gaintable=['g19_d2usb.ms.allpcal','g19_d2usb.ms.fluxcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],spwmap=[[0],[0],[],[]],
gainfield=['6','6','9','9'])
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="time",yaxis="amp",field='6',
avgchannel='3072',ydatacolumn='corrected')
J1911-201 1mm 17 Jul 2005 11:38 SMA 274.5 1.88 +/- 0.13 mgurwell 1mm 05 Sep 2005 08:10 SMA 221.4 1.99 +/- 0.12 mgurwell
Since Uranus is resolved we apply the solutions from 3C454.3 to achieve at lest some reduction in instrumental gain variations.
applycal(vis='g19_d2usb.ms',spw='0~23', field='13',
gaintable=['g19_d2usb.ms.allpcal','g19_d2usb.ms.fluxcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],spwmap=[[0],[0],[],[]],
gainfield=['9','9','9','9'])
clearstat()
plotms(vis="g19_d2usb.ms",xaxis="uvdist",yaxis="amp",field='13',
avgchannel='3072',ydatacolumn='corrected')
A UV-distance plot of the expected flux of Uranus can be obtained from the SMA webpage. In future we will implement tools to use planets for absolute flux calibration.
applycal(vis='g19_d2usb.ms',spw='0~23', field='2,3,4,5,7,8',
gaintable=['g19_d2usb.ms.allpcalscan','g19_d2usb.ms.fluxcal',
'g19_d2usb.ms.bpoly7','g19_d2usb.ms.blcal2'],spwmap=[[0],[0],[],[]],
gainfield=['1,6','1,6','9','9'])
Split off target data for further inspection
split(vis="g19_d2usb.ms",outputvis='g19_d2usb_targets.ms',
field="2,3,4,5,7,8")
listobs(vis="g19_d2usb_targets.ms",verbose=F)
ID Code Name Right Ascension Declination Epoch 0 g19.3a 18:25:58.70 -12.03.57.80 J2000 1 g19.3b 18:25:57.40 -12.04.18.50 J2000 2 g19.3c 18:25:56.09 -12.04.28.20 J2000 3 g19.3d 18:25:54.60 -12.04.23.10 J2000 4 g19.3e 18:25:54.80 -12.04.43.80 J2000 5 g19.3f 18:25:53.30 -12.04.51.00 J2000
Tip: After splitting, the "corrected" data column in the original vis file will become the "data" and "corrected" columns and the field IDs are renumbered.
clearstat()
plotms(vis='g19_d2usb_targets.ms',xaxis="frequency",yaxis="amp",field='0',
avgtime='1e7',avgscan=True,avgbaseline=True)
clearstat()
plotms(vis='g19_d2usb_targets.ms',xaxis="time",yaxis="amp",field='',
avgchannel='3072',avgspw=True)
Data at times > 11:04:00 show lots of scatter: the elevation of these data are very low and are worth flagging. One can plotxy with xaxis="time", yaxis="elevation" to see this. For now to replot you must change the selection:
flagdata(vis="g19_d2usb_targets.ms",field="",timerange='>11:04:00')
Note that because the Doppler tracked frequency was 13CO (+ 10GHz in the USB), the velocity diplayed in in plotxy will not be correct unless you set the restfreq to the line of interest. [[plotms] Plotms] cannot do this yet.
CO(2-1) restfreq=230.53797 GHz
clearstat()
plotxy(vis="g19_d2usb_targets.ms",xaxis="velocity",yaxis="amp",
datacolumn="data",iteration="",selectdata=True,
antenna='',spw="0~23",field="0",timerange="",averagemode="vector",
restfreq='230.53797GHz',
width="1",timebin="all",crossscans=T,crossbls=T,
stackspw=False,subplot=111,interactive=T,figfile="")
The other weak line detected in this sideband is not visible in a vector average plot.
A-CH3OH (8 -1 8 0 -- 7 +0 7 0) 229.75876 GHz
Continuum imaging and subtraction
Next we want to make a continuum-free line dataset. We use field 0 to pick the line free spw. You need to make a clean mask. The strongest source is in the upper NE of the mosaic and there is a much weaker source to the SW corner.
clearstat()
plotxy(vis="g19_d2usb_targets.ms",xaxis="channel",yaxis="amp",
datacolumn="data",iteration="",selectdata=True,
antenna='',spw="0~23",field="0",timerange="",averagemode="vector",
restfreq='230.53797GHz',
width="1",timebin="all",crossscans=T,crossbls=T,
stackspw=False,subplot=111,interactive=T,figfile="")
The line is confined to spws 13~15.
Copy the original ms in case something goes wrong. Currently uvcontsub2 will change the input model and corrected columns, so it's best to make a back up. This behavior will change in future.
os.system('cp -r g19_d2usb_targets.ms g19_d2usb_targets_line.ms')
Now use new task uvcontsub2 to subtract the continuum. Unlike uvcontsub, this task will subtract the continuum estimate for spw that are not in the fitspw list. In future releases uvcontsub2 will likely replace uvcontsub. Setting fitspw='0~12,16~23' tells uvcontsub2 where to fit the continuum emission.
uvcontsub2(vis='g19_d2usb_targets_line.ms',fitspw='0~12,16~23',
solint='int',combine='spw',want_cont=True,spw='0~23')
The directory g19_d2usb_targets_line.ms.cont/ contains the estimated continuum, while g19_d2usb_targets_line.ms.contsub/ contains the continuum-subtracted line data.
Next we image the continuum data:
Tip: for sparse mosaics like this one, the subparameter ftmachine='ft' will typically give better results than the default ftmachine='mosaic'. For Nyquist sampled mosaics, ftmachine='mosaic' is the best choice, and the only choice for heterogeneous arrays. Also note that in a mosaic, the rms noise changes as a function of position. Therefore, the rms noise that you calculate from the radiometer equation is only valid where the combined primary beam response of the mosaic is near one. [[clean] Clean] weights the decision of what to clean next by the primary beam response function (PBRF), so emission near PBRF=1 will be cleaned faster than elsewhere. Thus, if you have emission away from the "sweet spot(s)" you will need to clean to a threshold lower than you might expect from the anticipated rms noise. Development is on-going to provide other options which may work better for the case of strong emission near image boundaries.
clean(vis='g19_d2usb_targets_line.ms.cont',imagename='g19_d2usb_cont',
field='',spw='0~23',
mode='mfs',niter=200,gain=0.1,threshold=0.0,
psfmode='clark',imagermode='mosaic',scaletype='SAULT',
ftmachine='ft',
interactive=T,imsize=500,cell="0.5arcsec",
phasecenter="J2000 18h25m56.09 -12d04m28.20",
pbcor=F,minpb=0.2)
viewer('g19_d2usb_cont.image')
Here you can see one stronger continuum source to the NE (18:25:58.5 -12:03:58.9) and one weak one to the SW (18:25:52, -12:04:53). The weak one is only visible after one round of cleaning. Because the mosaic is sparse you should make a clean mask to get the best cleaned image.
Make a dirty image of the continuum subtracted data, excluding the spws which contain line emission. You should see nothing but noise.
clean(vis='g19_d2usb_targets_line.ms.contsub',imagename='g19_d2usb_contsub',
field='',spw='0~12,16~23',
mode='mfs',niter=0,gain=0.1,threshold=0.0,
psfmode='clark',imagermode='mosaic',scaletype='SAULT',
ftmachine='ft',
interactive=F,imsize=500,cell="0.5arcsec",
phasecenter="J2000 18h25m56.09 -12d04m28.20",
pbcor=F,minpb=0.2)
You can look at the image with the viewer; you should see nothing because the continuum has been subtracted.
viewer('g19_d2usb_contsub.image')
Spectral line imaging
This image selects a channel range suitable to image the 12CO(2-1) line. Notice use of restfreq parameter to get velocity scale correct.
clean(vis='g19_d2usb_targets_line.ms.contsub',imagename='g19_d2usb_coline',
field='',spw='',
mode='velocity',start='-40km/s',nchan=50,width='3km/s',
interpolation='linear',
niter=1000,gain=0.1,threshold=0.2,
psfmode='clark',imagermode='mosaic',scaletype='SAULT',
ftmachine='ft',restfreq='230.53797GHz',
interactive=T,npercycle=400,
imsize=500,cell="0.5arcsec",
phasecenter="J2000 18h25m56.09 -12d04m28.20",
pbcor=F,minpb=0.15)
It is essential to run with interactive=T and make a clean mask. A clean mask is available in the original data directory spw_fits_files. To use the pre-made mask, run:
clean(vis='g19_d2usb_targets_line.ms.contsub',imagename='g19_d2usb_coline',
field='',spw='',
mode='velocity',start='-40km/s',nchan=50,width='3km/s',
niter=1000,gain=0.1,threshold=0.2,
psfmode='clark',imagermode='mosaic',scaletype='SAULT',
ftmachine='ft',restfreq='230.53797GHz',
interactive=F,npercycle=400,
imsize=500,cell="0.5arcsec",
mask='spw_fits_files/coline.mask',
phasecenter="J2000 18h25m56.09 -12d04m28.20",
pbcor=F,minpb=0.15)
<\source>
View the image produced:
<source lang="python">
viewer('g19_d2usb_coline.image')
Now make 0th and 1st moment maps.
# 0th moment map
immoments(imagename='g19_d2usb_coline.image',moments=[0],axis='spectral',
chans='12~39',outfile='g19_d2usb_coline.mom0')
viewer('g19_d2usb_coline.mom0')
# 1st moment map
immoments(imagename='g19_d2usb_coline.image',moments=[1],axis=3,
chans='12~39',outfile='g19_d2usb_coline.mom1',
includepix=[0,2])
immath(outfile='g19_d2usb_coline.mom1masked',mode='evalexpr',
expr='"g19_d2usb_coline.mom1"["g19_d2usb_coline.mom0">9]')
viewer('g19_d2usb_coline.mom1masked')
By clicking on "folder" icon in viewer window you can bring up the moment0 as a contour image. The strange appearence of the the mom1 map toward the NE source is probably due to more than one outflow being superposed.
Note that one could and should correct the image for the primary beam response using immath to divide the image by the .flux image. One would then need to make a mask for the moment images in order to hide the ugly stuff at the edges.
