NGC3256Band3 for CASA 3.3: Difference between revisions
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[Also provide links to the calibrated data (but maybe not here?)] | [Also provide links to the calibrated data (but maybe not here...maybe better at end of calibration page?)] | ||
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This output shows that three fields were observed: 1037-295, Titan, and NGC3256. Field 0 (1037-295) will serve as the gain calibrator and bandpass calibrator; Titan will serve as the flux calibrator; and NGC3256 is, of course, the science target. | This output shows that three fields were observed: 1037-295, Titan, and NGC3256. Field 0 (1037-295) will serve as the gain calibrator and bandpass calibrator; field 1 (Titan) will serve as the flux calibrator; and field 2 (NGC3256) is, of course, the science target. | ||
Note that there are more than four SpwIDs even though the observations were set up to have four spectral windows. The spectral line data themselves are found in spectral windows 1,3,5,7, which have 128 channels each. The first one (spw 1) is centered on the CO(1-0) emission line in the galaxy NGC 3256 and is our highest frequency spectral window. There is one additional spectral window (spw 3) in the Upper Side Band (USB), and there are two spectral windows (spw 5 and 7) in the Lower Side Band (LSB). These additional spectral windows are used to measure the continuum emission in the galaxy, and may contain other emission lines as well. | Note that there are more than four SpwIDs even though the observations were set up to have four spectral windows. The spectral line data themselves are found in spectral windows 1,3,5,7, which have 128 channels each. The first one (spw 1) is centered on the CO(1-0) emission line in the galaxy NGC 3256 and is our highest frequency spectral window. There is one additional spectral window (spw 3) in the Upper Side Band (USB), and there are two spectral windows (spw 5 and 7) in the Lower Side Band (LSB). These additional spectral windows are used to measure the continuum emission in the galaxy, and may contain other emission lines as well. | ||
Revision as of 21:32, 19 May 2011
Overview
[To be written by Eric]
Retrieving the Data
The data were taken in six different datasets over two consecutive nights: April 16-17, 2011. There are three datasets for April 16th and three for April 17th. Here we provide you with "starter" datasets, where we have taken the raw data in ALMA Science Data Model (ASDM) format and converted them to CASA Measurement Sets (MS). We did this using the importasdm task in CASA.
[What else are we going to do to the data we provide?]
Along with the Measurement Sets, we also provide some tables that you will need for the calibration. These include the System Temperature (Tsys) tables, which contain corrections for atmospheric opacity, and Water Vapor Radiometer (WVR) tables, which contain the atmospheric phase corrections determined by the water vapor radiometers on each antenna.
You can download the data here: [Provide link to the raw .ms files in tar'd, gzip'd format]
Once the download has finished, unpack the file:
# In a terminal outside CASA
tar -xvf ngc3256band3.tgz
[Also provide links to the calibrated data (but maybe not here...maybe better at end of calibration page?)]
Initial Inspection and A priori Flagging
We will eventually concatenate the six datasets used here into one large dataset. However, we will keep them separate for now, as some of the steps to follow require individual datasets (specifically, the application of the Tsys and WVR tables). We therefore start by defining an array 'basename' that includes the names of the six files. This will simplify the following steps by allowing us to loop through the files using a simple for-loop in python.
# In CASA
basename=['uid___A002_X1d54a1_X5','uid___A002_X1d54a1_X174','uid___A002_X1d54a1_X2e3','uid___A002_X1d5a20_X5','uid___A002_X1d5a20_X174','uid___A002_X1d5a20_X330']
The usual first step is then to get some basic information about the data. We do this using the task listobs, which will output a detailed summary of each dataset supplied.
# In CASA
for name in basename:
listobs(vis=name+'.ms')
The output will be sent to the CASA logger. You will have to scroll up to see the individual output for each of the six datasets. Here is an example of the most relevant output for the first file in the list.
Fields: 3 ID Code Name RA Decl Epoch SrcId nVis 0 none 1037-295 10:37:16.0790 -29.34.02.8130 J2000 0 38759 1 none Titan 00:00:00.0000 +00.00.00.0000 J2000 1 16016 2 none NGC3256 10:27:51.6000 -43.54.18.0000 J2000 2 151249 (nVis = Total number of time/baseline visibilities per field) Spectral Windows: (9 unique spectral windows and 2 unique polarization setups) SpwID #Chans Frame Ch1(MHz) ChanWid(kHz)TotBW(kHz) Ref(MHz) Corrs 0 4 TOPO 184550 1500000 7500000 183300 I 1 128 TOPO 113211.988 15625 2000000 113204.175 XX YY 2 1 TOPO 114188.55 1796875 1796875 113204.175 XX YY 3 128 TOPO 111450.813 15625 2000000 111443 XX YY 4 1 TOPO 112427.375 1796875 1796875 111443 XX YY 5 128 TOPO 101506.187 15625 2000000 101514 XX YY 6 1 TOPO 100498.375 1796875 1796875 101514 XX YY 7 128 TOPO 103050.863 15625 2000000 103058.675 XX YY 8 1 TOPO 102043.05 1796875 1796875 103058.675 XX YY Sources: 48 ID Name SpwId RestFreq(MHz) SysVel(km/s) 0 1037-295 0 - - 0 1037-295 9 - - 0 1037-295 10 - - 0 1037-295 11 - - 0 1037-295 12 - - 0 1037-295 13 - - 0 1037-295 14 - - 0 1037-295 15 - - 0 1037-295 1 - - 0 1037-295 2 - - 0 1037-295 3 - - 0 1037-295 4 - - 0 1037-295 5 - - 0 1037-295 6 - - 0 1037-295 7 - - 0 1037-295 8 - - 1 Titan 0 - - 1 Titan 9 - - 1 Titan 10 - - 1 Titan 11 - - 1 Titan 12 - - 1 Titan 13 - - 1 Titan 14 - - 1 Titan 15 - - 1 Titan 1 - - 1 Titan 2 - - 1 Titan 3 - - 1 Titan 4 - - 1 Titan 5 - - 1 Titan 6 - - 1 Titan 7 - - 1 Titan 8 - - 2 NGC3256 0 - - 2 NGC3256 9 - - 2 NGC3256 10 - - 2 NGC3256 11 - - 2 NGC3256 12 - - 2 NGC3256 13 - - 2 NGC3256 14 - - 2 NGC3256 15 - - 2 NGC3256 1 - - 2 NGC3256 2 - - 2 NGC3256 3 - - 2 NGC3256 4 - - 2 NGC3256 5 - - 2 NGC3256 6 - - 2 NGC3256 7 - - 2 NGC3256 8 - - Antennas: 7: ID Name Station Diam. Long. Lat. 0 DV04 J505 12.0 m -067.45.18.0 -22.53.22.8 1 DV06 T704 12.0 m -067.45.16.2 -22.53.22.1 2 DV07 J510 12.0 m -067.45.17.8 -22.53.23.5 3 DV08 T703 12.0 m -067.45.16.2 -22.53.23.9 4 DV09 N602 12.0 m -067.45.17.4 -22.53.22.3 5 PM02 T701 12.0 m -067.45.18.8 -22.53.22.2 6 PM03 J504 12.0 m -067.45.17.0 -22.53.23.0
This output shows that three fields were observed: 1037-295, Titan, and NGC3256. Field 0 (1037-295) will serve as the gain calibrator and bandpass calibrator; field 1 (Titan) will serve as the flux calibrator; and field 2 (NGC3256) is, of course, the science target.
Note that there are more than four SpwIDs even though the observations were set up to have four spectral windows. The spectral line data themselves are found in spectral windows 1,3,5,7, which have 128 channels each. The first one (spw 1) is centered on the CO(1-0) emission line in the galaxy NGC 3256 and is our highest frequency spectral window. There is one additional spectral window (spw 3) in the Upper Side Band (USB), and there are two spectral windows (spw 5 and 7) in the Lower Side Band (LSB). These additional spectral windows are used to measure the continuum emission in the galaxy, and may contain other emission lines as well.
Spectral windows 2,4,6,8 contain channel averages of the data in spectral windows 1,3,5,7, respectively. These are not useful for the offline data reduction. Spectral window 0 contains the WVR data. You may notice that there are additional SpwIDs listed in the "Sources" section which are not listed in the "Spectral Windows" section. These spectral windows are reserved for the WVRs of each antenna (seven in our case). At the moment, all WVRs point to spw 0, which contains nominal frequencies. The additional spectral windows (spw 9-15) are therefore not used and can be ignored.
Another important thing to note is that the position of Titan is listed as 00:00:00.0000 +00.00.00.0000. This is due to the fact that for ephemeris objects, the positions are currently not stored in the asdm. This will be handled correctly in the near future, but at present, we have to fix this offline. We will correct the coordinates below by running the procedure fixplanet.
There were seven antennas in the array for these observations. Note that numbering in python always begins with "0", so the antennas have IDs 0-6. To see what the antenna configuration looked like at the time of the observations, we will use the task plotants. Since the configuration did not change during the course of the observations, we will simply look at the first dataset from the list.
# In CASA
plotants(vis=name[0]+'.ms', figfile='ngc3256band3_plotants.png')
This will plot the antenna configuration on your screen as well as save it under the specified filename for future reference. This will be important later on when we need to choose a reference antenna, since the reference antenna should be close to the center of the array (as well as stable and present for the entire observation).
The first editing we will do is some a priori flagging. We will start by flagging the shadowed data and the autocorrelation data:
# In CASA
for name in basename:
flagdata(vis=name+'.ms', flagbackup = F, mode = 'shadow')
flagautocorr(vis=name+'.ms')
There are a number of scans in the data that were used by the online system for pointing calibration. These scans are no longer needed, and we can flag them easily by selecting on 'intent':
# In CASA
for name in basename:
flagdata(vis=name+'.ms', mode='manualflag', flagbackup = F, intent='*POINTING*')
Similarly, we can flag the scans corresponding to atmospheric calibration:
# In CASA
for name in basename:
flagdata(vis=name+'.ms', mode='manualflag', flagbackup = F, intent='*ATMOSPHERE*')
We will then store the current flagging state for each dataset using the flagmanager:
# In CASA
for name in basename:
flagmanager(vis = name+'.ms', mode = 'save', versionname = 'Apriori')
We will continue with some initial flagging/corrections specific to these datasets. For uid___A002_X1d54a1_X174.ms there is a outlying feature in spw=7, antenna DV04. This corresponds to scans 5 and 9, so we flag those data:
# In CASA
flagdata(vis='uid___A002_X1d54a1_X174.ms', mode='manualflag',
antenna='DV04', flagbackup = F, scan='5,9', spw='7')
Antenna DV07 shows large delays for the first three datasets. We correct this by calculating a K-type delay calibration table with gencal. The parameters are the delays measured in nanoseconds, first cycling over polarization product, and then over spectral window (thus giving eight numbers in total). Before creating these tables, make sure to delete any existing versions.
# In CASA
for i in range(3): # loop over the first three ms's
name=basename[i]
os.system('rm -rf '+name+'_del.K')
gencal(vis=name+'.ms', caltable=name+'_del.K',
caltype='sbd', antenna='DV07', pol='X,Y', spw='1,3,5,7',
parameter=[0.99, 1.10, -3.0, -3.0, -3.05, -3.05, -3.05, -3.05])
[MARTIN, HOW DID YOU GET THESE PARAMETERS? I ASSUME YOU FIT THE WRAPPING SOMEHOW AND PERHAPS WE SHOULD MENTION IT]
We will apply these K tables to the data in the next section.
WVR Correction and Tsys Calibration
First, we apply the delay correction table and the WVR calibration tables to the data. We do this in two steps, first cycling over the three datasets from the first day of observations because we have to correct the delay error for DV07 for those data. For the last three datasets, taken during the second day, we do not need to correct the delays, so we just apply the WVR tables. For both types of tables, we will use interpolation "nearest". [WHY?]
# In CASA
for i in range(3): # loop over the first three data sets
name=basename[i]
applycal(vis=name+'.ms', flagbackup=F, spw='1,3,5,7',
interp='nearest', gaintable=[name+'_del.K',name+'.W'])
for i in range(3,6): # loop over the last three data sets
name=basename[i]
applycal(vis=name+'.ms', flagbackup=F, spw='1,3,5,7',
interp='nearest', gaintable=name+'.W')
Now we split out the datasets with delays and WVR tables applied. These datasets are given the extention "_K_WVR" to indicate that the delay tables and WVR tables have been applied. Again, we are careful to remove any previous versions of the split ms's before running the split command.
# In CASA
for name in basename:
os.system('rm -rf '+name+'_K_WVR.ms*')
split(vis=name+'.ms', outputvis=name+'_K_WVR.ms',
datacolumn='corrected')
Next we do the Tsys calibration. Tsys measurements correct for the atmospheric opacity (to first-order) and allow the calibration sources to be measured at elevations that differ from the science target. The Tsys tables for these datasets were provided with the downloadable data. We will start by inspecting them:
# In CASA
for name in basename:
plotcal(caltable='tsys_'+name+'.cal', xaxis='freq', yaxis='amp',
spw='1,3,5,7', timerange='<2020', subplot=221, overplot=False,
iteration='spw', plotrange=[0, 0, 40, 180], plotsymbol='.',
figfile='tsys_per_spw'+name+'.png')
Note that we only plot the spectral windows with the spectral line data, and we set timerange="<2020" because... [WHY?] In addition to plotting on your screen, the above command will also produce a plot file (png) for each of the six datasets.
The plots look acceptable upon examination, so we will apply the Tsys tables with applycal: We do this for each field separately so that the appropriate calibration data are applied to the right fields. The "field" parameter specifies the field to which we will apply the calibration, and the "gainfield" parameter specifies the field from which you wish to take the calibration solutions from the gaintable.
# In CASA
for name in basename:
for field in ['Titan','1037*','NGC*']:
applycal(vis=name+'_K_WVR.ms', spw='1,3,5,7', flagbackup=F, field=field, gainfield=field,
interp='nearest', gaintable=['tsys_'+name+'.cal'])
We then split out spectral windows 1,3,5,7. This will get rid of the channel averaged spectral windows, as well as spw 0, which is the one for the WVR data. It will also remove the "WVR placeholder" spectral windows.
# In CASA
for name in basename:
os.system('rm -rf '+name+'_line.ms*')
split(vis=name+'_K_WVR.ms', outputvis=name+'_line.ms',
datacolumn='corrected', spw='1,3,5,7')
The WVR and Tsys tables are now applied in the DATA column of the resultant measurement sets. The new data sets have the extension "_line" to indicate that these only contain the line data, and no longer the "channel average" spectral windows. These measurement sets therefore have four spectral windows.
Now that we have applied the Tsys calibration and WVR corrections, we can concatenate the six individual data sets into one big measurement set. We define an array "comvis" that contains the names of the measurement sets we wish to concatenate, and then we run the task concat.
# In CASA
comvis=[]
for name in basename:
comvis.append(name+'_line.ms')
os.system('rm -rf ngc3256_line.ms*')
concat(vis=comvis, concatvis='ngc3256_line.ms')
---More to come here--- [STILL?]
Additional Data Inspection
Now that the data are concatenated into one dataset, we will do some additional inspection. First we will plot amplitude versus channel, averaging over time and baselines in order to speed up the plotting process.
# In CASA
plotms(vis=ngc3256_line.ms',xaxis='channel',yaxis='amp',
averagedata=T,avgbaseline=T,avgtime='1e8',avgscan=T)
From this plot we see that the edge channels have abnormally high amplitudes. We will use flagdata to remove some channels from both sides of the bandpass:
# In CASA
flagdata(vis = 'ngc3256_line.ms', flagbackup = F, spw = ['*:0~10','*:125~127'])
Next, we will look at amplitude versus time, averaging over
Titan is our primary flux calibrator. However, for the second day of observations, Titan had moved to close to Saturn, and the rings move into the primary beam. [Check this be using plotms, plot amp vs. uvdist.]. We therefore flag the Titan scans for the second day:
# In CASA
flagdata(vis = 'ngc3256_line.ms', flagbackup = F,
timerange='>2011/04/16/12:00:00', field='Titan')
Now fix the position of Titan in the combined data set. The position of Titan is set to 00,00, but the following procedure will replace that with the position that the telescopes were actually pointing at and recalculates the uvw coordinates:
# In CASA
execfile(os.getenv("CASAPATH").split(' ')[0]+"/lib/python2.6/recipes/fixplanets.py")
fixplanets('ngc3256_line.ms', 'Titan', True)
Baselines with DV07 have very high amps in YY in the last spectral window:
# In CASA
flagdata(vis='ngc3256_line.ms', flagbackup=F, spw='3',
correlation='YY', mode='manualflag', selectdata=T,
antenna='DV07', timerange='')
Baselines with DV08 have very low amps for the last data set. Only for the last spectral window, and only YY
# In CASA
flagdata(vis='ngc3256_line.ms', flagbackup=F, spw='3',
correlation='YY', mode='manualflag', selectdata=T,
antenna='DV08', timerange='>2011/04/17/03:00:00')
Baselines with PM03 have low amps at 2011/04/17/02:15:00. Only for the first spectral window
# In CASA
flagdata(vis='ngc3256_line.ms', flagbackup=F, spw='0',
mode='manualflag', selectdata=T, antenna='PM03',
timerange='2011/04/17/02:15:00~02:15:50')
Baselines with PM03 have low amps at 2011/04/16/04:15:15. Only for the spectral windows 2 and 3
# In CASA
flagdata(vis='ngc3256_line.ms', flagbackup=F, spw='2,3',
mode='manualflag', selectdata=T, antenna='PM03',
timerange='2011/04/16/04:13:50~04:18:00')
Bandpass Calibration
Before we do the bandpass calibration, we use gaincal to determine phase-only gaincal solutions for the bandpass calibrator, to correct for any phase variations with time. In these data, the phase calibrator and bandpass calibrator are the same source, so we just run this on 1037. For the solution interval we use solint='inf', which means that one gain solution will be determined for every scan. For our reference antenna, we choose PM03. The average of channels 40 to 80 is used to determine the antenna-based phase solutions. The output calibration table is named "ngc3256.G1".
# In CASA
gaincal(
vis = 'ngc3256_line.ms', caltable = 'ngc3256.G1', spw = '*:40~80', field = '1037*',
selectdata=T, solint= 'int', refant = 'PM03', calmode = 'p')
[IS SOLINT='INF' REALLY THE RIGHT THING TO DO? I WAS ALWAYS TAUGHT TO USE SOMETHING SHORT FOR THIS, LIKE THE INTEGRATION TIME...] -> Yes, changed to int
We check the time variations of the phases with plotcal. We make plot of the XX and YY polarization products separately and make different subplots for each of the spectal windows. This is done by selecting iteration of 'spw' and subplot=221. and generate png plots
# In CASA
plotcal(
caltable = 'ngc3256.G1', xaxis = 'time', yaxis = 'phase',
poln='X', plotsymbol='o', plotrange = [0,0,-180,180], iteration = 'spw',
figfile='phase_vs_time_XX.G1.png', subplot = 221)
# In CASA
plotcal(
caltable = 'ngc3256.G1', xaxis = 'time', yaxis = 'phase',
poln='Y', plotsymbol='o', plotrange = [0,0,-180,180], iteration = 'spw',
figfile='phase_vs_time_YY.G1.png', subplot = 221)
Now that we have a first measurement of the phase variations as function of time, we can determine the bandpass solutions with bandpass, using the phase calibration table 'on-the-fly'.
First, plot the phase as a function of frequency for 1037. We use avgscan=T and avgtime='1E6' to average in time over all scans, and coloraxis='baseline' is used to colorize by baseline.
# In CASA
plotms(vis='ngc3256_line.ms', xaxis='freq', yaxis='phase', selectdata=True,
field='1037*', avgtime='1E6', avgscan=T, coloraxis='baseline', iteraxis='antenna')
and the amplitudes
# In CASA
plotms(vis='ngc3256_line.ms', xaxis='freq', yaxis='amp', selectdata=True, spw='*:10~120',
field='1037*', avgtime='1E6', avgscan=T, coloraxis='baseline', iteraxis='antenna')
Bandpass calibration, using the first gaincal on-the-fly
# In CASA
bandpass(vis = 'ngc3256_line.ms', caltable = 'ngc3256.B1', gaintable = 'ngc3256.G1',
field = '1037*', minblperant=3, minsnr=1, solint='inf',
bandtype='B', fillgaps=1, refant = 'PM03', solnorm = F)
# In CASA
plotcal(caltable = 'ngc3256.B1', xaxis='freq',yaxis='phase', spw='',
subplot=212, overplot=False, plotrange = [0,0,-70,70],
plotsymbol='.', timerange='')
plotcal(caltable = 'ngc3256.B1', xaxis='freq',yaxis='amp', spw='',
subplot=211, overplot=False,
figfile='bandpass.B1.png', plotsymbol='.', timerange='')
[MOVE THIS SOMEWHERE ELSE?]
Get flux density for Titan using the Butler-JPL-Horizons 2010 model. The flux density of Titan is 296 mJy
# In CASA
setjy(vis='ngc3256_line.ms', field='Titan', spw='', modimage='',
scalebychan=False, fluxdensity=-1,
standard='Butler-JPL-Horizons 2010')
Plot amplitude as function of uv distance for Titan for the remaining data. It looks unresolved
# In CASA
plotms(vis='ngc3256_line.ms', xaxis='uvdist', yaxis='amp',
ydatacolumn='corrected', selectdata=True, field='Titan',
spw='', averagedata=True, avgchannel='128', avgtime='',
avgscan=True, avgbaseline=F)
Gain Calibration
Now do a new gaincal, using the bandpass on-the-fly
# In CASA
gaincal(vis = 'ngc3256_line.ms', caltable = 'ngc3256.G2', spw =
'0:30~90,1:30~90,2:30~90,3:30~90', field = '1037*,Titan',
solint= 'inf', selectdata=T, solnorm=False, refant = 'PM03',
gaintable = ['ngc3256.B1'], calmode = 'ap')
Generate plots:
# In CASA
plotcal(caltable = 'ngc3256.G2', xaxis = 'time', yaxis = 'phase',
poln='X', plotsymbol='o', plotrange = [0,0,-180,180], iteration
= 'spw', figfile='phase_vs_time_XX.G2.png', subplot = 221)
plotcal(caltable = 'ngc3256.G2', xaxis = 'time', yaxis = 'phase',
poln='Y', plotsymbol='o', plotrange = [0,0,-180,180], iteration
= 'spw', figfile='phase_vs_time_YY.G2.png', subplot = 221)
plotcal(caltable = 'ngc3256.G2', xaxis = 'time', yaxis = 'amp',
poln='X', plotsymbol='o', plotrange = [], iteration = 'spw',
figfile='amp_vs_time_XX.G2.png', subplot = 221)
plotcal(caltable = 'ngc3256.G2', xaxis = 'time', yaxis = 'amp',
poln='Y', plotsymbol='o', plotrange = [], iteration = 'spw',
figfile='amp_vs_time_YY.G2.png', subplot = 221)
# In CASA
fluxscale( vis='ngc3256_line.ms', caltable='ngc3256.G2',
fluxtable='ngc3256.G2.flux', reference='Titan',
transfer='1037*', append=False)
