VLA CASA Calibration Pipeline 5.6.2

Advisory to users (Feb. 11, 2020; updated)

A pipeline bug in CASA 5.6.2-2 was discovered that impacts the restoration of calibrations for projects calibrated between October 21, 2019 and February 10, 2020. A pipeline fix was introduced with CASA 5.6.2-3 and the archived calibrations have been corrected. Users can now properly restore data on their own or using archive-new.

 

General Description

The VLA calibration pipeline performs basic flagging and calibration using CASA. It is currently designed to work for Stokes I continuum data (except P-band), but may work in other circumstances as well. Each astronomical Scheduling Block (SB) observed by the VLA is automatically processed through the pipeline. The VLA calibration pipeline does the following:

• Loads the data into from the archival format (Science Data Model-Binary Data Format [SDM-BDF]) to a CASA MeasurementSet (MS), applies Hanning smoothing (when the data were not frequency averaged by the VLA correlator), and obtains information about the observing set-up from the MS;
• Applies online flags and other deterministic flags (shadowed data, edge channels of sub-bands, etc.);
• Prepares models for primary flux density calibrators;
• Derives pre-determined calibrations (antenna position corrections, gain curves, atmospheric opacity corrections, requantizer gains, etc.);
• Iteratively determines initial delay and bandpass calibrations, including flagging of RFI (Radio Frequency Interference) and some automated identification of system problems;
• Derives initial gain calibration, and derives the spectral index of the bandpass calibrator;
• RFI flagging is done on data with the initial calibration applied;
• Derives final delay, bandpass, and gain/phase calibrations, and applies them to the data;
• Runs the RFI flagging algorithm on the target data;
• Calculates data weights based on the inverse square RMS noise of the MS;
• Creates diagnostic images of calibrators.

For more information about pipeline heuristics, please see the pipeline presentations from the 2019 VLA Data Reduction workshop.

In addition to the CASA integrated pipeline (available with the CASA package), a scripted pipeline is available for some CASA versions that may be useful. Please see the VLA scripted calibration pipeline web page for details.

Please see the Release Notes and Known issues below. For questions, suggestions, and other issues encountered with the pipeline, please submit a ticket to the Pipeline Department of the NRAO Helpdesk.

 

VLA Pipeline 5.6.2 Release Notes

• Flux density calibration now makes use of the hifv_fluxboot2 task, featuring outlier rejection for better flux density bootstrapping, usage of CASA task flux scale, multi-order spectral fitting depending on fractional bandwidth, and a global flux density fit across all observed bands in a dataset
• hifv_flagbaddef will no longer flag single spectral windows; RFI could erroneously trigger flagging of an entire spectral window prior to RFI flagging
• Support for uv-range selection of calibrators using flux.csv to enable easier calibration of data observed with a resolved calibrator. Optimal for calibrator that is point-source dominant, but some large-scale resolved structure.
• The pipeline has now implemented quality assessment (qa) score heuristics for all pipeline stages.
• Warnings will shown the antenna name rather than antenna ID, e.g., ea14 vs. 14
• See also the ALMA pipeline documentation for general, non VLA specific infrastructure changes

Obtaining the Pipeline

The pipeline is released and included with CASA, the Obtaining CASA webpage has links to the CASA version with the most recent VLA pipeline and provides access to older versions.

The scripted pipeline versions may continue to get updates in addition to the integrated versions for those who require greater flexibility when modifying their reduction procedures. If you are interested in obtaining the scripted pipeline, please see the Scripted Pipeline page.

 

Pipeline Requirements

1. The VLA calibration pipeline runs on each completed SB (typically a single SDM-BDF) separately; there is currently no provision for it running on collections of SBs.
2. The pipeline relies on correctly set scan intents. We therefore recommend that every observer ensures that the scan intents are correctly specified in the Observation Preparation Tool (OPT) during the preparation of the SB (see OPT manual for details). Typical intents are:
   
   • CALIBRATE_FLUX (required): flux density scale calibration scans (toward one of the standard VLA calibrators 3C48, 3C138, 3C147, or 3C286), the pipeline will use the first field with this intent; if this intent is not present, the pipeline will fail
   • CALIBRATE_AMPLI and CALIBRATE_PHASE (required): temporal complex gain/phase calibration; if these intents are not present, the pipeline will fail
   • CALIBRATE_BANDPASS (optional): scan that is used to obtain the bandpass calibration (only the first instance of CALIBRATE_BANDPASS is used regardless of the band; therefore multi-band scheduling blocks may encounter problems when different bandpass calibrators are used); if not present, the first field with scan intent CALIBRATE_FLUX will be used for bandpass calibration
   • CALIBRATE_DELAY (optional): delay calibrator scan; if not present the first scan with a CALIBRATE_BANDPASS intent is used for delay calibration, and if that one is not available delays are calculated using the first CALIBRATE_FLUX scan.
3. The pipeline also currently requires a signal-to-noise of >~3 for each spectral window of a calibrator per integration (for each channel of the bandpass).

 

Automatic Processing for Science Observations

Starting with Semester 2013A D-configuration, a version of the calibration pipeline has been run automatically at the completion of all astronomical scheduling blocks, except for P-band observations, with the resulting calibration tables and flags archived for future use. At NRAO we execute the standard pipeline, which implies that it is optimized for Stokes I continuum processing, independent of the actual science goal. A user may therefore decide to re-run the pipeline after making appropriate modifications.

Investigators are notified when the calibrated data are ready for download; detailed quality assurance checks can be performed by NRAO staff upon request. The calibrated visibility data are retained on disk for 15 days after the pipeline has completed to enable investigators to download and image at their home institution or remotely using NRAO computing resources. Calibrated data can also be restored after this nominal time period by re-generating the MS from the raw SDM-BDF data file downloaded from the NRAO archive and applying the saved calibration and flag tables. See the section "Restore calibration from archived products" for details on the restoration procedures. To request any of the automatic pipeline processed data, please submit a ticket to Pipeline Department of the NRAO Helpdesk.

Science Ready Data Products (SRDP) Processing

Starting in June 2019, a subset of VLA projects will undergo a more rigorous quality assurance process as part of the NRAO SRDP Initiative. As of September 2019 this was being done on most A and B rated single-band, continuum-only projects observing at X-band and above. Users will be delivered calibrated data that may have additional flagging applied and are expected to be ready for imaging by the user.

Running the Pipeline

The pipeline can take a few hours to a few days to complete depending on the specifics of the observation; ensure that your process can run for the full duration without interruption. Also, make sure that there is enough space in your directory as the data volume will increase by a factor of about four. There are several ways to run the pipeline and, in most cases, we recommend starting with the raw data (an SDM-BDF) that can be requested from the NRAO archive. Place your data (preferably the SDM-BDF, but an MS is also acceptable) in its own directory for processing. For example:

#In a Terminal
mkdir myVLAdata
mv mySDM myVLAdata/
cd myVLAdata

Next, start CASA from the same directory where you placed your SDM-BDF. Note: do not try to run the pipeline from a different directory by giving it the full path to a dataset, as some of the CASA tasks require the MS to be co-located with its associated gain tables. And do not try to run the pipeline from inside the SDM-BDF or MS directories themselves. While SDM-BDFs and MSs are directories, they should always be treated as single entities that are accessed from the outside. It is also important that a fresh instance of CASA is started from the directory that will contain the SDM-BDF or MS, rather than using an existing instance of CASA and using "cd" to move to a new directory from within CASA, as the output plots will then end up in the wrong place and potentially overwrite your previous pipeline results.

 

Starting CASA with Pipeline Tasks

To start CASA with the pipeline from your own installation type:

#In a Terminal
casa --pipeline

Note that starting CASA without the --pipeline option will start CASA without any of the pipeline-specific tasks. (In turn, if you try to use 'casa --pipeline' for manual data reduction, plots that are using matplotlib, like plotcal, will not work; use 'casa'  without --pipeline for manual data reduction.)  

If you are at the New Mexico Array Science Center (NMASC) or using NRAO computing resources at the NMASC, we provide a shortcut to the latest CASA version that includes the pipeline. To start this version, type:

#In a Terminal
casa-pipe

To list other versions of CASA with the pipeline that are available at the NMASC, type:

#In a Terminal
casa-pipe -ls

To start a particular version, type:

#In a Terminal
casa-pipe -r <full text from version list>

Now that CASA is open, there are several ways to start the pipeline.

The CASA homepage has more information on using CASA at NRAO.  

 

Method 1: import hifv

The pipeline comes with several predefined sets of instructions, called recipes, to accommodate for different needs: one for VLA data, one for ALMA data, one for VLASS, etc. Once started, the pipeline does not require any further input from the user and should run to completion automatically. The default VLA recipe for Stokes I continuum is called hifv which stands for 'heuristics, interferometry, VLA'. To use this VLA data recipe, you first need to import it into CASA via the following command from the CASA prompt:

# In CASA
import pipeline.recipes.hifv as hifv

and then start the pipeline via:

# In CASA
hifv.hifv(['mySDM'])

where mySDM is the name of the SDM-BDF from your observations.

 

Method 2: casa_pipescript.py

If you have a 'casa_pipescript.py' file (see example below) from any previous pipeline run using the same CASA version, this file may be edited to add the SDM-BDF (or MS) name to this file and executing it directly in CASA. For this to work, the 'casa_pipescript.py' must be in the same directory where you start CASA with the pipeline. Once CASA is started (same steps as above) type:

#In CASA
execfile('casa_pipescript.py')

 

Method 3: One Stage at a Time

You may notice that the 'casa_pipescript.py' is a list of specific CASA pipeline tasks being called in order to form the default pipeline. If desired, one could run each of these tasks one at a time in CASA to inspect intermediate pipeline products as an example.

If you need to exit CASA between stages, you can restart the pipeline where you left off. However, in order for this to work, none of the files can be moved to other directories. First, use the CASA pipeline task h_resume after starting CASA again. This will set up the environment again for the pipeline to work. Type:

# In CASA
h_resume()

Now, you may start the next task in your list.

 

What you get: Pipeline Products

VLA pipeline output includes data products such as calibrated visibilities, a weblog, and all calibration tables. Note that the automated execution at NRAO will also run an additional data packaging step (hifv_exportdata' which moves most of the files to an upper level '../products' directory. This step is omitted in the manual execution and all products remain within the 'root' directory where the pipeline was executed.

The most important pipeline products include (mySDM is a placeholder for the SDM-BDF name):

• A MeasurementSet (MS) 'mySDM.ms' with applied flags and calibrated visibilities in the CORRECTED_DATA column that can be used for subsequent imaging (root directory).
• A weblog that is accessible via pipeline-YYYYMMDDTHHMMSSS/html/index.html, where the YYYYMMDDTHHMMSSS stands for the pipeline execution time stamp (multiple pipeline executions will result in multiple weblogs). The weblog contains information on the pipeline processing steps with diagnostic plots and statistics. An example is given in the VLA pipeline CASA guide.
• Calibrator images for all spws (files start with 'oussid*' in the root directory).
• All calibration tables and the 'mySDM.ms.flagversions' directory that contains various flag backups made at various stages of the pipeline run (see section Calibration Tables).
• The casapy-YYYYMMDD-HHMMSS.log CASA logger messages (in pipeline-YYYYMMDDTHHMMSSS/html/).
• 'casa_pipescript.py' (in pipeline-YYYYMMDDTHHMMSSS/html/), the script with the actually executed pipeline heuristic sequence and parameters. This file can be used to modify and re-execute the pipeline (see section The casa_pipescript.py file).
• 'casa_commands.log' (in pipeline-YYYYMMDDTHHMMSSS/html/), which contains the actual CASA commands that were generated by the pipeline heuristics (see section The casa_commands.log file).
• The output from CASA's task listobs is available at 'pipeline-YYYYMMDDTHHMMSSS/html/sessionSession_default/mySDM.ms/listobs.txt' and contains the characteristics of the observations (scans, source fields, spectral setup, antenna positions, and general information).
• As previously mentioned in Automatic Processing for Science Observations, calibrated MSs are only stored at NRAO for a period of 15 days. After that period, the pipeline products need to be re-applied to the raw data that have to be downloaded in the SDM-BDF format from the archive. To prepare for this restoring procedure, NRAO adds the hifv_exportdata pipeline task as a last step. This task packages calibration tables in 'unknown.session_1.caltables.tgz' and flag backups in 'mySDM.ms.flagversions.tgz'. An additional text file, 'mySDM.ms.calapply.txt', is also produced by hifv_exportdata that CASA task applycal uses when restoring the calibration. The restoring process itself is performed by a script called 'casa_piperestorescript.py'. See the section Restore calibration from archived products for details on the restoration procedures.

 

The Pipeline Weblog

Information on the pipeline run can be inspected through a weblog that is launched by pointing a web browser to file:///<path to your working directory>/pipeline-YYYYMMDDTHHMMSSS/html/index.html. The weblog contains statistics and diagnostic plots for the SDM-BDF as a whole and for each stage of the pipeline. The weblog is the first place to check if a pipeline run was successful and to assess the quality of the calibration.

An example walkthrough of a pipeline weblog is provided in the VLA Pipeline CASA guide.

Note that we regularly test the weblog on Firefox. Other browsers may not display all items correctly.

 

Calibration Tables

The final calibration tables of the pipeline are (where mySDM is a placeholder for the SDM-BDF name):

mySDM.ms.hifv_priorcals.s5_3.gc.tbl : Gaincurve
mySDM.ms.hifv_priorcals.s5_4.opac.tbl : Opacity
mySDM.ms.hifv_priorcals.s5_5.rq.tbl : Requantizer gains
mySDM.ms.hifv_priorcals.s5_6.ants.tbl : Antenna positions (if created)
mySDM.ms.finaldelay.k : Delay
mySDM.ms.finalBPcal.b : Bandpass
mySDM.ms.averagephasegain.g : Temporal Phase offsets
mySDM.ms.finalampgaincal.g : Flux calibrated Temporal Gains 
mySDM.ms.finalphasegaincal.g : Temporal Phases

 

The casa_pipescript.py File

The pipeline sequence of the pipeline heuristic steps are listed in the 'casa_pipescript.py' script that is located in the pipeline-YYYYMMDDTHHMMSSS/html (where YYYYMMDDTHHMMSSS is the timestamp of the execution) directory. A typical 'casa_pipescript.py' has the following structure (where mySDM is again a placeholder for the name of the SDM-BDF raw data file and will have the name of the one that was processed):

__rethrow_casa_exceptions = True
context = h_init()
context.set_state('ProjectSummary', 'observatory', 'Karl G. Jansky Very Large Array')
context.set_state('ProjectSummary', 'telescope', 'EVLA')
try:
    hifv_importdata(vis=['mySDM'], createmms='automatic',\
                    asis='Receiver CalAtmosphere', ocorr_mode='co',\
                    nocopy=False, overwrite=False)
    hifv_hanning(pipelinemode="automatic")
    hifv_flagdata(tbuff=0.0, flagbackup=False, scan=True, fracspw=0.05,\
                  intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*,\
                  *UNKNOWN*, *SYSTEM_CONFIGURATION*, *UNSPECIFIED#UNSPECIFIED*',\
                  clip=True, baseband=True, shadow=True, quack=True, edgespw=True,\
                  autocorr=True, hm_tbuff='1.5int', template=True, online=True)
    hifv_vlasetjy(fluxdensity=-1, scalebychan=True, spix=0, reffreq='1GHz')
    hifv_priorcals(tecmaps=False)
    hifv_testBPdcals(weakbp=False)
    hifv_flagbaddef(doflagundernspwlimit=False)
    hifv_checkflag(pipelinemode="automatic")
    hifv_semiFinalBPdcals(weakbp=False)
    hifv_checkflag(checkflagmode='semi')
    hifv_semiFinalBPdcals(weakbp=False)
    hifv_solint(pipelinemode="automatic")
    hifv_fluxboot2(fitorder=-1)
    hifv_finalcals(weakbp=False)
    hifv_applycals(flagdetailedsum=True, gainmap=False, flagbackup=True,\
                   flagsum=True)
    hifv_targetflag(intents='*CALIBRATE*,*TARGET*')
    hifv_statwt(datacolumn='corrected')
    hifv_plotsummary(pipelinemode="automatic")
    hif_makeimlist(nchan=-1, calcsb=False, intent='PHASE,BANDPASS', robust=-999.0,\
                   parallel='automatic', per_eb=False, calmaxpix=300,\
                   specmode='cont', clearlist=True)
    hif_makeimages(tlimit=2.0, hm_perchanweightdensity=False, hm_npixels=0,\
                   hm_dogrowprune=True, hm_negativethreshold=-999.0, calcsb=False,\
                   hm_noisethreshold=-999.0, hm_fastnoise=True, hm_masking='none',\
                   hm_minpercentchange=-999.0, parallel='automatic', masklimit=4,\
                   hm_nsigma=0.0, target_list={}, hm_minbeamfrac=-999.0,\
                   hm_lownoisethreshold=-999.0, hm_growiterations=-999,\
                   overwrite_on_export=True, cleancontranges=False,\
                   hm_sidelobethreshold=-999.0)
    hifv_exportdata(gainmap=False, exportmses=False, exportcalprods=False)
finally:
    h_save()

(Note that executions at NRAO may show small differences, e.g., an additional final hifv_exportdata step that packages the products to be stored in the NRAO archive.)

The above is, in fact, a standard user 'casa_pipescript.py' file for the current CASA and pipeline version (download to edit and run yourself) that can be used for general pipeline processing after inserting the correct mySDM filename in hifv_importdata.

The pipeline run can be modified by adapting this script to comment out individual steps, or by providing different parameters (see the CASA help for the parameters of each task). The script can then be (re-)executed via:

# In CASA
execfile('casa_pipescript.py')

We will use this method later for an example where we modify the script for spectral line processing.

General modifications to the script include setting '__rethrow_casa_exceptions = False' to suppress CASA error messages in the weblog and 'h_init(weblog=False)' for faster processing without any weblog or plotting.

 

The casa_commands.log File

casa_commands.log is another useful file in pipeline-YYYYMMDDTHHMMSSS/html (where YYYYMMDDTHHMMSSS is the timestamp of the pipeline execution) that lists all the individual CASA commands that the pipeline heuristics (hifv) tasks produced. Note that 'casa_commands.log' is not executable itself, but contains all the CASA tasks and associated parameters to trace back the individual data reduction steps.

 

Restore calibration from archived products

To apply the calibration and flag tables produced by the pipeline, we recommend using the same version of CASA used by the pipeline as well as the same version of the pipeline. The version of both the pipeline and CASA used may be confirmed via the main "Observation Overview Page", the home page of the weblog. We recommend starting with a fresh SDM-BDF, although a fresh MS should work, too. There may be small differences in the final result or statistics if online flags were applied when requesting the MS.

In order for the pipeline to work properly, please follow the steps below to prepare your directory and calibration files for application. In addition to the raw SDM-BDF you will need the following pipeline products: 'unknown.session_1.caltables.tgz', 'mySDM.ms.flagversions.tgz', 'mySDM.ms.calapply.txt', 'unknown.pipeline_manifest.xml', and 'casa_piperestorescript.py' (where mySDM is a placeholder for the SDM-BDF name). To ensure everything is correctly placed for the script to apply calibration, please follow these steps:

1. Create a directory where you will work, call it something like "restoration".
   

   mkdir restoration

2. Go into your restoration directory and create three new directories named exactly as follows:
   

   mkdir rawdata working products

3. Place the raw SDM-BDF into the "rawdata" directory.
   

   mv /path/to/fresh/data/mySDM rawdata/

4. Place 'unknown.session_1.caltables.tgz', 'mySDM.ms.flagversions.tgz', 'unknown.pipeline_manifest.xml', and 'mySDM.ms.calapply.txt' into the "products" directory
   

   mv *.tgz products/
   mv *.xml products/
   mv *.txt products/

5. Place the 'casa_piperestorescript.py' file into the "working" directory
   

   mv casa_piperestorescript.py working/

6. The 'casa_piperestorescript.py' looks similar to the 'casa_pipescript.py', but runs a special hifv_restoredata pipeline task to apply flags and calibration tables, followed by hifv_statwt. Edit the hifv_restoredata call to include "../rawdata/" in front of the name of the SDM-BDF (mySDM), e.g.:
   

   __rethrow_casa_exceptions = True
   h_init()
   try:
     hifv_restoredata (vis=['../rawdata/mySDM'], session=['session_1'],\
                      ocorr_mode='co',gainmap=False)
     hifv_statwt()
   finally:
     h_save()
   

7. From the "working" directory, start CASA:
   

   casa --pipeline

   
   or if you use computers at the NMASC:
   

   casa-pipe

8. Start the restore script from the CASA prompt:
   

   # In CASA
   execfile('casa_piperestorescript.py')

9. Enjoy calibrated data once the process finishes.

Note that if the original pipeline was run in parallel mode, a multi-MS (MMS) is created. The restor will only work for MMSs if the data has the same shape. More specifically, the restoration of the flags can only be achieved if the MSs have identical structure. All production pipeline runs at NRAO are serial.  

 

Quality (QA) Assessment Scores

Each pipeline stage has a quality assessment (qa) score assigned to it. The values range from 0 to 1 where 

0.9-1.0 Standard/Good     (green color) 
0.66-0.90 Below Standard  (blue color; also shown as a question mark symbol) 
0.33-0.66 Warning         (amber color; cross symbol) 
0.00-0.33 Error            (red color; cross symbol) 

We recommend that all pipeline stages and the relevant products are checked. Below standard and Warning scores should receive extra scrutiny. These scores often refer to large fractions of flagging that is applied to the data, but may also point out other issues where in fact additional flagging may be required. The qa section in at the bottom of the weblog of each stage will provide more information about the particular origin of each score. Errors are usually very serious issues with the data or processing and should be resolved in any case. 

Examples for qa scores are provided in the Pipeline CASAguide.

 

Further flagging

 

Using a flagging template

Although the pipeline attempts to remove most RFI, there are still many cases where additional flagging is required. The pipeline will then be re-started with the additional flags pre-applied.

The best way to do so is to inspect the data and to record all the required flags in a flagging template. See the CASA flagdata task help for the details on the format. Here is an example for a template:

mode='manual' scan='1~3'           #flags scans 1 to 3
mode='clip' clipminmax=[0,10]     #flags data outside an amplitude range
                                  #here all amplitudes larger than 10 Jy
# this line will be ignored
mode='quack' scan='1~3,10~12' mode='quack' quackinterval=1.0  #removes first second 
                                                 #from scans 1-3 and 10-12

The most important modes are manual to flag given time ranges, antennas, spws, scans, fields, etc., and clip to flag data exceeding threshold amplitude levels.

Flagging templates can be saved in text files with any given name, e.g. 'myflags.txt'. In 'casa_pipescript.py' modify the parameters of the hifv_flagdata task; change template=True and add filetemplate='myflags.txt' .

 hifv_flagdata(tbuff=0.0, flagbackup=False, scan=True, fracspw=0.05, \
  intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*, *UNKNOWN*, \
  *SYSTEM_CONFIGURATION*, *UNSPECIFIED#UNSPECIFIED*', clip=True, baseband=True, \
  shadow=True, quack=True, edgespw=True, autocorr=True, hm_tbuff='1.5int', \
  template=True, filetemplate='myflags.txt', online=True)

The default for filetemplate is 'mySDM.flagtemplate.txt'. Therefore, flag files with this name would not require filetemplate to be specified.

 

Interactive Flagging

For some data it is not straightforward to derive flagging commands that can be placed in a template. In that case, one may use the interactive plotms or viewer/msview CASA GUIs to flag data directly in the MS. Re-execution of the pipeline (via the casa_pipescript.py file) will be possible, but a few steps require attention:

• Since Hanning smoothing was likely performed in the initial pipeline run, one should turn off Hanning smoothing for all re-executions. Otherwise the frequency resolution degrades more and more and flags will be extended to neighboring channels by smoothing an already flagged MS. To do so, comment out hifv_hanning in the 'casa_pipescript.py' file (see the section on "Spectral Line" for a similar example).
• By default, the pipeline will always revert back all flags to their original state that are saved in the 'mySDM.ms.flagversions' file. It will thus ignore all modifications that were made afterwards. To avoid resetting all flags, one should manually flag the MS and place it in a new directory. Do NOT copy over the related 'mySDM.ms.flagversions' directory. Then run the pipeline with the flagged MS as input to hifv_importdata via the modified 'casa_pipescript.py' file (it is possible to also run hifv.hifv(['MeasurementSet']) but remember that this will repeat Hanning smoothing). With this procedure the pipeline will not be able to recover original flags and will proceed with the manual, interactive flags that the user has applied directly to the MS.

Flag the Flux Calibration Gain Table

Sometimes the gain solutions of the flux calibrator are not good for all antennas, even with the rejection performed by hifv_fluxboot2. It is possible to flag the solutions directly in the 'fluxgaincal.g' calibration table. The CASA task plotms can be used for the flagging. The pipeline can use the flagged table, say 'fluxgaincal_edited.g' for the flux calibration by modifying the hifv_fluxboot2 call in the 'casa_pipescript.py' as follows:

hifv_fluxboot2(caltable='fluxgaincal_edited.g')

 

Avoiding a Specific Reference Antenna

In some cases, the pipeline may chose a reference antenna that is not ideal for calibration purposes. The pipeline algorithm picks an antenna (actually a ranked list of antennas) that is not heavily flagged and that is close to the center of the array. Other factors, e.g. phase jumps, or bad deformattors that are not caught in the hifv_flagbaddef stage may still be present on the reference antenna and then be reflected on all solutions. When this happens, it is advisable to tell the pipeline not to use a specific antenna as a reference antenna. This can be achieved by the parameter refantignore that is available in some hifv tasks. E.g. if we want to avoid that the pipeline uses antenna 'ea28' as a reference antenna, the casa_pipescript.py can be modified as follows (changes are shown in red in hifv_testBPdcals, hifv_semiFinalBPdcals, hifv_solint, hifv_fluxboot2, hifv_finalcals):    

__rethrow_casa_exceptions = True
context = h_init()
context.set_state('ProjectSummary', 'observatory', 'Karl G. Jansky Very Large Array')
context.set_state('ProjectSummary', 'telescope', 'EVLA')
try:
 hifv_importdata(vis=['mySDM'], \ 
  createmms='automatic', asis='Receiver CalAtmosphere', ocorr_mode='co', \ 
  nocopy=False, overwrite=False)
 hifv_hanning(pipelinemode="automatic")
 hifv_flagdata(tbuff=0.0, flagbackup=False, scan=True, fracspw=0.05, \
  intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*, *UNKNOWN*, \
  *SYSTEM_CONFIGURATION*, *UNSPECIFIED#UNSPECIFIED*', clip=True, baseband=True, \
  shadow=True, quack=True, edgespw=True, autocorr=True, hm_tbuff='1.5int', \
  template=True, online=True)
 hifv_vlasetjy(fluxdensity=-1, scalebychan=True, \
spix=0, reffreq='1GHz')
 hifv_priorcals(tecmaps=False)
 hifv_testBPdcals(weakbp=False, refantignore='ea28')
 hifv_flagbaddef(doflagundernspwlimit=True)
 hifv_checkflag(pipelinemode="automatic")
 hifv_semiFinalBPdcals(weakbp=False, refantignore='ea28')
 hifv_checkflag(checkflagmode='semi')
 hifv_semiFinalBPdcals(weakbp=False, refantignore='ea28')
 hifv_solint(pipelinemode="automatic", refantignore='ea28')
 hifv_fluxboot2(pipelinemode="automatic", refantignore='ea28')
 hifv_finalcals(weakbp=False, refantignore='ea28')
 hifv_applycals(flagdetailedsum=True, gainmap=False, flagbackup=True, flagsum=True)
 hifv_targetflag(intents='*CALIBRATE*,*TARGET*')
 hifv_statwt(pipelinemode="automatic")
 hifv_plotsummary(pipelinemode="automatic")
 hif_makeimlist(nchan=-1, calcsb=False, intent='PHASE,BANDPASS', robust=-999.0, \
  per_eb=False, calmaxpix=300, specmode='cont', clearlist=True)
 hif_makeimages(tlimit=2.0, hm_minbeamfrac=-999.0, hm_dogrowprune=True, \
  hm_negativethreshold=-999.0, calcsb=False, target_list={}, \ 
  hm_noisethreshold=-999.0, hm_masking='none', hm_minpercentchange=-999.0, \ 
  parallel='automatic', masklimit=4, hm_lownoisethreshold=-999.0, \
  hm_growiterations=-999, cleancontranges=False, hm_sidelobethreshold=-999.0)
finally:
 h_save()

 

Modifying the Pipeline for non-Stokes I Continuum Data

The pipeline is developed for the Stokes I continuum case. But it is possible to modify the 'casa_pipescript.py' and run the pipeline for other use cases:

 

Spectral Line

The pipeline is not optimized for calibrating spectral line data. Some pipeline steps of the regular VLA pipeline may be detrimental for spectral line setups and need to be modified or turned off. Calibrators also require enough signal-to-noise to reliably derive bandpasses, gains, phases, etc. for the typically more narrow spectral line spectral windows (spws) and channels. The pipeline will also flag edge channels for each spw. If the spectral line happens to be located on an spw edge, additional modifications to the script may be necessary.

The 'cont.dat' file

The easiest way to run the pipeline on data with spectral lines is to prepare a file, 'cont.dat', that specifies the frequencies only containing continuum (no spectral line). This will protect some procedures of the pipeline from being applied to spectral lines (see below).

The 'cont.dat' file has the following format:

Field: FIELDNAME1

SpectralWindow: SPWID1
freqrange1 LSRK (in GHz, LSRK) 
freqrange2 LSKR (in GHz, LSRK) 

SpectralWindow: SPWID2
freqrange1 LSRK (in GHz, LSRK) 
freqrange2 LSRK (in GHz, LSRK) 
... 


Field: FIELDNAME2

SpectralWindow: SPWID1
freqrange1 LSRK (in GHz, LSRK) 
freqrange2 LSRK (in GHz, LSRK) 
... 

where FIELDNAMEx is the field name for each source. This provides the flexibility to define different continuum ranges for different targets. SPWIDn stands for the spw ID. Field names and spw ids can be found in the listobs output. An example with fields M82 and NGC3077 may look like:

Field: M82

SpectralWindow: 19
37.104~38.29GHz LSRK
38.30~39.104GHz LSRK

SpectralWindow: 37
31.360~32.123GHz LSRK
32.130~33.360GHz LSRK

Field: NGC3077

SpectralWindow: 37
31.360~32.123GHz LSRK
32.130~33.360GHz LSRK

For the field M82 this file defines spw 19 frequency ranges 37.104 – 38.290 GHz and 38.300 – 39.104 GHz as containing only continuum. This would be a setup where the line is found in the 10 MHz between 38.290 – 38.300 GHz. It also treats frequencies below 37.104 GHz and above 39.104 GHz the same as spectral lines. This can be used, for example, to exclude edge channels from being part of the autoflagging and weight calculations. Analogously, a spectral line falling in the 7 MHz range between 32.123 – 32.130GHz (between the two continuum ranges in spw 37) will be protected by the specification for spw 37 for both the M82 and NGC3077 fields.

'cont.dat' shall be placed in the root directory where the SDM-BDF resides and where the pipeline is executed. The pipeline will automatically pick up the file, there is no need to explicitly provide the file name in 'casa_pipescript.py'.

 

Pipeline Modifications for Spectral Line Data

In addition to creating a 'cont.dat' file, we advise to modify the following tasks in 'casa_pipescript.py' for spectral line data:

• hifv_hanning: Hanning smoothing lessens the Gibbs ringing from strong spectral features, usually strong, narrow RFI, or very strong spectral lines such as masers. Hanning smoothing, however, reduces the spectral resolution. Therefore, depending on the data and the science case, one may or may not choose to apply Hanning smoothing. Disable the application of Hanning-smoothing in the pipeline if such smoothing is not needed or desired by commenting out hifv_hanning or simply removing the step from 'casa_pipescript.py'.
• hifv_flagata: The pipeline, by default, flags 5% of the data on each spw edge as well as the first and last 20MHz of the lowest and highest frequency (assuming that those are the baseband edges). In some cases, for example spectral surveys, lines may fall right on such frequencies. The edgespw, fracspw, and baseband parameters in hifv_flagata can be adjusteded to flag different percentages of the edges.
• hifv_targetflag: Flagging prior to this step was only applied to the calibrator scans, which should be line-free. But hifv_targetflag attempts to auto-flag all fields including target fields. The rflag mode in CASA's flagdata is designed to remove outliers that deviate from a mean level. Strong spectral lines can fulfill this criterion and be flagged. The 'cont.dat' file will ensure that rflag will only be applied to the continuum frequency ranges specified in it. Alternatively, hifv_targetflag can be turned off completely, or, by specifying intents='*CALIBRATE*' (and thereby omitting '*TARGET*'), one can restrict the flagging to the calibrator data only, leaving the target data (scans with the TARGET intent) untouched. In either case, we recommend manual flagging for the spectral line frequency ranges after the pipeline has finished processing.
• hifv_statwt: A similar argument applies to the hifv_statwt step, where the visibilities are weighted by the square of the inverse of their RMS noise. Strong spectral lines will increase the RMS and will therefore be down-weighted. The cont.dat file will restrict statwt to only use the continuum frequency ranges for the rms and weight calculations and thus prevent the inclusion of spectral features. Alternatively, hifv_statwt can be excluded from the pipeline altogether and the CASA task statwt can be executed manually after the pipeline has finished, where statwt's parameter fitspw should be set to continuum channels only.

 

Given the above, we recommend to carefully prepare 'cont.dat' and modify 'casa_pipescript.py' as follows. The SDM-BDF name (here: mySDM) and maybe other parameters will have to be adapted for the run:

 

__rethrow_casa_exceptions = True
context = h_init()
context.set_state('ProjectSummary', 'observatory', 'Karl G. Jansky Very Large Array')
context.set_state('ProjectSummary', 'telescope', 'EVLA')
try:
 hifv_importdata(vis=['mySDM'], \ 
  createmms='automatic', asis='Receiver CalAtmosphere', ocorr_mode='co', \ 
  nocopy=False, overwrite=False)
 # Hanning smoothing is turned off in the following step. 
 # In the case of extreme RFI, Hanning smoothing, however, 
 # may still be required.
 #hifv_hanning(pipelinemode="automatic")
 hifv_flagdata(tbuff=0.0, flagbackup=False, scan=True, fracspw=0.05, \
  intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*, *UNKNOWN*, \
  *SYSTEM_CONFIGURATION*, *UNSPECIFIED#UNSPECIFIED*', clip=True, baseband=True, \
  shadow=True, quack=True, edgespw=True, autocorr=True, hm_tbuff='1.5int', \
  template=True, online=True)
 hifv_vlasetjy(fluxdensity=-1, scalebychan=True, \
spix=0, reffreq='1GHz')
 hifv_priorcals(tecmaps=False)
 hifv_testBPdcals(weakbp=False)
 hifv_flagbaddef(doflagundernspwlimit=True)
 hifv_checkflag(pipelinemode="automatic")
 hifv_semiFinalBPdcals(weakbp=False)
 hifv_checkflag(checkflagmode='semi')
 hifv_semiFinalBPdcals(weakbp=False)
 hifv_solint(pipelinemode="automatic")
 hifv_fluxboot(pipelinemode="automatic")
 hifv_finalcals(weakbp=False)
 hifv_applycals(flagdetailedsum=True, gainmap=False, flagbackup=True, flagsum=True)
 # Keep the following two steps in the script if cont.dat exists. 
 # Otherwise we recommend to comment out the next two tasks, 
 # or at least remove '*TARGET*' from the hifv_targetflag call 
 hifv_targetflag(intents='*CALIBRATE*,*TARGET*')
 hifv_statwt(pipelinemode="automatic")
 hifv_plotsummary(pipelinemode="automatic")
 hif_makeimlist(nchan=-1, calcsb=False, intent='PHASE,BANDPASS', robust=-999.0, \
  per_eb=False, calmaxpix=300, specmode='cont', clearlist=True)
 hif_makeimages(tlimit=2.0, hm_minbeamfrac=-999.0, hm_dogrowprune=True, \
  hm_negativethreshold=-999.0, calcsb=False, target_list={}, \ 
  hm_noisethreshold=-999.0, hm_masking='none', hm_minpercentchange=-999.0, \ 
  parallel='automatic', masklimit=4, hm_lownoisethreshold=-999.0, \
  hm_growiterations=-999, cleancontranges=False, hm_sidelobethreshold=-999.0)
finally:
 h_save()

If a spectral line happens to be close to edge channels, one can decide to turn off edge channel flagging by setting the parameter edgespw=False in hifv_flagdata (if the line falls on the edge of a baseband, one may also consider to set baseband=False to avoid flagging the outer 10 baseband edges):

hifv_flagdata(tbuff=0.0, flagbackup=False, scan=True, fracspw=0.05, \
  intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*, *UNKNOWN*, \
  *SYSTEM_CONFIGURATION*, *UNSPECIFIED#UNSPECIFIED*', clip=True, \
  baseband=True, shadow=True, quack=True, edgespw=False, autocorr=True, \ 
  hm_tbuff='1.5int', template=True, online=True)

or one can choose to reduce the fraction of edge channels being flagged. In the example below, we reduce the number to 1% on each end of each spw:

hifv_flagdata(intents='*POINTING*,*FOCUS*,*ATMOSPHERE*,*SIDEBAND_RATIO*,\
                   *UNKNOWN*, *SYSTEM_CONFIGURATION*,\
                   *UNSPECIFIED#UNSPECIFIED*', flagbackup=False, scan=True,\
                   baseband=True, clip=True, autocorr=True,\
                   hm_tbuff='1.5int', template=True, online=True,\
                   tbuff=0.0, fracspw=0.01, shadow=True, quack=True,\
                   edgespw=True)

But note that including edge channels in the calibration may introduce uncertainties given that spw edges have low signal-to-noise and may contain correlator artifacts. Inspect the data to ensure the spw edges are usable.

 

Once all modifications are made, run the pipeline as:

# In CASA

execfile('casa_pipescript.py')

After the calibration has been obtained, the run can be followed up with CASA's flagdata mode='rflag' and statwt commands if required (e.g. if 'cont.dat' was not used).

 

Polarization Calibration

We are currently developing polarization calibration heuristics for the VLA pipeline. At this stage, however, the VLA pipeline does not derive and apply polarization calibration. If the scan intents included proper polarization intents (CALIBRATE_POL_LEAKAGE and CALIBRATE_POL_ANGLE), the pipeline will run with refantmode='strict', which is desireable for polarization calibration. The user may perform polarization calibration steps after the pipeline was run by using the pipeline calibration tables for pre-calibration as required.

Polarization calibration steps are explained in the 3C75 CASA guide (in particular the D-term and crosshand delay calibration will be required). We also refer to the corresponding chapter in CASAdocs.

 

Mixed setups

If data were obtained in mixed correlator modes, the different parts (e.g., spectral line and continuum, or different frequency bands) it may be advisable to separate the data first and then the individual parts can be calibrated via the default pipeline or by executing modified 'casa_pipescript.py' scripts. To start with, we recommend to import the SDM to an MS by applying online flags at the same time. The corresponding CASA importasdm command would look like:

# In CASA
importasdm(asdm='mySDM', vis='mySDM.ms', ocorr_mode='co',\
           applyflags=True, savecmds=True, tbuff=1.5,\
           outfile='mySDM.flagonline.txt')

Note that we apply the online flags via applyflags=True but still save the flag commands in an outfile in case one would like to inspect those. We set tbuff=1.5 to extend the flags to 1.5 times the integration time (which the pipeline would do in hifv_flagdata).

After that step, use the CASA command split to separate the individual parts of the data to be processed separately. Modify 'casa_pipescript.py' and use each new separate MS as input in hifv_importdata.

 

Weak Calibrators

The VLA pipeline requires a minimum signal-to-noise of ~3 for each spw (each channel for the bandpass) and calibrator scan. If this criterion is not met, the pipeline will likely fail. We are currently implementing additional heuristics to deal with weak calibration sources. This code will be available in upcoming versions of the VLA pipeline.

 

Partially Frequency Averaged Data 

The pipeline invokes Hanning smoothing when frequency averaging at the VLA correlator is turned off. In that case, Hanning smoothing can fix the Gibbs ringing for strong narrow spectral features (e.g., RFI or maser lines). When the online frequency averaging is turned on, however, adjacent channels do not exhibit the typical Gibbs zig-zag pattern anymore and Hanning smoothing should not be applied for further processing. The pipeline currently detects if any spectral window was pre-averaged in frequency on the VLA correlator. In that case, it turns the Hanning smoothing off for all data. If one has an SDM where some spws are frequency averaged and some are not, the pipeline should be stopped after hifv_importasdm. The frequency averaged and non-averaged spws should then be separated into individual MSes using the CASA task 'split'. The pipeline can be started again on the individual MSes. 

Incorrect scan intents

As mentioned in the "Pipeline Requirements", scan intents tell the pipeline which scans and fields are used for flux, delay, bandpass, gain and phase calibration. Scan intents should be set up correctly in the OPT before submitting the schedule block for observation.

When incorrect scan intents are identified after observations, one can still change the SDM-BDF with updated scan intents, although some care will be required.

The SDM-BDF metadata is structured in the form of XML files that can be edited. We provide a small Scan Intent Editing Perl Script to do this. The script is pretty self-explaining and can add and delete scan intents to any scan.  

Alternatively, the SDM can also be manually edited. Great care, however, should be taken not to corrupt the structure of the SDM-BDF/xml. We therefore advice not to edit the SDM-BDF/xml manually but to use the Perl script instead.

However, to edit the xml manually, cd into the SDM and edit the file 'Scan.xml'. We strongly recommend creating a backup copy of the 'Scan.xml' file in case the edits corrupt the metadata.

'Scan.xml' is divided into individual <row></row> blocks that identify each scan.

An example of a scan with a single scan intent (here: OBSERVE_TARGET) may look like:

   <row>
       <scanNumber>1</scanNumber>
       <startTime>4870732142800000000</startTime>
       <endTime>4870732322300000256</endTime>
       <numIntent>1</numIntent>
       <numSubscan>1</numSubscan>
       <scanIntent>1 1 OBSERVE_TARGET</scanIntent>
       <calDataType>1 1 NONE</calDataType>
       <calibrationOnLine>1 1 false</calibrationOnLine>
       <sourceName>J1041+0610</sourceName>
       <flagRow>false</flagRow>
       <execBlockId>ExecBlock_0</execBlockId>
   </row>

We can now change the scan intent, e.g., from OBSERVE_TARGET to CALIBRATE_AMPLI by simply updating the <scanIntent> tag:

   <row>
       <scanNumber>1</scanNumber>
       <startTime>4870732142800000000</startTime>
       <endTime>4870732322300000256</endTime>
       <numIntent>1</numIntent>
       <numSubscan>1</numSubscan>
       <scanIntent>1 1 CALIBRATE_AMPLI</scanIntent>
       <calDataType>1 1 NONE</calDataType>
       <calibrationOnLine>1 1 false</calibrationOnLine>
       <sourceName>J1041+0610</sourceName>
       <flagRow>false</flagRow>
       <execBlockId>ExecBlock_0</execBlockId>
   </row>

If we want to add a second intent, we will have to make additional changes. Let's add CALIBRATE_PHASE:

   <row>
       <scanNumber>1</scanNumber>
       <startTime>4870732142800000000</startTime>
       <endTime>4870732322300000256</endTime>
       <numIntent>2</numIntent>
       <numSubscan>1</numSubscan>
       <scanIntent>1 2 CALIBRATE_AMPLI CALIBRATE_PHASE</scanIntent>
       <calDataType>1 2 NONE NONE</calDataType>
       <calibrationOnLine>1 2 false false</calibrationOnLine>
       <sourceName>J1041+0610</sourceName>
       <flagRow>false</flagRow>
       <execBlockId>ExecBlock_0</execBlockId>
   </row>

Inside <scanIntent> we added the second intent, but also increased the second number from 1 to 2. In addition, we specified <numIntent> to be 2, and added a second entry to <calDataType> and <calibrationOnLine>. For the latter two, we also updated the second number from 1 to 2.

Analoguously, if we now add a third intent, CALIBRATE_BANPDASS, to the same scan, the <row> will look like:

   <row>
       <scanNumber>1</scanNumber>
       <startTime>4870732142800000000</startTime>
       <endTime>4870732322300000256</endTime>
       <numIntent>3</numIntent>
       <numSubscan>1</numSubscan>
       <scanIntent>1 3 CALIBRATE_AMPLI CALIBRATE_PHASE CALIBRATE_BANDPASS</scanIntent>
       <calDataType>1 3 NONE NONE NONE</calDataType>
       <calibrationOnLine>1 3 false false false</calibrationOnLine>
       <sourceName>J1041+0610</sourceName>
       <flagRow>false</flagRow>
       <execBlockId>ExecBlock_0</execBlockId>
   </row>

Check with CASA's listobs on the imported MS (after importing the data to an MS via importasdm or importevla) if the scan intents are now displayed as desired. Revert back to the original 'Scan.xml' if the above was not successful and contact the NRAO helpdesk for advice.

 

Allowed Intents

CALIBRATE_AMPLI : Amplitude calibration scan
CALIBRATE_PHASE : Phase calibration scan
CALIBRATE_BANDPASS : Bandpass calibration scan
CALIBRATE_DELAY : Delay calibration scan
CALIBRATE_FLUX : flux measurement scan.
CALIBRATE_POINTING : Pointing calibration scan
CALIBRATE_POLARIZATION : Polarization calibration scan
CALIBRATE_POL_LEAKAGE : Polarization Leakage calibration scan
CALIBRATE_POL_ANGLE : Polarizaiton Angle calibration scan
OBSERVE_TARGET : Target source scan
CALIBRATE_ATMOSPHERE : Atmosphere calibration scan
CALIBRATE_FOCUS : Focus calibration scan. Z coordinate to be derived
CALIBRATE_FOCUS X : Focus calibration scan; X focus coordinate to be derived
CALIBRATE_FOCUS Y : Focus calibration scan; Y focus coordinate to be derived
CALIBRATE_SIDEBAND_RATIO : measure relative gains of sidebands.
CALIBRATE_WVR : Data from the water vapor radiometers (and correlation data) are used to derive their calibration parameters.
DO_SKYDIP : Skydip calibration scan
MAP_ANTENNA_SURFACE : Holography calibration scan
MAP_PRIMARY_BEAM : Data on a celestial calibration source are used to derive a map of the primary beam.
TEST : used for development.
UNSPECIFIED : Unspecified scan intent
CALIBRATE_ANTENNA_POSITION : Requested by EVLA.
CALIBRATE_ANTENNA_PHASE : Requested by EVLA.
MEASURE_RFI : Requested by EVLA.
CALIBRATE_ANTENNA_POINTING_MODEL : Requested by EVLA.
SYSTEM_CONFIGURATION : Requested by EVLA.
CALIBRATE_APPPHASE_ACTIVE : Calculate and apply phasing solutions. Applicable at ALMA.
CALIBRATE APPPHASE PASSIVE : Apply previously obtained phasing solutions. Applicable at ALMA.
OBSERVE_CHECK_SOURCE

 

Known Issues

This section will be updated as the pipeline continues to be developed. The comments below are general to most pipeline versions, including the current, production pipeline used for VLA data. The current production version is CASA 5.6.2-3.

• The VLA Calibration Pipeline produces a dataset that can be used as a starting point by the user for self-calibration and imaging of science targets. Note that the pipeline does not do any self-calibration of fields that are not specified as calibrators.

• The pipeline in CASA 5.6.2, pipeline revision Pipeline-CASA56-P2-B.42904, had a problem affecting the FSID.ms.calapply.txt file used during a calibration restore (the original output from the pipeline is not affected, but any pipeline calibration restore process would be. The problem is a duplication of all calibration tables in the applycal call listed in this text file, and applying these twice to the MS results in incorrect calibration. All affected pipeline products in the NRAO archive will be fixed, but for any calibration tar files already downloaded, a fix is available in the form of a script, fixcal.py, which should be run from the products directory created by untarring the calibration tar file. This script, requring Python 2, will read the FSID.ms.calapply.txt file and create a new, correct applycal call version of this file, while moving the bad version to FSID.ms.calapply_bad.txt. This issue is resolved in CASA-pipeline 5.6.2-3. If you have any questions about this, please submit a ticket the Pipeline Department of the NRAO Helpdesk. 
  
• Although the hifv_fluxboot2 task performs more aggressive clipping of the gain solutions used for flux density boot strapping, in some cases (especially at high frequencies, for datasets that may have suffered from pointing or other problems) the default flux density scale may be uncertain if outlier rejection was not sufficient. For projects that may require very accurate flux density scales, a user may want to flag the flux gain table by hand and/or use the scripted pipeline.
  
• The pipeline does not fully support multi-band datasets, this is because the pipeline only derives a single minimum solution interval and maximum solution interval for the entire execution, regardless of the optimal solution intervals for each band. For instance a C-band and Ka-band resource may have 5 second and 2 second integration times, respectively. However, the minimum solution interval would be chose to be 5 seconds by the pipeline. This can lead to unwanted decorrelation in calibration at the higher frequencies. Users are currently advised to split their data into a single MS per band and run the pipeline on them separately. Proper multi-band support is planned for a future release. The pipeline also requires that the same bandpass and flux density calibrators are used in each band.
  
• The pipeline effectively calibrates each spectral window separately. This means that the signal-to-noise ratio (s/n) on the calibrators needs to be sufficiently high that solutions can be obtained within the solution intervals specified in the pipeline. For the delay calibrator, this means a s/n>3 per integration time, t(int); for the bandpass calibrator, a s/n>5 is required for solution times up to 10*t(int); for the gain calibrator a s/n>3 is required for solution times up to 10*t(int), and >5 for a scan average. Following the guidelines for the strength of gain calibrators as a function of observing bandwidth in the Guide to Observing with the VLA for the high frequency end of Q-band will be reasonably safe for all frequencies, although very narrow spectral channels may be problematic. In these cases the data may need to be calibrated by hand, using polynomial bandpass fitting instead.
• The pipeline does not currently support partially frequency averaged data, see section on this subject.
• The pipeline is not compatible with P-band observations (even if the SB is P-band only) due to the lack of models in CASA for P-band. For this case, the pipeline would assume a 1 Jy, flat spectral index model making all flux densities derived by the pipeline arbitrary. The pipeline heuristics have not been validated to produce reliable calibrations for P-band data at present.
• The CASA pipeline is not designed to automatically handle spectral line observations, a modified recipe can be used along with additional information in the cont.dat fie.
• The pipeline does not currently perform polarization calibration; however, if the polarization intents were set properly, the output of the calibration pipeline may be used as the staring point for polarzation calibration following the Stokes I calibration.
• The calibration pipeline supports calibration of OTF mosaic data for the VLA Sky Survey (VLASS) using a specific calibration recipe that is only validated for S-band.
• When plotting a very large number of spws, the thumbnails in hifv_makeimages may not always be present in the weblog, the CASA images themselves are still present
• The pipeline currently fails when a CALIBRATE_PHASE or CALIBRATE_AMPLI is added to a scan that already has a CALIBRATE_FLUX or CALIBRATE_BANDPASS scan intent.
• For information about know issues affecting previous release, please see the Known Issues page.

 

Previous Pipeline Releases:

CASA 5.4.1/5.4.2 Pipeline web page