Pipeline: Frequent VLA problems
The VLA pipeline delivers calibrated data and some initial images of VLA observation runs. The quality of the calibration and imaging products is usually assessed through the weblog that is created in each pipeline run (see also the VLA Pipeline guide). During the observations, the VLA may have encountered technical problems that are reflected in various ways in the weblog, where graphs show the behavior of the calibration tables as a function of time, frequency, polarization, etc., and analytical numbers describe the amount of flagging, derived fluxes, image statistics, etc.
Here we would like to briefly describe common VLA observing problems, how they are identified in the pipeline calibration weblog, and how they can be addressed.
Radio Frequency Interference
By far the biggest problem is radio frequency interference (RFI). RFI is produced by internal and external sources, can be terrestrial or from satellites that operate at or spill into the observed frequency. For the VLA, please find more information on the Radio Frequency Interference webpage. Although weak RFI may only slightly raise the noise of an image with little influence on the calibration tables, stronger RFI will produce artifacts that may render the data (target and calibrators) unusable, if not adequately flagged. An example for strong RFI is shown below. Flagging procedures are outlined in the VLA topical CASA guide on flagging.
It is important that all data are free of
FIX: Weak, intermittent RFI will increase the noise and be down-weighted in the imaging in the hifv_statwt task. Strong RFI needs to be flagged and only clean data should be calibrated and imaged. Flagging can be manual or automatic.
At higher frequencies the VLA requires regular pointing calibrations. Each pointing run will reposition the antennas to be centered on a strong source with known position. If the pointing solution fails, the amplitude of the source will drop, or drift away from the center of the antenna with the highest gain. A typical graph looks like the one shown below. The pointing solution for the first half of the run failed, which results in the source drifting away from the center of the primary beam. After a pointing update in the middle of the run, the antenna is positioned properly again (the very last data points are actually a different source, hence the drop at the edge).
FIX: If the pointing is only off by a small amount, the gain calibration will take care of it. If it is off by a large amount, the data for this period and antenna needs to be flagged.
Various hardware failures can cause the phase for a given antenna to be unstable in time, often with sudden, large changes in phase over time. Depending on where the problem is, this may affect just a portion of the data or up to all data on a given antenna. In the first example below, only one baseband's data is affected (large changes at each data point) while the other baseband remains near zero and is not affected. This plot, from the pipeline's Final phase gain cal section found in the 'hifv_finalcals' stage, shows the final phase solutions found for each calibrator (using the long solution interval).
Typical phase variations for low frequency data are a few degrees. For high frequencies tens of degrees can occur, and the cycle time between the phase calibrator and the target needs to be reduced to adequately track and interpolate the phase variations as a function of time. If the phases vary more than 360 degrees between two phase calibrator scans, then the data are completely decorrelated and cannot be calibrated anymore.
FIX: If there are phase jumps, usually the data for the affected time range needs to be flagged for the antenna(s).
The digital transmission system (DTS) of each VLA antenna includes a formatting stage to convert the electronic to an optical signal before it is injected on the optical fiber link. On the correlator end the signal will be deformatted back to an electronic signal. Occasionally, the timing on the deformatter can be misaligned which results in very strong amplitude or phase slopes as a function of frequency. When this occurs, then the data are corrupt and the entire affected baseband per polarization of an antenna need to be flagged. Frequently the error shows up similar to an abs(sin) or a 'bouncing' signal across a baseband for one polarization, or, in other terms, various numbers of 'V' shapes in the data, usually in the middle of a baseband.
FIX: The data for this baseband, antenna and polarization need to be flagged.
Under some circumstances, the WIDAR correlator writes exact zeros. The pipeline will usually flag them automatically. If not, they can be removed with CASA's flagdata task, using the option mode='clip' with clipzeros=True or flag the zeros by hand.
FIX: The pipeline will usually catch them. If not, use CASA's flagdata task.
Baseband and Subband Edges
If spw roll-off frequency edges are very steep, they can degrade gain and phase solutions. Frequently this is not a big problem, but if the gain for the edge channels is close to zero, a division by the bandpass for these channels can get extremely noisy. This is particularly true for baseband edges. The edgespw, fracspw, and baseband parameters in hifv_flagdata can be adjusted to flag different percentages of the edges (see also VLA pipeline pages). The edges can also be flagged with the CASA task flagdata, or by hand.
FIX: Adjust the relevant parameters in hifv_flagdata and re-run the pipeline.
Strong RFI can bring the the digital and analog receiver system into a non-linear regime (also known as compression). This is especially a problem in L and S bands. Simple RFI flagging alone will not be sufficient to remove compression. The affected antennas/spw/pols will likely need to be flagged.
FIX: For strong compression, flag the affected data. Weak compression may increase the Tsys.
Some calibrator sources are not perfect point sources. For the VLA standard flux calibrator sources, models are provided within CASA. For resolved phase calibrators, the uv-range can be restricted during the solve for the calibration tables. Often, significant structure is noticeable directly in the visibility data. Figures 4a and 4b show, respectively, the visibility data for an unresolved and a resolved calibrator.
A solution is to use the flux.csv table. It is usually generated for ALMA in a pipeline run, but can be created before a VLA run. The uv-ranges listed there will be used in the processing. The format is like:
and an example entry would be:
for a uvrange of 21000-110000 lambda.
Above, ms is the MS name, field and spw are the IDs (not names, the ID will only be known once the data is in MS format and after executing listobs), I, Q, U, V are the Stokes flux densities in Jy (note that entries for the VLA will be ignored here, so a nominal I=1Jy will be ok), uvmin and uvmax are the uv ranges in units of lambda. Only one spw (the first) is used per field, other entries will be ignored. If uvmax is provided as 0 lambda, then this creates an inequality and uvmax is unbounded.
FIX: Restrict the uv-range for the calculations of the calibration tables. The flux.csv table can be used.
If the intents of the data are set incorrectly for the observations, the pipeline will use the wrong calibrators for the calibration. Usually this can be fixed by overwriting the intents. The VLA pipeline webpage provides instructions and a script to do this. For more complicated setups, like multiple calibrators or bands with separate calibrator scans, data may be split into smaller MSs that contain only the relevant calibrators for each target, or data reduction by hand may be needed.
Non-ideal reference antenna
Sometimes, if the reference antenna has some issue, like RFI or extreme flagging, it is advisable to switch to a different reference antenna. Use the 'refantignore' keyword to disallow the use of this antenna as a reference. The Pipeline Page provides details on the usage of this keyword.
FIX: Use 'refantignore' to remove a problematic antenna from the list of possible reference antennas.
Extreme Solution Intervals
If the hifv_solint stage shows extreme values for the short and/or long solution intervals, then the data should be inspected and flagged.
FIX: Flagging bad data.
Weather can be good or bad. Bad weather can introduce extreme phase jumps, large increase in Tsys, or pointing errors. Flagging times during bad weather may help. The CASA task statwt will down-weight some noise variations. Also selfcal (Topical Guide: VLA Self-calibration Tutorial) will correct for phase variations. In extreme cases, however, flagging is the only method.
For some SBs the weather data are missing from the header. This is usually not a big problem. The data can be filled, however, on request. Please contact the NRAO helpdesk.
FIX: Statwt, selfcal, or flagging.
The pipeline will correct for some degree of decorrelation for all calibrators. In extreme cases, however, data need to be flagged. If decorrelation is strong, it can be assumed that the target also shows significant decorrelation. Self-calibration will be advised if the source flux is sufficient. A CASA guide for self-calibration is provided: Topical Guide: VLA Self-calibration Tutorial.
FIX: Self-calibration. In extreme cases: flagging.
The pipeline flags shadowed antennas by default. If not all of shadowing is captured, or if the shadowing criteria shall be loosened (e.g. allow a small amount of shadowing), then this can be controlled by the CASA task flagdata 'mode='shadow'. After manually flagging the data, he 'hifv_flagdata' task call should then be modified ('shadow=False') to not do additional shadowing flagging.
FIX: in CASA: flagdata mode='shadow'
Bad data due to failed switches should be flagged.
FIX: Flag the affected data.