EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EP107B_2. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: wo aug 22 19:50:01 CEST 2018 burns@jive.eu

General Comments. ( Brief data summary and scan listing )
EP107B, 1.6 GHz experiment on 17th Nov 2017.
Participating stations: Jb, Ef, Wb, O8, Mc, Tr, T6, Sh, Ur, Sv, Zc, Bd, Hh, Cm, Da, Kn, Ta
You can find information on individual stations at:
http://www.evlbi.org/user_guide/EVNstatus.txt.

The following are plots from the EVN pipeline analysis, in which the refant was: Ef


Plots of the autocorrelations
Comments.
Auto-corr Amplitude vs frequency plots for each station showing all IFs and Pols. RFI can easily be found by looking at the continuum source scans in this plot.

Plots of the uncalibrated amplitude and phase against time
Comments.
Amp and phase vs time, for the whole experiment. Shows visibilities on all baselines to the refant. All IFs and Pols shown. This is a good place to look for stations that missed scans during the experiment.

Plots of the uncalibrated amplitude and phase against frequency channel
Comments.
Uncalibrated, vector averaged, cross power specra for baselines to the refant. No bandpass done yet. This is a good place to look check how well detected sources are on each baseline.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel
Comments.

TSYS against time
Comments.
Plots of system temperature vs time for each station (and each IF). Flat-line plots indicate that this information was not available for a given station, in which case we create a generic tsys table scalled to the station's gain (Jy/K).

Telescope sensitivities from the a priori TSYS and Gain curves (the square of this number gives the antenna noise (SEFD) in Jy - the smaller the better).
Comments.
Gain info in CL2, determined using tsys tables. Plot shows Gain vs time for each station, each IF and each Pol.

Fringe-fit phase solutions (not available) (including Parallactic Angle correction).
Comments.
Pot of CL3. This is the CL table generated using CL2 (amplitude cal) and SN2 (FRING solutions). Plot shows phase calibration data vs time. Missing data indicate possible issues in those previous steps. If the data are complete (all stations and most scans present) then use this table to phase-reference the target.

Fringe-fit delay solutions (not available)
Comments.
Plot of SN2. Shows delay vs time from FRING results (usually only calibrators and reference sources). This is a good place to look for times where FRING failed to get solutions. Here FRING uses a signal to noise cutoff of 7. If FRING fails a lot it would be a good idea to retry with a lower signal to noise cutoff. This is the line pass data. We expect better FRING solutions in the continuum data.

Fringe-fit rate solutions (not available)
Comments.
SN2 as abover, but for rate.

Telescope bandpasses (not available)
Comments.
Plot of BP1; the bandpass characteristic of each station, determined using the brightest source(s) in the experiment. Look for small dispersion in the phase data, this indicates a high signal to noise - which will lead to better bandpass characterisation.

Calibrated amplitude and phase against time (not available) (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Plot of visibilities vs time for all baselines to the refant, after applying CL3. This is a good place to look for quickly checking the success of the antab (CL2) and FRING (CL3) stages of the pipeline.

Calibrated amplitude and phase against frequency channel (not available)
Comments.
Amp and phas vs frequency plots for all baselines to refant, after applying CL3 and BP1. If CL3 and BP1 are good you will get flat phase and amplitude profiles, therefore this is a good place to check the success of CL2 and particluarly BP1 for each scan/baseline/IF/Pol.

Naturally weighted dirty map (not useful for bright sources) produced before self-cal of:
Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
Individual plots for each source that was used in FRING. Shows phase selfcal solutions (SN1 after SPLIT). This is particularly useful to check if the reference source could be self-calibrated, and to look for missing scans/antennae. These are more useful in the continuum pass data.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
Individual plots for each source that was used in FRING. Shows amplitude selfcal solutions (SN2). This table is important to properly calibrate amplitudes from stations that had to use generic tsys tables (see TSYS, above). These are more useful in the continuum pass data.

Telescope sensitivities (not available) (the total AMP gain applied during both a priori and self calibration; the square of this number gives the antenna noise (SEFD) in Jy).
Comments.
Plot of CL4 which shows amplitude calirations determined from CL3 and the amplitude selfcal solutions from SN2 (from CALIB_AMP2, above). Comparison with GAIN plot (above) reveals the accuracy of the apriori amplitude calibration derived from the TSYS tables - this is particularly important for stations that have generic generated TSYS tables; Tsys may benefit from aditional scalling if there is a large differnce in SENS and GAIN plots.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
Calibrated visibilities and the source model of:
Calibrated visibilities against u,v distance for:
u,v coverage for:
Crude maps of sources: