EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EJ010. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Mon Jun 25 10:32:36 CEST 2012 campbell@jive.nl

General Comments. ( Brief data summary and scan listing )
EJ010 had 12 stations, 8 16MHz IFs, two polarizations 16 frequency points per IF/pol, and 2s integrations. Considerably more information is included in the experiment's cover letter on the standard-plots portion of the EVN Archive. In the pipelining, the target source was treated as a regular source, bypassing the phase-referencing. The SOLINT was set manually to 90s. Ef, and then Wb were used as the reference stations.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.702 . ERI* = 0.702 . The losses include Ur having no correlatable data (not included in the 12 stations), On missing about 3hr due to pack problems, Ef missing about 2.5hr (on-and-off) due to azimuth control failures, Jb having no fringes early in the experiment, and Sv's LCP channles having extremely low amplitude.

Plots of the autocorrelations
Comments.
Each scan plotted separately, all stations.

plots of the uncalibrated amplitude and phase against time
Comments.
Full-experiment for Ef-* & Wb-* baselines, no calibration applied. A 2.5 minute plot-averaging was used.

Plots of the uncalibrated amplitude and phase against frequency channel
Comments.
Scalar averaged Ef-* & Wb-* baselines, each scan plotted separately. No calibration applied yet.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel (not available)
Comments.

TSYS against time
Comments.
TY1 table, each IF/pol on a separate plot.

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 amplitude from CL2 table.

Fringe-fit phase solutions (including Parallactic Angle correction).
Comments.
CL3 station phase solutions -- CL3 = CL2+SN2, thus also includes the initial amplitude/parallactic angle calibration from CL2 and the fringe solutions from SN2. Traces for both the target and phase-ref source can be seen.

Fringe-fit delay solutions
Comments.
SN2 station delay solutions for the fringed sources, each IF/pol on a separate plot. A few outliers in some IFs (Mc, Tr). Traces for both the target and phase-ref source can be seen. For this experiment, one lag corresponds to 1/32 microsecond of delay.

Fringe-fit rate solutions
Comments.
SN2 station rate solutions. A few outliers in some IFs of a couple stations. Traces for both the target and phase-ref source can be seen.

Telescope bandpasses
Comments.
Bandpass table 1. 3C345 was used for bandpass calibration.

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Full-experiment for Ef-* & Wb-* baselines, calibrated with CL3. The 2.5-min plot-averaging still applied.

Calibrated amplitude and phase against frequency channel
Comments.
Ef-* baselines calibrated with CL3 and BP1. The amp and phase plots self-scale, not necessarily going down to 0 in the case of the amps.

Naturally weighted dirty map (not useful for bright sources) produced before self-cal of:
3C345: pdf (not available) , or FITS (not available) .
1152+199: pdf (not available) , or FITS (not available) .
J1143+18: pdf (not available) , or FITS (not available) .
Comments.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
3C345: pdf (not available) , or FITS (not available) .
1152+199: pdf (not available) , or FITS (not available) .
J1143+18: pdf (not available) , or FITS (not available) .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C345 .
1152+199 .
J1143+18 .
Comments.
Plots of post-SPLIT tables SN1 for the sources that have been individually fringed.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C345: pdf , or text file , or statistical summary .
1152+199: pdf , or text file , or statistical summary .
J1143+18: pdf , or text file , or statistical summary .
Comments.
As above, but for the post-SPLIT table SN2.

Telescope sensitivities (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.
CL4 gain-amp.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
3C345 .
1152+199 .
J1143+18 .
Comments.
Separate files per (fringed) source, showing closure phase plots for all the triangles. Only stokes=I shown.

Calibrated visibilities and the source model of:
3C345 .
1152+199 .
J1143+18 .
Comments.
For each (fringed) source, plots of amp/phase on Ef-* & Wb-* baselines, calibrated with (post-SPLIT) table CL3, with a model-line overplotted.

Calibrated visibilities against u,v distance for:
3C345: pdf , or png .
1152+199: pdf , or png .
J1143+18: pdf , or png .
Comments.
For each source, a plot of amp vs. |uv| distance.

u,v coverage for:
3C345: pdf , or png .
1152+199: pdf , or png .
J1143+18: pdf , or png .
Comments.
For each source, a plot of the u-v coverage.

Crude maps of sources:
3C345: pdf , or FITS .
1152+199: pdf , or FITS .
J1143+18: pdf , or FITS .
Comments.
For each source, a CLEAN map resulting from the automated fringing and self-cal iterations (or phase-referencing) in the pipeline script.