EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment GB075C. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Sun Jan 31 14:21:08 CET 2016 mao@jive.eu

General Comments. ( Brief data summary and scan listing )
L-band experiment, observed on 29 May 2015. GB075C contains 8 x 16MHz bands and 4 x polarizations, each with 32 frequency points. BLLAC was used as the fringe-finder.
18 stations scheduled (8 EVN stations)

The EVN reliability indicator (ERI) for this experiment was ERI = 0.64 . ERI* = 0.64 . The ERI* value takes into account that:
- NT had no data
- KY is flagged out for half of the time
Note that only EVN stations contribute to the ERI statistics.
The ERI value also takes into account losses that are outside the station's control, of which there were none for this experiment.

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-* & Nl-* baselines, no calibration applied. A 1.5 minute plot-averaging was used.

Plots of the uncalibrated amplitude and phase against frequency channel
Comments.
Scalar averaged Ef-* & Nl-* baselines, each scan plotted separately. No calibration applied yet. JB IF3 is weak on both pols. KP and FD show a slope of increasing amp with frequency, possibly due to being at the edge of the band. IF 1 on KP may need to be flagged.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel
Comments.
Note that the feedback form says that MH has crossed pols but that is not obvious in these plots.

TSYS against time
Comments.
TY1 table, each IF/pol on a separate plot. The ANTAB information for the VLBA stations was derived from the 80-Hz continuous-cal system as read from its effect on the stations' sampler statistics during correlation.

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. GAIN looks high for the KVN stations in the first half..

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.

Fringe-fit delay solutions
Comments.
SN2 station delay solutions for the fringed sources, each IF/pol on a separate plot.

Fringe-fit rate solutions
Comments.
SN2 station rate solutions.

Telescope bandpasses
Comments.
Bandpass table 1. BLLAC was used for bandpass calibration. Some more edge channel flagging may be beneficial.

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Full-experiment for Ef-* & Nl-* baselines, calibrated with CL3. A 1.5 minute plot-averaging was used.

Calibrated amplitude and phase against frequency channel
Comments.
Ef-* & Nl-* 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:
2013+370: pdf (not available) , or FITS (not available) .
CYG-A: pdf (not available) , or FITS (not available) .
BLLAC: pdf (not available) , or FITS (not available) .
Comments.
Naturally weighted dirty maps of phase-referenced sources. NA here

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
2013+370: pdf (not available) , or FITS (not available) .
CYG-A: pdf (not available) , or FITS (not available) .
BLLAC: pdf (not available) , or FITS (not available) .
Comments.
Uniformly weighted dirty maps of phase-referenced sources. NA here

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
2013+370 .
CYG-A .
BLLAC .
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.
2013+370: pdf , or text file , or statistical summary .
CYG-A: pdf , or text file , or statistical summary .
BLLAC: 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:
2013+370 .
CYG-A .
BLLAC .
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:
2013+370 .
CYG-A .
BLLAC .
Comments.
For each (fringed) source, plots of amp/phase on Ef-* & Nl-* baselines, calibrated with (post-SPLIT) table CL3, with a model-line overplotted.

Calibrated visibilities against u,v distance for:
2013+370: pdf , or png .
CYG-A: pdf , or png .
BLLAC: pdf , or png .
Comments.
For each source, a plot of amp vs. |uv| distance.

u,v coverage for:
2013+370: pdf , or png .
CYG-A: pdf , or png .
BLLAC: pdf , or png .
Comments.
For each source, a plot of the u-v coverage.

Crude maps of sources:
2013+370: pdf , or FITS .
CYG-A: pdf , or FITS .
BLLAC: 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.
The peak fluxes for the calibrator sources seem to be ~<2x too low??