EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EP075G_1. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: lun nov 11 16:09:34 CET 2013 agudo@jive.nl

General Comments. ( Brief data summary and scan listing )
EP075G had 12 stations (10 of them providing good data), 8 16MHz IFs, 2 polarizations, 32 frequency points per IF/pol, and 4s integrations. Considerably more information is included in the experiment's cover letter on the standard-plots portion of the EVN Archive. The SOLINT was set to the scan length. Ef (and then Wb, Tr) were used as the reference stations.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.530 . ERI* = 0.682 . The losses include: all data from Sv (no data was recorded from this station, no disk-packs available because of problems on their delivery) and from Sh (too low amplitudes on baselines with Sh all along the observations, phases are also too noisy, no fringe solutions on baselines with Sh even for the fringe finder). Weather losses contribute to the ERI, but not the ERI*. Flagging of entire subbands to mitigate the effect of RFI are considered weather losses. We took into account some RFI losses for this project. These correspond to the subband flags because of RFI specified in file ep075g_.chflag that were used as inputs for running the EVN pipeline on the data.

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-* baselines, no calibration applied. A 2 minute plot-averaging was used.

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

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

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. 4C39.25 and J1128+5925 were used for bandpass calibration.

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Full-experiment for Ef-* baselines, calibrated with CL3.

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:
ARP299A: pdf , or FITS .
J1128+5925: pdf (not available) , or FITS (not available) .
4C39.25: pdf (not available) , or FITS (not available) .
Comments.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
ARP299A: pdf , or FITS .
J1128+5925: pdf (not available) , or FITS (not available) .
4C39.25: pdf (not available) , or FITS (not available) .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
ARP299A (not available) .
J1128+5925 .
4C39.25 .
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.
ARP299A: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J1128+5925: pdf , or text file , or statistical summary .
4C39.25: 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:
ARP299A (not available) .
J1128+5925 .
4C39.25 .
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:
ARP299A (not available) .
J1128+5925 .
4C39.25 .
Comments.
For each (fringed) source, plots of amp/phase on Ef-* baselines, calibrated with (post-SPLIT) table CL3, with a model-line overplotted.

Calibrated visibilities against u,v distance for:
ARP299A: pdf , or png .
J1128+5925: pdf , or png .
4C39.25: pdf , or png .
Comments.
For each source, a plot of amp vs. |uv| distance.

u,v coverage for:
ARP299A: pdf , or png .
J1128+5925: pdf , or png .
4C39.25: pdf , or png .
Comments.
For each source, a plot of the u-v coverage.

Crude maps of sources:
ARP299A: pdf , or FITS .
J1128+5925: pdf , or FITS .
4C39.25: 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.