EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EP087A_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: Tue Jul 23 17:44:53 CEST 2013 campbell@jive.nl

General Comments. ( Brief data summary and scan listing )
EP087A had 10 good stations, 8 16MHz IFs, 4 polarizations, 32 frequency points per IF/pol, and 1s integrations. Considerably more information is included in the experiment's cover letter on the standard-plots portion of the EVN Archive. This pipelining corresponds to the multiple phase-center output target ARP299B. In the pipelining, the target sources were treated as phase-reference targets and were not separately fringe-fit. The SOLINT was set automatically to a value commensurate with a typical reference-source scan. Ef, then Wb, and then Ys, were used as the reference stations.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.569 . ERI* = 0.599 . The losses include Sv, Zc, & Bd being completely lost, Ur missing 7 of the 16 channels due to VSI-geo BBC/bit-stream patching, and Tr missing about an hour. Ef's loss of about an hour-and-a-half for snow is reflected in the ERI, but not the ERI*.

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

plots of the uncalibrated amplitude and phase against time
Comments.
Full-experiment for Wb-* 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 Wb-* baselines, each scan plotted separately. No calibration applied yet.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel
Comments.
Scalar averaged Wb-* baselines showing LR, each scan plotted separately. No calibration applied yet.

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 (Mc and Tr missed the 4C39.25 scans, so would have been lost in the pipelining without another BP calibrator).

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Full-experiment for Wb-* baselines, calibrated with CL3. The 1.5-min plot-averaging still applied.

Calibrated amplitude and phase against frequency channel
Comments.
Wb-* 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:
ARP299B: pdf , or FITS .
4C39.25: pdf (not available) , or FITS (not available) .
J1128+5925: pdf (not available) , or FITS (not available) .
Comments.
Naturally-weighted dirty maps of the phase-referenced-to sources.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
ARP299B: pdf , or FITS .
4C39.25: pdf (not available) , or FITS (not available) .
J1128+5925: pdf (not available) , or FITS (not available) .
Comments.
Uniformly-weighted dirty maps of the phase-referenced-to sources.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
ARP299B (not available) .
4C39.25 .
J1128+5925 .
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.
ARP299B: pdf (not available) , or text file (not available) , or statistical summary (not available) .
4C39.25: pdf , or text file , or statistical summary .
J1128+5925: 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:
ARP299B (not available) .
4C39.25 .
J1128+5925 .
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:
ARP299B (not available) .
4C39.25 .
J1128+5925 .
Comments.
For each (fringed) source, plots of amp/phase on Wb-* baselines, calibrated with (post-SPLIT) table CL3, with a model-line overplotted.

Calibrated visibilities against u,v distance for:
ARP299B: pdf , or png .
4C39.25: pdf , or png .
J1128+5925: pdf , or png .
Comments.
For each source, a plot of amp vs. |uv| distance.

u,v coverage for:
ARP299B: pdf , or png .
4C39.25: pdf , or png .
J1128+5925: pdf , or png .
Comments.
For each source, a plot of the u-v coverage.

Crude maps of sources:
ARP299B: pdf , or FITS .
4C39.25: pdf , or FITS .
J1128+5925: 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.