EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment RG002. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Fri Mar 5 13:13:38 CET 2010 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
C-band e-EVN ToO run on 2-3 March 2010. The scheduled data rate was 1024 Mbps. Participating telescopes were Ef, Cm, Jb2, Kn, Mc, Sh, and Wb. Ef was limited to 512 Mbps (problem at the receiving side); Ef could not join the whole time to this ToO because of other VLBI observations. There was a clock jump in Medicina at ~2:15 UT. Cm had no fringes - Kn was added as a substitute. Arecibo could not join because it was still broken. Shanghai was limited to 256 Mbps in this run. Medicina was limited to 896 Mbps. Westerbork IF1 was dead. Because of the small number of telescopes, different data rates, and no Ef-Sh common visibility in the timerange when Ef could join, most of the IFs do not have 4 telescopes for amplitude self-calibration. The imaging part of the pipeline was run for AIPS IF2.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.65 . ERI* = 0.65 . (Kn=1, Jb2=1, Mc=0.56, Ef=0.5, Sh=1, Wb=0.875)

Plots of the autocorrelations
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plots of the uncalibrated amplitude and phase against time
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Mc: initial poor weights. Clock jumped at around 2:15 UT. Data transfer stopped at around 4 UT.
Wb: IF1 dead.

Plots of the uncalibrated amplitude and phase against frequency channel
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The uncalibrated amplitude and phase of the crosshand correlations against frequency channel
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TSYS against time
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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).
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Fringe-fit phase solutions (including Parallactic Angle correction).
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Fringe-fit delay solutions
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Fringe-fit rate solutions
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Telescope bandpasses
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Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
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Calibrated amplitude and phase against frequency channel
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Naturally weighted dirty map (not useful for bright sources) produced before self-cal of:
M87: pdf (not available) , or FITS (not available) .
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Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
M87: pdf (not available) , or FITS (not available) .
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Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
M87 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
M87: pdf , or text file , or statistical summary .
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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).
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Residual closure phase (visibility closure phase with model closure phase subtracted) for:
M87 (not available) .
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Calibrated visibilities and the source model of:
M87 .
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Calibrated visibilities against u,v distance for:
M87: pdf , or png .
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u,v coverage for:
M87: pdf , or png .
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Crude maps of sources:
M87: pdf , or FITS .
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