EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment ET031A. 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 Jun 26 14:24:13 CEST 2015 zparagi@jive.eu

General Comments. ( Brief data summary and scan listing )
ET031A, L-band e-VLBI trigger on 2015 June 23-24. Participating telescopes were Effelsberg, Hartebeesthoek, Jodrell Bank (MkII), Medicina, Onsala, Sheshan, Torun, and Westerbork.

The following subbands were flagged in this pipeline because they were corrupt/highly unstable due to strong RFI or for another reason: Jb IF4-5, IF7; Tr IF1, IF6-7; Mc:IF1-2, IF8, Wb: IF2. Some additional flagging might help the data processing/imaging. Note the area is strongly scatter-broadened at the L-band. Weak/no fringes at Shanghai is not purely for this reason though.

The target V404Cyg was phase-referenced to J2025+3343. Note WSRT had roblems with producing the cal file, and there were no Tsys data recorded in the logs for Jb2. Used nominal gains for these telescopes (scaled ~to real performance based on the initial pipeline results on EC052E and ET031A).

The EVN reliability indicator (ERI) for this experiment was ERI = 0.57 . ERI* = 0.87 . (Ef=1, Hh=0.88/1, Jb2=0.63/1, Mc=0.63/1, On=1, Sh=0.5, Tr=0.63/1, Wb=0.88/1)

Plots of the autocorrelations
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plots of the uncalibrated amplitude and phase against time
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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:
3C395: pdf (not available) , or FITS (not available) .
V404CYG: pdf , or FITS .
3C454.3: pdf (not available) , or FITS (not available) .
J2025+3343: 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:
3C395: pdf (not available) , or FITS (not available) .
V404CYG: pdf , or FITS .
3C454.3: pdf (not available) , or FITS (not available) .
J2025+3343: 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.
3C395 .
V404CYG (not available) .
3C454.3 .
J2025+3343 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C395: pdf , or text file , or statistical summary .
V404CYG: pdf (not available) , or text file (not available) , or statistical summary (not available) .
3C454.3: pdf , or text file , or statistical summary .
J2025+3343: 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:
3C395 .
V404CYG (not available) .
3C454.3 .
J2025+3343 .
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Calibrated visibilities and the source model of:
3C395 .
V404CYG (not available) .
3C454.3 .
J2025+3343 .
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Calibrated visibilities against u,v distance for:
3C395: pdf , or png .
V404CYG: pdf , or png .
3C454.3: pdf , or png .
J2025+3343: pdf , or png .
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u,v coverage for:
3C395: pdf , or png .
V404CYG: pdf , or png .
3C454.3: pdf , or png .
J2025+3343: pdf , or png .
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Crude maps of sources:
3C395: pdf , or FITS .
V404CYG: pdf , or FITS .
3C454.3: pdf , or FITS .
J2025+3343: pdf , or FITS .
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