EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment RP024D. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Mon Oct 17 12:11:23 CEST 2016 zparagi@jive.eu

General Comments. (Brief data summary (not available) and scan listing (not available) )
RP024D, L-band ToO e-VLBI experiment, fourth epoch on 24 May 2016. Participating telescopes were Arecibo, Effelsberg, Jodrell Bank (LT), Medicina, Onsala (25m), Torun, Westerbork (single dish). Unlike EP100, Arecibo did take part in the VLBI phase-referencing of the ms-transient candidate.

The target FRB121102 was phase-referenced to the nearby source J0529+3209 (checked in RP024A). Fringe-finder 0234+285, and the ICRF calibrator used as phase-reference in RP024A, J0518+3306, were also observed for a short time. A phase-referencing scan was included between J0529+3209 (new p-ref) and J0530+3301 (p-ref check source). Two scans were added on a bright test pulsar: J0528+2200 was phase-referenced to J0521+2112.

The EVN reliability indicator (ERI) for this experiment was ERI = 1 . ERI* = 1 . (Ef=1, Jb1=1, Mc=1, On=1, Tr=1, Wb=1, Ar=1)

Plots of the autocorrelations (not available)
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Plots of the uncalibrated amplitude and phase against time (not available)
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Plots of the uncalibrated amplitude and phase against frequency channel (not available)
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The uncalibrated amplitude and phase of the crosshand correlations against frequency channel (not available)
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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 (not available) (a priori amplitude calibration and fringe-fit solutions applied).
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Calibrated amplitude and phase against frequency channel (not available)
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Naturally weighted dirty map (not useful for bright sources) produced before self-cal of:
J0529+3209: 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:
J0529+3209: 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.
J0529+3209 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J0529+3209: 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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Ar issues?

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
J0529+3209 (not available) .
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Calibrated visibilities and the source model of:
J0529+3209 (not available) .
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The phase-reference source J0529+3209 data show that Ar amplitudes vary strongly through the experiement, while SEFDs do not change that much. Pointing error?

Calibrated visibilities against u,v distance for:
J0529+3209: pdf (not available) , or png (not available) .
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u,v coverage for:
J0529+3209: pdf (not available) , or png (not available) .
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Crude maps of sources:
J0529+3209: pdf , or FITS .
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