EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment RSF08. 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 Mar 8 15:22:03 CET 2016 zparagi@jive.eu

General Comments. ( Brief data summary and scan listing )
RSF08, L-band short experiment in regular session 2/2015. Participating telescopes were Badary, Effelsberg, Jodrell Bank (LT), Hart, Medicina, Onsala (25m), Seshan, Svetloe, Torun, Urumqi, Westerbork (single dish) and Zelenchukskaya. There was a problem with recording at Urumqi.

The target J2216+0124 wasphase-referenced to J2217+0220. Another calibrator observed: J2148+0657.

Nominal SEFDs were used for a-priori amplitude calibration for the following telescopes: Bd, Jb1, Sh, Sv, Zc. The FT factors were adjusted in the antab file based on initial pipeline results. Note this is just a best-effort attempt: both calibrators appeared resolved. The large correction needed for Hart (FT=0.3) is actually suspicious, because Hart calibration is usualy much better. In case of Jb and Sh it is not clear if the correct gain curves were used -check!

The EVN reliability indicator (ERI) for this experiment was ERI = 0.83 . ERI* = 0.83 . (Bd=1, Jb1=1, Ef=0.9, Hh=1, Mc=1, On=1, Sh=1, Sv=1, Tr=1, Ur=0, Wb=1, Zc=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 (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 (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:
J2216+0124: pdf , or FITS .
J2148+0657: pdf (not available) , or FITS (not available) .
J2217+0220: 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:
J2216+0124: pdf , or FITS .
J2148+0657: pdf (not available) , or FITS (not available) .
J2217+0220: 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.
J2216+0124 (not available) .
J2148+0657 .
J2217+0220 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J2216+0124: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J2148+0657: pdf , or text file , or statistical summary .
J2217+0220: 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:
J2216+0124 (not available) .
J2148+0657 .
J2217+0220 .
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Calibrated visibilities and the source model of:
J2216+0124 (not available) .
J2148+0657 .
J2217+0220 .
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Calibrated visibilities against u,v distance for:
J2216+0124: pdf , or png .
J2148+0657: pdf , or png .
J2217+0220: pdf , or png .
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u,v coverage for:
J2216+0124: pdf , or png .
J2148+0657: pdf , or png .
J2217+0220: pdf , or png .
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Crude maps of sources:
J2216+0124: pdf , or FITS .
J2148+0657: pdf , or FITS .
J2217+0220: pdf , or FITS .
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