EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment RG001A. 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 May 26 16:27:27 CEST 2009 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
K-band e-EVN ToO run on 23 May 2009. Aggregate bitrate was 512 Mbps with 2-bit sampling. There were in 4*16MHz subbands in both RCP and LCP. The target source was J0948+0022, the fringe-finder 1055+018, and an additional amplitude calibrator was 0805-077. Participating telescopes were Shanghai, Kashima (no fringes), Mopra, Hobart (a single LCP subband), Effelsberg, Medicina, Onsala, Jodrell Bank and Cambridge. Yebes could not participate because the Internet connection broke at the observatory. Hobart fringe were not found initially because of a setup problem, which was fixed before the global part started. Lost about 20 minutes after the global part ended, trouble with starting the new correlation job.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.61 . ERI* = 0.85 . (Cm=0.92, Jb2=0.92, Mc=0.92, Ef=0.92, On=0.92, Sh=0.97, Ys=0/1)

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:
0805-077: pdf (not available) , or FITS (not available) .
1055+018: pdf (not available) , or FITS (not available) .
J0948+0022: 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:
0805-077: pdf (not available) , or FITS (not available) .
1055+018: pdf (not available) , or FITS (not available) .
J0948+0022: 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.
0805-077 .
1055+018 .
J0948+0022 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
0805-077: pdf , or text file , or statistical summary .
1055+018: pdf , or text file , or statistical summary .
J0948+0022: 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:
0805-077 .
1055+018 (not available) .
J0948+0022 .
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Calibrated visibilities and the source model of:
0805-077 .
1055+018 .
J0948+0022 .
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Calibrated visibilities against u,v distance for:
0805-077: pdf , or png .
1055+018: pdf , or png .
J0948+0022: pdf , or png .
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u,v coverage for:
0805-077: pdf , or png .
1055+018: pdf , or png .
J0948+0022: pdf , or png .
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Crude maps of sources:
0805-077: pdf , or FITS .
1055+018: pdf , or FITS .
J0948+0022: pdf , or FITS .
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