EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EJ016A. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.


Last updated: Wed Jul 27 19:24:36 CEST 2016 burns@jive.eu


General Comments. ( Brief data summary and scan listing )
EJ016A, L-band VLBI experiment on 2016 March 03. Participating telescopes were Jb, Wb, Ef, Mc, O8, T6, Ur, Tr, Sv, Zc, Bd, Sr. You can find information on individual stations at: http://www.evlbi.org/user_guide/EVNstatus.txt.


The EVN reliability indicator (ERI) for this experiment was ERI = 0.8 . ERI* = 0.8 . (Jb=1, Wb=1, Ef=1, Mc=1, Nt=0, O8=1, T6=0, Ur=1, Tr=1, Sv=1, Zc=1, Bd=1, Sr=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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IF 8 for Sv, Zc and Bd did not make it into the data. Also, due to unphysical TSYS values derived from the station log from Sv we had to fudge IF 1 in both RCP and LCP to match the others (I simply re-used IF 2 TSYS values). You could just flag IF1 if it looks suspicious to you, but, lookng at the FRING results of Sv - IF1 seems ok to use. IFs 8, as mentioned earlier, didnt make it as far as fring (Sv, Zc, Bd).


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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You can see some messy results at all stations at about 21:30 UT. This is just because the refant, Sr, must have had bad solutions. It should be fine on non-Sr baselines.


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:
HS0810: pdf , or FITS .
4C39.25: pdf (not available) , or FITS (not available) .
J0813+25: 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:
HS0810: pdf , or FITS .
4C39.25: pdf (not available) , or FITS (not available) .
J0813+25: 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.
HS0810 (not available) .
4C39.25 .
J0813+25 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
HS0810: pdf (not available) , or text file (not available) , or statistical summary (not available) .
4C39.25: pdf , or text file , or statistical summary .
J0813+25: 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:
HS0810 (not available) .
4C39.25 .
J0813+25 .
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Calibrated visibilities and the source model of:
HS0810 (not available) .
4C39.25 .
J0813+25 .
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Calibrated visibilities against u,v distance for:
HS0810: pdf , or png .
4C39.25: pdf , or png .
J0813+25: pdf , or png .
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u,v coverage for:
HS0810: pdf , or png .
4C39.25: pdf , or png .
J0813+25: pdf , or png .
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Crude maps of sources:
HS0810: pdf , or FITS .
4C39.25: pdf , or FITS .
J0813+25: pdf , or FITS .
Comments.
The bright calibrator is seen nicely, the reference source is also imaged (see ej016a_J0813+25_ICLN_2.pdf). You should get good results with these data!