EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EM117B_1. 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 Aug 10 13:17:48 CEST 2016 burns@jive.eu

General Comments. ( Brief data summary and scan listing )
EM117B, 6.7 GHz VLBI experiment on 2016 Feb 28. Participating telescopes were Ef, Wb, Jb, Mc, O8, Nt, Tr, Ys, Hh, Sr, Ir. 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 . (Ef=1, Wb=1, Jb=0.8, Mc=1, O8=1, Nt=1, Tr=0, Ys=1, Hh=1, Sr=1, Ir=0.9)

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
Comments.
Jb LCP only seems to detect the bright calibrators. RCP is fine, but that probably means Jb wont contribute much to polarisation measurememnts. Maybe if your data reduction is more thorough you could possibly retreive the LCP too.

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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Again you can see the LCP RCP difference for Jb (see FRING DELAY note)

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:
J1331+3030: pdf (not available) , or FITS (not available) .
J2202+4216: pdf (not available) , or FITS (not available) .
3C345: pdf (not available) , or FITS (not available) .
G25.65+1.05: pdf , or FITS .
J1821-0502: pdf (not available) , or FITS (not available) .
Comments.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
J1331+3030: pdf (not available) , or FITS (not available) .
J2202+4216: pdf (not available) , or FITS (not available) .
3C345: pdf (not available) , or FITS (not available) .
G25.65+1.05: pdf , or FITS .
J1821-0502: pdf (not available) , or FITS (not available) .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1331+3030 .
J2202+4216 .
3C345 .
G25.65+1.05 (not available) .
J1821-0502 .
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1331+3030: pdf , or text file , or statistical summary .
J2202+4216: pdf , or text file , or statistical summary .
3C345: pdf , or text file , or statistical summary .
G25.65+1.05: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J1821-0502: pdf , or text file , or statistical summary .
Comments.

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).
Comments.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
J1331+3030 .
J2202+4216 .
3C345 .
G25.65+1.05 (not available) .
J1821-0502 .
Comments.

Calibrated visibilities and the source model of:
J1331+3030 .
J2202+4216 .
3C345 .
G25.65+1.05 (not available) .
J1821-0502 .
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Calibrated visibilities against u,v distance for:
J1331+3030: pdf , or png .
J2202+4216: pdf , or png .
3C345: pdf , or png .
G25.65+1.05: pdf , or png .
J1821-0502: pdf , or png .
Comments.

u,v coverage for:
J1331+3030: pdf , or png .
J2202+4216: pdf , or png .
3C345: pdf , or png .
G25.65+1.05: pdf , or png .
J1821-0502: pdf , or png .
Comments.

Crude maps of sources:
J1331+3030: pdf , or FITS .
J2202+4216: pdf , or FITS .
3C345: pdf , or FITS .
G25.65+1.05: pdf , or FITS .
J1821-0502: pdf , or FITS .
Comments.
Reference source was clearly imaged, along with the other continuum sources. This data set should be fine for phase referencing.