EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment RL003. 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 Nov 30 11:46:41 CET 2010 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
C-band e-VLBI ToO observed on 23-24 November 2010. The scheduled data rate was 1024 Mbps. Participating telescopes were Ef, Cm, Hh, Jb2, On, Mc, Sh, Tr, Ys and Wb. Mc and Ys were limited to 896 Mbps. Due to Merlin limitation, Cm had data only in one subband. Sh was limited to 256 Mbps.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.98 . ERI* = 0.98 . (Ef=0.99, Cm=1, Hh=0.9, Jb2=1, On=1, Mc=1, Sh=1, Tr=1, Ys=1, Wb=1)

Plots of the autocorrelations
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plots of the uncalibrated amplitude and phase against time
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Note sources had very low elevation at start.
Ef: initially partly blocked by hills. ~10 minutes late becuase of SU problem.
Hh: missed first half hour because of Mk5/correlator SU problems;
and had trouble keeping up with 1024 Mbps till 20:30 UT.
Sh: target set at ~23:40 UT.

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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Note target was very bright, increasing the Tsys significantly. Apparently, Tsys was not correctly determined at all times for On and Mc.
Ar,Cm: used nominal Tsys.
Ef: extra attenuation added for target.
Jb: bad CAL measurements, used scaled TPI.
Tr: no CAL measurements done, used nominal Tsys.

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:
CRAB-1: pdf , or FITS .
J0518+2054: 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:
CRAB-1: pdf , or FITS .
J0518+2054: 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.
CRAB-1 (not available) .
J0518+2054 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
CRAB-1: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J0518+2054: 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:
CRAB-1 (not available) .
J0518+2054 .
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Calibrated visibilities and the source model of:
CRAB-1 (not available) .
J0518+2054 .
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Calibrated visibilities against u,v distance for:
CRAB-1: pdf , or png .
J0518+2054: pdf , or png .
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u,v coverage for:
CRAB-1: pdf , or png .
J0518+2054: pdf , or png .
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Crude maps of sources:
CRAB-1: pdf , or FITS .
J0518+2054: pdf , or FITS .
Comments.