EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EK037_2. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Thu Nov 10 19:07:16 CET 2016 burns@jive.eu

General Comments. ( Brief data summary and scan listing )
EK037, 22 GHz VLBI experiment on 2016 June 8th. Participating telescopes were Ef, Jb, On, Mc, Nt, Sr, Tr, Ys, Mh, Ku, Ky, Kt, Sv, Zc, Bd. 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 = . ERI* = .

Plots of the autocorrelations
Comments.
As with the continuum data, careful RFI flagging is recommended.

Plots of the uncalibrated amplitude and phase against time
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Plots of the uncalibrated amplitude and phase against frequency channel
Comments.
The maser is detected on all baselines, see pages 675 to 678 for CEPA-HW2 and 683 to 686 for CEPA-HW3 (Earlier scans have no Noto station)

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.
As with the cont. data, FRING should be done on a low SNR, or do inverse phase referencing.

Fringe-fit rate solutions
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Telescope bandpasses
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Looks fine

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:
J2202+4216: 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:
J2202+4216: 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.
J2202+4216 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J2202+4216: 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).
Comments.
Looks fine

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
J2202+4216 .
Comments.

Calibrated visibilities and the source model of:
J2202+4216 .
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Calibrated visibilities against u,v distance for:
J2202+4216: pdf , or png .
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u,v coverage for:
J2202+4216: pdf , or png .
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Crude maps of sources:
J2202+4216: pdf , or FITS .
Comments.