EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EP064G. 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 Sep 8 11:01:19 CEST 2009 yang@jive.nl

General Comments. ( Brief data summary and scan listing )
C band phase-referencing experiment, observed on 11 Jun 2009. Data rate was 1 Gbps (8 X 16 MHz subbands, dual polarization, two-bit sampling). The target sources IRAS1949 was calibrated using the phase-reference sources J1941-0511. 3C286 was also observed as calibrators. 3C345 was the fringe finder.

12 stations participated. Urumqi used a recording rate of 512 Mbps.

The EVN reliability indicator (ERI) for this experiment was ERI = 1 . ERI* = 1 . (Ef=1, Mc=1, Cm=1, On=1, Jb=1, Ur=1, Ys=1, Tr=1, Kn=1, Wb=1, Nt=1, Sh=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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Jb: Tsys was too high for IF 1 and 2.

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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Refant=Ef.

Fringe-fit delay solutions
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Fringe-fit rate solutions
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Telescope bandpasses
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Sh: unusual bandpass in IF 5-8.

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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Some sensitive baselines (e.g. Ef -- Wb) had a phase pattern across each subband on the scale of a few degree during the scan of the brighter sources. This is the Gibbs phenomenon, a kind digital effect caused by the sharp edge at baseband. Try to use the paramether "smooth" (e.g. Hanning smooth) in AIPS to reduce the effect.

Naturally weighted dirty map (not useful for bright sources) produced before self-cal of:
3C286: pdf (not available) , or FITS (not available) .
3C345: pdf (not available) , or FITS (not available) .
IRAS1929: pdf , or FITS .
J1941-0511: pdf (not available) , or FITS (not available) .
Comments.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
3C286: pdf (not available) , or FITS (not available) .
3C345: pdf (not available) , or FITS (not available) .
IRAS1929: pdf , or FITS .
J1941-0511: pdf (not available) , or FITS (not available) .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C286 .
3C345 .
IRAS1929 (not available) .
J1941-0511 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C286: pdf , or text file , or statistical summary .
3C345: pdf , or text file , or statistical summary .
IRAS1929: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J1941-0511: 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).
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Residual closure phase (visibility closure phase with model closure phase subtracted) for:
3C286 .
3C345 .
IRAS1929 (not available) .
J1941-0511 .
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Calibrated visibilities and the source model of:
3C286 .
3C345 .
IRAS1929 (not available) .
J1941-0511 .
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Calibrated visibilities against u,v distance for:
3C286: pdf , or png .
3C345: pdf , or png .
IRAS1929: pdf , or png .
J1941-0511: pdf , or png .
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u,v coverage for:
3C286: pdf , or png .
3C345: pdf , or png .
IRAS1929: pdf , or png .
J1941-0511: pdf , or png .
Comments.

Crude maps of sources:
3C286: pdf , or FITS .
3C345: pdf , or FITS .
IRAS1929: pdf , or FITS .
J1941-0511: pdf , or FITS .
Comments.
All the calibrators were detected.