EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EF015_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: Fri Sep 8 14:55:06 CEST 2006 bignall@jive.nl

General Comments. ( Brief data summary and scan listing )
6GHz spectral line (excited OH) experiment, observed on 11 Jun 2006. Data rate was 32 Mbps (2 X 0.5 MHz subbands, 4x oversampling, dual polarization, two-bit sampling). In the pipeline, the target source 'W3OH' was calibrated using 'J0207+6246'. '3C84' was the fringe finder.
8 stations participated. The MERLIN antenna at Darnhall was used in place of Cambridge. The MkII telescope at Jodrell has no good LCP data in this band, as there was a problem with their BBC #3.
This page shows data from the second correlator pass (i.e. the second subband in the schedule at 6031 MHz)

The EVN reliability indicator (ERI) for this experiment was ERI = 0.86 . ERI* = 0.86 . (JB=0.5, EF=1, ON=1, MC=1, TR=0.95, NT=1, DA=1, WB=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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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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Noto has very low sensitivity at this frequency and FRING did not find good solutions on the (continuum) phase reference source. However masers are clearly detected in the spectra.

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:
3C84: pdf (not available) , or FITS (not available) .
W3OH: pdf , or FITS .
J0207+6246: 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:
3C84: pdf (not available) , or FITS (not available) .
W3OH: pdf , or FITS .
J0207+6246: 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.
3C84 .
W3OH (not available) .
J0207+6246 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C84: pdf , or text file , or statistical summary .
W3OH: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J0207+6246: 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:
3C84 .
W3OH (not available) .
J0207+6246 .
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Calibrated visibilities and the source model of:
3C84 .
W3OH (not available) .
J0207+6246 .
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Calibrated visibilities against u,v distance for:
3C84: pdf , or png .
W3OH: pdf , or png .
J0207+6246: pdf , or png .
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u,v coverage for:
3C84: pdf , or png .
W3OH: pdf , or png .
J0207+6246: pdf , or png .
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Crude maps of sources:
3C84: pdf , or FITS .
W3OH: pdf , or FITS .
J0207+6246: pdf , or FITS .
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