EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EC030. 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 18 10:01:55 CEST 2009 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
L-band e-EVN run on 11 September 2009. The data rate was 512 Mbps. Participating telescopes were Ef, Jb1, Cm(+Kn), Mc, On, Sh, Tr and Wb. Cambridge and Knockin was limited to 128 Mbps (Merlin limitation). The targets J1036+1326 and J1353+5725 were phase-referenced to J1025+1253 and J1408+5613, respectively. Because of the slewing limitations, the Lovell Telescope (Jb1) skipped every other reference scans. RFI caused some problems for most stations, especially Medicina and Onsala. Wb IF1 was noisy. The Lovell Telescope had low sampler statistics, sensitivity was somewhat reduced. The telescope was taken offline at ~9 UT. Due to a miscommunication between Jodrell Bank and JIVE, the Lovell Telescope data were correlated with the MarkII telescope coordinates. Use CLCOR to correct for that, before fringe-fitting. MERLIN telescopes had the data in IFs 3-4. Shanghai data rate was limited to 256 Mbps.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.88 . ERI* = 0.88 . (Ef=1, Jb1=0.5, Cm=1 (Kn=1), Mc=0.96, On=1, Sh=1, Tr=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
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TSYS against time
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Mc, Tr TPI off?
WB IF1 noisy data.

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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High fringe delay, rate and phase residuals for JB because the wrong coordinate was used for correlation.

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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Mc could not slew to OQ208 at 10:10 UT?

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:
J1036+1326: pdf , or FITS .
J1025+1253: pdf (not available) , or FITS (not available) .
OQ208: pdf (not available) , or FITS (not available) .
J1408+5613: pdf (not available) , or FITS (not available) .
J1353+5725: pdf , or FITS .
Comments.

Uniformly weighted dirty map (not useful for bright sources) produced before self-cal of:
J1036+1326: pdf , or FITS .
J1025+1253: pdf (not available) , or FITS (not available) .
OQ208: pdf (not available) , or FITS (not available) .
J1408+5613: pdf (not available) , or FITS (not available) .
J1353+5725: pdf , or FITS .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1036+1326 (not available) .
J1025+1253 .
OQ208 .
J1408+5613 .
J1353+5725 (not available) .
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1036+1326: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J1025+1253: pdf , or text file , or statistical summary .
OQ208: pdf , or text file , or statistical summary .
J1408+5613: pdf , or text file , or statistical summary .
J1353+5725: pdf (not available) , or text file (not available) , or statistical summary (not available) .
Comments.
The amplitude calibration of this experiment was generally very good, but somewhat higher amplitude selfcal solutions are expected for Jb, Kn and Cm (that vary from IF to IF).
Ignore Sh large corrections -this is due to pipeline imaging limitations at high resolution (sparse uv-coverage, no short spacings for Shanghai).

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:
J1036+1326 (not available) .
J1025+1253 .
OQ208 .
J1408+5613 .
J1353+5725 (not available) .
Comments.

Calibrated visibilities and the source model of:
J1036+1326 (not available) .
J1025+1253 .
OQ208 .
J1408+5613 .
J1353+5725 (not available) .
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Calibrated visibilities against u,v distance for:
J1036+1326: pdf , or png .
J1025+1253: pdf , or png .
OQ208: pdf , or png .
J1408+5613: pdf , or png .
J1353+5725: pdf , or png .
Comments.

u,v coverage for:
J1036+1326: pdf , or png .
J1025+1253: pdf , or png .
OQ208: pdf , or png .
J1408+5613: pdf , or png .
J1353+5725: pdf , or png .
Comments.

Crude maps of sources:
J1036+1326: pdf , or FITS .
J1025+1253: pdf , or FITS .
OQ208: pdf , or FITS .
J1408+5613: pdf , or FITS .
J1353+5725: pdf , or FITS .
Comments.