EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EI009A_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 Oct 19 12:44:32 CEST 2007 bignall@jive.nl

General Comments. ( Brief data summary and scan listing )
Spectral line phase-referencing experiment at 1612 MHz, observed on 10 Jun 2007. Data rate was 128 Mbps (1 X 1 MHz subband and 3 X 4 MHz subbands, each sampled at 8 Ms/sec, dual polarization, two-bit sampling). The target source 'IRAS1828' was calibrated using the phase-reference source 'J1832-10'. 'J1743-03' was the fringe finder. The data were correlated in two passes. The plots below show data from the line pass (1 MHz subband with 1024 frequency points).
8 stations participated.

The EVN reliability indicator (ERI) for this experiment was ERI = 0.93 . ERI* = 0.93 . (EF=1, WB=1, MC=1, NT=1, TR=0.88, HH=1, CM=1, JB=0.88)

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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Wb: some anomalously high values, may need flagging.

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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Solutions not found for many data in the pipeline. A different calibration procedure, probably using solutions from J1743-03 then fringe-fitting on J1832-10 after averaging IFs in the continuum pass, should be used.

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:
J1743-03: pdf (not available) , or FITS (not available) .
IRAS1828: pdf , or FITS .
J1832-10: 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:
J1743-03: pdf (not available) , or FITS (not available) .
IRAS1828: pdf , or FITS .
J1832-10: 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.
J1743-03 .
IRAS1828 (not available) .
J1832-10 .
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Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1743-03: pdf , or text file , or statistical summary .
IRAS1828: pdf (not available) , or text file (not available) , or statistical summary (not available) .
J1832-10: 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:
J1743-03 .
IRAS1828 (not available) .
J1832-10 (not available) .
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Calibrated visibilities and the source model of:
J1743-03 .
IRAS1828 (not available) .
J1832-10 (not available) .
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Calibrated visibilities against u,v distance for:
J1743-03: pdf , or png .
IRAS1828: pdf , or png .
J1832-10: pdf (not available) , or png (not available) .
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u,v coverage for:
J1743-03: pdf , or png .
IRAS1828: pdf , or png .
J1832-10: pdf (not available) , or png (not available) .
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Crude maps of sources:
J1743-03: pdf , or FITS .
IRAS1828: pdf , or FITS .
J1832-10: pdf (not available) , or FITS (not available) .
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