EVN User Experiment Pipeline Feedback
Pipeline feedback for experiment ER014.
If you have any comments on this experiment please email
the
address below.
Last updated: Wed Mar 12 09:51:41 CET 2003
zparagi@jive.nl
|
General Comments.
(
Brief data summary and
scan listing.)
EVN-MERLIN C-band continuum experiment using 128-4-2 observing mode, resulting in four 8 MHz IFs (16 MHz/polarization). There were 8 EVN telescopes participating (EbCmWbOnMcNtTr). Effelsberg was the reference antenna in the pipeline processing of the data. The fringe-finder was DA193.
The EVN reliability indicator was ERI=ERI*=0.96 (Mc=1, Ef=0.99, Tr=0.98, Wb=1, On=1, Jb=1, Cm=0.89, Nt=1)
in this experiment. ERI gives you an estimate of the ratio of observed/good visibilities to the
expected number visibilities. ERI* is the same but excluding data loss due to e.g. bad weather.
Plots of the autocorrelations.
Comments.
Plots of the uncalibrated amplitude and phase against time.
Comments.
Problems with Eb during the first DA193 scan. Target sources seem to be detected.
Plots of the uncalibrated amplitude and phase against frequency
channel.
Comments.
Cm: L2 has low amplitude.
TSYS against time.
Comments.
Cm: no Tsys data are available
Wb: missing Tsys between UT 0:00-8:00 on the 2nd day of observations
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).
Comments.
On: 30-40% less sensitive than expected, especially in the second half of the observations.
See the EVN Status Tables.
Fringe-fit phase solutions.
Comments.
Fringe-fit delay solutions.
Comments.
For DA193
Fringe-fit rate solutions.
Comments.
For DA193
Telescope bandpasses.
Comments.
Cm: large phase variation in the bandpass is introduced by the microwave link between Cm and Jb
Calibrated amplitude and phase against time
(a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Calibrated amplitude and phase against frequency channel.
Comments.
Cm: L2 is low
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
Naturally weighted dirty map produced before self-cal of:
DA193.
Comments.
Uniformly weighted dirty map produced before self-cal of:
DA193.
Comments.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Also available as a text file.
Comments.
Cm: very large corrections in L2
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.
Cm: L2 is much less sensitive than expected (by a factor of 10 in Tsys)
On: low sensitivity is not corrected by selfcal
Residual closure phase (visibility closure phase with model closure phase subtracted) for:
DA193.
Comments.
Non-closing errors are small, except in the first DA193 scan for some telescopes
(Eb did not detect the source)
Calibrated visibilities and the source model of:
DA193.
Comments.
Calibrated visibilities against u,v distance for:
DA193. postscript , png (smaller)
Comments.
u,v coverage for:
DA193
postscript, png (smaller)
Comments.
Crude map of DA193 from the pipeline.
Comments.