EVN User Experiment Pipeline Feedback
Pipeline feedback for experiment UAH5.
If you have any comments on this experiment please email
the
address below.
Last updated: Fri Dec 13 15:37:49 MET 2002
biggs@jive.nl
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General Comments.
(
Brief data summary and
scan listing.)
This experiment was ad hoc and observed on 28 April 2000, outside of any EVN session. The observing frequency was 5 GHz and the observing setup, with 8 8-MHz IFs and 1-bit sampling, gave a recording rate of 128 Mb/s. Only LCP was recorded. Six telescopes were scheduled (Jb (mk2), Wb (RT7), On, Mc, Nt and Tr), but On did not ultimately take part. A attenuator problem at Tr severely degraded the sensitivity of this telescope for the majority of the experiment. The reference antenna was Jb with Nt the second choice. Station positions were updated compared to those used in the correlation.
Plots of the autocorrelations.
Comments.
Tr: first IF is dead.
Mc: band changes midway through the experiment corresponding to dead data and no measured Tsys.
Plots of the uncalibrated amplitude and phase against time.
Comments.
Tr: most data is very weak.
Resolution on one calibrator source is obvious.
Plots of the uncalibrated amplitude and phase against frequency
channel.
Comments.
CygX-3 clearly detected on Jb-Wb baseline.
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel.
Comments.
Not applicable.
TSYS against time.
Comments.
Jb: no Tsys.
Wb: 20% jump in Tsys at 5:30 to 7:00.
Nt: no Tsys from 4:30 to 5:30.
Mc: no Tsys from 5:30 to 8:00.
Tr: attenuator problem obvious.
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.
Jb, Tr: SEFD about as expected according to EVN status table
Mc, Nt: SEFD a bit higher than expected according to EVN status table
Wb: Tony Foley gave 600 as a rough SEFD for a single Wb antenna so this indicates that the telescope is approximately as expected although it could be performing a little under par.
Fringe-fit phase solutions.
Comments.
Tr: Solutions are found in other IFs despite low sensitivity.
Jb: Phase is entirely due to new station position (reference antenna).
Fringe-fit delay solutions.
Comments.
No comments.
Fringe-fit rate solutions.
Comments.
No comments.
Telescope bandpasses.
Comments.
No comments.
Calibrated amplitude and phase against time
(a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Systematic amplitudes.
Calibrated amplitude and phase against frequency channel.
Comments.
Mc: IF8 has low amplitude.
Nt: IF5 has low amplitude.
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
Solutions for J2052+3635 are in general reasonable.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Also available as a text file.
Comments.
Solutions for J2052+3635 are in general reasonable.
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.
As amplitude solutions are generally ~unity then sensitivities are little changed from above.
Residual closure phase (visibility closure phase with
model closure phase subtracted) for J2052+3635.
Residual closure phase (visibility closure phase with
model closure phase subtracted) for J2025+3343.
Comments.
Pretty good. Torun phases are reasonably well constrained.
Calibrated visibilities and the source model of
J2052+3635.
Calibrated visibilities and the source model of
J2025+3343.
Comments.
No comments.
Calibrated visibilities against u,v distance for
J2052+3635.
Calibrated visibilities against u,v distance for
J2025+3343.
Comments.
J2052+3635: some very high amplitudes.
u,v coverage for
J2052+3635.
u,v coverage for
J2025+3343.
Comments.
J2025+3343: sparse.
J2052+3635: much better.
Crude map of J2052+3635 from the pipeline.
Crude map of J2025+3343 from the pipeline.
Comments.
J2025+3343: not bad.
J2052+3635: excellent. Compares very favourably with a VLBA 13-cm map.