EVN User Experiment Pipeline Feedback
Pipeline feedback for experiment EB023C.
If you have any comments on this experiment please email
the
address below.
Last updated: Wed Nov 26 17:19:36 CET 2003
bignall@jive.nl
|
General Comments.
(
Brief data summary and
scan listing.)
This is an EVN+MERLIN continuum experiment at 18cm, recorded at 128Mb/s (dual polarisation, two bit sampling, 2 IFs per polarisation). Participating stations were Jb (Lovell), Wb (tied-array - 13 ants!), Eb, On, Mc, Tr, Sh, Ur, Cm, Nt, Hh - all stations produced fringes. Most data for Ur IF2, LCP are flagged due to bad sampler statistics (same problem was also noted for the corresponding BBC in other experiments from the same session).
The EVN reliability indicator was ERI=0.89 (Jb=1.0, Wb=1.0, Eb=0.97, On=1.0, Mc=0.96, Tr=0.92, Sh=1.0, Ur=0.8, Cm=0.8, Nt=1.0, Hh=0.97) 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 excludes data lost due to e.g. bad weather (0.89).
Plots of the autocorrelations.
Comments.
Ur: Missing most LCP data from IF2 (see general comments above).
Plots of the uncalibrated amplitude and phase against time.
Comments.
Sh: Ends early as sources set.
Plots of the uncalibrated amplitude and phase against frequency
channel.
Comments.
None.
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel.
Comments.
None.
TSYS against time.
Comments.
Cm: none available - nominal sensitivity assumed.
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.
Most telescopes have expected sensitivity as tabulated in EVN status table
Recall that Cm is forced to have nominal sensitivity.
Fringe-fit phase solutions.
Comments.
Nice phase connection generally seen.
Fringe-fit delay solutions.
Comments.
All solutions are less than few tens of nanoseconds.
Fringe-fit rate solutions.
Comments.
All solutions are within a few mHz of zero.
Telescope bandpasses.
Comments.
None.
Calibrated amplitude and phase against time
(a priori amplitude calibration and fringe-fit solutions applied).
Comments.
None.
Calibrated amplitude and phase against frequency channel.
Comments.
None.
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
None.
Naturally weighted dirty map produced before self-cal of:
OQ208.
J1118+1234.
3C286.
Comments.
None.
Uniformly weighted dirty map produced before self-cal of:
OQ208.
J1118+1234.
3C286.
Comments.
None.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Also available as a text file.
Comments.
None.
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.
None.
Residual closure phase (visibility closure phase with model closure phase subtracted) for:
OQ208.
J1118+1234.
3C286.
Comments.
None.
Calibrated visibilities and the source model of:
OQ208.
J1118+1234.
3C286.
Comments.
None.
Calibrated visibilities against u,v distance for:
OQ208. postscript , png (smaller)
J1118+1234. postscript , png (smaller)
3C286. postscript , png (smaller)
Comments.
None.
u,v coverage for:
OQ208
postscript, png (smaller)
J1118+1234
postscript, png (smaller)
3C286
postscript, png (smaller)
Comments.
None.
Crude map of OQ208 from the pipeline.
Crude map of J1118+1234 from the pipeline.
Crude map of 3C286 from the pipeline.
Comments.
None.