EVN User Experiment Pipeline Feedback
Pipeline feedback for experiment EL031B.
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address below.
Last updated: Thu Dec 4 13:59:12 CET 2003
reynolds@jive.nl
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General Comments.
(
Brief data summary and
scan listing.)
This is an EVN K band observation to phase reference between the bright water maser in U Her and two astrometric refernce sources. The observations employes 2x2 8MHz basebands with the water maser in the first. Scheduled telescopes were Mc, On, Ef, Nt, Cm, Jb, Mh. Mc did not produce fringes. Various telescopes had very strong spikes in their autocorrelations. Note that On RR is really also LL! Because this is reverse phase referencing on a line source, there are hardly any selfcal solutions. So very few maps and sensitivity plots make sense.
The ERI comes out at Ef(1/1),On(0.5/0.5),Jb(1/1),Mc(0/1),Nt(0.8/1), Cm(0.5/1),Mh(0.8/1) yielding 0.46. Nothing of this was weather or RFI related (ie I believe the RFI to be local). The most serious limitation of this experiment is not reflected in this; the Ef slew rate limiting the on source time in K band phase referencing.
Plots of the autocorrelations.
Comments.
Strong spike can be seen at Cm. Also Nt has a spike and something present at On. The Jb bandpass is wobbly, possible sidelobes of another problem.
Plots of the uncalibrated amplitude and phase against time.
Comments.
Cm band 2 saturated, MH and Nt playback problems in RR.
Plots of the uncalibrated amplitude and phase against frequency
channel.
Comments.
Cm 2nd IF data not often usable, always a spike. Nt and Mh often miss RR data (due to playback).
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel.
Comments.
NA
TSYS against time.
Comments.
No values for Cm
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.
Flat for Cm
Fringe-fit phase solutions.
Comments.
I guess this is normal.
Fringe-fit delay solutions.
Comments.
OK, but not too much SNR.
Fringe-fit rate solutions.
Comments.
see delay
Telescope bandpasses.
Comments.
First band mostly OK, but noisy this way.
Calibrated amplitude and phase against time
(a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Not very useful for this experiment.
Calibrated amplitude and phase against frequency channel.
Comments.
Not very useful for this experiment.
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Comments.
Not very useful for this experiment.
Naturally weighted dirty map produced before self-cal of:
1611+343.
Comments.
Not very useful for this experiment.
Uniformly weighted dirty map produced before self-cal of:
1611+343.
Comments.
Not very useful for this experiment.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
Also available as a text file.
Comments.
Not very useful for this experiment.
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.
Not very useful for this experiment.
Residual closure phase (visibility closure phase with model closure phase subtracted) for:
1611+343.
Comments.
NA
Calibrated visibilities and the source model of:
1611+343.
Comments.
Calibrated visibilities against u,v distance for:
1611+343. postscript , png (smaller)
Comments.
Not very useful for this experiment.
u,v coverage for:
1611+343
postscript, png (smaller)
Comments.
Not very useful for this experiment.
Crude map of 1611+343 from the pipeline.
Comments.
Not very useful for this experiment.