EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment GS021B. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Wed Oct 6 13:22:06 CEST 2004 biggs@jive.nl

General Comments. ( Brief data summary and scan listing )
This is a Global VLBI imaging experiment at 18cm (dual polarisation, 2 IFs). Particpating EVN stations were Ef, Jb, Mc, Nt, Tr, Wb and On. The reference antenna for calibration and plotting was Ef. The EVN reliability indicator was ERI=0.96 (Ef=0.96, Jb=0.98, Mc=0.98, Nt=1.00, Tr=1.00, Wb=0.95, On=1.00). ERI gives you an estimate of the ratio of observed/good visibilities to the expected number. ERI* is the same, but excludes data lost due to circumstances out of the EVN's control e.g. bad weather (ERI*=0.96).

Plots of the autocorrelations .
Comments.
Jb: Strong RFI in IF2.

Plots of the uncalibrated amplitude and phase against time .
Comments.
Hn: Last data bad - source setting?

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
None.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel (not available) .
Comments.
n/a.

TSYS against time .
Comments.
Jb: Values definitely seem to be affected by RFI in IF2.
Mc: Some sign of RFI ook.

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 predicted sensitivity as given in the EVN Status Table).
Nt: Gain values start rather high, but decline to close to theoretical.
Tr: Values are about three times greater than theoretical, but consistent between IFs!

Fringe-fit phase solutions (including Parallactic Angle correction).
Comments.
Values are interpolated across entire experiment!
Ef: variation reflects parallactic angle.

Fringe-fit delay solutions .
Comments.
None.

Fringe-fit rate solutions .
Comments.
None.

Telescope bandpasses .
Comments.
None.

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Br: Missing data probably due to bad playback.

Calibrated amplitude and phase against frequency channel .
Comments.
None.

Naturally weighted dirty map produced before self-cal of:
4C39.25: postscript , or FITS .
J1740+5211: postscript , or FITS .
Comments.
None.

Uniformly weighted dirty map produced before self-cal of:
4C39.25: postscript , or FITS .
J1740+5211: postscript , or FITS .
Comments.
None.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
4C39.25.
J1740+5211.
Comments.
None.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
4C39.25: postscript , or text file .
J1740+5211: postscript , or text file .
Comments.
In general, the amplitude calibration seems to have been good.
Jb: Large corrections in IF2.
Tr: Large, but consistent, corrections.

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:
4C39.25 .
J1740+5211 .
Comments.
J1740+5211: Hn triangles show bad data.

Calibrated visibilities and the source model of:
4C39.25 .
J1740+5211 .
Comments.
None.

Calibrated visibilities against u,v distance for:
4C39.25. postscript , or png (smaller)
J1740+5211. postscript , or png (smaller)
Comments.
None.

u,v coverage for:
4C39.25. postscript , or png (smaller)
J1740+5211. postscript , or png (smaller)
Comments.
None.

4C39.25: postscript , or FITS .
J1740+5211: postscript , or FITS .
Comments.
Source is detected at the centre of each map. J0154+4743 in particular may have a second component.