EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment EG029. If you have any comments on this experiment please email the address below.
A detailed description of the pipeline output is available.

Last updated: Mon Apr 11 16:30:04 CEST 2005 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
5cm experiment observed on 4/5 November 2004 (session 3/2004), recorded at 32 Mbit/s. There was one channel x 2 polarizations, correlated with 1024 spectral points. Eight stations were in the experiment. Jodrell Bank MkII telescope was replaced by Darnhall in the UK. Westerbork used a single dish only.

Due to a temporary correlator problem, some data were corrupted in R1 on baselines 3-8 (Ef-Wb) and 4-8 (On-Wb). These have been flagged - for final calibration please use the flag file from this pipeline ("AIPS calibration tables" link: FG.1 in eg029.tasav.FITS).

The EVN Reliability Indicator (the ratio of the expected to the observed number of good visibilities) is estimated as ERI=0.98 (Cm=0.99, Ef=1.0, W1=0.94, Da=.098, On=1.0, Mc=1.0, Nt=1.0 Tr=1.0). These were all technical problems.

Plots of the autocorrelations .
Comments.
Cm: RFI in R1
Ef: some RFI, both polarizations
On: weak RFI in both polarizations
Tr: strong, permanent RFI in L1

Plots of the uncalibrated amplitude and phase against time .
Comments.
Ef-Wb baseline shows flagged data due to correlator problem in R1. On-Wb baseline was also affected.

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.

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

TSYS against time .
Comments.
No Tsys for Cm and Da - nominal gains used.

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.
Ef, Mc and Tr seems to be more sensitive than expected; On seem to be somewhat less sensitive. See the EVN Status Table.

Fringe-fit phase solutions (including Parallactic Angle correction).
Comments.

Fringe-fit delay solutions .
Comments.

Fringe-fit rate solutions .
Comments.
Residual rates are high for Noto.

Telescope bandpasses .
Comments.

Calibrated amplitude and phase against time (a priori amplitude calibration and fringe-fit solutions applied).
Comments.

Calibrated amplitude and phase against frequency channel .
Comments.

Naturally weighted dirty map produced before self-cal of:
DA193: postscript , or FITS .
J0518+3306: postscript , or FITS .
Comments.

Uniformly weighted dirty map produced before self-cal of:
DA193: postscript , or FITS .
J0518+3306: postscript , or FITS .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
DA193.
J0518+3306.
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
DA193: postscript , or text file .
J0518+3306: postscript , or text file .
Comments.

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.
After selfcal Tr sensitivity is fixed to the expected value. Ef and Mc are still a bit more sensitive than expected. See the EVN Status Table.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
DA193 .
J0518+3306 .
Comments.

Calibrated visibilities and the source model of:
DA193 .
J0518+3306 .
Comments.

Calibrated visibilities against u,v distance for:
DA193. postscript , or png (smaller)
J0518+3306. postscript , or png (smaller)
Comments.

u,v coverage for:
DA193. postscript , or png (smaller)
J0518+3306. postscript , or png (smaller)
Comments.

DA193: postscript , or FITS .
J0518+3306: postscript , or FITS .
Comments.