EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment N04U1. 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 Jul 14 15:10:32 CEST 2004 reynolds@jive.nl

General Comments. ( Brief data summary and scan listing )
Network monitoring experiment N04U1. This is a UHF experiment observed on 13 July 2004. There are 2 subbands of 4MHz bandwidth, with 4 polarizations and 64 channels per subband/polarization. 4 stations successfully participated - Ef, Wb, On, Nt. On did not produce fringes in IF L2. Nt joined the experiment late due to a problem with the Mk5 recorder and recorded LCP only (receiver limitation). Ur did not produce any fringes and the Tr tape was unreadable.
The EVN Reliability Indicator (ERI) for this experiment was ERI=ERI*=0.32 (Ef=1.0, Wb=1.0, On=0.75, Ur=0, Nt=0.7, Tr=0).

Plots of the autocorrelations .
Comments.
Strong interference at Onsala and Noto.

Plots of the uncalibrated amplitude and phase against time .
Comments.
Ur: no fringes.
On: no fringes in IF L2 (corresponds to VC03).
Nt: weak fringes in RCP are in fact crosshand fringes. Nt uses an LCP-only receiver. The 'RCP' data is flagged during amplitude calibration.

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
On, Nt: RFI also shows up in the cross-correlations.

The uncalibrated amplitude and phase of the crosshand correlations against frequency channel .
Comments.

TSYS against time .
Comments.
Ef, Wb, Nt: no calibration information available - approximations 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.

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

Fringe-fit delay solutions .
Comments.

Fringe-fit rate solutions .
Comments.

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 .
Comments.
Dirty map not useful for this bright source

Uniformly weighted dirty map produced before self-cal of:
DA193: postscript , or FITS .
Comments.
Dirty map not useful for this bright source

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

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
DA193: postscript , or text file .
Comments.
Only IF L1 had sufficient data for amplitude self-calibration.

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.
Only IF L1 had sufficient data for full sensitivity calculation.

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

Calibrated visibilities and the source model of:
DA193 .
Comments.

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

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

DA193: postscript , or FITS .
Comments.