EVN User Experiment Pipeline Feedback

Last updated: Tue Jun 1 17:44:42 CEST 2004 reynolds@jive.nl

General Comments. ( Brief data summary and scan listing )
This is an EVN continuum experiment at C band, observed on 31 Oct 2003. There are 4 subbands and 4 polarizations with 16 channels per subband. 8 stations successfully participated - Ef, Wb, On, Mc, Nt, Ur, Sh, Hh. In addition, Jb and Tr were scheduled but Tr did not participate due to a tape recorder problem and Jb produced no fringes due to an LO offset.

The EVN Reliability Indicator (ERI) for this experiment was ERI=ERI*=0.55 (Ef=0.99, Wb=0.9, Jb=0, On=1, Mc=1, Nt=1, Tr=0, Ur=0.9, Sh=0.9, Hh=1), where Ur and Sh are only expected to produce data in the LCP channels.

Plots of the autocorrelations .
Comments.

Plots of the uncalibrated amplitude and phase against time .
Comments.
Wb has no detection on a couple of scans at between approx 9:00 and 10:00 due to a failure of the local data acquistion system.

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
Nt: IFs R4 and L1 have low amplitude.

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

TSYS against time .
Comments.
Ur: used non-cooled receiver, so Tsys is very high.

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.
Ur: used non-cooled receiver, so sensitivity is low.
Sensitivities seem reasonable for other stations.

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

Fringe-fit delay solutions .
Comments.

Fringe-fit rate solutions .
Comments.

Telescope bandpasses .
Comments.
Bandpass shapes are good.

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

Calibrated amplitude and phase against frequency channel .
Comments.
Nt: IFs R4 and L1 still have low amplitude after calibration. Should be adjusted.

Naturally weighted dirty map produced before self-cal of:
J1310+3220 .
J1407+2827 .
J2136+0041 .
Comments.
Dirty maps not useful for these bright sources.

Uniformly weighted dirty map produced before self-cal of:
J1310+3220 .
J1407+2827 .
J2136+0041 .
Comments.
Dirty maps not useful for these bright sources.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1310+3220.
J1407+2827.
J2136+0041.
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1310+3220: postscript , or text file .
J1407+2827: postscript , or text file .
J2136+0041: postscript , or text file .
Comments.
Amplitude corrections for On are relatively large.

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.
Ur: very low sensitivity, as expected.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
J1310+3220 .
J1407+2827 .
J2136+0041 .
Comments.

Calibrated visibilities and the source model of:
J1310+3220 .
J1407+2827 .
J2136+0041 .
Comments.

Calibrated visibilities against u,v distance for:
J1310+3220. postscript , or png (smaller)
J1407+2827. postscript , or png (smaller)
J2136+0041. postscript , or png (smaller)
Comments.
The dip in amplitude on source 2136+0041 at approximately 80 MegaWavelengths, is probably due to real source structure (see the USNO image database for comparison). The overall amplitude calibration seems reasonable.

u,v coverage for:
J1310+3220. postscript , or png (smaller)
J1407+2827. postscript , or png (smaller)
J2136+0041. postscript , or png (smaller)
Comments.

Crude map of J1310+3220 from the pipeline .
Crude map of J1407+2827 from the pipeline .
Crude map of J2136+0041 from the pipeline .
Comments.