EVN User Experiment Pipeline Feedback

Last updated: Thu Oct 21 10:41:00 CEST 2004 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
UHF spectral line experiment recorded at 64 Mbps (2*4MHz IFs, two polarizations, two bit sampling). The array consisted of Onsala, Westerbork, Effelsberg, Noto, Torun and Urumqi. The observing frequency was ~995 MHz. Recorded on disks, except in Torun and Urumqi.

Urumqi produced no fringes in the UHF session. Torun recorded two linear polarizations, Noto a single linear polarization. The others recorded circular polarization. Severe RFI was reported from the stations.

The fringe finders were 3C345 and 4C39.25. J1339+6328 was a phase calibrator nearby the target. The data could not be imaged with the pipeline. The RFI situation was very bad in this experiment. The only known technical problems were the no fringes for Urumqi, and some data loss for Noto in the correlator. Torun no fringes is probably due to the very strong RFI.

The estimated ERI (ratio of the number of good visibilities to the expected number of visibilities) is 0.35. Ignoring the Tr losses due to RFI, we get ERI*= 0.63. The individual stations contribute to these losses as the following (1 meaning perfect data all the time): Ef - 1.00, Ur - 0.00, Wb - 1.00, On - 1.00, Tr - 0.00, Nt - 0.48/0.50 (a single receiver)

Plots of the autocorrelations .
Comments.
RFI situation is very bad.

Plots of the uncalibrated amplitude and phase against time .
Comments.
Only the calibrator data are shown

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
RFI is clearly present in cross-hands data
Wb: IF1 has strong band-edge cutoffs (see station feedback on the tied arrray)

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

TSYS against time .
Comments.
The Tsys measurements may be corrupted due to the RFI situation in this band.

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.
Tr seems to be more sensitive than expected (SEFD=2000 Jy, see the EVN Status Table). There was a new receiver installed before the EVN session.
Nt: also had a new receiver with previously unknown gain

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:
J1339+6328: postscript , or FITS .
3C345: postscript , or FITS .
Comments.

Uniformly weighted dirty map produced before self-cal of:
J1339+6328: postscript , or FITS .
3C345: postscript , or FITS .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1339+6328.
3C345.
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1339+6328: postscript , or text file .
3C345: 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.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
J1339+6328 .
3C345 .
Comments.

Calibrated visibilities and the source model of:
J1339+6328 .
3C345 .
Comments.

Calibrated visibilities against u,v distance for:
J1339+6328. postscript , or png (smaller)
3C345. postscript , or png (smaller)
Comments.

u,v coverage for:
J1339+6328. postscript , or png (smaller)
3C345. postscript , or png (smaller)
Comments.

J1339+6328: postscript , or FITS .
3C345: postscript , or FITS .
Comments.