EVN User Experiment Pipeline Feedback


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

Last updated: Fri Dec 3 15:45:56 CET 2004 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
Multi-wavelength SS433 monitoring campaign, second epoch EVN 6cm experiment. Recorded on disk-only at 256 Mbps using 8 channels and 2-bit sampling, which resulted in 4x8 MHz channels in each polarizations.

This was the first astronomical experiment with the new, cooled 6cm receiver in Urumqi. Produced good data, altogether with Ef, Wb, Sh and Tr. There were no fringes to Noto.

Besides the target source, SS433, two calibrators were observed: 3C454.3 and J1832+1357. Pipeline imaging was not successful for these sources given the sparse data available.

The ratio of the expected to the observed number of good visibilities is estimated as ERI=ERI*=0.64 (Ef=1.0, Wb=1.0, Sh=0.5/0.5 (had LCP only), Nt=0.0, Tr=1.0, Ur=1.0).

Plots of the autocorrelations .
Comments.

Tr: RFI(?) in channels L4/R4

Plots of the uncalibrated amplitude and phase against time .
Comments.
Nt: no fringes

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
Nt: no fringes
Tr: L4/R4 show RFI leaking through

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

TSYS against time .
Comments.
Tr Tsys high in R3-R4.

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 gaincurve seemed to be corrupt and so it was made flat (applied gains from N04C2). (For nominal SEFDs, see the EVN Status Table).

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.
The apparent loss of Sh and Ur data is due to the weakness of the target source on these long baselines.

Calibrated amplitude and phase against frequency channel .
Comments.
The apparent loss of Sh and Ur data is due to the weakness of the target source on these long baselines.

Naturally weighted dirty map produced before self-cal of:
3C454.3: postscript , or FITS .
J1832+1357: postscript , or FITS .
Comments.

Uniformly weighted dirty map produced before self-cal of:
3C454.3: postscript , or FITS .
J1832+1357: postscript , or FITS .
Comments.

Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C454.3.
J1832+1357.
Comments.

Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
3C454.3: postscript , or text file .
J1832+1357: postscript , or text file .
Comments.
Corrections are in general small.

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.
Compare the data with the nominal SEFDs listed in the EVN Status Table.

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
3C454.3 .
J1832+1357 .
Comments.

Calibrated visibilities and the source model of:
3C454.3 .
J1832+1357 .
Comments.

Calibrated visibilities against u,v distance for:
3C454.3. postscript , or png (smaller)
J1832+1357. postscript , or png (smaller)
Comments.

u,v coverage for:
3C454.3. postscript , or png (smaller)
J1832+1357. postscript , or png (smaller)
Comments.

3C454.3: postscript , or FITS .
J1832+1357: postscript , or FITS .
Comments.
Not enough data to make a useful image with the pipeline.