EVN User Experiment Pipeline Feedback


Pipeline feedback for experiment CHAKA. 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 15:25:43 CET 2004 zparagi@jive.nl

General Comments. ( Brief data summary and scan listing )
Multi-wavelength SS433 monitoring campaign, first 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, but L1-2 were dead. Ef, Wb, On and Tr were OK. There were no fringes to Noto.

Besides the target source, SS433, two calibrators were observed: 3C454.3 and J1832+1357. Pipeline maging 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*=0.57 (Ef=1.0, Wb=1.0, On=0.9, Nt=0.0, Tr=1.0, Ur=0.75).

Plots of the autocorrelations .
Comments.

Tr: RFI in channels L4/R4

Plots of the uncalibrated amplitude and phase against time .
Comments.
Nt: no fringes
Ur: L1-2 dead

Plots of the uncalibrated amplitude and phase against frequency channel .
Comments.
Nt: no fringes
Tr: L4/R4 show RFI leaking through
Ur: L1-2 dead

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

TSYS against time .
Comments.
Do not understand Tr Tsys data (see below).

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). There must be a problem with the Tsys as well, since the sensitivites are still not in full agreement with the nominal values (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.
A little On data lost.

Calibrated amplitude and phase against frequency channel .
Comments.

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. Tr has high corrections n L2 and R3 (up to a factor of 2 in Tsys). Ur has high correction in R3 as well.

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.
Tr sensitivity is as expected, after self-calibration. See the EVN Status Table).

Residual closure phase (visibility closure phase with model closure phase subtracted) for:
3C454.3 (not available) .
J1832+1357 .
Comments.

Calibrated visibilities and the source model of:
3C454.3 (not available) .
J1832+1357 .
Comments.

Calibrated visibilities against u,v distance for:
3C454.3. postscript (not available) , or png (smaller) (not available)
J1832+1357. postscript , or png (smaller)
Comments.

u,v coverage for:
3C454.3. postscript (not available) , or png (smaller) (not available)
J1832+1357. postscript , or png (smaller)
Comments.

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