EVN User Experiment Pipeline Feedback
Pipeline feedback for experiment EM049.
If you have any comments on this experiment please email
the
address below.
A detailed
description of the pipeline output is available.
Last updated: Thu Mar 4 19:33:05 CET 2004
bignall@jive.nl
|
General Comments.
(
Brief data summary
and
scan listing
)
This is an EVN spectral line experiment at 5cm observed on 9 June 2003. The data were correlated with 1024 spectral channels, dual polarization, no cross-pols. 6 stations participated: Jb, Cm, Ef, On, Mc, Tr. Mc did not produce any fringes at 5cm in this session, and Tr failed for this experiment due to loss of the maser lock.
The EVN Reliability Indicator (ERI) for this experiment was ERI=0.28 (Jb=Cm=Ef=1, On=0.46, Mc=Tr=0). ERI*=0.4 (Jb=Cm=Ef=On=1, Mc=Tr=0). ERI gives you an estimate of the ratio of observed/good visibilities to the expected number of visibilities. ERI* is the same but excludes data lost due to e.g. bad weather. In this case On was unable to observe for just over half of the experiment due to high wind.
Plots of the autocorrelations
.
Comments.
RFI is a problem, especially at Cm and to a lesser degree at On.
Plots of the uncalibrated amplitude and phase against time
.
Comments.
Plots of the uncalibrated amplitude and phase against frequency
channel
.
Comments.
Some RFI is also evident in cross-correlations.
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel
(not available)
.
Comments.
TSYS against time
.
Comments.
No Tsys for Cm.
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.
Cm: assumed SEFD=500 Jy, which has large uncertainty.
Other antennas have expected sensitivity as tabulated on the EVN status sheet.
Fringe-fit phase solutions
(including Parallactic Angle correction).
Comments.
Fast phase wraps for Cm.
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.
Flagging of more channels in the high end of the band is advisable.
Naturally weighted dirty map produced before self-cal of:
J1955+5131
.
J1924+1540
.
J1642+3948
.
Comments.
Uniformly weighted dirty map produced before self-cal of:
J1955+5131
.
J1924+1540
.
J1642+3948
.
Comments.
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1955+5131.
J1924+1540.
J1642+3948.
Comments.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
J1955+5131:
postscript
, or
text file
.
J1924+1540:
postscript
, or
text file
.
J1642+3948:
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:
J1955+5131
.
J1924+1540
.
J1642+3948
.
Comments.
Calibrated visibilities and the source model of:
J1955+5131
.
J1924+1540
.
J1642+3948
.
Comments.
Calibrated visibilities against u,v distance for:
J1955+5131.
postscript
, or
png (smaller)
J1924+1540.
postscript
, or
png (smaller)
J1642+3948.
postscript
, or
png (smaller)
Comments.
u,v coverage for:
J1955+5131.
postscript
, or
png (smaller)
J1924+1540.
postscript
, or
png (smaller)
J1642+3948.
postscript
, or
png (smaller)
Comments.
Crude map of J1955+5131 from the pipeline
.
Crude map of J1924+1540 from the pipeline
.
Crude map of J1642+3948 from the pipeline
.
Comments.
All 3 sources are clearly detected