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.