EVN User Experiment Pipeline Feedback
Last updated: Tue Sep 8 17:01:19 CEST 2009
yang@jive.nl
General Comments.
(
Brief data summary
and
scan listing
)
L band phase-referencing experiment, observed on 3 Jun 2009. Data rate was 1 Gbps (8 X 16 MHz subbands, dual polarization, two-bit sampling). The target sources IRAS1929 was calibrated using the phase-reference sources J1941-0511. '3C286' were also observed as calibrators. '3C345' was the fringe finder.
11 stations participated. Urumqi did not have fringes due to failure of data recording. Cm and Kn shared the same diskpack. Due to a problem of bad disks, they lost some data (scan 13-15, 25-27, 29-33,58-63, 68-69, 77-81, 94-99, 106-128). The 14 MHz signal was fed into IF 3 and 4.
The EVN reliability indicator (ERI) for this experiment was
ERI = 0.68 . ERI* = 0.68 .
(Ef=1,Mc=1,Cm=0.6,On=1,Jb=1,Ur=0,Tr=1,Kn=0.6,Wb=1,Nt=1,Sh=1)
Plots of the autocorrelations
Comments.
plots of the uncalibrated amplitude and phase
against time
Comments.
EF: IF1 was flagged in scan 58 - 63 due to the low weight. UR: no fringes. MC: IF1 was flagged out due to the low amplitude and weight.
Plots of the uncalibrated amplitude and phase
against frequency channel
Comments.
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel
(not available)
Comments.
TSYS against time
Comments.
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.
Fringe-fit phase solutions
(including Parallactic
Angle correction).
Comments.
Fringe-fit delay solutions
Comments.
Fringe-fit rate solutions
Comments.
Telescope bandpasses
Comments.
Sh: weired bandpass shape in IF 7 and 8.
Calibrated amplitude and phase against time
(a
priori amplitude calibration and fringe-fit solutions applied).
Comments.
Calibrated amplitude and phase against frequency
channel
Comments.
Gibbs phenomenon on some sensitive baselines during the scans of bright sources. It was caused by the sharp edge of baseband.
Naturally weighted dirty map (not useful for bright sources)
produced before self-cal of:
IRAS1929:
pdf
, or
FITS
.
3C345: pdf (not available)
, or
FITS (not available)
.
J1941-0511: pdf (not available)
, or
FITS (not available)
.
3C286: pdf (not available)
, or
FITS (not available)
.
Comments.
Uniformly weighted dirty map (not useful for bright sources)
produced before self-cal of:
IRAS1929:
pdf
, or
FITS
.
3C345: pdf (not available)
, or
FITS (not available)
.
J1941-0511: pdf (not available)
, or
FITS (not available)
.
3C286: pdf (not available)
, or
FITS (not available)
.
Comments.
Phase corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
IRAS1929 (not available)
.
3C345
.
J1941-0511
.
3C286
.
Comments.
Amplitude corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
IRAS1929: pdf (not available)
, or
text file (not available)
, or
statistical summary (not available)
.
3C345:
pdf
, or
text file
, or
statistical summary
.
J1941-0511:
pdf
, or
text file
, or
statistical summary
.
3C286:
pdf
, or
text file
, or
statistical summary
.
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:
IRAS1929 (not available)
.
3C345
.
J1941-0511
.
3C286
.
Comments.
Calibrated visibilities and the source model of:
IRAS1929 (not available)
.
3C345
.
J1941-0511
.
3C286
.
Comments.
Calibrated visibilities against u,v distance for:
IRAS1929:
pdf
, or
png
.
3C345:
pdf
, or
png
.
J1941-0511:
pdf
, or
png
.
3C286:
pdf
, or
png
.
Comments.
u,v coverage for:
IRAS1929:
pdf
, or
png
.
3C345:
pdf
, or
png
.
J1941-0511:
pdf
, or
png
.
3C286:
pdf
, or
png
.
Comments.
Crude maps of sources:
IRAS1929:
pdf
, or
FITS
.
3C345:
pdf
, or
FITS
.
J1941-0511:
pdf
, or
FITS
.
3C286:
pdf
, or
FITS
.
Comments.