EVN User Experiment Pipeline Feedback
Last updated: Tue Sep 8 14:17:02 CEST 2009
yang@jive.nl
General Comments.
(
Brief data summary
and
scan listing
)
S/X band network monitoring experiment, observed on 17 Jun 2009. Data rate was 256 Mbps (8 X 8 MHz subbands, RCP polarization, 2 bit sampling at the EVN stations, 1bit sampling at Kunming). The source 4C 39.25, 1156+295, and OQ208 were observed. The data were correlated in two passes. One is for S band data. The other is for X band data. Here, it is X-band pypeline result.
8 stations participated. It is the first time for the Kunming 40m radio telescope to participate the EVN experiment. The first fringes to the Kunming telescope were successfully detected at S band. Due to problems of 20 kHz LO offset and sideband swap (U->L) at X band, no fringes to the Kunming telescopes were found in the clock search. Yebes did not participate the obserations due to failure of the H-maser. Noto had an unlocked BBC.
The EVN reliability indicator (ERI) for this experiment was
ERI = 0.75 . ERI* = 0.75 .
(Ef=1, Mc=1, On=1, Ur=1, KM =1, Nt=0.88, Wb=1, Sh=1, Ys=0)
Plots of the autocorrelations
Comments.
No RFI found at X band
plots of the uncalibrated amplitude and phase
against time
Comments.
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.
SOINT = 0.5 minute. Ef: reference antenna. Wb: delay jump because the lightpath swap in IF1, 2, 4.
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.
Naturally weighted dirty map (not useful for bright sources)
produced before self-cal of:
1156+295: pdf (not available)
, or
FITS (not available)
.
4C39.25: pdf (not available)
, or
FITS (not available)
.
OQ208: pdf (not available)
, or
FITS (not available)
.
Comments.
Uniformly weighted dirty map (not useful for bright sources)
produced before self-cal of:
1156+295: pdf (not available)
, or
FITS (not available)
.
4C39.25: pdf (not available)
, or
FITS (not available)
.
OQ208: pdf (not available)
, or
FITS (not available)
.
Comments.
Phase corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
1156+295
.
4C39.25
.
OQ208
.
Comments.
Amplitude corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
1156+295:
pdf
, or
text file
, or
statistical summary
.
4C39.25:
pdf
, or
text file
, or
statistical summary
.
OQ208:
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:
1156+295
.
4C39.25
.
OQ208
.
Comments.
Calibrated visibilities and the source model of:
1156+295
.
4C39.25
.
OQ208
.
Comments.
Calibrated visibilities against u,v distance for:
1156+295:
pdf
, or
png
.
4C39.25:
pdf
, or
png
.
OQ208:
pdf
, or
png
.
Comments.
u,v coverage for:
1156+295:
pdf
, or
png
.
4C39.25:
pdf
, or
png
.
OQ208:
pdf
, or
png
.
Comments.
Crude maps of sources:
1156+295:
pdf
, or
FITS
.
4C39.25:
pdf
, or
FITS
.
OQ208:
pdf
, or
FITS
.
Comments.