EVN User Experiment Pipeline Feedback
Last updated: Fri Feb 11 17:46:02 CET 2005
zparagi@jive.nl
General Comments.
(
Brief data summary
and
scan listing
)
K-band experiment observed on 3 November 2004 (session 3/2004), recorded at 256 Mbps. There were four 8 MHz channels in both polarizations. The calibrator sources in this experiment were 0212+735 and GT0032+61 - the latter was too weak to fringe-fit. This is the line correlation (pass 2, first channel with 2048 lags, no crosshands) pipeline. The continuum data have been pipelined as well.
There were seven stations in this experiment: Mc, Ef, On, Mh, Cm, Nt and Ro70. The MkII telescope in Jodrell Bank was not available due to engineering work. From 17:06 to 19:06 UT Noto stopped observing because of high winds. There was not enough time left in the schedule for Robledo to change tape. Onsala had a new receiver, LCP only.
The EVN Reliability Indicator (for the continuum data, including all channels) is estimated as ERI=0.87 (Mc=1.0, Ef=1.0, On=0.5/0.5 (LCP only), Mh=1.0, Cm=0.25/0.5 (1st channel practically lost), Nt=0.9 (due to high winds), Ro=0.99). ERI*=0.91, this includes only technical problems at the telescopes.
Plots of the autocorrelations
.
Comments.
Some RFI seen at the stations, probably internal.
Plots of the uncalibrated amplitude and phase against time
.
Comments.
2 hours of data missing at Nt because of bad weather, see above.
Plots of the uncalibrated amplitude and phase against frequency
channel
.
Comments.
Apperent no detection at Noto is simply due to high rates - good data were obtained at the station.
Cm: because of an inaccurate LO setup, the lower half of L1/R1 is cut off.
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.
The big dishes, Ef and Ro seem to be less sensitive than expected - because of the strong line source? See the EVN Status Table.
Noto R1 seems to be less sensitive than expected.
Fringe-fit phase solutions
(including Parallactic Angle correction).
Comments.
Fringe-fit delay solutions
.
Comments.
Nt: large residual delays because of a clock problem, see below.
Fringe-fit rate solutions
.
Comments.
Nt: high residual rates - H-maser was settling down after a reset.
Telescope bandpasses
.
Comments.
Calibrated amplitude and phase against time
(a priori amplitude calibration and fringe-fit solutions applied).
Comments.
Data only of 0212+735.
Calibrated amplitude and phase against frequency channel
.
Comments.
Data only of 0212+735.
Naturally weighted dirty map produced before self-cal of:
0212+735:
postscript
, or
FITS
.
Comments.
Uniformly weighted dirty map produced before self-cal of:
0212+735:
postscript
, or
FITS
.
Comments.
Phase corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
0212+735.
Comments.
Amplitude corrections applied to a priori calibrated and fringe-fitted data by self-calibration.
0212+735:
postscript
, or
text file
.
Comments.
Nt R1 has large corrections, factors of 2-5 in Tsys.
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.
After self-calibration it seems that indeed the Nt R1 channel was very insensitive - see notes above.
Residual closure phase (visibility closure phase with model closure phase subtracted) for:
0212+735
.
Comments.
Calibrated visibilities and the source model of:
0212+735
.
Comments.
Calibrated visibilities against u,v distance for:
0212+735.
postscript
, or
png (smaller)
Comments.
u,v coverage for:
0212+735.
postscript
, or
png (smaller)
Comments.
0212+735:
postscript
, or
FITS
.
Comments.