EVN User Experiment Pipeline Feedback
Last updated: Mon Feb 27 12:19:54 CET 2006
reynolds@jive.nl
General Comments.
(
Brief data summary
and
scan listing
)
L band spectral line experiment, observed on 5 Nov 2005. Data rate was 32 Mbps (2 X 0.5 MHz subbands, dual polarization, two-bit sampling, 4 times oversampling). The experiment was originally scheduled as a phase-referencing experiment, but initial tests indicated that the phase-reference target separation was too large, and so the pipeline does not attempt to do phase referencing.
Two spectral lines were observed and were correlated and pipelined in separate passes. This is the pipeline page for subband 1.
8 stations were scheduled. Cambridge did not participate because of failed power supply in the VLBI rack. Onsala was stowed for a large part of the experiment due to winds.
The EVN reliability indicator (ERI) for this experiment was
ERI = 0.66 . ERI* = 0.75 .
(JB=1, Wb=1, Ef=1, Mc=1, Ur=1, On=0.58 [On*=1], Tr=1, Cm=0)
Plots of the autocorrelations
Comments.
Jb: some RFI.
Mc: strong RFI in RCP
Tr: some RFI. On: LCP bandpass is very 'spiky' - RFI?
plots of the uncalibrated amplitude and phase
against time
Comments.
Plots of the uncalibrated amplitude and phase
against frequency channel
Comments.
RFI noted in autocorrelations is not visible any of the cross-correlations.
The uncalibrated amplitude and phase of the crosshand
correlations against frequency channel
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.
Fring fitting appears reasonable, even for the spectral line source. However, this should probably be repeated with a narrower channel selection.
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:
3C345: pdf (not available)
, or
FITS (not available)
.
W75N: pdf (not available)
, or
FITS (not available)
.
OQ208: pdf (not available)
, or
FITS (not available)
.
J2052+3635: pdf (not available)
, or
FITS (not available)
.
Comments.
Uniformly weighted dirty map (not useful for bright sources)
produced before self-cal of:
3C345: pdf (not available)
, or
FITS (not available)
.
W75N: pdf (not available)
, or
FITS (not available)
.
OQ208: pdf (not available)
, or
FITS (not available)
.
J2052+3635: pdf (not available)
, or
FITS (not available)
.
Comments.
Phase corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
3C345
.
W75N
.
OQ208
.
J2052+3635
.
Comments.
Amplitude corrections applied to a priori calibrated and
fringe-fitted data by self-calibration.
3C345:
pdf
, or
text file
, or
statistical summary
.
W75N:
pdf
, or
text file
, or
statistical summary
.
OQ208:
pdf
, or
text file
, or
statistical summary
.
J2052+3635:
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:
3C345
.
W75N
.
OQ208
.
J2052+3635
.
Comments.
Calibrated visibilities and the source model of:
3C345
.
W75N
.
OQ208
.
J2052+3635
.
Comments.
Calibrated visibilities against u,v distance for:
3C345:
pdf
, or
png
.
W75N:
pdf
, or
png
.
OQ208:
pdf
, or
png
.
J2052+3635:
pdf
, or
png
.
Comments.
u,v coverage for:
3C345:
pdf
, or
png
.
W75N:
pdf
, or
png
.
OQ208:
pdf
, or
png
.
J2052+3635:
pdf
, or
png
.
Comments.
Crude maps of sources:
3C345:
pdf
, or
FITS
.
W75N:
pdf
, or
FITS
.
OQ208:
pdf
, or
FITS
.
J2052+3635:
pdf
, or
FITS
.
Comments.