AIPS HELP file for SDTUV in 31DEC18
As of Wed Sep 19 17:12:31 2018
SDTUV: Task to convert SD table files to UV like data.
INNAME Input SD table file name.
INCLASS Input SD table file class
INSEQ -1.0 9999.0 Input SD table file seq. #
INDISK 0.0 9.0 Input SD table file disk #.
INEXT Input table extension type
INVERS Input table file version no.
OUTNAME Output UV file name (name)
OUTCLASS Output UV file name (class)
OUTSEQ -1.0 9999.0 Output UV file name (seq. #)
OUTDISK 0.0 9.0 Output UV file disk unit #.
APARM Control info:
1 = CS table interval 0=none
2 .ge. 0 => SCAN rand. parm.
3 .gt. 0 => spline fitting
4 Spline smoothness parm.
5 .gt. 0 => median win. width
7 Max. dev. per receiver
8 Max. no. rcx. exceeding (7)
BPARM Task enrichment parm.
1 .gt. 0 => replace bad RA's
2 .gt. 0 => beam for lat. foc
3 .gt. 0 => patch 140 ft dec.
ARRAY2 Baseline table (20,2)
(i,1) = declination i
(i,2) = baseline i
Task: This task will create an AIPS uv data file and fill it by
converting a single dish table to uvlike data. If
requested, CS (calibration) and NX (index) tables will
be created and filled.
Several filtering methods are available for removing
a baseline from the data.
INNAME.....Input SD table file name (name).
INCLASS....Input SD table file name (class).
INSEQ......Input SD table file name (seq. #).
INDISK.....Disk drive # of input table file.
INEXT......Table extension type. ' '=>'SD'
INVER......Table extension version. 0=> convert all.
OUTNAME....Output UV file name (name). Standard behavior
with default 'UV DATA FILE'.
OUTCLASS...Output UV file name (class). Standard defaults.
OUTSEQ.....Output UV file name (seq. #). 0 => highest unique.
OUTDISK....Disk drive # of output UV file. 0 => highest disk
with space for the file.
1 = CS table interval in min. If < 0 then no CS
or NX tables are written.
2 If the value is .ge. 0 then SCAN and SAMPLE
random parameters are added if appropriate.
3 If the value is greater than 0 then a cubic
spline is fitted to the median value in blocks
APARM(3) samples long. The spline is then used
to subtract the baseline.
4 Smoothness factor, any positive number. Larger
values give better fit, smaller a smoother
curve. 0 => 1.
5 If the value is larger than 0 then the median
value in a sliding window APARM(5) samples wide
is used as an estimate of the baseline and
7,8 If the value of (7) is larger than 0 then an
interference detector is invoked. For each time
sample and receiver the difference between the
value and the mean of the preceeding and
following time samples is computed. If more than
APARM(8) receivers have a difference exceeding
APARM(7) then that time sample is flagged.
BPARM......If BPARM(1) .gt. 0 then the 300 foot bad RA problem
will be patched up.
If BPARM(2) .gt. 0 then a gain correction will be
made for the lateral (off axis) defocusing error.
BPARM(2) is the beam offset (degrees) that gives
3 dB loss in gain (field of view).
If BPARM(3) .gt. 0 then the declination error in
the 140 ft telescope pointing program will be
ARRAY2.....This contains a table of baselines to subtract
as a function of declination. This is mostly
useful for Meridian transit measurments. Baseline
temperatures to be removed can be specified at up
to 20 arbitrary declinations. The range of
declinations in the table MUST enclose all
declinations present in the data and at least 3
points must be included. The order is in
ascending (north positive) declination.
A cubic spline interpolation is used.
ARRAY2(i,1) = declination i
ARRAY2(i,2) = baseline temperature i.