AIPS HELP file for OOFRING in 31DEC21
As of Fri Dec 4 3:31:18 2020
OOFRING: procedure to fringe fit data with spectral index opts
Input uv data.
INNAME UV file name (name)
INCLASS UV file name (class)
INSEQ 0.0 9999.0 UV file name (seq. #)
INDISK 0.0 9.0 UV file disk drive #
OUTNAME Name to use for OOSUB output
' ' -> INNAME
DOKEEP -1.0 1.0 > 0 -> keep divided uv data
Data selection (multisource):
BCHAN 0.0 2048.0 Lowest channel number 0=>all
ECHAN 0.0 2048.0 Highest channel number
ANTENNAS Antennas to select. 0=all
DOFIT Subset of ANTENNAS list
for which solns are desired.
UVRANGE Range of uv distance for full
WTUV Weight outside UVRANGE 0=0.
WEIGHTIT 0.0 3.0 Modify data weights function
CLEAN map (optional)
IN2NAME Cleaned map name (name)
IN2CLASS Cleaned map name (class)
IN2SEQ 0.0 9999.0 Cleaned map name (seq. #)
IN2DISK 0.0 9.0 Cleaned map disk unit #
INVERS -1.0 46655.0 CC file version #.
NCOMP # comps to use for model.
1 value per field
FLUX Lowest CC component used.
NMAPS 0.0 4096.0 No. Clean map files
ONEFREQ -1.0 1.0 > 0 => CC model from only
one frequency (group)
CMETHOD Modeling method:
CMODEL Model type: 'COMP','IMAG'
'SUBI' (see HELP re images)
SMODEL Source model, 1=flux,2=x,3=y
See HELP SMODEL for models.
Solution control adverbs:
REFANT Reference antenna
SEARCH 0.0 1000.0 Prioritized reference antenna
list - supplements REFANT
- but only if APARM(9)>0
SOLINT Solution interval (min)
0 => 10 min
SOLSUB Solution subinterval
SOLMIN Min solution interval
APARM General parameters
1=min. no. antennas
2 > 0 => data divided
3 > 0 => avg. RR,LL
4 > 0 => avg. freq. in IFs
5 = 1 => combine all IFs
= 2 => also MB delay
= 3 => combine IFs in
= 4 => combine IFs in
= N => combines IFs in
SEE HELP WARNING
6=print level, 1=some
7=SNR cutoff (0=>5)
8=max. ant. # (no AN)
9 > 0 => do exhaustive
10 > 0 -> fit dispersion
and IF group delay after
fit of SB delays
DPARM Delay-rate parameters
1=no. bl combo. (def=3)
2=delay win (nsec), if <0
no delay search done
3=rate win (mHz)
4=int. time (sec)
0 => min. found in data
5 >0 => don't do ls. soln
6 >0 => don't avg. in freq
7 >0 => don't rereference
8 > 0 => activate zero'ing
9 > 0 => do not fit rate
ANTWT Ant. weights (0=>1.0)
BIF First IF included when
APARM(5) > 0
EIF Last IF included when
APARM(5) > 0
BPARM Task enrichment parameters
(1) Antenna diameter (m)
0 -> no correction
(2) Omit CC options
(3) spectral index radius
0 -> no correction
FQTOL Frequency tolerance in kHz
(primary beam & spec index)
IN3NAME Spectral index image name
IN3CLASS Spectral index image class
IN3SEQ Spectral index image sequence
IN3DISK Spectral index image disk
IN4NAME Spectral curvature name
IN4CLASS Spectral curvature class
IN4SEQ Spectral curvature sequence
IN4DISK Spectral curvature disk
BADDISK 0.0 15.0 Disk no. not to use for
Task: This procedure allows frequency-dependent modeling options to
be applied to calibrator data prior to fringe fitting. The
task OOSUB divides the frequency-dependent model into the data
set making a temporary data set. Then FRING determines the
group delay and phase rate calibration to be applied to the uv
data. A solution (SN) table will be left for a multi-source
data set. SN tables will be attached to the INPUT data file
using TACOP to copy that extension file from the temporary data
set usd by FRING to the original input data set. The temporary
data set may be kept or deleted after the TACOP.
This procedure does not apply data selection and
calibration adverbs to the input data set. You must apply
these with SPLIT or SPLAT (or other tasks) to make a data set
consisting solely of the edited/calibrated data that you wish
to fringe fit.
Model images made with both values of IMAGR's DO3DIMAG
option are handled correctly, as are multi-scale images. Set
NMAPS = NFIELD * NGAUSS.
FRING now uses dynamic memory throughout, allowing large
delay-rate searches no matter what size the pseudo AP may be.
Of course, your computer must have enough memory to support
INNAME.....Input UV file name (name). Standard defaults.
INCLASS....Input UV file name (class). Standard defaults.
INSEQ......Input UV file name (seq. #). 0 -> highest.
INDISK.....Disk drive # of input UV file. 0 -> any.
OUTNAME....Name to use for OOSUB output with class 'OOFRI1'
Can be used to avoid conflict between multiple uses of
OOFRING. ' ' -> INNAME.
DOKEEP.....> 0 => keep the file produced by OOSUB containing the
input data divided by the model and the SN table
produced by FRING
<=0 => delete this temporary file after TACOP.
BCHAN......First channel to use. 0=>all.
ECHAN......Highest channel to use. 0=>all higher than BCHAN
ANTENNAS...A list of the antennas to have solutions determined. If
any number is negative then all antennas listed are NOT to
be used to determine solutions and all others are. All 0 =>
DOFIT......A list of the antennas for which solutions should or
should not be determined. If DOFIT = 0, all antennas are
solved for. If any entry <= -1, , then DOFIT is taken as
the list of antennas for which no solution is desired; a
solution is found for all antennas not in DOFIT. If any
entry of DOFIT is non-zero and all are >= 0, then only
those antennas listed in DOFIT will be solved for - all
other selected antennas will not be solved for.
NOTE: THIS OPTION MUST NOT BE USED UNLESS YOU UNDERSTAND
IT FULLY. Basically, it should be used to solve for the
gains of "poor" antennas after the "good" antennas have
been fully calibrated. Antennas included in ANTENNAS but
not in DOFIT are assumed to have a complex
gain/delay/rate of (1,0,0,0) and the gains/delays
produced will be very wrong if this is not the case.
See HELP DOFIT.
The following may be used for all data files (except as noted):
UVRANGE....The range of uv distance from the origin in kilowavelengths
over which the data will have full weight; outside of this
annulus in the uv plane the data will be down weighted by a
factor of WTUV.
WTUV.......The weighting factor for data outside of the uv range
defined by UVRANGE.
WEIGHTIT...If > 0, change the data weights by a function of the
weights just before doing the solution. Choices are:
0 - no change weighting by 1/sigma**2
1 - sqrt (wt) weighting by 1/sigma may be more stable
2 - (wt)**0.25
3 - change all weights to 1.0
The following specify a CLEAN model to be used if a single source was
specified in CALSOUR:
IN2NAME....Cleaned map name (name). Standard defaults.
Note: a CLEAN image for only a single-source may
be given although it may be in a multi-source file.
If the source table contains a flux, then that flux will
be used to scale the components model to obtain the
stated total flux. This is needed since initial Cleans
may not obtain the full flux even though they represent
all the essentials of the source structure.
IN2CLASS...Cleaned map name (class). Standard defaults.
IN2SEQ.....Cleaned map name (seq. #). 0 -> highest.
IN2DISK....Disk drive # of cleaned map. 0 => any.
INVERS.....CC file version #. 0=> highest numbered version
NCOMP......Number of Clean components to use for the model, one
value per field. If all values are zero, then all
components in all fields are used. If any value is not
zero, then abs(NCOMP(i)) (or fewer depending on FLUX and
negativity) components are used for field i, even if
NCOMP(i) is zero. If any of the NCOMP is less than 0,
then components are only used in each field i up to
abs(NCOMP(i)), FLUX, or the first negative whichever
comes first. If abs(NCOMP(i)) is greater than the number
of components in field i, the actual number is used. For
NCOMP = -1,0
says to use one component from field one unless it is
negative or < FLUX and no components from any other
field. This would usually not be desirable.
NCOMP = -1000000
says to use all components from each field up to the
first negative in that field.
NCOMP = -200 100 23 0 300 5
says to use no more than 200 components from field 1, 100
from field 2, 23 from field 3, 300 from field 5, 5 from
field 6 and none from any other field. Fewer are used if
a negative is encountered or the components go below
FLUX.......Only components > FLUX in absolute value are used in the
NMAPS......Number of image files to use for model. For multi-scale
models, set NMAPS = NFIELD * NGAUSS to include the Clean
components of the extended resolutions. If more than one
file is to be used, the NAME, CLASS, DISK and SEQ of the
subsequent image files will be the same as the first file
except that the LAST 3 or 4 characters of the CLASS will
be an increasing sequence above that in IN2CLASS. Thus,
if INCLASS='ICL005', classes 'ICL005' through 'ICLnnn'
or 'ICnnnn', where nnn = 5 + NMAPS - 1 will be used. Old
names (in which the 4'th character is not a number) are
also supported: the last two characters are '01' through
'E7' for fields 2 through 512. In old names, the highest
field number allowed is 512; in new names it is 4096.
ONEFREQ....In IMAGR, a CC file is made from the "average" of all
channels included in the bandwidth synthesis. But it is
also possible to make the model image(s) from a single
frequency (or from frequencies within FQTOL anyway).
Set ONEFREQ = 1 if the model was made this way, leave it
zero if all frequencies were included in the model.
CMETHOD....This determines the method used to compute the model
'DFT' uses the direct Fourier transform, this method is
the most accurate.
'GRID' does a gridded-FFT interpolation model computation
' ' allows the program to use the fastest method
CMODEL.....This indicates the type of input model; 'COMP' means that
the input model consists of Clean components, 'IMAG'
indicates that the input model consists of images.
'SUBI' means that the model consists of a sub-image of
the original IMAGR output. If CMODEL is ' ' Clean
components will be used if present and the image if not.
SUBI should work for sub-images made with DO3DIM true and
sib-images of the central facet made with DO3DIM false,
but probably will not work well for shifted facets with
DO3DIM false. Use BLANK rather than SUBIM in such cases.
CALIB will set a scaling factor to correct image units
from JY/BEAM to JY/PIXEL for image models. If the source
table contains a flux, then that flux will be used to
scale the components model to obtain the stated total
flux. This is needed since initial Cleans may not obtain
the full flux even though they represent all the
essentials of the source structure.
SMODEL.....A single component model to be used instead of a CLEAN
components model; if abs (SMODEL) > 0 then use of this
model is requested.
SMODEL(1) = flux density (Jy)
SMODEL(2) = X offset in sky (arcsec)
SMODEL(3) = Y offset in sky (arcsec)
SMODEL(4) = Model type:
0 => point model
1 => elliptical Gaussian and
SMODEL(5) = major axis size (arcsec)
SMODEL(6) = minor axis size (arcsec)
SMODEL(7) = P. A. of major axis (degrees)
2 => uniform sphere and
SMODEL(5) = radius (arcsec)
The following control how the solutions are done, if you don't
understand what a parameter means leave it 0 and you will probably get
what you want.
REFANT.....The desired reference antenna for phases.
SEARCH.....List of Prioritized antennas to be used when APARM(9)>0.
This adverb supplements REFANT. Along with APARM(9)>0,
it is recommended that SEARCH be filled
with a list of antennas whose order reflects the user's
notion of which baselines will be easiest to find fringes
on. All baselines to each antenna in SEARCH will be
searched in order looking for fringes. All remaining
baselines will then be searched. Choosing SEARCH wisely
will speed the FFT portion of FRING. The antenna chosen
in REFANT is treated as SEARCH(0), ie all baselines to
it are searched first.
SOLINT.....The solution interval (min.) You really should set this;
longer values are allowed beginning with 15OCT96.
0 => 10 minutes for all inputs
If SOLINT > Scan/2 (in Multisource) SOLINT = Scan.
SOLSUB.....The begin time for the next interval in advanced from the
current one by SOLINT / SOLSUB where 1 <= SOLSUB <= 10.
0 -> 1. This is to produce solutions at sub-intervals of
SOLINT based on SOLINT length of averaging.
SOLMIN.....Minimum number of subintervals to be used in a solution.
0 -> SOLSUB.
APARM......General control parameters.
APARM(1)...Minimum number of antennas allowed for a solution. 0 => 3.
APARM(2)...If > 0 then the input data has already been divided by a
model; only solutions will be determined.
APARM(3)...If > 0 then average RR, LL
APARM(4)...If > 0 average all frequencies in each IF before the
solution and in the output for single source files.
APARM(5)...WARNING: IF THE FREQUENCY INCREMENT BETWEEN IFS THAT WILL
BE INCLUDED IN A GROUP HAS THE OPPOSITE SIGN FROM THE
FREQUENCY INCREMENT BETWEEN CHANNELS IN THE IFS OF THAT
GROUP, YOU SHOULD NOT USE THE FOLLOWING
(SET APARM(5)=0 ONLY).
If = 1 then make a combined solution for the IFs;
If <= 0 then make separate solutions.
If = 2 do separate least squares fits for single- and
multi-band delays. This option will override APARM(4)
> 0. WARNING: multi-band delays derived by this method
cannot be smoothed.
If = 3 then make solutions combining IFs 1 through NIF/2
and IFs NIF/2+1 through NIF. This may be appropriate
for the EVLA in which the first NIF/2 are from
hardware IF AC and the others are from hardware BD.
If = 4 then make solutions combining IFs 1 through NIF/4,
NIF/4+1 through NIF/2, NIF/2+1 through 3*(NIF/4),
and IFs 3*(NIF/4)+1 through NIF. This may be
appropriate for the EVLA for 3-bit sampling in which
each quarter passes through separate hardware and
hence has separate delay errors.
NOTE - APARM(10) can partly override this - causing the
task to fit a delay in each IF and then to fit a
dispersion across all IFs plus delay for each group of
IFs. The output SN table will contain dispersion values
plus the single-band delays and phases corrected for the
APARM(6)...Print flag, -1=none, 0=time every 10th time, 1=time,some
info, 2=more including the antenna signal to noise ratio,
3=a very great deal.
APARM(7)...The minimum allowed signal-to-noise ratio. 0 => 5
APARM(8)...If there is no antenna (AN) table with the input file then
the maximum antenna number in the file should be entered in
APARM(9)...If > 0, perform exhaustive baseline search in the initial
FFT stage. Normally, the first stage of FRING is to FFT
individual baselines searching for initial estimates of the
residual phases, rates, and delays. This stage is notable
in that FRING gives up too easily - only baselines to the
user-selected REFANT and one other antenna are searched.
APARM(9)>0 instructs FRING to exhaustively search for
initial estimates for each antenna's errors. See SEARCH
above as well.
APARM(10)..If > 0, causes the task to fit a delay in each IF and then
to fit a dispersion plus a delay for each group of IFs to
the SB delays in all IFs. The output SN table will
contain dispersion values plus the single-band delays and
phases corrected for the dispersion.
Delay-rate control parameters:
DPARM......Delay rate parameters.
DPARM(1)...Number of baseline combinations to use in the initial,
coarse fringe search (1-3). Larger values increase the
point source sensitivity but reduce the sensitivity to
extended sources when an accurate model is not available.
DPARM(2)...The delay window to search (nsec) centered on 0 delay.
0 => full Nyquist range defined by the frequency spacing.
If DPARM(2) < 0.0 no delay search will be performed.
DPARM(3)...The rate window to search (mHz) centered on 0 rate.
0 => full Nyquist range defined by the integration time.
DPARM(4)...The minimum integration time of the data (sec);
0 => search the data to find the minimum integration
The correct minimum of all baselines should be supplied.
DPARM(5)...If > 0 then don't do the least squares solution. If the
least squares solution is not done then only the coarse
search is done and much less accurate solutions are
DPARM(6)...If > 0 then the output data will not be averaged in
frequency else, all frequencies in each IF will be
averaged. Affects single source files only.
DPARM(7)...If > 0 then the phase, rate and delays will not be
re-referenced to a common antenna. This option is only
desirable for VLBI polarization data.
DPARM(8)...DPARM(8)>0 allows zero'ing of RATE, DELAY, and/or PHASE
solutions. ** Note that the ZEROing is done _AFTER_ the
FRING solution is found, this is not the mechanism for
turning off the DELAY, RATE, or PHASE search, see
DPARM(2-3) for that capability. **
DPARM(8) value zero RATES? zero DELAYs? zero PHASEs?
0 No No No
1 Yes No No
2 No Yes No
3 Yes Yes No
4 No No Yes
5 Yes No Yes
6 No Yes Yes
7 Yes Yes Yes
DPARM(9)...> 0 => supress fitting for rate (rather than just zero
the fit afterwards). This assumes that the true rate is
small and causes all the data in SOLINT to be averaged
before being fed to the fitter. DPARM(8)=1 is not needed
in this case.
ANTWT......Antenna weights. These are additional weights to be
applied to the data before doing the solutions, one per
antenna. Use PRTAN to determine which antenna numbers
correspond to which antennas.
BIF........First IF included when APARM(5)=1,3,4 (all IFs receive the
solution found for the appropriate group of IFs, but only
BIF-EIF are used to find it).
EIF........Last IF included when APARM(5)=1,3,4 (all IFs receive the
solution found for the appropriate group of IFs, but only
BIF-EIF are used to find it).
BPARM......Correction control parameters (SEE EXPLAIN IMAGR):
(1) If > 0 then make frequency dependent primary beam
corrections assuming an antenna diameter of IMAGRPRM(1)
meters. Note that VLA and ATCA arrays (TELESCOPE
header parameter) use the default primary beam
parameters defined elsewhere in AIPS, while other
antennas actually use IMAGRPRM(1) as the diameter of a
"standard" telescope. See FQTOL below also.
(2) If BPARM(1) > 0, you may omit selected CCs from the
operation based on position:
BPARM(2) <= 0 : Include all CCs
= 1 : Omit CCs within the main beam at
= 2 : Omit CCs within the main beam at
= 3 : Omit Ccs outside the main beam at
= 4 : Omit CCs outside the main beam at
(3) 1 => use a spectral-index image represented in
IN3NAME, IN3CLASS, IN3SEQ, IN3DISK below to correct the
Clean component model for each channel. IN4NAME et al
will also be used as a curvature image iff IN3NAME are
BPARM(3)-0.5 is used as a radius in pixels over which
the spectral index image is averaged. When it is small
(0 < BPARM(3) <~ 1), the spectral index is interpolated
rather than averaged. See FQTOL below as well. When
doing spectral index, the primary beam correction
(BPARM(1)) costs very little extra. This parameter is
IMAGRPRM(17) in IMAGR.
FQTOL......Frequency tolerance in kHz. Spectral channels with FQTOL
are handled together (use the same average CC model) when
applying the primary beam and spectral index
corrections. Default is to do each channel separately
which can take a long time.
IN3NAME....Image name of spectral index image; no default.
IN3CLASS...Image class of spectral index image; no default.
IN3SEQ.....Image sequence of spectral index image; 0 -> highest.
IN3DISK....Disk of spectral image image; 0 -> any.
IN4NAME....Image name of spectral index curvature image; no default.
Curvature images should be base 10 rather than base e -
they differ by a factor of 2.3. Also the reference
frequency is 1.0 GHz. These are changes done 2010-07-13.
IN4CLASS...Image class of spectral index curvature image; no
IN4SEQ.....Image sequence of spectral index curvature image;
0 -> highest.
IN4DISK....Disk of spectral curvature image image; 0 -> any.
BADDISK....A list of disk numbers to be avoided when creating scratch
For some basic introduction to fringe fitting, please see the discussions
Thompson, Moran, and Swenson
Felli and Spencer
Perley, Schwab, and Bridle
The AIPS cookbook also describes how and when FRING should be used.