AIPS HELP file for VTESS in 31DEC24
As of Thu Apr 25 22:01:47 2024
VTESS: Task which deconvolves sets of images by the MEM
INPUTS
Dirty image
INNAME Image name (name)
INCLASS Image name (class)
INSEQ 0.0 9999.0 Image name (seq. #)
INDISK Image disk drive #
Beam image
IN2NAME Image name (name)
IN2CLASS Image name (class)
IN2SEQ -1.0 9999.0 Image name (seq. #)
IN2DISK Image disk drive #
Default level image
IN3NAME Image name (name)
IN3CLASS Image name (class)
IN3SEQ -1.0 9999.0 Image name (seq. #)
IN3DISK Image disk drive #
Output VTESS image
OUTNAME Image name (name)
OUTCLASS Image name (class)
OUTSEQ -1.0 9999.0 Image name (seq. #)
OUTDISK Image disk drive #
Restored image
OUT2NAME Image name (name)
OUT2CLAS Image name (class)
OUT2SEQ -1.0 9999.0 Image name (seq. #)
OUT2DISK Image disk drive #
NMAPS 1.0 990.0 Number of maps to deconvolve
NITER * Maximum # of iterations
NOISE * 0.0 Required residual, units are
(Jy/BEAM) VERY IMPORTANT
FLUX Zero spacing Flux (Jy)
BLC 0.0 4096 Bottom left corner of VTESS
TRC 0.0 4096 Top right corner of VTESS
DOTV * -1.0 2.0 TV display of VTESS image ?
PRTLEV * -1.0 1.0 Lots of messages ?
PBSIZE PB FWHM in arcseconds CHANGED
< 0 - no PB correction (int.
or single dish images)
= 0 - use PBPARM
> 0 - use Gaussian
BMAJ FWHM (asec) Convolving beam
BMIN FWHM (asec) Convolving beam
BPA PA (degrees) Convolving beam
PBPARM Beam parameters:
(1) Cutoff 0 -> 0.07
(2) > 0 -> Use (3)-(7)
(3)-(7) Beam shape
BADDISK Disks to avoid for scratch.
HELP SECTION
VTESS
Type: Task
Use: VTESS performs a non-linear deconvolution of dirty beams from
dirty images by the Maximum Entropy method. It is specially
designed for different types of images which have been
interpolated to the same grid. It can combine single dish and
interferometer images ! It will also now add residuals a la
CLEAN
Adverbs:
INNAME......The dirty image name. Standard defaults.
INCLASS.....The dirty image class. Standard defaults.
INSEQ.......The dirty image seq. #. 0 => highest.
If NMAPS > 1 then images having sequence
numbers INSEQ,INSEQ+1,...,INSEQ+NMAPS-1 are
operated on.
INDISK......The dirty image disk drive #. 0 => any.
IN2NAME.....The beam image name. blank => INNAME,
otherwise standard behavior.
IN2CLASS....The beam image class. Standard behavior
except blank => 'RBEAM' if INCLASS = 'RMAP'
'LBEAM' if INCLASS = 'LMAP'
'IBEAM' if INCLASS = anything
else
IN2SEQ......The beam image seq . #. 0 => INSEQ,
use -1 to get highest.
If NMAPS > 1 then images having sequence
numbers INSEQ,INSEQ+1,...,INSEQ+NMAPS-1 are
operated on.
IN2DISK.....The beam image disk drive #. 0 => any.
******** If a default image is not specified completely, then
a flat default will be used. Usually the flat
default will work satisfactorily. *********
IN3NAME.....The default image name. Standard defaults.
except blank => use flat default.
IN3CLASS....The default image class. Standard defaults.
except blank => use flat default.
IN3SEQ......The default image seq. #. 0 => use flat
default, set IN3SEQ to -1 to get highest.
IN3DISK.....The default image disk drive #. 0 => use flat
default.
OUTNAME.....The VTESS image name. Standard defaults.
OUTCLASS....The VTESS image class. Standard behavior with
default = 'xVT' if INCLASS = 'xMAP' where x is
any character
'VT' if INCLASS = anything else
OUTSEQ......The VTESS image seq. #. 0 => highest unique.
If >0; image will be created if new,
overwritten if image name exists.
OUTDISK.....The VTESS disk drive no. 0 => highest with space
OUT2NAME....The convolved image name. Standard defaults.
OUT2CLAS....The convolved image class. Standard behavior with
default = 'xVTC' if INCLASS = 'xMAP'
'VTC' if INCLASS = anything else
OUT2SEQ.....The convolved image seq. #. 0 => highest unique.
If >0; image will be created if new,
overwritten if image name exists.
OUT2DISK....The VTESS disk drive no. 0 => highest with space
NMAPS.......Number of maps to be deconvolved. Must be in
sequence starting at INSEQ.
NITER.......VTESS iteration limit. 0 => 5. If less than
Zero then will go to ABS(NITER) iterations
or stop at soluton, else increase accuracy of
solution as iteration proceeds.
Can be changed by TELL.
**********************************************************************
NOISE.......The target R.M.S. residuals for each image are NOISE
(Jy/beam). This is the most important parameter in the
deconvolution. It controls the quality of the final
VTESS image. If it is too high, VTESS will not do much
deconvolution; if it is too low, VTESS will raise the zero
levels creating falsely high fluxes. VTESS tries to get
the fit to be less than 1.05 SIGMA.
Can be changed by TELL.
NOISE(64) is used for all fields(maps) > 64.
**********************************************************************
FLUX........Zerospacing of the VTESS image. Three cases :
a. > 0 = >VTESS tries to get within 5 percent of FLUX
b. = 0 => VTESS estimates it. Often does well.
c. < 0 => VTESS estimates it using ABS(FLUX) as
an initial guess (better than putting zero)
BLC.........Bottom left corner of VTESS image, BLC(3) gives
the channel number to deconvolve.
TRC.........Top right corner of image; both BLC and TRC
default do that the inner quarter is chosen.
DOTV........Display VTESS map on TV channel 1. >= 0 => yes.
If true, you may stop the VTESSing with TV button
D after each map is displayed. To see residual
image set DOTV = 2. Can be changed by TELL.
PRTLEV......Print lots of informative messages ? > 0 => yes.
Can be changed by TELL.
PBSIZE......Size of primary beam in arcsec, FWHM of Gaussian model.
One number per field.
If = 0, use PBPARM beam with defaults suitable to the
VLA.
If < 0, do no primary beam correction, e.g. usually for
fields that are not interferometer data but can
be specified for interferometer images if
desired
If > 0, use a Gaussian of FWHM of PBSIZE(I).
PBSIZE(64) is used for fields > 64.
BMAJ........FWHM in arcseconds of the restoring beam. The
final image is convolved with this beam, and the
residuals are added to form a pseudo-CLEAN image.
If BMAJ < 0.0, then no restoration if performed.
If BMAJ = 0.0, then the beam is fitted to obtain
BMAJ, BMIN, BPA.
BMIN........FWHM in arcseconds of the minor axis of the
restoring beam.
BPA.........Position angle in degrees of the restoring beam.
PBPARM......Primary beam parameters:
(1) Lowest beam value to believe: 0 -> 0.07 Sources
outside this range are ignored.
(2) > 0 => Use beam parameters from PBPARM(3)-PBPARM(7)
Otherwise use default parameters for the VLA (or
ATCA where appropriate)
(3-7)..For all wavelengths, the beam is described by the
function:
1.0 + X*PBPARM(3)/(10**3) + X*X*PBPARM(4)/(10**7) +
X*X*X*PBPARM(5)/(10**10) + X*X*X*X*PBPARM(6)/(10**13)
X*X*X*X*X*PBPARM(7)/(10**16)
where X is (distance from the pointing position in arc
minutes times the frequency in GHz)**2.
See explain for details
BADDISK.....This array contains the numbers of disks on which
it is desired that scratch files not be located.
BADDISK has no effect on input and output maps.
EXPLAIN SECTION
VTESS : Task which deconvolves sets of images
DOCUMENTOR: T.J.Cornwell NRAO/VLA
DATE OF DOCUMENTATION: 15 January 1991
RELATED PROGRAMS: UVMAP,UTESS,APCLN,IMAGR,APVC,STESS,LTESS
VERSION: 15JUL91
PURPOSE
VTESS is designed to handle the deconvolution of different types
of images. It can handle up to 4080 or so different dirty images and
beams which have been calculated on the same size grid. Both
interferometric and focal plane images can be treated, and for the
former, primary beam attenuation can be corrected. For focal plane
images, assymetrical PSFs can be deconvolved.
VTESS performs a deconvolution of the dirty beam from the dirty
map by the Maximum Entropy Method MEM. There are, in general, many
solutions to the deconvolution problem; of these VTESS selects the
solution having the greatest entropy:
H = Sum over all pixels ( h(pixel Brightness))
where h has the form : - f*log(f/m) where m is the default brightness
and f is the pixel brightness. This measures the lack of dispersion in
pixel values and thus the maps tend to be smooth in this sense. Given
no data the output image is just the default image. There are other
justifications for maximising H but these are not widely accepted. The
pragmatic view is that VTESS maps of extended emission seem to be more
aesthetically pleasing than those produced by the CLEAN deconvolution
algorithm. In particular, CLEAN maps of large sources seem to show a
mottled structure, which is caused by the assumptions inherent in the
CLEAN algorithm, and which is not present on the corresponding VTESS
maps. VTESS may run faster than APCLN on images spanning many
(>100,000) resolution elements.
There are several undesirable features of VTESS maps of which the
user should be aware. First, the response to a point source in the map
is manifestly signal-to-noise dependent, the resolution decreasing
with signal strength. To some extent this can be masked by convolving
with a beam of known resolution as is done in the CLEAN algorithm. The
consequence is that comparison with other maps is difficult. Secondly,
the map is totally positive and biased. A map will always show some
emission in nominally blank regions but this background will be very
flat if FLUX has been chosen correctly. This bias is negligible on
regions of emission which are much brighter than the noise level.
Thus, the map is mainly useful for qualitative information unless it
is convolved down to lower resolution. On the other hand, the images
may often be superior in quality to CLEAN images and may take less CPU
time to compute. This is especially true for large images where the
sidelobe level is quite low e.g. rms less than 1 percent. Quite often VTESS
produces the most useful image.
VTESS actually maximises H subject to the constraints that the
r.m.s. residual be equal to one sigma ( using the Lagrange Multiplier
ALPHA ) and that the total flux be FLUX ( using the multiplier BETA ).
For the maximisation of the objective function a modified
Newton-Raphson approach is used. Non-diagonal elements of the Hessian
matrix are neglected. For one input image, each step or iteration
requires two 2-D FFTs and so is roughly equivalent to one major cycle
of APCLN. The cost of extra fields is roughly proportional.
This is an experimental program and so all feedback is welcome.
Send any comments, abusive or complimentary, to Tim Cornwell at the
Array Operations Center.
COMMENTS
MAPUNITS :
The final units of the map are Jansky per pixel. If you prefer
other units of brightness such as Kelvin then AXDEFINE can be used to
change the header.
To obtain an image which can be compared with the CLEAN image set
BMAJ >= 0.0. If BMAJ = 0.0 then a fit will be made to the dirty beam
to find a suitable CLEAN beam, otherwise the specified beam will be
used. This restored image will come out as OUT2NAME.OUT2CLAS.OUT2SEQ
on dish OUT2DISK.
ALIASING :
To overcome aliasing problems, which can be disastrous in an
algorithm which enforces positivity, only a quarter of the map is
allowed to be non-zero. BLC and TRC control the location of the
quarter within the dirty image. The default is such that the inner
quarter is choosen. If TRC is more than half an axis length from BLC
then it will be truncated.
CONVERGENCE :
For maps of reasonable signal to noise 100 - 1000 about
15 - 30 iterations are needed.
An automatic stopping criterion is included. It stops if:
1. NITER < 0
2. ABS(total flux-FLUX) < 0.05*FLUX
*** only if FLUX > 0 ***
3. rms residual < 1 sigma
This criterion has developed by trial and error, and has no real
theoretical justification. It may be too optimistic in that the image
is still changing significantly. If you believe this to be the case
then restart with NITER > 0 and stop by hand. Note however that the
minimum brightness is poorly defined and has little meaning so don't
worry too much about it.
Some combinations of inputs parameters will not allow a VTESS
image. For example, in nearly all cases there is no positive image
with the correct flux (FLUX) which fits the data exactly (NOISE=0.0).
However if you set FLUX too large then an exact fit can be achieved.
DEFAULT IMAGE :
*************************************************************
NORMALLY YOU CAN IGNORE THIS POSSIBILITY BY LEAVING
IN3NAME,IN3CLASS,IN3SEQ,IN3DISK blank.
*************************************************************
The default image determines what the image looks like if there
is no data. Any data cause perturbations away from this image. The
default "default" image is flat and so VTESS tries to make the output
image as flat as is allowed by the data. An non-flat default is
helpful in cases where a flat default fails. An example is the
deconvolution of an image containing a point source in rather diffuse
extended emission. Plain VTESS will usually leave the sidelobes of
the point source buried in the diffuse emission. A default level of a
point source in an extended Gaussian may well help. Another useful
mode is to use a low resolution image as the default. Failing such an
image, the following procedure gives good results : run to convergence
with a flat default, use CONVL to smear out the resulting image
(FACTOR=1 to preserve units of Jy/Pixel), then use this smeared image
as the default and run to convergence. The resulting image has less
bias and suppresses low level noise well.
A default image can be generated using the task IMMOD. This is
useful for planets, the Sun etc. Note that the units are Jy/pixel.
MOSAICING or TESSELATION :
One of the most important features of VTESS is its ability to
form mosaics of a large object spanning many pointing centers. For
example, at 20cm, this allows imaging of objects larger than the size
of the primary beam (30'). When observing, you must take data at many
different pointing centers. VTESS will then joint them smoooothly. It
knows about the VLA primary beam, and uses a model due to Perley,
truncated at the 7 percent level.
Furthermore, singe dish data can be introduced to give the short
spacing information missing from the interferometer data.
Interferometric data can be corrected for the primary beam
pattern. At the moment, the I'th field is corrected for a circular
Gaussian of FWHM PBSIZE(I) arcsec centered on the pointing center. If
PBSIZE(I) is zero, the PBPARM parameters are used instead (see
below). The defaults are appropriate for the VLA. If PBSIZE(I)<0.0
then no correction is performed; that field is assumed to refer to a
focal plane image such as that measured by an optical telescope or a
single dish.
The pointing center is specified in the header by the Keywords
'OBSRA', 'OBSDEC'. It will only show up in IMHEADER if it is different
from the phase tracking center. VTESS will report the values of the
pointing center used after conversion to pixels.
The related program STESS will make an image of the sensitivity
function for a mosaic. This is the sum of the primary beams, each
weighted by the appropriate inverse variance (i.e. NOISE(I)**-2). Once
you have set up the parameters for VTESS in mosaicing mode, it is a
good idea to run STESS and look at the sensitivity image. It should be
fairly smooth and uniform, except for the effects of the cutoff in the
primary beam model.
Sky-curvature effects will be important in some circumstances and
will hinder the use of VTESS. For 20cm and shorter in the C and D
configurations, you can usually get away with mapping each primary
beam separately. The procedure is:
1. Observe at the requisite number of pointing centers, spaced
every HWHM (e.g. 15 arcmin at 20cm).
2. Calibrate, edit each field separately.
3. Run UVMAP on each field separately WITHOUT any phase shifts.
The size of each field must be double the full primary beam
size (e.g. 512**2 with 15" cellsize is fine for 20cm D-array).
4. Choose one centrally-located field as the center of the
coordinate system to be used. Pad the map and beam for this
field up to twice the maximum field of view. The task PADIM
does this nicely. This resulting image is the reference field
image.
5. Put all the other images onto the same grid. OHGEO or HGEOM
are very convenient for this: put the reference field image in
slot two, and the image to be converted into slot one.
6. Pad the beams out to the required size. Really you should do
step 5 on each beam but the shift will come out incorrectly
then.
7. Set up the parameters for VTESS, and then run STESS to check
the sensitivity function.
8. Run VTESS!
RESTARTING :
VTESS can be restarted by simply filling in OUTNAME, OUTCLASS and
OUTSEQ with the parameters of a map. NITER must, of course, be larger
than the previous stopping point. Unlike CLEAN one can start from any
initial estimate, hence it is efficient to keep iterating on the same
image while changing the input dirty map by selfcalibration or by data
editting. Similarly any of the control parameters may be changed in
flight.
VTESS writes the current image to the output file every iteration
so that if it crashs, simply clear the write status and start from
that iteration. If it crashs while writing the output image then tough
luck, you will have to start again.
Between iterations the values of ALPHA and BETA are stored in
REAL*4 words 127 and 128 of the Catalog header.
NOISE :
One crucial control parameter is NOISE. This determines the level
of fit attempted. It should be comparable to the r.m.s. noise level in
a blank region of a CLEAN map thus if the data is reasonably
well-calibrated this will be close to the theoretical noise level.
Specifying too large a number will lead to an overly smooth map. Too
small a number will prevent convergence since there will be no
positive map which fits the data to that level. A useful strategy is
to initially underestimate NOISE and then stop after a number of
iterations and reset it to the level acheived up to that point.
FLUX :
FLUX specifies how the zero spacing flux is to be
estimated. There are three cases :
a. You specify a known or guessed value which must be fit
to within 5 percent. Set FLUX to a positive number. This is quite
important on weak sources since after accounting for all the
power in the source VTESS will put power into the sidelobes thus
biasing the total flux by a large amount and overfitting to
the other visibility samples.
b. If you have no idea what the zero spacing flux is
then leave FLUX = 0.0. VTESS will attempt to estimate it.
c. If you have a rough idea (within a factor of 2 say)
then set FLUX to the negative of your guess e.g. FLUX=-2.0
VTESS will then do a reasonable job of estimating the true
value.
GENERAL TIPS :
If the gradient starts to increase dramatically
after a number of iterations then the problem that you have
given is probably too difficult. Stop and reconsider the
input parameters; in particular, NOISE and FLUX. Usually
setting these too low will cause problems.
Point sources often cause problems so it is a good
idea to remove them using CLEAN. If you set BMAJ to -1 and put
BOXs around the points then the output image will be the dirty
image minus the point sources. Then put this image into the
slot for the dirty image.
Preconvolving the dirty image with a CLEAN beam will
usually improve the quality of the result and "fix" the
resolution to be that of the CLEAN beam. Convergence is also
improved.
Over-sampling of the image plane will slow VTESS so
restrict the number of points per beam to less than about
7 or 8.
OPTICAL DATA :
VTESS can be used to deconvolve optical images. The main
difference from interferometric images is that the noise is
independent in the image plane; it assumes that the image is
not photon limited i.e. it uses a chi-squared test between the
convolved image and the dirty map. You will need a dirty
beam to put into IN2NAME,IN2CLASS,IN2SEQ,IN2DISK. There are at
least three ways to do this :
1. Guess a simple Gaussian form and use IMMOD to generate
an image containing it.
2. Use IMFIT to fit an number of Gaussians to a star in the
field. Then use IMFIT as in 1.
3. Cut a star out from the field using COMB then use GEOM
to edge it out to the full size with zeroes.
VTESS has two different units that it works with : Jy/beam
and Jy/pixel. If the beam volume is normalised to unity then
these are the same; if the beam peak is normalised to unity
then they differ by the number of pixels per beam. In radio
interferometry the latter is the usual convention but in
optical work the former will be more convenient so I recommend
that you normalise the dirty beam by it's volume and put
NPOINTS = 1.
For optical data, PBSIZE for that field must be set to a
negative number.
BMAJ,BMIN,BPA:
If BMAJ > 0.0, then a CLEAN-type image is formed by
convolving the output image with an elliptical Gaussian and
adding the residuals. If the program is mosaicing, then the
residuals are linearly corrected for the primary beams before
this addition. The units of the final restored image are
JY/BEAM. Agreement with a CLEAN image will be generally good,
but VTESS will slightly underestimate the peaks and will give
a smoother restoration. If mosaicing, then the VTESS image
will contain significantly more extended emission.
EXECUTION TIMES :
Typical CPU time for running VTESS in an otherwise empty
VAX 11/780 with FPS120B array processor is:
128 x 128 0.20 min/iter/field
256 x 256 0.53 min/iter/field
512 x 512 1.9 min/iter/field
1024 x 1024 7.2 min/iter/field
2048 x 2048 28.5 min/iter/field
Typical CPU time for running VTESS in an otherwise empty
CONVEX C-1 is:
128 x 128 0.02 min/iter/field
256 x 256 0.1 min/iter/field
512 x 512 0.4 min/iter/field
1024 x 1024 1.6 min/iter/field
2048 x 2048 6.4 min/iter/field
Wall clock times will be at least two to three times these
numbers. If the map is mainly filled by emission then the
APCLN runtimes will be comparable to these.
DISK SPACE :
The amount of scratch disk space allocated for the
following image sizes is :
Radio data Optical data
256 x 256 2176 blocks 5376 blocks
512 x 512 8704 blocks 21504 blocks
1024 x 1024 34816 blocks 86016 blocks
2048 x 2048 139264 blocks 344064 blocks
NX x NY 4.25*NX*NY/128 10.5*NX*NY/128
REFERENCES
Cornwell T.J., and Evans K.F., "A simple Maximum Entropy
deconvolution algorithm", Astronomy and Astrophysics, (1985)
Burch,S.F, Gull,S.F., and Skilling,J., "Image restoration by a
powerful Maximum Entropy method", Computer Vision, Graphics and
Image processing, 23, 113-128 (1983).
--------------------------------
Primary beam correction
VTESS corrects an image for the primary beam attenuation of
the antennas. The function used to model the primary beam for normal
VLA frequencies
F(x) = 1.0
+ parm(3) * 10E-3 * x
+ parm(4) * 10E-7 * x*x
+ parm(5) * 10E-10 * x*x*x
+ parm(6) * 10E-13 * x*x*x*x
+ parm(7) * 10E-16 * x*x*x*x*x
where x is proportional to the square of the distance from the
pointing position in units of [arcmin * freq (GHz)]**2, and F(x)
is the multiplicative factor to divide into the image intensity at the
distance parameter x. For other antennas, the user may read
in appropraite constants in PBPARM(3) through PBPARM(7). The
flag, PBPARM(2) must be set to a positive number to invoke this
option and PBPARM(3) must not be zero.
This correction scales with frequency and has a cutoff
beyond which the map values are set to an undefined pixel value GIVEN
in PBPARM(1). At the VLA frequencies the default cutoff is
1.485 GHz 29.8 arcmin
4.885 GHz 9.13 arcmin
15 GHz 2.95 arcmin
22.5 GHz 1.97 arcmin
and occurs at a primary beam sensitivity of 2.3 percent of the value at
the beam center. Corrections factors < 1 are forced to be 1.
The estimated error of the algorithm is about 0.02 in (1/F(x))
and thus leads to very large errors for x>1500, or at areas
outside of the primary response of 20 percent. The cutoff level
may be specified with DPARM(1).
Default values of PBPARM for the VLA are given by Perley's fits:
0.0738 GHz -0.897 2.71 -0.242
0.3275 -0.935 3.23 -0.378
1.465 -1.343 6.579 -1.186
4.885 -1.372 6.940 -1.309
8.435 -1.306 6.253 -1.100
14.965 -1.305 6.155 -1.030
22.485 -1.417 7.332 -1.352
43.315 -1.321 6.185 -0.983
For the ATCA, these are by default:
1.5 GHz -1.049 4.238 -0.8473 0.09073 -5.004E-3
2.35 -0.9942 3.932 -0.7772 0.08239 -4.429E-3
5.5 -1.075 4.651 -1.035 0.12274 -6.125E-3
8.6 -0.9778 3.875 -0.8068 0.09414 -5.841E-3
20.5 -0.9579 3.228 -0.3807 0.0 0.0
For the Karl G Jansky VLA ("EVLA"), the defaults are frequency
dependent. If the observing frequency is between two tabulated
frequencies, then the beam is computed for each of the tabulated
frequencies and then interpolated to the observing frequency. The
values used are far too numerous to give here, see EVLA Memo 195,
"Jansky Very Large Array Primary Beam Characteristics" by Rick Perley,
revision dated June 2016. Obtain it from
http://library.nrao.edu/evla.shtml
RICK PERLEY'S (OLD) REPORT
Polynomial Coefficients from LSq Fit to VLA Primary
Beam raster scans.
Functional form fitted:
1 + G1.X^2 + G2.X^4 + G3.X^6
where X = r.F,
and r = radius in arcminutes
F = frequency in GHz.
Fits were made to 3 percent cutoff in power for 24 antennas.
Poor fits, and discrepant fits were discarded, and the most
consistent subset of antennas had their fitted coefficients
averaged to produce the following 'best' coefficients.
Freq. G1 G2 G3
1.285 -1.329E-3 6.445E-7 -1.146E-10 *
1.465 -1.343 6.579 -1.186 "
4.885 -1.372 6.940 -1.309
8.435 -1.306 6.253 -1.100
14.965 -1.305 6.155 -1.030
22.485 (old) -1.350 6.526 -1.090 *
22.485 (new) -1.417 7.332 -1.352
43.315 -1.321 6.185 -0.983
The estimated errors (from the scatter in the fitted
coefficients) are generally very small:
G1: .003 at all bands except Q (.014)
G2: .03 to .07 at all bands except Q (.15)
G3: .01 to .02 at all bands except Q (.04)
R. Perley 21/Nov/00
* The 1.285 and 22.485 old feed values are not used.