Applications of
Two-Dimensional
Vidicon Photometry:
Venus
by
Philip Henry Schaller, Jr.
Submitted in
Partial Fulfillment
of the Requirements for the
Degree of Master of Science
at the
Massachusetts Institute of
Technology
June, 1973
Department of_
Certified
ht
nd Planetary Sciences, May 11, 1973
by:_
Accepted by:
Chairman, Departmental Committee on Graduate
Students
TABLE OF CONTENTS
Acknowledgements
.......
........................
2
g.....................
3
A.
INTRODUCTION
B.
GRAY SCALE EXPANSION ............................
6
C.
IMAGE REFLECTION AND
8
D.
LAPLACIAN IMAGE .
10
E.
INTENSITY TRAVERSES
12
F.
CONCLUSIONS
References
.............
Figure Captions
Figures
Appendix
...
..............
ROTATION
.................
..
.14
....
.......................
g....
o........ e
..
... .....
..
..
....
..... .....
..
...
....
.... ....... ....
....
15
e*
....
..
16
...
19
54
ACKNOWLEDGEMENTS
I would like to thank my advisor, Thomas B. McCord,
and all my friends at MITPAL for their help.
Also,
thanks go to R. Beebe and others at the New Mexico University for supplying their photographic plates for comparison.
3
A.
INTRODUCTION
The vidicon tube and the theory of its operation, and
an operating camera and data system have been described by
McCord and Westphal (1972).
The hardware and software sys-
tems have been described in
detail by Kunin (1972).
This
thesis describes one application of the vidicon system to
as astronomical problem.
It has been known for some time that the planet Venus
exhibits a featureless shroud of clouds in the visible portion of the spectrum.
In the ultraviolet portion, however,
features are visible (Boyer and Guerin 1969)
Reese 1972).
(Scott and
These features, and in particular the curious
"Y"-shaped cloud which rotates around the planet in approximately four days, are of extremely low contrast.
Conventional
photographic pictures are printed on high contrast paper
to bring out the low contrast clouds.
is
The vidicon system
ideally suited for this problem for three reasons.
1) The system has a wide dynamic range, incorporating
many 5ray levels.
2) The system is
3)
linear over this wide dynamic ranSe.
The data are already in digital form.
Analyses of the vlidican imaeas are simple using a computer.
The yidicon images presented in this thesis were taken
usinS the Kitt Peak National Observatory 84" telescope on
April 23, 24, 25, and 26, 1972.
The first night the instru-
ment was mounted at the Coude focus.
The other nights it was
mounted at the Cassegrain focus.
Film photographs were taken
the same nights at the New Mexico State University.
Thirteen vidicon images were selected for study in
this thesis.
These represent the best pictures at each of
the several wavelengths taken during each night of the run.
On the first night (the only Coude pictures) the Y-shaped
cloud had apparently rotated out of view.
The second night
many quality pictures were obtained at .358, .383, and .402
microns.
The cloud is clearly visible on this night although
only one of the branches of the Y is seen.
The third night
only three pictures were obtained and were of less quality
than the night before.
The final night all pictures were
taken through infared filters (see figures 1-13).
Figures 14 through 17 are the best pictures taken with
conventional photographic plates during each night of the
run.
They are all at .37 microns.
vidicon pictures should be noted.
Correspondence with the
They also show only one
branch of the Y cloud and confirm the phase of the cloud
during this time.
The approximately four-day rotation can
be observed, noting that the cloud was rotated out of view
on the night of the 23rd.
These pictures, however, are not
suitable for entering into the rotation rate controversy
of 4 or 4.5 days (Boyer and Guerin 1969) (Scott and Reese
1972).
Various image processing techniques were developed in
the course of this thesis research which were used to enhance
the cloud features above the background planet.
The remainder
5
of this thesis is devoted to a description of these techniques
and their application to the Venus cloud problem.
While the
data were not taken for the purpose of this thesis, a good
deal of it war, usable.
Although no great scientific prob-
lems were solved, it is hoped that this work will be the guide
for future Venus research.
I
B.
GRAY SCALE EXPANSION
To make such low contrast features such as the Y cloud
on Venus more visible, various image enhancements can be
performed on the computer.
The first of these attempts at
The vidicon
contrast enhancement is gray scale expansion.
system has 256 gray levels.
The actual feature may extend
over only tens of gray levels.
These gray levels are line-
arly expanded over the full 0 to 255 range.
Points else-
where in the picture falling below 0 are set to 0 and those
rising above 255 are set to 255.
As the contrast is enhanced (see figures 18-22), two
effects are noticeable.
1) The size of the image decreases
until under almost total contrast enhancement the image almost disappears.
This is due to less and less of the image
falling into the selected range of gray levels for total
expansion.
2) Artificial contours are introduced by the
quantization noise.
When only a few gray levels are used to
cover the entire range of light levels, noticeable (to the
eye) distinct changes in light level are visible across the
image.
While the original pictures had eight bits of tray
resolution, every contrast enhancement of a factor of two
reduces the number of significant bits by one.
Thus these
contours are not inherent to the actual image (which is continuous), but are introduced by the necessity of making
arbitrary decision
levels in digitizing the data.
Since our object data is at one end of the gray scale,
a logarithmic enhancement built into the film converter was
7
also tried.
(see figures 23-27)
not show much improvement.
The resulting images do
The vidicon system also contains
a routine to contrast enhance an overexposed image without
loss of precision, as well as the normal overexposed image
reducing routines.
C. IMAGE REFLECTION AND ROTATION
The usual method of mapping a feature which appears
only at selected wavelengths is to divide the picture at one
of the selected wavelengths by the same scene at another,
but featureless, wavelength.
cannot be done,
In this case, however, this
The scattering function of the CO2 atmos-
phere, which is superimposed on the feature, is a strong
function of wavelength and hence cannot be divided out.
As noted before, only one branch of the Y seems to be
visible on this occasion,
The southern hemisphere can be
divided by the northern hemisphere at the same wavelength
(using the same picture, obviously), and thus eliminate the
CO2 scattering function.
(This assumes a certain symmetry
about the function, of course.)
The vidicon system now
contains a routine to reflect a picture about an arbitrary
axis in the plane of the picture.
The problems of such a
reflection on a discrete grid of points are obvious, but
the results are remarkably good.
Note that the proper com-
bination of two reflections can produce an arbitrary rotation
about an axis perpendicular to the plane of the picture.
The reflected image of Venus is divided by the original
and then contrast enhanced.
are now immediately obvious.
the reflection axis.
(see figures 28-42)
Two things
1) There is a symmetry about
Where the image is dark on one side,
it is light on the other side and vice versa.
So in the
same picture we have the southern hemisphere divided by the
northern hemisphere juxtaposed with the northern hemisphere
divided by the southern hemisphere.
effect to this process.
2) There is an edge
The reflection, while good, is not
perfect and the limbs of the planet in the two images.(orginal and reflected) do not match up exactly.
Since the
light level changes rapidly across the limb, the division
process greatly enhances the edge.
makes it worse.
Contrast enhancement
The problems of contrast enhancement men-
tioned in the previous section also apply here.
10
D.
LAPLACIAN IMAGE
Another method of enhancing low contrast features is
that of the Laplacian.
Being a second derivative operator,
the Laplacian is not sensitive to overall reflectivity levels
or their uniform variations.
flectivity variations.
It yields only changes in re-
These are most often due to fine
detail in the image.
The discrete Laplacian is performed on the image by
subtracting the average level of the right nearest neighbors
of a point from the level of the point.
(Rosenfeld 1969)
The resultant values are then contrast enhanced.
(see
figures 43-55) The absolute values of the Laplacian may
also be used for display.
(see figures 56-68)
Two items are noticeable in these pictures.
1) The
ones taken at the Cassegrain focus show a considerable edge
effect whereas the Coude pictures do not.
This is due to
our now enlarged raster (nine points instead of one) when
taking the Laplacian.
In the Cassegrain images the entire
disk of the planet is approximately 32 points wide, while
the Coude images show a disk 128 points wide.
Since the
Coude image is of smaller scale and the limb varies more
slowly, the effect of the larger raster is not noticeable.
One might try to circumvent this purely mechanical
problem by enlarging the smaller picture in the computer
before taking the Laplacian.
common and both have problems,
Two methods of enlarging are
a) Each point is mapped
into, say, four points at the same gray level.
Its
problem is graininess.
The Laplacian pictures appear
grainy enough without making them worse by this method.
b) Each of the four points in the enlarged picture can be
interpolated in gray level between the positions of the
original gray levels.
This is an expensive process and
does not yield enough quality to make it worthwhile.
Fre-
quently, artificial contours are introduced and are enhanced
by the Laplacian process.
Both these methods suffer from
the problems associated with displaying a supposedly continuous function on a discrete grid,
(see previous section)
2) The second branch of the Y cloud is now discernable.
This has been unnoticed by any of the previously
mentioned methods, which shows the power of this technique.
ow
E.
INTENSITY TRAVERSES
While the CO2 scattering function is a complication
for the purpose of observing the Y cloud, it is interesting
in its own right.
(see Appendix)
This data is presented
in the format of intensity traverses.
The intensity of the
image is scanned along a line perpendicular to the planet's
terminator.
All plots begin with the limb on the left and
end with the terminator on the right.
The organization of
these 117 intensity traverses is first by image and then by
latitude,
In order there are nine plots for each of the
thirteen previously mentioned selected images corresponding
to figures one through thirteen, respectively.
In each set
of nine, the plots start at the northern end of the planet
and end at the southern end.
Note that in some cases, the
first or last plot misses the planet altogether.
The fifth
plot in the sequence is reliably along the equator.
The
lines of traverse are as close to being at equivalent latitudes as is possible on a discrete grid, and very close in
equivalent distance.
A normalized distance scale, as well
as the start and end points for each traverse, is given.
Note that the traverses were taken before correction due to
the mirror image reflection by the Cassegrain focus.
is apparent in the absolute coordinates only.
This
Also note
that the plots of the Coude images span about 128 points,
making the Coude traverses appear smoother.
For interpretation, the plots at similiar latitudes, but
through different filters, may be overlayed to show the
13
wavelength dependence of the CO2 scattering function.
features, such as the Y cloud, seem to be masked by the
small samplinp rate when the cloud was visible.
Small
14
F.
CONCLUSIONS
The first data from the two-dimensional vidicon
photometer are at least as good as that obtainable from
conventional photographic film techniques.
cessin
Further pro-
to bring out desired features is readily and easily
done through computer techniques.
These techniques produce
better and cleaner results With more and more sophisticated
methods.
The next method to be tried should be some form
of high pass filtering in the spatial frequency domain.
Noise filtering can easily be done along with this.
Further observations of Venus with the vidicon system
should span at least five nights in order to see one
complete cloud c.ycle.
The image should be as large as
possible without reaching the edge of the target.
Since the
cloud feature spans just 10 or 20 gray levels out of 200,
the exposure should be such that the brightest part of
the image is near the top of the gray scale range.
Overexposed images should be retaken, as it is at best
difficult to retrieve the information.
Images should be
taken at several wavelengths during each night and
repeated on the other nights.
Adequate loggin5 of the
setup of the observations and the data taken will ease
the burden of the data reduction.
REFERENCES
Boyer, C. and P. Guerin (1969).
Etude de la rotation
retrograde, en 4 jours, de la couche exterieur
nuageuse de Venus.
Kunin, J. S. (1972).
Icarus 11, 338-355.
A Technique for Two-Dimensional
Photoelectronic Astronomical Imaging, with Application to Lunar Spectral Reflectivity Studies.
Thesis.
Master's
Massachusetts Institute of Technology.
McCord, T. B. and J. A. Westphal (1972).
Two-dimensional
Silicon Vidicon Astronomical Photometer.
Opt.
11, 522-526.
Rosenfeld, A. (1969).
Picture Processing b
Computer.
Academic Press, 94-102.
Scott, A. H. and E. J. Reese (1972).
Rotation.
Icarus 17, 589-601.
Venus:
Atmospheric
16
FIGURE CAPTIONS
North is to the top and east is to the right, unless
otherwise rioted.
(Planetocerntric coordinates)
1
4/24/72
Fi lter: .358 microns
2
4/23/72
.383
3
4/24/72
.383
4
4/25/72
383
5
4/23/72
.402
6
4/24/72
.402
7
4/23/72
.564
8
4/26/72
.906
9
4/26/72
10
4/26/72
1.00
11
4/26/72
1.05
12
4/26/72
13
4/26/72
14
4/22/72
"'
.37
"
15
4/23/72
"9
.37
9
16
4/24/72
"9
.37
"
17
4/25/72
"9
.37
"
18
gray levels
10 to 200 of figu re 3
Notes
double exposure
.948
"9
"HB
1.10 microns
19
-9
60 to 200
20
"n
100 to 200
New Mexico State
University
"9
"
160 to 200
21
22
"f
23
figure 18
130 to 200
with logarithmic e nhancement
24
figure 19
25
figure 20
26
figure 21
27
figure 22
28
same as figure 3
29
reflection of figure 28
30
figure 28 divided by figure 29
31
gray levels
with logarithmic enhancement
"
10 to 245 of figure 30
32
"1
20 to 235
"
33
"o
30 to 225
"
34
"1
40 to 215
"
35
"f
50 to 205
"
36
"f
60 to 195
"
37
"f
70 to 185
38
"f
80 to 175
39
"
40
"t
100 to 155
41
"f
110 to 145
"
42
"o
120 to 135
"
43
44
45
46
47
48
49
50
o90
to 165
Laplacian of figure 1
"t
Note:
second branch
of Y cloud
Notes
second branch
of Y cloud
2
Laplacian of figure 9
10
53
11
54
12
55
13
56
Absolute value of Laplacian of figure 1
57
2
58
3
59
60
62
8
64
9
65
10
66
11
67
12
68
13
FIGURES
20
Figure 1
Pigure 2.
Figure 3
Figure 4
2Z
Figure 5
Figure 6
Figure 7
Figure 8
Figure 9
Figure 10
Figure 11
Figure 12
26
Figure 13
Figure 14
Figure 15
Figure 16
26
Figure 17
Figure 18
29
Figure 19
Figure 20
30
Figure 21
Figure 22
Figure 23
Figure 24
3z
Figure 25
Figure 26
33
Figure 27
Figure 28
3Sf
Figure 29
Figure 30
35
Figure 31
Figure 32
36
Figure 33
Figure 34
3?
Figure 35
Figure 36
38
Figure 37
Figure 38
39
Figure 39
Figure 40
40
Figure 41
Figure 42
4'
Figure 43
Figure 44
42.
Figure 45
Figure 46
Figure 47
Figure 48
44
Figure 49
Figure 50
45
Figure 51
Figure 52
%I'
Figure 53
Figure 54
Figure 55
Figure 56
SjB
Figure 57
Figure 58
i9
Figure 59
Figure 60
Figure 61
Figure 62
Figure 63
Figure 64
51-
Figure 6.5
Figure 66
53
Figure 67
Figure 68
APPENDIX
z,-.
I-
z
~48
8
8M.00
0.
0.10
PC
o.30
a'1o
329.0
.50
PGSIT ION
0.
w
0.70
0.80
0'.90
121.0
1'.00
153.0
VENUS
FILT=.356 EXP-.42
4/24/72
926
PRL217 009
>- p
zi
8.
.0
.0
O.0
0.30
O.50
C.40
rS
133.0
0.60
0. 70)
0.30
I TIN
FILT=.35
EXPw.42.,
4/24/72
t0
165. D
IWO0
117.0
VEtIUS
0.30
928
PRL217 009
VD43S0
)J
28.
8"
I
C
LI
I 7
u.a0
137.0
113.0
.o10
U
0.20
..
6.0
1
.4o0
*
0.so
PSIT ICN
o-.o
-I
0.y 7
o'. 0
0.o
16.0
15.0
VENUS
FILT=.3G& EXP-.42
4/24/72
928
PRL217 009
Veases
b"
I-
c.oo
.o.i
0.10
0.,0
0...
0si
0.60
U.,0
-- O
POSITION
VENUS
FILT.36 EXP~-.q2
4/2q/72
0.90
1.0
373.0
141.0 141.0
928
PRL217 009
veoses
cr
84
*z
8.D
0.g
i'.o
1m7.0
137.0
VENUS
FIL7=.3S EXP-.42
4/24/72
928
PRL217 009
..
8
1 Vees
0
8
4~4
U,
z
lii
I-- F.
z
0.730
2419.0a
101.0
VENUS
0'.50
POS1I71GN
FILT=.356 EXP-.12
4/24/72
1is.0
928
PRL217 009
58
B.
2:'lii
I2:
b.42
S
-D.00
0.20
0.10
o.so
n.so
POSITION
o.Wo
0.70
o.so
o.s
1~.o
12a.o
07.0
VENUS
FILT=.3S8 EXP-.42
4/24/72
928
PRL217 009
vueses
'IJ
I--
8
0.10
0.go
0.3
0.40
167.0
0.
POS1TIGN
0.60
0.70
Owo
1.00
109.0
83.0
VENUS
O.no
FILT'.356 EXP-.42
4/24/72
928
PRL217 009
Von SIM
59
B
:i.
4
1AJ
I-.
zb.48
S
B
,-.
---.-.-------
____
l' 20
0'.s0
0'l
.w
261.0
09.0
-.
O'.so
POSIT ION
d. w
0.70
.so
.go
19'.0
121.D3
VENUS
FILT=.356 EXP-.42
4/24/72
928 PRL217 009
B.
VEeWSa
tz
-d.jo -
020
0.30
0.11
J37.0
0.60
0.70
0.90
090
1.00
1,.0
J37.0
I69.
YaH06
O.50
POSITI0Mt
FI LT=.383 EXPA4,0
4/23/7Z 1000
PAL216 018
-
60
8.
%.n
ot
a o
0.10
o'.so
wn
.70
o.so
w~
I'.
POSI TION
147.0
153.0
VENUS
FILT=.383 EXP-6.0
4/23/72 1000
PRL216 018
.
-D
.....
l
8~
8
0 n o.00.co t3.sJ
157.0
sv~oPGSi
0.10 O.so 0.5
0.70
T7 1ON
FILT:.3U3 EXP-65.0
4/23//2 1086
0.9.
6I1.1
137.1
V1N11S1
0.80
PRIL216 a018
VtM651.4
61
8
u6i
8
8S.
'~8
Wbao
o.lo
. o'.o o'
0.20
o'.50
1st~o POSIT ION
.o
.1G
1'.'
.ow
.su
iei~o
VENUS
.a
71.0
-
o.0
FILT=.363 EXP-6.0
4/23/72 1000
FRL216 018
-0
S
zn
~8.
i.oa
0.10
0A~g
0.so
0.4L0
O.!o
0.60
0..0
0.80
0.9
rr,.o
VDIJUS
7 1.0
73.0(I
It 15Ir .33- fXP-6.0
4/23/72 1000
PAL216 010
-D
62.
2
0"I
uJ
5z
88
0.
.0.0
POSITION01.0
187.0
89.0
s?.0
VENUS
4/23/72 1000
FILT=.383 EXP-6.O
PL216 018
"I
* -'F)
(;)Iu,
lq I
I.-
8.
1',
* *1
Ii.
i~*'
hi. ~
INIC I
1~ ,.t~
vLT~1.)
I
J
J
0.~n
f.il.
i ~;
1.~r3
1~'7.it
I 111' 1
:' j,
" -l tI 13
.-n-
63
z-en-
S-
93.00
0.10
0.20
0.s0
0.10
0.30
FILT=.383 EXP-6.0
VENUS
.
.0c.80
4/23/72 1000
0.70
0.80
PRL216 018
0.90
1.00
-D3
to
8
F8.
en-
z-
'.if
o.
o
f.e
U.Nal
u.fu
U.60
0.71
0.80
0.9.
P03'rifeS.,.
'ii .u
%fViNiIt-,
'I-30'PXP-.31/53/72
1
PRL-216 018
--)
64
V"0o3C
8
8
POO.,I7 1ON
121.0
'113.0.15.
FILT=.383 EXP-.1 S
VENUS
4/24/72
923
PRL217 O0
8-
X.-
U.I()
)~'!~. fl
)(f~i. Li
V It Kil;
OA~fl
(I. 3n
0.
410
0.Gil
P '0,31 UIjN
CD
0.*70
0.0)0
,.
Ltyj
y 1 '*.
VoEsse
65
8
I
13
8
<.4--
--
-_________
I"b.a
0.2 0
o.wo
.o w o.sa
POSITION
129.0
105.0
. . w
.70
0.ea
0.s
1.00
157.0
VENUS
4/24/72 923 PRL217 00S
FILT=.383 EXP-.15
z-.
1II3.
;
in.
l
1'i
~
e
I '1i
.
E.XPs'i
- .
I
4 /-1/i
nn
-w
1.6:-m
n'.:nI'
u.n Ii,
u.so
.0
tr:,. r
:.
PH
1'/ 005
66
157.0
" "''
VENUS
ul
z--
FILT=.303 EXF-.1S
''%
'.
4/24/72
.
923
em.o
-
FRL217 005
-0
.-
]
.L0
0.10
0.20
0.30
0.40
0.50
POSITION17.
0.60
0.*0
--
141.017-
VB.I Ili
F L .:.33 X-.15
4l/2.:i/72
92c'3 PF1L217 005
O.0
O.E
1.L
177.0
121.0
ga.0
59.0
VENUS
FILT=.383 EXF-.IS-
4/24/72 923
PRL217 005
8
vDesse
S
B
8
POSIT I CN
19. 0
VENU'ji
-fl
117.0
FILr=.365 EXP-.1!
4/24/72 b23
FAL217 L005
vecese
Uzj
8L
8z
'10
0.0
o.e
.
53.0SIION
51.0
.70
0.80
0.90
1.0
.
113.0
FILT=.383 EXP-.1S
VENUS
4/24/72
923
PRL217 005
8.
8J
8
.-
9sc.
o 0 .10~~ao
f.0
0n
~ir]
PG(1'110N
0.e
0.'
.
21?.n
VDIUS I
80Te
0.0
I.00
ei.n
FILT=..3=
-3 XP--.14
4/i5/72
9o
FRL218 071
.
69
&-4
D.co
12.0
oao
0.!0
0.9
f'(S1TI ON
VENUS
FILT=.383 EXF-.L
t
4&/2S/72
2.0
110.0
902
FARL21EI 071
-
cSf
.8
0. Mo
cbo
Gf
D
01
P031
T 1
i .
VFl.4LJfll
VEUU5P--Il FqlT.~sl 1L i 2 90?
rAL210 071
veessa
0.20
.so
0.. 0
0.6.
POSI TION
sea.0
129.0
VENUS
0.0
0.so
.1a
FILT=.363 EXP-.l t 4
1ie.0
03.
4/2S/72
902
PRL218 071
yeeam
'Vil
VENI Is
o.so o.'a
o.'rs
o.co
0.70
o.60
0.90
PO(317 1 ON
FILT=.3P3 EXP'-.14&
41/2'L/72
902
FRL210 071
--
-.c0
-
ees.
71
21 .0
' "''
1111.0
141.0
' ' '
137.0
FILT=.363 EXP-.4t t
VENUS
4/25/72
902
-0
FAL218 071
8
8
.
a,.iu
0. M
.w
P..sa
FA L'D'83 E0.l'
0.70
PQSJ3"'-~
147.0
)u).13
4 /25/72
902 PRL-216 071
.81
0.9
1.no
^
72
8
8I'13
8B
8
'
|
c.no
u.lo
'
'
.
w
.o w
.w
10&.0
14o.0
VENUS
d.co
.m
POSIION
a.so
d'. w
t'.00
11r.0
14s.0
FILT=.363 EXP-.
902
I& 4/2S/72
FAL210 071
-D
I-.
zw-.
uJ
F-
ufl1.0
0-
1
[.
117.0
vin.n
VER BS
191-0
FI ='MEXP--14l 14/1-:1/72
9,1.2 PTIL2163 071
vecD2C
>-B
z-.
8
8
8
.to
.
20
.o30
153.o
FILT=.402 EXP-1.0
VENUS
Pd S ITIN
o.so
4/23/72 1002
---
I-
0' m
0.a w
0.s
67.0
137.0
PRL216 020
veaO#c
tu
I--
28
8
0.7U
153.0i
VDBJUS 1
0.0
0..L
I I(1.
V1Th43'i
FILi:~.Lifl~ LXS'-~1 .0
tj/~.)~j'7,3 ~flji
I'.m
rnL'~I5 020
P11Lc216
--0 0
Va,4O2C
ruL 1 LUN
173.0
137.0
FILT=.402 EXP-1.0
VENUS
77.0
4/23/72 1002
-0
PRL216 020
g.venoac
.
8
ha
z-
8
. 0..0.70
.....
0.0
0.no
POSH7 1
VENUC~
rILTh.4C2
EXP-1.0
4/i3/72
1.
a7.0
1002
P14L216 020
-0
VenOPC
75
>.co
VE6.0
97.0
73.0
VENUS
FILT=.402 EXP-1.0
4/23/72 1002 PRL216 020
8~
8
(-
z
.M
tIj
8
8
a~m
7u
nas
otwo
7
P7.0
00.0
Fil T=.4ti2 EXP-1.0
4/23/72 1.012
PHL216 020
-
IM.-
VENUSJ
FILT=.'I02 EXP-1.0
0.2uP oIee12
'/23/72
1002
IrFL216i 020
O
.
67.
FilT.m.(Th,2 EXP--1 .0
4/~23/'12? 10J2
020
FAL.216
rL 600-
-0
77
Bn9
z
9 .a
o. io
Go
ol w
o~o
0.110
d. -M
DOS5IT ION
d.so
137.0
9.0
I1.0
IILT=. 1102 EXF-1.0
VENUS
'&/23/72
1.002 12AL216 020
vemaoam
8vBu
f-7.1--.-----------
9J~o0.10 0.~1
fly)
fl.1~POS 17
1
ONt~1
7~0.J
vIt Y.';
09
AM;3. L'
i r..n
)fl?.rs
IM.0
FIL'I'--. 110? ['Xl'-. (13
FAI
PRI.P.17 023
v~emOA
78
8.Lu
81
:81
'.oo
0.10
.o a
o. W
M~.0
7.0
VENUS
POSITION
.
.5
.io.70
o.o
'w-
-.
0
lES.o
FILT=.402 EXP-.03
4/24/72
947 PRL217 023
z
8-
In
P~.0
V'(45
~. ELM
U.1'1)
T 1N
4/24/7P
157.
,3
£47 PRL2J17 023
79
8*
lLi
8.
I'
8
CV. w
0.o 0
. 20
d.0
0.
a. w
so
Pc(SI TION
1.0
0. w
1-70
0.30
0-so0
I.c0
161.0
121.0
VENUS
4/24/72
FILT=.402 EXP-.03
947
PRL217 023
VEME0A
in-
z
zj
8
8
S2r1
DADO
PS
I
o
0.76
.0
20
117.0
-I".
VE NUS5
.3
1.0
N
FIVfIi.LT-r.2 LCXP-..03
4/241/72
947
PFIL217 023
-
vool"
80
137.0
51.0
VENUS
Ues.0
211.0
FILT=.402 EXF-.03
4/2'i/72
9L&7 PFL217 023
veft"O
/u(t
P)11.0
77.0
v['01-11i
Viii*~f'~ IiU;
.
1,1- Yt.O~ iWj1/4 ijtf7
I'lull' ( 123
81
8
z
-
coO
0.20
o.go
0.so
0.no
0.so
1.60
0.70
.
w
.o
2'.00
P1SIT1ON
)tus.0
Uas. 0
75.0
FILT=.402 EXP-.03
VENUS
4/24/72
947
PRL21 7 023
VD4Mo
8
8-
9.|
Ch.un
0.lo
a.e -nau
1,10" V.5 NOc
U7.;-
000
S1.n
tLco
181.3
2tUl.L
FaLO
VLtNUS 1
0.so
iil.: .4
D:P-- [x .039
/4/~/ f17 rL.217
23
82
8
%I-
2nR
81
930cc
~----I
0.20
I
0.~0
'.o
'.50
29.0
27.0
VENUS
FILT=.56I EXP-.20
d.so
POSITION
D.)o
.?o
.w
.so
W5.0
MID.
4/23/72 1011
FRL216 027
~8.
.
8-
98.m
23.0
23;.'J'
T~
O.r'LI
-~~~1--~
.LO
u.roi
Co.(
P(Y31
1.o
0.70 1oo O.N
T
PRL216 027
(sNs59
-O
83
141.0
115.0
77.0
FIL7=.564I EXP-.20
VENUS
4/23172 toll
PRL216 027
-0
ve6Sa
i'.inl
141-0
V1-OS~1
.
--
-
~.-
T--
G-I-'.O'm g
tj~g//
11
r1L216 027
84
POSITION
IS&o
57.0
65.0
ee.o
VENUS
FILWT.564 EXP-.20
.UU~~~
~ I M),0
4/23/72 1011
FRL216 027
71 W 5.01.3 1.00
Uii.Ll
I. I.% IJUJ .I
lr.eio
1'.IJ
VIUUi
.|=00 Ex'-20
4/r>-/-2 1111 Ii
IL216 027
-
85
Vo.)C..AU
9b.w
o.o
0.50
o.so
POSI TION
0.1o
o
0.70
o.l.ao
t'. o
29.0
as.0
FILT=.S6q EXF-.20
VENUS
4/23/72 toll
PRL216 027
-0
z--
S.
*b,1ni
.co
0.3O
ry~r1
r.y'
0.rio
0.70
0.UO
0.9o
100
171.0L75.0
17.1
63.0
VDUS
11
PRL216 027
-0
86
VFts
M7.0
a
81.0
0J&I4R
L
IU1.0
VENUS5
EXI'-.20
FIT.~
4/23/72 ltl
rAL216 027
-0
uj
10
111U
9~o
VUNU5.
OL'O
L7--.. r'4r
.~JJ
r
-.03
.
kl'
-l~~72
T
0.60
0000
T011
0.70
MPL219B
a~i~
110
0.9
i~
1.0
vtvwio
8?
VENUS5
FILT=.906 EXt~-.03
'1/25/72 0000 FARL219 110
MEel5A
w
F-
117.0
vPjlj(5
.IZ Ga0D
nAu05
V Ft'J~3
l'LT=. 5,5
I'Xr'-. 03
//?
000~f)
, P14.21 9 Ito
Vr.mSDmA
8/
8-.
8J,
8-
8
.ow
0'.10
o.o
o.so
o.3o
o.ao
.70
POSIT ION
119.0
0.S
t'. o
-1.00
87.0
139.0
FIL7=.906 EXPA-.03
VENUS
4/26/72 0000
PRL219 110
VM,5a
I-z
.
0.10
9.00
Vwit
VDUS
0.
o.3
FILT:-.06
0.110
0.!71
0..0 PTSw
FITZ 11-
^Xi'--.03
o.sgr
0.70
0.50
1
iOO~L1
/237
4/Lr5/712 C00 PRL21 9 110
0.Do0
001
-D
1.00
,,
nU
VDoMW
89
0.0
o.a
i0'.30
-
.-
ir--
0.1o 0.50
.
O.60
0.90
PMSIT ION
FILT=.906 EXP-.03
VENUS
0.90
1.00
,1.0
4/26/72 0000
FRL219 110
8.
.
8
cb.c
~
0.10
0.20
0.3
0. 0-
0.6b
.70
0.80
Ctr05- I w
3.0
14);.t]
VLl 11S
157.0
4/? UJ/72Q O010*RI. 219 2 1.0
90
Mew
8
z..d
1*J
8-
RI
.0~ 0.30
0.10
.1o
127.0
117.0
d. so
POSI TION
.Go
0.o w
.m
.Lo
103.0
FILT=.906 EXP=.03
VENUS
4I/26/72 0000
PRL21 9 110
v'EEne
I-J
8
SLO-10.11)
.. r
0..U
- - -
U.'.Ju
1-
0.4W
0.'./1
- - -- -
0.t0
- - -
0.'O
-- T -- - -- ---.-
- --
0.t0
.
1i'13.0
V 1 '. i
- - --
1.t
n-/.j.I
FILT
.M EXIw. 03
4/i/712 L(100 PML219 110
-O
voeren
C'b'.co
0.'.
0.50
o'.Ao
0.80
0.70
P1OSITION
1as.u
0.8o
.00
oao U
212.0
FILT=.948 EXP-.03
VENUS
4/26/72 0000 PRL219 114
S
vefnenl
S
S
8
.......-------
o .lu
G.20
a
.u.4 . !.]0 0.70
0.00 'D0.9
1.noi
W5.o
nn?. n
11).0
V1.flS
FLk.9 ~IF3[Xl. 3~ 42(i/72 0.00
PRI L219 114
POSITION
1s.0
dlo
.o
0'.7
1.00
97.o
117.0
VENUS
FILT=.948 EXP-.03
4/26/72 0000
PRL219 114
veesm
0r
0.30
0.40L
P.50
0.60
0.70
0.80
0.90
PLT;S I il
1.00
oNn.
n
13W.0
VPtJ IS 1
FILT:=.!4
1:IXf'..03
41/26~/72' 0000
PRLP19 114
-0
.
93
1'.00
PMSIT1ION
133.0
12B.0
VENUS
I.IUo
PRL219 114
4/26/72 0000
FILT=.948 EXP-.03
in
101.0
131.0
.
).fn
O.
o
.70
0.0
M
IS)A
;aE
VENUS
0.90
FI'
1 . r E +.0(3
4I/26/7? 000
PRL219 114
94
VENAea
....
..
0....
-
...
-
-
0'.50
-O
.POSIT IN
137.0
07.33
a. w0
.60
1.00
157.0
1111.0
. FILT=.948 EXP=.03
VENUS
4k/26/72 000
PRt.219 114q
rvew4
.0
0.10
0.00
u.'0
0.40
0-50
O-60
0.70
0.1f
n9
1.00
POSIT10
.
147.0
ViI lji)
163.0
FILT:-.-4 E0im.1 4/2jG/,' 000
PRL.21B 1-14tt
S
xL
6-1~
111.0
0.10
YxON
tOM,.0
VENUS
FILT=i.9tB EXP=.03
4/26/72 000
PRL219 I I
S
v~nms
S
8
8-
~~1
-- V------I
--
*~--------.
T
I V).t)
ti.'~;. ix
1M~.0
VII J.13
tl/ A-V*11 ' C1001(lb
FHL219 ItO
96
'a.
POSIT ION
)t47. 0
VENUS
FlLT=1.00 EXP=.03
q/26/72 0000
FRL219 Ile
-0
~0410O8
B
8
8
z
li~J
zI-
'8
8
__
9~.oo
203I
0.3G
117.0
1U9.D
FRA'"I.00 [--Xp-.O'i
(M.0 FRL.219 1to
-0
VENtC00a
151.0
127.0
119.0 1113.0
FILT=1.00 EXP--.03
VENUS
4/26/72 0000
PRL219 118
0.
0.
VENio00
8
z-|
8
b. w
n. to
o..u)
D.11
f.20
ira. n
1i~t. Li
0.Uo
0.90
1.01
14, 1.1)
ILA :-.
i.(InF Xt.03 1/.1//p
0 0 PRL IqI l
VEwtcxi
P057104
156.0
FILT=1.OO EXF1-.03
VENUS5
0.10
4/26/7' 0000
13.
PrL219 11.8"
aO
PO 71O
lu!"u
VENUS
VEULI~i
Ll:. I MIEXP.
tl/Lu/P JO
I"'AL.21!3 110
--D
99
veton rm
.
8
8
to
-
cb oo
0'. to
o'.eo
O.30
o'o
159.0
o'.so
M171N
0.so
o.o
107.0
157.0
151.0
VENUS
.90
4/26/72 0000 PRL219 118
FILT-1.00 EXI-.03
VeNID00
8i
8.
cbm 0.10
0A.2
01~0 0.10
Irm.
11J/.0
().R;
Tom
POSI At G
17..0
FIL.T.t4.00 EXt'~.03
4/26/72 0000
PAL21
I1t--
.71 080 09
100
VCrmois
ru-i i i UN
137.0
103.0
-
VENUS
FILT=1.0S EXP-.12
4/26/72 0000 PRL219 122
-0
VB41055
8
8I
ii
cb~
.c031r
ii
1Y4.0131.n
lus
va
I'l IL I T=.0l EX--. 12
PY)S
T
ou
0.10
0.7
0..
3a13
N07.0
4/26/72 0000 P3R-L219 122
-13
Pu.00
O
101
vwtoss
.00 0.10
0.70
5.0 '.80
0.go
P0317 ION
Iu%.u
0.90
0.t0
.o
137.0
IP.0
VENUS
FILT=1.05 EXP-.12
4/26/72 0000
PRL219 122
vmtosa
8
8.
boo
I)
VWU5
o.in
o.ro
,o
0.wo
- .r~O
0.60
PSS
FIL'l::-1.IlEXff.12 1/26 72" 0000
0.70
oa
.co
0.00
a
a143.
t&,
IGN
FL219 122
-0
102
Vt14tose
POSIT ION
111S.0
153.0
FIL-T=1.OS EXfP-.12
VFNUS
'i/26/7P
uAs.0
OWtL FRL2IS 122
VEN I USA
ZoR
4*I.(
VC1 11.15
0. 11Q
o. L'
vu 'It
FX T;-.
130
0.1W
j; Yf'-. 1.'
~~10,.7
It/
2
.8
/7a '-3
rAULTI
122
.10
1.)
103
Voft058
'Li
8
0
S...--I
"b~
. t
0o.20
0.30
o.no
o.so
o.ao
o.*;
o's.9o0'
P SIT710
19.0
1.0
*
VENUS
FILT=1.05 EXP-.12
117.0
161.0
4/26/72 0000
PRL219 122
VENIO!S
-.
tz-4
89.
8
8
...----------
-- ~,
----
..-..
..
'
-. 1
DAG I
-
1-011
-
-
.011'3.
0' 1
'
-
-
0.7
-
-
0.9
-
--
0,9.
~
-~~~
1.00
16-1.1
161.UJ
i.
vr
I!V
rf A ~-t
.r'
.1f5-.1
't/25/7 1)(11r PRL219 12?
.LV 1+
X -
z-
8
.bo
0.10
0.20
0.30
0.010
15/.0
FILT=t.OG EXP-.12
VENUS
0.50
0-so
0.60
POSIT ION
4&/26/72 00030 PRL219 122
z,-.
11.5
Iz
b
0.10
tr.
.0
U.a
0.
1..50
PG31IT f GN
.O
07.0031.00
o
VENUS '
r i L. T;-4 M VEI~t';
iIt
fi~
17.00
173.0
vYEian
117 .
0.90
F'ILZI
PAL219 fl?
126
105
S
'U
b-es
I
Si
QI
'.10
b'.D
.
o. o
o'. w
.0
119.0
l15.0
'.5
POSIT I N
do'
6'.o
a'.l w
1'.1o
131.0
VENUS
EXP-2. 0
FILT=HB
4/26/72 00003 PRL219 126
1.
9.0 0.10
0.30
0,40
121. 0
0.0
FDST I(N
.60
0.70
0.00
0.90
00, n
g1".0
121.0L
vEN
tI
FIL7=1171
i ~i2O ~
~
4/G7
10
O pr
PrLt13 12G
-0
106
VD*48s
z-
CT.D-
0g .10
'.ao
0.30
0.1o
0.50
0'80
70ru
0'.0
~
1~0.80
-
0.90
--
-e1
POSITION
VENUS
FILT=HB
EXP-2.0
4/26/72 0000 IRL219 126
-D
VEJaA
8i
I-
r.n, 3n oI1
i
9.0
11jt).n
vEl n'S
Fil.Te~ii EXP-20 426~/ 0100 t'RL219 126
107
cb
I*4a
B
B
vte.aw
cbo
6
o'.go
n.s0
0'n
o'.so
o.50
o.-o
0.80
o'.s
t'.00
O.1
POSIT IGN
VENUS
FILT=HB8
EXP-2.0
41/26/'72 0000
r
--- r----
u.o
a
n
1-,
PRL219 126
-0
-. ~0 ~ ~ .0~
101.0
vENt i
Ll:'H't
'"
/;,/72 -t.!t
IRL219 126
1 (y4
vW~IA
99.0
131.D
VENUS
FILT=HB
ilV0.3n
EXf'-2.0
'1/26/72 0000
FR1219 126
0 0
0.11
PSSTIIIR
r
I
(.,i --t iti
a
111;:161*74Z,
fjuclt
t 11.1.219
1;?(-)0
VENtt1s
'
'
0~t1
"
coeo
VENUS
IM
~~~W~~~~oN
-ZAD
POSIT10ON
1b5.0
1V.0
FIL T=l.10 EXP*-1. 2
133.0
1es.a
4/26/72 0000
-
FRL219 130
vtNLtos
Z
ILJ
b~42
ei.0
.10
0.20
J.30
(.'10
U.D
71 ONI
0-.)
.*0
167.0
VELU ltl',
FIL
l.10- EXIP-.I.( FRK'l9
PRI 2?19
1.0
0.80 U..0
15
1390
I'.
.
110
VEM1IIg
169.0
' ".'
1e.0y
VENUS
'J"
FILT=1.10 EXP-1.2
4/26/72 0000
PRL219 130
-0
8
VENIto
8I
/
8
8.
O
93.~0
-~~~~th
~~~~~T0At
0JI
0.1Wu
PG(SI T If
0
0.s
0.20
(L80
0.90
171.1
VEN*
ILTt. ; -10 t
'XP-. I/'e/7' 01() pit!
M19 130
-o
1.100
13.
VENt108
13.0
'
'1
lug. a
taso
FILTot.10 EXP-1.2
VENUS
VEN
4/26/72 0000
PRL219 130
-0
.10m
8I
IT; 0
/IL
.15.
VOU5
u
FILT, l.10 EX -.
4 / LY>j/7 0:10 p -,ic
F8L.2149 130)
-1)
~iEWUU8112
8
-
VEN110Bw
8
181.0
111s.0
FILT=t.10 EXP-1.2
VENUS
PRL218 130
4/25/72 0000
-D
8~~o
51
0.10
0.
Ev
0.31
a.1
0
0.7
.0
5.90 1.
ate0
8.).
'0.10
0.e!0
r~~sP~3rION
0.se
0.11a
(a.B)
0.70
0.80
0.i0
151.
VNIlis
t.00
t~
-17.
FIL T=z.10 EXPN-1.2
4-/26/7
0000
PRL219 130
-0
113
VIDA Ioft
tLJ
t42
8L1
d.o e
'-
'
o.sa
0.oso
POS ITION
11.0
'-
0.wo
d.2
d.so
0'.90
t00
I'm.,
1~3.0
VENUS
FIL T=1.10 E"XP--.
2
4/26/72 0000 PAL 219 130