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NASA TECHNICALMEMORANDUM
NASA T14-82449(NASA-tit-82489) KOHOU?BR, PHOTOBXTSIC 282-15007P402061APRI UP.ERIBINT (5233) Final Report(6181) 35 p BC ,031BY A01 CSCL 038
UaclaaG3/91 08578
KOHOUTEK PHOTOMETRIC PHOTOGRAPHY EKPERIMENT 6233?FINAL REPORT
C. A. Lundquist and P. D. Craven
Space Sciences Laboratory ^23Q5A
► ^ yO lh' ok 4r is pO wV^ ti
October 1981
NASA
George C. Marshall Space Flight CenterMarshall Space Flight Center, Alabama
WFC • /em 31" (Row Jww 1971)
1 ' W- _ - -
NASA T*.UWIL WARCHMEWWWAAM A&
4. TiTIA Apo IVW" L1t s. a^GAVIROctober 1 1
Ilk
i^tehi Pho etric Photography Experiment (5233) •.
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C. A. Lvnftist and P. D. Cram& PHMQRMlft OWPOISAM&M1 VPM T
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George C. Marshall Space Flight Center I I. COW MA" OR sun *,liarshal l Space Flight Center, Al abwr 312
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i:. 8000401106 A4MCY MAW MO AAQq MTechnical Nemoraafw
National Aeronautics and Space AdivinistrationWashington, O.C. 20546 14. SPOI!#O111MM AGENCY
1s. 8WftR MSI MV mom
Prepared by Space Sciences laboratory, Science and Engineering DirectorateI& ABSTRACT
This report presents the final results of the Skylab 4 experiment S233,Kohoutek Photometric Photography Experiment, which undertook is series of visiblelight photographs suitable for photometry and for a photographic history of CometKohoutek, The report explains the experiment c_crcept, the data reduction Method,and the results obtained.
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17, K" WORDS is, OISTRIMUTION STATEMENT
Comets Unclassified — Unlimited
Kohoutek
Photometric brightnessComet photography
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.
TABLE OF CONTENTS
file
I. EXPERItENT CONCEPT AND EXECUTION ................................ 1
II. PHOTOGRAPH STATISTICS ........................................... 2
III. COMA WMITUDE ........, .......................................... 13
IV. COMET TAIL ON DECENBER 22 4100 .... . .........................0.041.. 17
V. CALIBRATION OF MAGNITUOE ........................................ 22
VI. VIGNETTING .................... .....a ........ a ... a ... a ...... a.... 25
REFERENCES ............................................................ 30
1 ,
iii
Figure No.
1
2
3
4
5
6
7
8
LIST Of ILLUSTRATI0NS
Title Page
Comparison of 5233 results with the best-fit curvesdeveloped by Deutschmann for ground-basedobservation data ....................................... 1$
Comparison of 5233 results with the best-fit curvesof Kleine and Kohoutek ................................. 19
Comet Kohoutek in" from frame 6889 ................... 20
Digital representation from frame 6889 of the exposurevalues in the comet image after correcting for back-ground and vignetting effects .......................... 21
Density histogram for frame 6946 (Marshall scan) ....... 24
Reference stars and best-fit calibration curve derivedfrom them for frame 6779 ............................... 26
Reference stars and the calibration curve derivedfrom them for frame 6911 ............................... 27
Contours of the intensity pattern caused by vignettingthrough a Nikon lens similar to the one used forComet Kohoutek photography from Skylab ................. 28
. ,
LIST OF TABLES
Table No. Title Page
1 Exposure Sequences ..................................... 2
2 Photograph Characteristics ............................. 3
3 Related Data for All the Frames from Which a CometMagnitude Was Obtained ................................. 14
4 Comparison of the Magnitude Obtained from Skylab withthe Best-Fit Data of Deutschmann and Kleine andKohoutek ............................................... 16
iv
KOO= P! }T ET IC PHOTOGWE RINOff (S233)FIB. EMT
1. EXPERIWNT CONCEPT AND EXECUTION
The Kohoutek Photometric Photography Experit, S233, assigned to theSkylab 4 mission, undertook a series of visible light photographs suitablefor photometry ed for a photogra!=c history of the comet. This concep-tually side experiment evolver, U om a July 3, 1973 0 hM Neakpartersrequest to the Narshell Space Flight Center and the Johnson Space Centerfor an assessment of a program of Comet Kobe" observations utilizingexisting Skylab sensors or other instruments that could be_available intime for Skylab 4. One possible observation identified in response to thisrequest proposed the use of existing cameras to take comet photographsthrough the spacecro rlt windows. These observations were included in a setof new and amended experiments for Skylab 4 accepted by hMSA on October 23,1973. References 1 and 2 provide a sumeary of the various observations ofthe comet from Skylab.
The caoera available for the S233 photography wes a 35-m Nikon camerawith a 55-mm focal length, adjustable focus, f/1.2 tens E33. The field ofview was 36 by 24 degrees, which yields a 1.04 degree per mm image on thephotographic film. This film format seemed appropriate, inasmuch as a longcomet tail was expected. Also, camera pointing was to be accomplishedmanually by the Skylab crew, and an ample field of view was desirable toaccommodate pointing uncertainties.
The film selected was Kodak Plus-X Aerial 3401 on a thin base. Thechoice was made on the basis of availability, resolution, speed, radiationeffects, and other pertinent factors. Four cassettes of 60 exposures percassette were provided for the experiment.
The standard observation sequence adopted is shown in Table I. Theexposures focused at 15 ft produced a slightly out of focus image of thecomet and surrounding star field. This was done to insure that stellarimages to be used for photometric references would not have saturated coreswhich could have precluded accurate photometry. Based on premission tests,it was expected that for a 60-sec exposure focused at 15 ft, the fainteststar recorded would typically be 6-7 magnitude. For a 120-sec exposurefocused at infinity, the faintest star would typically be 9-10 magnitude.This sensitivity was considered adequate for the predicted magnitude of thecomet. These limiting magnitude values were obtained on the flight film.
ARD OBSERVATION SEQUENCE
60-sec exposure 15-ft focus
120-sec exposure infinity focus
60-sec exposure 15-ft focus
CALIBRATION SEQUENCE
Unexposed
10-sec exposure 15-ft focus
30-sec exposure 15-ft focus
60-sec exposure 15-ft focus
120-sec exposure 15-ft focus
120-sec exposure infinity focus
A calibration sequence of exposures, as shown in Table 1, was per-formed at least once on each roll of film to allow an observational check
of the density-versus-log-exposure curve for the film. Preflight and post-flight standard density step-wedge exposures were added to the film in each
cassette. The density-versus-log-exposure curve used in data analysis came
primarily from the step-wedge images which were added postflight.
The operation plan for the experiment called for a standard observation
sequence every 12 hr when possible during the Skylab 4 mission [4]. Thishad the objective of producing a uniform set of low resolution comet photo-
graphs. If obtained, such a set could serve as a reference record of the
gross changes in the comet appearance and magnitude.
After the successful completion of the Skylab 4 mission, the S233 films
were processed in the photographic laboratories at the Johnson SpaceCenter. The useful photographs were then identified by the investigators
at the Marshall Space Flight Center. Density values for these photographs
were subsequently measured with a microdensitometer at the Johnson Space
Center. These density data are the basic information from which the re-
sults discussed later are derived.
Of course, many details must be handled with care in the course of data
processing and analysis. These detailed topics, such as background cor-
rections and vignetting, are reviewed in the later sections of this report.However, the broad description of the experiment concept and execution
given in this section is sufficient to introduce a discussion of the re-
sults obtained. these are discussed in the next sections. Readers who are
interested specifically in how the results were derived can examine the
later sections.
II. PHOTOGRAPH STATISTICS
Table 2 characterizes each photograph from the four film cassettes
returned from Skylab 4 for the S233 experiment. Thirty-five standard or
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ORiGINAL PAGE IS
OF POOR QUALITY
calibration sequences recorded the comet successfully. Typically, the
Skylab attitude was being held inertially fixed during these exposures.
This distribution fell short of the goal of a sequence every half day
?g but, nevertheless, provided some interesting observations. The successful
' observations after perihelion were especially scant. When attemptedi1
sequences failed, the apparent reason is given in Table 2. The table indi-
cates with an underline which photographs were measured and analyzed. Most
of these were focused frames. This choice followed from the postflight
recognition that the comet did not become as bright as predicted during the
preflight planning, and saturation of the cores of stellar images was not a
significant problem. Use of the focused images gave a larger number of
` stars for reference and better signal-to-background ratios. When more than
I
one photograph in an observation sequence had comet images, only the best
frames were completely analyzed.
III. COMA MAGNITUDE
One result from the Comet Kohoutek photographs is a small sequence of
visible light measurements of the stellar magnitude of the comet coma. The
interesting topic that r ► ic3ht he addressed from these measurements is themanner in which the cola mndgnitude increases as the comet approaches the
Sun and decreases as the c":iot recedes. Conventionally, such data are
reduced to a constant Earth-comet distance (1 AU) and plotted versus the
log of comet heliocentric distance in astronomical units. When so dis-
played, the pre- and postperihelion curves may show a systematic displace-
ment for equal heliocentric distances.
Table 3 gives the result., of a final reduction of the successful 5233
observations. Except for the Nosorvations on Dore, ►her 2?, the data wereprocessed using digital compu'•., ►- .:r'es developed ii connection with theS233 experiment but designed to hdve Broader appl ico))i 1 ity to suhsedue,,it
problems of a similar nature [5].
One column in Table 3 gives the number of referew.e stars selected for
each frame to derive a calibration curve of stellar m;Jnitwle versus the
log of the summed image exposure. Visual stellar -magnitudes from the SAO
Star Catalog [6] were used, and stars selected were 1 4 1ri!.0 to spectral
classes F, G, and K. These choices correspond closest "o the expected
spectra of the comet and to the spectral response of the film-window-lens
system used to record the photographs. The magnit!uie-versus-log-exposure
curve then allowed a determination of the comet magnitude from the summed
exposure of the comet image. Table 3 also gives the magnitude range of
reference stars. In all but three instances, the comet magnitude was an
interpolation from the reference curve. For frames 6889, 6890, and 6916,
r extrapolation was necessary. Frame 6916 also had the lowest number of
reference stars; therefore, the determined comet magnitude is somewhat less
reliable for this case than for the other frames.
13
H^ NL^ ^! W O^ 1C N N O^ 10 N ^ 0^ m P'1 M r
d K
^n^n v v ^n ^n a •a, ,n .a o o a M .p
www^o
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N ^p ^p M O^ ^O N r to N
^O 10 to an U1 1n M1 U1 1n a ^ ^ M N ^D
{V p1 O '^i H r •' 1p M O V a N N m O %0h h h a; h m m m m r r h m1 1
CID1 1 1 1 1 1 1 1 1 1 1 1 1H'yyy ^ ^ RI m N m m m M N M N m m O m 1n
U' J Q a N 4 M N N N M 'Q M M M M M M ^}
%D OD N min
M V' n ON V N %D O% O r U1VJ p Hh1 ^
5
N v N n U1 N" M V V M M N N
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^ zsa
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_O ^_Q E \ \ \ \ \ \ \ \ \ \ \ \ \ \ \
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14
The observations on December 22 (frames 6889 and 6390) required special
treatment. They were taken under difficult circumstances -- only 6 days
before perihelion and 6 days before the cornet's apparent least solar
separation as seen from Earth. From Skylab, the comet rose only 3 min
before the Sun. Under these circumstances, some scattered sunlight from
the Earth's atmosphere on the horizon was illuminating Skylab, even though
the comet was somewhat above the horizon. This illumination scattered off
struts holding the Skylab solar instruments. Because these struts were in
the photographic field not far from the comet, the scattered light resulted
in an appreciable gradient within the background recorded around the comet.
Also, the comet image was near the edge of the photographs. Under these
peculiar circumstances, the computer codes used in the routine analyses
Were inadequate. Instead, the background was modeled in three distinct
regions by a linear function of the row and column coordinates of the
digitized data. This modeled background was subtracted from the comet
data.
In those cases, such as December 22, when an appreciable tail was
photographed, the coma in the tailward direction was treated as a region of
extent corresponding to that occupied by the opposite side of the coma.
That is, for the purpose of coma magnitude determination, the coma was
treated as a symmetric region.
The measured magnitudes from Table 3 can be compared with models of
coma magnitude-versus-heliocentric distance derived by other authors. For
comparison purposes, two typical models are used in Table 4.
The first model is due to Deutschmann [7]. As his preferred model, for
9 heliocentric distance, r, he gives:
Preperihelion
M = 5.95 .r - 0.92
Postperihelion
M = 6.86 ,r - 0.50.
This magnitude is tabulated in Table 4. For comparison with the obser-
ved magnitudes from Table 3, an aperture correction as applied by
Deutschmann must be made. He adopted -0.066 mag cm- 1 for refractors, which
results in a -0.30 magnitude correction for the lens of 4.6-cm aperture
used in the observations here. In Table 4, this correction is applied to
the Table 3 values, and differences between the observations and model are
shown.
Deutschmann also applies an observer correction to the data from each
observer. To examine this possibility for the data in Table 4, the
observations on frames 6PS9 and 6890 were excluded as physically not within
15
Ea4
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ao
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W u1 V1 ^ d' ^l1 tf1 ^ d' u1 c;' O O ^ M ^D3
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7
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16
the model scope (see later discussion). When an observer correction is
derived with the remaining data in Table 4, using the model values as a
reference, the observer correction is approximately ,± 0.1 magnitude, with
the sign depending on whether the questionable value for frame 6916 is
included. Therefore, no observer correction is applied. The small size of
this potential correction can be viewed as a favorable measure of the
analysis methods applied.
Figure 1 illustrates the Deutschmann model and the observations from
Table 4. The questionable value from frame 6916 is not shown.
A second model for comparison is one due to Kleine and Kohoutek [8].
They give:
Preperihelion
M = 5.11 + 6.38 log r
Postperi hel iun
M = 6.63 + 8.92 1 og r
For this model, an aperture correction, -0.037 mag cm- 1 , is specified bythe authors, which results in a -0.11 correction for the 4.6-cm aperture.
The values from this model and observed values corrected for aperture also
are given in Table 4. These are depicted in Figure 2.
The coma magnitudes for frames 6889 and 6870 are probably significantlybrighter than calculated from either model. Other authors have noted that
observations near perihelion were brighter than indicated by the various
models; for example, Jacchia [9].
IV. COMET TAIL ON DECEMBER 22
Two photographs made on December 22 recorded a tail cone 5 degrees
long. The comet image from frame 6889 is reproduced in Figure 3. Near its
end, the image of the tail is lost in the bright background near a dimly
illuminated spacecraft spar. Under more favorable circumstances, a longer
tail might have been detected.
Figure 4 is a digital representation of the exposure of the comet image
above background from frame 6889, after reduction using the appropriate
D-versus-log-E curve and camera vignetting curves as discussed earlier.
The contours in Figure 4 are drawn to show the extent u F the tail and someof the inner portion of the comet. Also shown at the same contour level as
that of the tail are contours of a known set of stars in the field.
The numbers shown in the figure are 100 times the actual exposure
values for each pixel after correcting for vigne t ting and subtracting the
M
17i
1
2
p 3f-zc^Q
4
5
POST- -PERIHELION
e
$ S233 DATA: O PRE—PERIHELION
O POST—PERIHELION
0
—0.6 —0.5 —0.4 —0.3 —0.2 —0.1 —0.0 0.1
LOG r
Figure 1. Comparison of S233 results with the model developed by Deutschmannfor ground-based observation data.
18
0 ! ! T
o S233 DATA: O PRE—PERIHELION
O O POST—PERIHELION
1
2
w 3d
ZC7Q2 4
5
POST—PERIHELION.,
6
0
—0.6 —0.5 -0.4 —0.3 —0.2 —0.1 0.0 0.1
LOG r
Figure 2. Comparison of S233 results with the model ofKleine and Kohoutek.
I
19
pRlC1Nhl. PAGE ISOF POCR QUALRY
Figure 3. Comet Kohoutek image from frame 6889.
20
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4 4 1 4 1 11 14 1 15 8 7 13 9 5 6 2 3 7 3 5 S 4 2 16 Ii I f 17 4 2 6 3 16 10 2 1 6 1
t 4 S 7 / 6 2 7 1 1 6 2 3 5 5 4 4 4 2 6 1 7 3 d 16 14 4 7 S
_ 3 4 13 2 4 2 1 1 2 4 3 10 4 4 3 5 5 9 < 1 12 8 . 3 13 5 7 1 2 6 1 5 2
5 c 6 1 7 9 14 1C 6 4 4 1 1 3 5 7 12 12 2 6 5 2 1 1 6 14, 1G a 2 a
13 E 2 < < 3 t a 1C t 2 11 Y 9 5 3 1 3 13 1 5 7 5 5 3 2 7 7 11 14 5 5 4 5 2 10 9 t 6 2
5 - - 4 4 3 5 20 16 1 2 4 6 4 S 12 . 2 1 13 1 1 4 3 5 1 • 5 2 8 7 9 6 3
4 2 i 7 it ll t 4 4 13 5 1 2 5 7 7 6 5 1S 15 4 6 7 IC 7 1 10 17 12 4 4 4 l4
4 1 1 1 [ 4 11 S S 5 5 6 4 2 12 15 1 4 2 a 10 5 3 6 4 20 18 4 11 _ 5 2 11 S 3 5 a S 12 12 11 13
IC ll 3 2 4 15 d 1 7 11 7 7 2 14 10 3 3 9 6 < 1 5 3 3 2 17 17 t a S 7 8 13 a 13 4 9 8 5 2 4 14
1 1 4 43 1 6 8 1 1 4 10 7 10 5 12 4 11 1 3 14 7 6 9 8 11 13 10 4 4 4 6 5 2 4 1 6 6 8
1 e t IS 13 t 3 1 I3 3 22 9 6 1 9 4 6 4 8 1 12 14 5 5 13 19 13 3 10 14 7 a 5 . 3 S 17 16 5 3 2 6
1 11 S 5 16 i4 l4 I4 Y 9 4 14 10 8 2 < 6 4 11 8 1 5 3 7 1S 25 8 3 S 5 6 4 6 5 IC 10 4 1 4 5 12 11 8 5 9
16 21 6 t . S 5 S 5 5 4 14 1^ 3 11 5 4 8 4 1 1 9 2 13 iJ 3 S 4 4 9 19 19 2 9 5 4 1 5 3 7 7 4 13 13 11 8 17 11 11 11
y 7 4 2 1 k 14 18 6 3 1J 5 6 2 8 1 9 5 2 1 6 1 1 t t lC 3 2 4 2 4 7 6 5 8 3 I a IO 9
4 S it 7 1 ii 13 14 4 0 6 i4 12 1 3 7 11 3 9 8 8 10 2 14 12 20 9 13 6 It 4 12 IC S 11 7 4 7 9 10 22 21 12 12 11 9 l3 it 7 19 14 6 6
I I S It 4 A. _ _ S It 7 t It 18 16 19 19 13 15 13 13 12 3 7 16 14 21 19 19 15 10 2 2 13 15 2? I3 23 17 It 24 It 17 21 S it 18 16 it 22 11 12 9 15
-14 IL 12 11 4 15 9 it 12 It 1 15 It 7 3 Y It IJ 10 It 1 16 24 18 2 2 19 28 14 14 10 8 17 15 16 it 2C 17 19 26 it 3C 31 21 21 32 34 29 11 13 If 30 35 35 29
7 6 t t 7 7 21 11 14 S S 21 36 It 21 14 27 43 28 18 13 8 20 23 31 24 16 11 17 38 23 19 30 28 33 21 18 22 2S 23 23 35 35 41 31 Ze 40 36 31 26 32 30 44 43
OR-GINAL PAGE IS OtiT FRAM.fbF POOR QUALIT Y
^DFigure 4. Digital representation from frame 6889 of the exposure values
in the comet image after correcting for background and
vignetting effects. The values shown are 100 times
the actual exposure values.21
background. To convert to radiance in 10th mag stars/degree 2 , one
should multiply each number by 1.53 x 102 . This value includes the
factor of 100 mentioned previously. (Each pixel covers 6.78 x 10-4
degree2.)
V. CALIBRATION OF MAGNITUDE
The procedure for calculating the comet magnitude from each frame takes
place in four steps. In step 1, the conversion curve from density to
exposure (i.e., the density-to-log-exposure curve) is determined. In step
2, the background exposure around each reference star to be used in the
calibration curve and around the comet is determined. Step 3 consists of
finding the signal (i.e., the sum oft background-corrected exposure
values) for each reference star image. Step 4 is the calibration of the
full frame and the determination of the comet wagnitude. This consists of
fitting a straight line to the reference stars and then calculating the
comet magnitude using this line.
All the densities were measured with the Optronics Spec Scan 3000
microdensitometer at the Johnson Space Center and were recorded in digital
form on magnetic tape. One frame, 6946, also was measured subsequently on
the Perkin-Elmer Micro 10 microdensitometer at the Marshall Space Flight
Center. Data from the Marshall scan for this frame are quoted in this
report, although the difference in the comet magnitude calculated from the
Johnson and Marshall data sets is small. In all cases, a 25-um square
aperture was used to digitize the density readings, and each reading was
separated from its neighbors by 25 um in both the X and Y directions. All
subsequent manipulation of these data uses copies, also on magnetic tape,
of the appropriate frames.
The density to exposure conversion was made using a look-up table.
Each density value was converted to an 8-bit gray scale value. This was a
convenience for working with the IBM 360 and other machines with which the
data reduction was done. A calibrated standard 21-step Kodak step-wedge
image placed or each roll of the film postflight provided the D-log-E curve
frm which the look-up table was generated. These images were placed on
the film using an exposure time of 60 sec.
Since the background varies over the area of a 35-mm frame, a value for
the background exposure was found for the area around each reference star
image and the comet image. This area, A B , was normally a 1500-um square
area centered on the image (star or comet). The background was defined to
be the average exposure value of all the exposures in the area. All the
exposure values used in the average were first corrected for vignetting.
Density values associated with stars or the comet were excluded from the
average by limiting the density values to a band around the mode of the
densities in the area; i.e.,
22
I E (_ OilEB N
AB
Vij
where Vij • vignetting for i,j point, Dmin :^ Dij ! Omax, and N is theactual number of data points used in the average. Of the 3600 possibledata points in AB , generally more than 75 percent were used to calculate
a background value. Qnin and ;ax were subjectively determined from a
density histogram, such as shown in Figure 5, constructed for each area
AB. The histogram shown in Figure 5 covers densities ranging from 30 to64. For this area, grin and ;ax were chosen to be 36 and 42, respectively.
The total exposure value ET for a given image on a frame was found by
summing all the exposure values, corrected for background and vignetting,in the image. A rectangular area AM around each image is defined as the
image area. These areas are generally, but not always, centered in the
corresponding square area AB used for determining the background. They
also varied in size depending mostly on the magnitude of the object butalso somewhat on its position in the frame. A small area (A M << AB ) isused for the sum in order to reduce the residual error resulting from the
small difference between the true and calculated background and to exclude
signal from other stars and sources. ET is defined as
r E..
ET(Nd = jIl V - EB(AB)ijwhere r = the total number of points in AM,
E the exposure of the point at coordinate point i,j,V = the vignetting value at the point i,j,
i,j the X and Y coordinates of the point,
and ¢ i, a c.;unter for the number of star images. In determining the
signal from the comet, only values from the coma were used. The tail was
excluded from AMC , the comet coma area, by defining the coma as sym-
metric around a line perpendicular to the head-tail direction. The bound-
aries of AMc in the tail direction were chosen to be the same distance
from the coma center as the coma edge opposite the tail.
A calibration curve was defined for each frame using the E T and mag-
nitude of the reference stars in that frame. The reference stars were
identified using the SAO catalogs. The visual magnitudes from the SAO
catalog were used in determining the calibration curve. Stars selected
for reference stars were limited to F, G, and K spectral classes, as noted
in Section III.
The calibration curve for the frame is defined as the least-square fit
of a straight line to all the reference stars using the equation
23
usSHWOHOWJ
U_
Q2
U7
Ni
CIA$ ^1010^ N^1p^^1^^WP1^-^N^l90^^N^
i i i i i
..............................• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • •• • • • • • • • • • • •• • • • • • • • • • • • •• • • • • • • • • • • • • •• • • • • • • • • • • • • •• • • • • • • • • • • • • • • •• • • • • • • • • • • • • • • • • • • • • • • •
J
O^ Ny Nto ^
Occ 0
W00 S1
iO SW ~
t3t^^Q OW ZW CyuOi 0 8J Z ^W :E Q_J Z
W W O^^0JO WHQWS¢^e. 3x
N WIr ZOO W W 2OQ m=QOCC Ox Q
Cu-SJZ V. W Z
W W W = ^Oao Z M- 3S J ;
0 ui W0 ON O W m
24
log ET(AMd - amt + b
where mt is the visual magnitude from the SAO catalog and a,b are constants
determined from the fit.
Figures 6 and 7 are examples of the data and calibration curves. The
comet magnitude is then found by inverting the preceding equation,
log ET(AMC b
me - a - a
The values found from this equation are given in Table 3 as the "measured
magnitude" of the comet. Crosses in Figures 6 and 7 mark the cometmagnitude on the calibration curve as determined from E T for the comet
for frames 6779 and 6911.
A measure of the error in this method can be given by the value of the
root mean square (RMS) of the standard deviations of the reference star
magnitudes from the several calibration curves. That is, the RMS repre-sents standard deviations of the individual differences between the magni-
tude of a star as determined by the calibration curve for an individual
frame and its value as given in the SAO catalog. The RMS standard devia-
tion call
for the frames used is
call ° 0.2.
Thus, on the average, any star's magnitude can be calculated to within 0.2
using this method.
VI. VIGNETTING
Direct measurement of the vignetting function of the specific lens used
for these photographs was not possible. The lens was left on board theSkylab workshop, and sufficient time was not available for such measurement
between the inception of this experiment and launch. Fortunately, measure-
ments of the vignetting function for several similar lenses had been made
for investigations on Apollo flights, in particular the Low BrightnessAstronomical Photography (S211) investigation for which R. D. Mercer was
the Principal Investigator. These data and how they are obtained are de-
scribed elsewhere [10, 11]. From the data, Mercer c_arluded that there was
little difference in vignetting patterns between the same lens type. We
agreed with this conclusion and, thus, decided to base our vignetting cor-
rection on a single data set. We chose the 180-sec exposure frame taken
through the Apollo 17 lens [10, 11] and a blue filter in cnle.r to obtain
coverage over as much area of the 35-mm frame as possible. Figure 8, takenfrom Alvord [10], shows contours of the intensity recorded on that frame.
The contours indicate the vignetting pattern used for the data reduction
25
0►
E
t
iN
tN
L4• NN^ O0! L> L7rL OJ
"D +-+
4u
L
u dc oo c
ar
bL NW r
C^m Ou r4 r
XW
4- Od
N }tJ tL 0)
^ uO C
IV 07t
N F-Lt0
N 01n
Ol 1^u %0ca a^L E
to-4- LW 4-O:
S-o
.4-
OJL7Im
I LL.
I 1 I 1 ^ 1 1 1 t I 1 1 I
N ^' O O O A IC 10 • A N ^" O3aniINJVw
26
N O a • 1% •to10
Z%J"J.IMUVWW
27
w ► uvK 4U^~(Y,
Figure 8. Contours of the intensity pattern
caused by vignetting thro l,gh a Nikon lens
similar to the one used in thisexperiment [10).
28
_ "
here. It should be noted that the blue filter had no effect on the vi-
gnetting pattern of the lens.
To simplify the procedure for vignetting correction and to reduce the
computer core storage requirements, smoothed exposure data from the framereferenced previously were fit with a curve of the form
V - a+BR +YR2.
To model the vignetting pattern, R during the fitting process was the
distance from the pattern center to the point in question. To compensate
for a difference between the enter of the vignetting pattern and the frame
center, the X and Y offsets were two other parameters (five in all) which
the computer program varied to find the best fit to the data. In applica-tion, however, R was used as the distance from frame center to the point inquestion because there was no way of knowing if an offset existed for the
actual lens or how far or in which direction to offset the pattern.
For the data of Figure 8, the constants are:
a - 1.9198,
B - -0.6861,
Y - -1.0032.
Since there are slight differences in the vignetting pattern between
lenses, one might expect a systematic error between the reference star magni-tudes and those calculated from the fit curve. Using scatter diagrams of
(M mea ured - M SAO versus R, no consistent systematic effect was found.
ThereTore, errors resulting from not using the exact vignetting pattern are
small.
29
REFERENCES
1. Snoddy, William C., and Barry, Richard J.: Comet Kohoutek Observa-tions from Skylab. The^Sk lab, Results, Vol. 31, Part 2, Advances in theAstronautical Sciences, Astronautical Society,, 1975, pp. 871-893.
2. Snoddy, William C., and Gary, G. Allen: Skylab Observations of CaretKohoutek. Scientific Investi gations on the Skylab Satellite. Progress iAstronautics and Aeronautics, Vol. 46 (Eds. M. Kent, E. 5tum inger, andS. Wu), American ns u e of Aeronautics and Astronautics, New York, 1976,pp. 237-249.
3. Craven, Paul D., Hembree, Ray V., and Lundquist, Charles A.: Photo-graphic Photometry from Skylab. Comet Kohoutek, NASA SP-355 (Ed. GilmerAllen Gary), Proceedings of a Workshop HeTT at MSFC, June 13-14, 1974,pp. 183-184 (1975).
4. MSFC Skylab Kohoutek Project Report. NASA TM X-64880, October 1974.
5. Barr, W. C., and Lybanon, M.: Program Documentation for Comet Kohou-tek Data Reduction. Memorandum Numbers 5E3010-1 through 5E3010-19, Com-puter Science Corporation, 1975 through May 1976.
6. Smithsonian Astrophysical Observatory Star Catalog, Smithsonian Institu-tion, Washington, D.C., 1966.
7. Deutschmann, W. A.: An Analysis of the Visual Magnitude of CometKohoutek. Center for Astrophysics Preprint No. 135; also Final Report onContract No. NAS8-30544, August 1974.
8. Kleine, T., and Kohoutek, L.: Photometric Parameters of Comet Kohou-tek 1973 XII. Comets Asteroids Meteorites: Interrelations Evolution andOrig ins. (Ed. a semme University oToledo, o e o, o,ecertEer 1977, pp. 69-76.
9. Jacchia, Luigi G.: The Brightness of Comets. Sky and Telescope,April 1974, p. 216.
10. Alvord, G. C.: Image Processing and Data Reduction of Apollo LowLight Level Photography. Contract No. NAS5-20683, State University of NewYork at A!bany, Computing Center, December 1974.
11. MercE,, . R. D.: Final Report, Apollo 5-211 Low Brightness, Astronom-ic,il Photography. Institute for Scientific and S pace Research, Inc.,Delmar, New York, recember 1974.
30
APPROVAL
KOHOUTEK PHOTOMETRIC PHOTOGRAPHY EXPERIMENT (S233)FINAL REPORT
By C. A. Lundquist and P. 01. Craven
The information in this report has beencontent. Review of any information concerninnuclear energy activities or programs has beeClassification Officer. This report, in itsto be unclassified.
reviewed for technical
g Department of Defense orn made by the MSFC Securityentirety, has been determined
US/Ii.A/1 -W- '000-
J. E. KINGSBURYActing Director, Space Sciences Laboratory
31*U.S GOVERNM[NT PRINTING C ► "ICE 1981- 51 071/09