the intensities of spectral lines in the ultra-violet solar spectrum...in order to measure the...
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The intensities of spectral linesin the ultra-violet solar spectrum
Item Type text; Thesis-Reproduction (electronic)
Authors Phillips, John G. (John Gardner), 1917-
Publisher The University of Arizona.
Rights Copyright © is held by the author. Digital access to this materialis made possible by the University Libraries, University of Arizona.Further transmission, reproduction or presentation (such aspublic display or performance) of protected items is prohibitedexcept with permission of the author.
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Link to Item http://hdl.handle.net/10150/553612
THE IUTKESITIES OF SPECTRAL USES
IS tm OLTRA-VIOIZf SOLAR SPECTRUM
by
John 0. Phillipe
A Thesis
submitted to the faculty of the
Department of Physics
in partial fulfillment:oft■ .— .'
the requirements for the degree of % '■
v - : - . . . "..y/'■ 'Master of Science
in the Graduate College
University of Arisona
1942
2-_
B R A R
TABLE OF CONTENTS
<£9 79/ -/
2,
CHAPTER PAGE
I. The Table of Equivalent Widths . . . . . . . 1
II. A Statistical Study of the Table ofEquivalent Widths . . . . . . . . . .12
III. A Curve of Growth of Spectral Lines . . . . . . 28
Bibliography . ............................. . 40
Appendix (Table 2 . ) ...........................41
$
1 4 . 4 U 7
ABSTRACT
Microphotonoter tracings were made of the spectra on seven plates
exposed to the ultra-violet solar spectrum in the wave-length region
X 3650-5915 A at Mount Wilson, All the measurable spectral lines on
the tracings were examined and the equivalent widths, the r ratios
between the immediate and true backgrounds, and the central intensities
with respect to these two backgrounds determined for 1100 lines. A
statistical study was made of the observations, with particular reference
to the determination of the true meaning of a Rowland Intensity. Finally
some of the observations on the heaviest Fe 1 lines wore used to
determine the excitation temperatures of the solar reversing layer and
to extend the curve of growth, determined at Harvard farther up the
damping curve.
Chapter I. The Table of Equivalent Widths
Introductiom
The application of the methods of spectroscopy to astrophysics!
problems is one of the most rapidly growing hranohes of astronomy at
the present time, and one of the moat fruitful. An investigation of the
wave lengths of the spectral lines penults one to make deductions as to
thA elements present in the stellar atmosphere, and the physical condi
tions, such as temperature, pressure, eto., at this surface. Similarly
a knowledge of the relative and absolute intensities of these lines
gives one an insight into the relative abundances of those elements,
as well as their temperature. ' :
In the visualc region of the solar spectrum, from A 4036 to
A §600, a very complete investigation of the relative intensities of the
Fraunhofer lines was made by C. W. Allen at the Commonwealth Solar
Observatory, in Australia. In order to extend the table to the near
ultraviolet. Dr. 0. F. Y/. Mulders la 1938 made a number of exposures
in this region using the 150-foot tower telescope of Mount Wilson
Observatory. Seven of these plates, covering the region X 3500-3900 A,
were sent to the University of Arisons. Using these plates, in 1959
Leon Blitser of the University of Arizona made a very accurate deter
mination of the excitation temperature of the Solar Reversing Layer,
which he described in a thesis submitted to the University^, and in a
1. Blitxer, Leon, The Temperature of the Solar Reversing Layer from Relative Intensities of the kotatlonaT tines of CyanogenTni brary, University of Arizona. ~
2.
publication that appeared in tit® Astrophysieal Journal^.
The PI ate si ' " ' ' : ‘ ' '
(From information supplied by to*. F. W. Mulders.)^ . .
The seven plates measured were taken with the 150-foot tower
telescope and 75-foot spectrograph at the Mount Wilson Observatory,
which forms an image of the sum 17 inches in diameter. Undisturbed
regions in the center of the disk .were chosen. The spectra were taken
in the second order using a plane grating made by Mlehelson. The dis
persion on the plates is 1 Angstrom per. 5 millimeters, and the theore
tical resolving power is 150,000. . ;
From three to five exposures were made on each plate. The plates,
their spectra and the exposure times are given in Table I.
The slit width, was 0.002 inches throughout. A Written filter ISA■ ! - x:
was used to cut off all radiation longer than 4000 A, and thus to elim
inate scattered light. A vibrating step slit was used to calibrate the
plate• The widths of the slits of this step slit formed a regular pro
gression, and it was assumed that the intensity of the light passing
through each slit was proportional to its width. In this way a relative
intensity scale was impressed on the plate. The slit widths were*
4.975 ma 0.6585.375 0.4662.212 0.5221.477 0.2540.977
2. Blitter, Leon, Ap. J., 91, 421, 1940.5. From information supplied by Dr. 6. F. W. Mulders in a letter
to Dr. F. E. Boach.
5.
Table IPlate Number Wave Length Range
1 XSSSOSS15 A
2 , ' X5725-5810 A
3 X 3810-3890 A
4 X 3780-5860 A
5 X 3855-3915 A
6 X3715-8795 A
7 X 3620-5685 A
Exposure Eumber Exposure TimeOC 90 min.P ISOy 240oi 40 min.P 60- y 80
10040 min.60
y V 80.<f 100
' U 15 min.p ar 29<T 396 SO
y 14 min .P 20
27/ 366 mot 14 min.p 20
• r 27... f.,. 35
6 45
eC 35 min.P 50r 90
4.
Cramer’s contrast plates were used. They were developed with D-ll
(Eastman Kodak) developer for 6 minutes at a temperature of 68® F.During the development process they were brushed to eliminate Eberhard
effects. : , - . y :■ : y ' '
The Microphotcmstw fraoings. ' - ' ' - '' " - ■'
Tracings of the heaviest spectrum on each plate were made with the
Moll mierophotometer of the Steward Observatory. This instrument had
recently been improved by the substitution of a photoelectric cell for '
the thermopile with ahich the instrument had been supplied, and the use
of a Leeds and Korthrup galvanometer of very short period. The current
sensitivity of this galvanometer is 8 x l(f9 amp/mm., and its period is 0.8 seconds. The recording drum carries a sheet of photosensitive paper
42 centimetere long, and it is connected to the driving clock through
a gear-box so that it can be rotated at two different rates of speed with
respect to the plate, the speeds such that the paper moves slither 4 dr 42 times as fast as the plate. Since the dispersion of the plates was
l/3 A per millimeter, it can be seen that at the two speeds each tracing
would cover about 2.8 or SO Angstroms respectively.
The theoretical resolving power of the spectrograph with which the
spectrograms were made was 180,000. At the mean wave length of AS722 A, this would mean that two lines would just be resolved if their centers
were only 0.028 A apart. Now the slit width of the micropbotometer was
0*07 mm, and the amplification of the image of the spectrum at the slit was about 6.5, so that 0.011 mm of the plate was covered by the slit at
any one time. For the dispersion of the plates this ease out to be
0.0037 A, which meant that the micro photon® ter had a resolving power about
seven times as great as tbs spectrograph. Thus all the detail on the
plate urns accurately reproduced on our tracings. ,
Since the opacity of a photographic emulsion is not directly pro-.v. ■ ■■ -
portlonal to the intensity of the light producing the opacity, it m s• • . - . ■ •
necessary to know the calibration curves of the plates in terms of
galvanometer deflections on the tracings in order to interpret these
deflections in terms of Intensities. These calibration curves were
derived from the exposed strips produced by the vibrating step slit. A
cross-section across the strips m s chosen at a wave length close to the
mean for the tracing that had just been made. Each of the strips in this
cross-section was then placed before the micro photometer el it in turn
and the corresponding galvanometer deflection recorded on the same
tracing as had been exposed when the spectrum m s traced. This m s done
immediately after the tracing m s made, before the instrument had been■ ■disturbed in any way. The resulting galvanometer deflections were allowed
to fall on the tracing, which m s rotated. Since the relative widths
of the vibrating step slits could be interpreted as relative intensities,
a plot of these widths against the resulting galvanometer deflections
gave one a calibration curve by means of ski oh deflections on the tracing
could be interpreted in terms of relative intensities.
Low magnification tracings were first made of each of the darkest
spectra on the seven plates. Since each plate covered about eight
, Angstroms, three tracings covered each plate. Calibrations were impressed
on each of these tracings, and calibration curves drawn on semi-logarithmic
paper. On each tracing a few of the most prominent lines were identified
toy moans of Howland charts. Knowing the magnifications of the micro-
photometer , and the dispersion of the plates, the horizontal scales of
the high and low magnification tracings were computed to toe 125.4 and
11.54 mm. per Angstrom respectively. Thus, knowing these scales and the
wave lengths of a few lines on each tracing, accurate scales were drawn
on all the lew magnification tracings by means 1 of which all the other lines on the tracings could be identified. This very greatly facilitated
the identification of the spectral lines on the hig£ magnification
tracings which were made later. ,
The experience with the low magmifleation tracings led to tie belief
that for at least a half-hour at a time the adjustments of the micro-
photometer remained practically constant. Therefore, since with the high
magnification a tracing was made in about five minutes, a series of
calibrations wasu impressed on each fourth tracing only. Care was taken
during the changing of paper not to alter the zero point of the galvanometer,
or the light intensity through the microphotmeter, in any way. At the
end of the fourth tracing in each group, after the calibrations had been
made, the plate was removed and dusted, the zero point of the galvanometer
was checked, and the clear glass deflection was noted, after which a further
set of fbur tracings was made. In this way 34 low and 389 high magnifi
cation tracings were made.
The tracings were developed with D-ll (Eastman) developer and fixed
with unhardened hypo solution. The hardener was omitted in order to
eliminate any inaccuracies due to the emulsion stretching during hardening.
8.
7
The Continuous Background.
In order to measure the intensities of spectral lines it was
necessary to know what the intensity of the light would have been at that
point had the line not been present. In the solar spectrum, and in the
ultra-violet in particular, so many contributing elements are present
that there are very few points in the spectrum where absorption does not
take place. Mulders4 has made a study of the percent of radiation
absorbed by all the spectral lines in successive spectral regions. This
information is plotted in Figure 1.
3000
Figure 1. The Percent Absorption by the Fraunhofer Lines for Various Spectral Regions in the Solar Spectrum (Mulders^).
The region that we are concerned with, from /'3530-3915 A, is
indicated by the horizontal line on the graph. It can be seen that this
is one of the most highly absorbed regions of the spectrum, about 35 6 of
the light being absorbed on the average by the lines. At probably no
point in this region is the radiation completely unabsorbed, so that we
4. Mulders, 0. F. W.t equivalent Widths of Fraunhofer-Lines in the Solar Spectrum. Dies. Utrecht, 19&4. oee Also: 1. Unsdld* Physik der Sternatmosph&ren, p. 37.
8.
have no definite method for determining where this continuoae straight
line should W dr aim. Arbitrarily it was decided to draw a straight line
Arot^h the two lowest points on the low nagnifleatlm traetage, and to
assume that that line would hare been the galvanometer deflection for the
unabsorbed radiation, keeping in mind always that this was an arbitrary
assumption. ■' :; ; : ' -
In order to carry this sero absorption ^^kgrmmd mmr to the high
magnification tracings, the relative intensities of the background were
determined, with respect to the central intensity of some convenient
spectral lime. This relative intensity was as sumd to be the same on both
the high and low magnification tracings, or*
where is the measured central intensity of the line on the low
magnification tracing,
I], is the measured intensity of the continuous background on
the low magnification tracing,
I p is the measured central intensity of the same line on the
hlg& magnification tracing,
1 , is the unknown intensity of the continuous background on
the high magnification tracing. .
The above assumption that the relative intensities of "the, background were
the same on the two magnifications could be considered true if*
(l) The slit width of the microphotoaeter was the same for the two
--'■■■■■■■tracings.
9.
(2) The clear glass deflection iras the seme,.
(3) The sane spectrum was used.
The above equation could be solved for the unknown intensity to gives
Using this equation background lines e drawn on all the high
magnification tracings.
Blended Linest ■' ' - ' ' ' '' ' ' ' '
Only the very Waviest lines could be extrapolated down to the con
tinuous background with any degree of certainty. Most of the fainter
lines were found to be blended with either the wings of the very heavy
lines, with which this region of the spectrum was filled, or with each
ether. In the case of the lines blended in wings, Thackeray® draws a
straight line across the base of the line, and calls it the Immediate
background. He then defines a quantity r as;-V ■ ■ - " ' f -■ ■ ' ’ . ' - " V ■ , :* :■ •’ ■■ ■ ■ ■■ : , . :/
. T « Xi
where 1^ is the int«aeity of the iaseedlate background at the center • of the line, ' : ' - - T '
is the intensity of the continuous background at the eimter
-■ of the line. : ' ' ' /'v ’v
Bxis qimntity r Is a measure of the blending of the line.
In many cases of lines blended with each other, one half ef the
line might be unblended. In this event only the unblended half of the 5
5. Thackeray, A.D. Ap.J., 84, 433,1936.
10.
line nas measured, and the line assumed to be symmetrical. In the sun this
antH^tion aas justified since the light had been received from an undis
turbed region in the center ofthe disk* * Other lines had to he discarded
since they were too badly blended with their neighbors.
Determination of Equivalent Width:
Since spectral lines have contours of varying shapes and different
central intensities, it is convenient to define their intensities in terms
of the widths of some arbitrary lines of standard shape and central inten
sity, where tho widths of the lines are the only quantities Thick vary
■with intensity. The arbitrary shape is taken as rectangular, and the
central intensity, vhich would of course be the intensity over the whole
rectangular line, is zero. The width:, of each a line, which absorbs the
same amount of radiation as some spectral line, is known as the Equivalent
*ldth of that spectral line. Equivalent widths are usually given in milli-
Angstroma.
In order to determine the equivalent width of a line, the deflections
of the galvanometer are measured on the tracing of the line for its center
and for equally-spaced points to the left end right of the center out to
the wings, both for the line and the immediate background. The corresponding
intensities were then found, and the relative intensities of the points on
the line with respect to the corresponding points on the issaediate back
ground. These relative intensities were then plotted against the distances
from the line center, and the resulting curve integrated. Knowing the
scales of the tracing and the plot, the equivalent width of tho line was
11.
then immediately found.
The Table of Equivalent Widths.
Using the foregoing method, the equivalent widths of all measurable
spectral lines were determined in the region 3530-3915 A. These values
are tabulated in Table II.6In columns 1 and 2 the wave lengths of the spectral lines and their
Howland Intensities are given. In column 3 the equivalent widths are given
in milli-Angstroms, and the corresponding values of r in column 4. The
last two columns give the central intensity of each line both with respect
to the immediate background and the continuous or true background.
(For Table 2, see Appendix, page 41) 6
6. The information in columns 1 and 2 is taken from C. E. St. John et al. Revision of Rowland* e Preliminary Table of Solar Spectrum Wavelengths"! BereafEer in this paper this publication will be called tho Revised Rowland.
12
Chapter II
A Statistical Study of the Table of Equivalent Widths
The statistical study was divided roughly into two partsi
(1) A study of the effect of blending upon the equivalent width
of a blended line
(2) A study of the effect of the blending of a line upon its
central Intensity, both with respect to the immediate and the true back
ground, This led to the discussion of the true significance of the
Rowland Intensities.
In addition there were miscellaneous studies, such as the relation
ship between central intensity and equivalent width.
It is of interest to know the numbers of lines of different Rowland
intensity actually measured, and to compare this with the nimber actually
present in the Revised Rowland for the same spectral region. This infor
mation is plotted in Figure 2.
Figure 2. The Humber of Spectral Lines of Different Rowland Intensities Measured in the Region A 3530-3915 A.Closed circles ■ the number of lines measured.Open circles * the number of lines actually present in this region
with each Rowland Intensity
__ .
18.
From this plot it can be seen that comparatively few of the faint lines of
Rowland Intensity less than 0 were measured. This is due to the fact that
many of them were too faint to measure, or were blended with heavier lines.
Progressively more of the lines were measured as we go to heavier and
heavier lines, as might be expected.
the Effect of Blending upon Equivalent Widths
The measures were divided into groups according to their Rowland
intensity, and then further subdivided according to their respective values
of r, the limiting values of r for each subdivision being 0.90 to 1.00,
0.80 to 0.89, etc. The resulting averages are given in Table 3s
Table 5
1.1. Log r
9,.98 9.95 9.68 9.1SI >. 9.74 9.68 9.164log* Vo logW So log! So logW Ho logW So loeW Ho lo8W No
-3 0.90 10 0.30 2 0.48 2
-2 0.91 24 0.89 11 0.84 8-1 1.08 50 1.03 52 0.88 13 0.84 7 1.00 60 1.24 88 1.20 41 1.16 59 1.04 22 1.08 18 1.04 11 1.84 4
1 1.60 61 1.53 70 1.48 49 1.59 56 1.29 52 1.54 14 1.14 7
2 1.76 84 1.69 48 1.65 56 1.60 25 1.48 27 1.26 7 1.41 7
8 1.80 32 1.76 34 1.77 51 1.74 14 1.64 11 1.58 6 1.51 24 2.02 19 1.85 21 1.86 20 1.72 IS 1.64 10 1.92 1 1.47 4
5 2.09 8 1.92 12 1.83 7 1.85 4 1.76 6 1.52 2 1.18 2
The differences between the values of log W for each log r and the value
for log r = 0.00 were then found. The means for each log r and all Rowland
14
Intensity groups were found* They are listed in the first two columns
of Table 4.
In Figure 3 A log W is plotted against log r. A smooth solid
curve has been drawn through the points*
f
Figure 3* The Decrease in the Intensity of Spectral Lines with Increase
in r*
It is interesting in this connection to compare these results with
those of the theoretical discussion of Thackeray?. He found that with an
error of less than 3#,
W . rW1
where fi is the equivalent width of a blended line,
Ai* is the corresponding intensity of the unblended line.
The dotted curve of Figure 3 shows the decrease in the equivalent
width with increased r based on this theory of Thackeray’s. It can be 7
7. Thackeray, Ap. J., 84, 433, 1936
Table 4
log r h log WImmediate ^ 06 ® Background
• TrieContinuum
9.98 0.026 0.000 O.OO©
9.93 0.097 0.013 -0.082
9.88 0.152 0.029 -0.068
9.81 0.228 0.080 -0.106
9.74 0.282 0.081 -0.129
9.65 0.347 0.100 -0.206
9.54 ' 0.401 0.161 -0.238
Table 6.
:. I. W(r-1)
W(Are)
WMulders
ImmediateBackground
TrueBackground
-3 8.3 6.1 vo.s; 91.94 % 79.35 %
-2 8.9 7.6 2.6 90.41 80.07
-1 12 10 6.8 89.12 78.98
0 19 15 17 83.49 62.27
1 43 30 36 71.52 62.43
2 62 43 60 60.44 44.48
3 69 56 80 64.16 . 41.60
4 105 70 104 50.07 36.44
5 , 121 78 140 47.64 83.22
16
seen that the two curves are approximately the same.
The curve on Figure 3 shows that within a Rowland Intensity group
the equivalent width decreases in proportion to the increase of blending.
In fact, the amount of decrease of the equivalent width is on the average
the amount that Thackeray predicts will be the decrease in the intensity
for a blended line. Thus we may say that, 6n the average,lines of the same
Rowland Intensity regardless of the degree of blending are produced by
transitions by the same numbers of atoms.
The Significance of a_ Rowland Intensity*
As a preliminary to the meaning of a Rowland Intensity, the equiva
lent widths in Table 3 were averaged over each Rowland Intensity and
tabulated in column 3 of Table 5. The data in the first and third columns
of this table were plotted in Figure 4.
Figure 4. The Relationship Between W and Rowland Intensity.
Mulders^ obtained values for the relation between W and Rowland Intensity for X 3900, which are tabulated in the fourth column of
Table 5. A comparison of the values of W obtained by us and by Mulders
shows that they are in good agreement except for negative Rowland
Intensity groups. In these groups the values that we obtained were very
much greater than those of Mulders. That may be explained by saying that
it was due to the selection of the lines in those groups, only the heavier
lines in each group being measured, and thus the intensities of the averages
in these groups were weighted on the heavy side.
As a further preliminary the central intensities of each line, with
respect to each background, were averaged over each Rowland Intensity
group. These averages are found in Table 5, in the last two columns.
These figures were plotted in Figure 5, which gives the relationship between
Rowland Intensity and the central intensity with respect to the immediate
background (closed circles) and with respect to the true continuum (open
circles). — " i i i •" i ■
Figure 5. The Relationship Between Rowland Intensity and Central Intensity.
When this plot was made the expectation was that the shapes of the
two curves would give a clue as to which of the two central intensities
were used by Rowland in his determination of the intensities of the lines.
However, the tw> curves looked equally good, so that no decision could be
made at this point.
An attempt was made to decide which of the two curves was the more
18.
Important by determining the probable errors of the averages. These are
listed In Table 6.
■ Table 6. ;; ,
R. I. e . i . P. E. C. I. P. E. wt.Immediate True
—5 0.919 0.015 0.794 0.024 17
0.906 0.004 0.784 0.010 49
-1 0.888 0.004 0.786 0.008 85
0 0.832 0.006 0.625 0.007 169
1 0.703 0.004 0.519 0.004 272
2 0.607 0.006 0.440 0.006 186
5 0.642 0.005 0.416 0.006 1*94 0.497 0.007 0.562 0.006 92
6 0.476 0.012 0.849 0.008 45
6 0.422 0.016 0.322 0.009 24
7 0.879 0.014 0.514 0.008 118 0.282 0.017 0.263 0.012 9
9 0.326 0.026 0.262 0.026 510 0.270 0.020 0.250 0.017 7
12 0.280 0.054 0.260 0.044 216 0.280 0.007 0.260 0.016 5
20 0.180 0.160 0.006 226 0.200 0.200 ' 1
These probable errors did not furnish a solution to ithe problem
sinoe a glance at the table shows that they are of the samei order of
19.
magnitude.
A determination of the degree of modification of the central intensity
with varying r was then determined. Within each Rowland Intensity group
the observations were divided according to their r, using the same divisions
of r as were used for the Equivalent Vlfidth study. The observations were
then averaged and the logarithms of the averages found. The observations
in the first r group (from r = 0.90 to 1.00) were considered as being
essentially unblended, and the differences were found, between the logarithms
of the averages for all the other groups and the logarithm of the average
for this group. Finally all the Rowland Intensity groups were averaged
together. The resulting averages are listed in colxsnns three and four of
Table 4, and plotted against log r in Figure 6.
o.oo-p -0.04-C3O -0.08 - < - 0 1 2 -
Figure 6. The Modification of the Central Intensity of a Line with Increase of r for Constant Rowland Intensity.Closed circles » central intensity with respect to true background Open circles « central intensity with respect to immediate background
This is a very interesting graph. It shows that within a Rowland Intensity
group, the central intensity of a line with respect to the immediate back
ground is increased with increased blending, whereas the opposite Is found
20
in the case of the central intensity with respect to the true continuum.
This result seems to indicate that the background against which
Rowland estimated his intensities lay somewhere between these two extremes.
Possibly a background could be drawn tangent to the general trend of the
intensities in the wings of the heavier lines. The background Rowland used
was probably determined by the amount of spectrum he could see at any one
time through the viewing microscope of his measuring machine, which at
best would be a rather local estimate.
Finally it is of interest to compare the Central Intensity of a line
with its Equivalent Width. Since the Equivalent Width of a line was
measured with respect to the immediate background, it was plotted against
the central intensity with respect to that same background. The data in
Table 5 venr used and the plot is shown in Figure 7.40 ----- — j------
------ — -
...
— --- f---------
—
60
/
y60
90
-,
yy :; ;
'
i i i lil MSS M MID 20 «0
— w — * -r
m i *
Figure 7. The Relationship Between the Central Intensity of a Spectral Line and its Equivalent Width, both with Respect to the Immediate Background of the Line.
This graph is of interest in that it shows that for lines up to an intensity
of about 50 milli-Angstroms, the central Intensity, or line depth, of the
line Is a good Index of its total Intensity. The curve may be compared
#ith that derived by Woolley9 for the nave length region A 4040-4274.The two curves are practically identical, but since the wave length regions
covered are different, they cannot profitably be drawn on the same graph.
The experimental re suit ssh own in figure 7 bear out the theoretical
explanation of the manner in "which the spectral lines increase in intensity
with an increase of the number of atoms undergoing the necessary transition
to produce the line. It has been shown theoretically that the frequency
of the light absorbed by an atom is not only dependent upon the energy dif
ference between the initial and final energy levels of the jumping electron,
but also upon the velocity of the kinetic motion of the atom in the line of
sight. We might conceivably then erect two perpendiculars on either side
of the wave length absorbed by an atom at rest with respect to the observer,
the distance between each perpendicular and the central frequency being &
function of the temperature of the gas. The spectral line will then build
up within these perpendiculars, and since in general the kinetic motions of
the atoms are at random, the line will conform closely in shape to the sta
tistical bell curve. The amount of radiation absorbed will be proportional
to the central intensity until the central intensity approaches 100% absorption. As this point is reached the line begins to fill in the area enclosed
between the perpendiculars, so that the total anount of radiation absorbed,
shioh can be expressed in terms of an equivalent width, increases much more
9. Woolley, B.v.d.B., Ann. Solar Phys. Obs., Cambridge 5, 2, 1953.See also: A. OnsBid, Phyaik Aer SternatmosphBren, p. 215T
rapidly than the central Intensity. Figure 7 shows that tills asymotry
begins to appear for equivalent widths of 50 milli-Angstroms in the sun.
For hotter stars the kinetic motions of the gasses of the atmosphere of the
star will be greater, which means that the two perpendiculars will be
farther apart, and the line will become more intense before this asymmetry
appears. The opposite takes place for stars which are cooler.
under-
A Curve of Growth of Spectral Linos
A curve showing the relationship between the number of atoms
going a given transition and the intensity of the resulting spectral line
is known as a Curve of Growth of the lines. These curves may be deter
mined from either a theoretical or experimental basis.
Theoretically two factors enter into the determination of the shape
of tile curve of growth. For fainter linos the Doppler broadening, which
is due to the kinetic motions of the atoms, is the mere influential. This
effect was described in the previous chapter. Were this the only factor
to be taken into consideration, the curve would approach some maximum
Intensity asymptotically for increase in the number of atoms. However ,
before this condition is reached, another factor influencing the intensity
of the line comes into play. This is the damping factor, brought about by..
the damping of the vibrations of the atoms undergoing transition. This
factor is influential in producing broad wings of absorption on either side
of the portion of the line whose width is determined by Doppler width.
Uasbld*0 has discussed the influence of each of these factors separately. He gives for the line contour due to the Doppler broadening
(itesSld, equation 89,9)i V
Chapter III
24.
* <5 1 . C j /Z <• ifl
■where H0 s the intensity;, at the center of the line Aw = the total absorption of the line
ZJtO_ s the Doppler Width of the line
C .■ ... - A
where e * the charge of the electron
m s tho m s s of the electron
e' /s the velocity. of light
r a * the number of absorbing or scattering atoms over
; : a square centimeter croee-section of the stellar
•. ■' atmosphere ‘ /
i t h oseillatcr strength of the line.
For the case of dsaping broadening, Unsflld’sequationhasthisform . .
(DnsflId, equation $9,16):
J_. . fZjjc— , Xhc 1o
where v • the difference in frequency between a point 'in a line-and the
line centetf. divided by the Doppler width
a • the damping! constant divided by the Doppler width.
The only variable in the third term for any single spectral line is HE,
so that this equation! Whows that for heavy lines, the total absorption
of the line inoreasesUlinearly with increase in the number of oscillators,
in fact, proportional;-to J .
Between these two extrme solutions, numerical methods have to be
25.
0
0
used, combining these two equations.;"r ; . "1 *1 ■ " : ;
MenzelA and his co-workers derived similar equations for the curve
of growth, they were also able to derive an equation that satiafaetorlly
approximated the curve of growth in the intervening section between those
dominated by either the Doppler or damping broadening.
Their three equations arei
(l) For faint lines*
J T 7
(2) For very heavy lines*
V T * f f V j — V
x ;rr
(S) For intermediate lines*
/
J-/.jfJrrf r— 7 -ill*.I + If-*-
..........W w equivalent width
X ■ nave length .
v ■ the root neon square kinetio velocity of the atoms
c * the velocity of li^it
" frequency of the radiation
P * the damping constant, defined as the sum of the reciprocal
mean life-times of the upper and lower states in the atomic
transition
Ji. * the charge on the electron
-p - the oscillator strength 11
11. Mensel, Donald H., Ap. J., 84, 462, 1956.
0
26.
The equations of BasSM can be shown to be essentially the
of Menzel. Make the following substitutions*
as those
1
z r J if-
Then the equation for G becomes*
TTjt1 tt / o r.c - N H ^
This shows that C is equivalent to X of Mensel except for the quantity H,
iriaich Mensel incorporates into his value of K, and RQt which Mensel asswes
to bo unity.
Using this substitution, and assuming that:/ W _ A X _ ;
- y . " (J ' X ' " '• v 'Unsbld’s equation for the absorption of a line influenced by Doppler
broadening alone becomes $ ,
which is the same as the equation given by Mensel except for the appearance
of Rc- , , .... . - . - •
Similarly for the case of damping broadening» UnsBld’s equation becomes
eeuivalenttothat of Menselif we substitute for a the ratio for which it is
the symbol*a =
■ Y'
where Jf is the damping constant.
Making this substitution, UnsBld’s equation beoc
I
& > 2. ( «•/ \ Rt I?,'
27.
0
0
again equivalent to Kernel's equation except for the appearance of the
quantity Eq in the equation.
It is of value to compare the notations used by TJnsBld and Menzel
in these equations. The following table gives the symbols used by theso
two investigators for the same quantities*Table 7.
Quantity Symbol
' ■ - ■ fmsSM Menzel
Optical depth at ©water of line 0 %oBomber of absorbing or scattering atoms over a square centimeter cross-section of the stellar atmosphere ' M HEquivalent width in Angstroms V ' w ■
Boot-mean-square kinetic velocity of atoms i. V
Damping constant r r
Intensity at center of line ' : " . V :Oscillator strength r r
Kamel shows that the quantity Xq nay be evaluated by making
appropriate transformations. The final equation derived for Xq is*
there Ha = the total number of atoms of the given element in the
particular stage of ionisation considered,
the ionisation potential of the level
k s the Boltzmann factor
b(T)« the partition function*
28
(r(T)- *to . 4t
where eo*- is the stetistical weight of the i^h level.
^ a a constant, i M c h enters into the equation
idiere QT^is the seuare of the first order electric, : , ... . -- I - : . :between the two electronic configuratione, and h is Planck* s
constant
x the atomic weight
T * the absolute temperature
8 a the theoretical strength of a multiplet within an array of
aultiplets ' ,
e ■ the theoretical strength of a line in a given multiplet
* m the sum. of the strengths of all the lines of a given multiplet.
a relative intensity scale. . ^
in array is & e nano given to the group of lines re suiting from the
transition of the orbital electrons of an atom from one configuration to
between any particular L in the initial configuration to any ether L in the
final configuration, subject to certain restrictions, brings about a group
another. Within each configuration the electrons may occupy several
different energy levels.
Of primary importance is the azimuthal quantum number L. A transition
*9.
0
•f related spectral lines known as a multlplet. In a given configuration
electrons may have different energies depending upon the way in which the
azimuthal and spin quantum, numbers add up, A transition between an energy
level in the initial configuration and an energy level in the final con
figuration gives rise to a single spectral lime.
How Hfcite*2 M s computed the relative intensities of spectral lines
within a multlplet, and Goldberg‘S M s determined the relative intensities
@£ multlplets within the more important arrays. Using this material it is
possible to determine the relative intensities of all the lines of a given
multlplet, and then to make the comparison between multlplete.
When the multlplet# are plotted together on a relative intensity
scale, they will in general be displaced horizontally with respect to each
otMr, and It will be found t M t the multlplet# of higher excitation poten
tial for the lower levels are to the right of those with a lower excitation
potential. In order to bring the multlplet# onto a single curve of growth
for the array, it is necessary to make the Boltzmann temperature correction.
Involving the term*
■€
or, since we are using logarithms, (— , which may be transformed to
(—y # ) where 0 * 5040
Here we may follow either of two procedures. We may either assume
an excitation temperature f and compute the resulting correction, or we
may elide the curves arbitrarily together amd determine the correction. 12 13
12, White, H. 1,, Introduction to Atomic Spootra, p, 439 ot seq.13. Goldfeorg, Leo, Ap. J., 82, 1 7 IdSS.9
30.
Menzel^* has derived a very convenient method for determining the tempera
ture. He defines a quantity Y as the difference in logarithms between the
unknown value of X© and the computed value X^, defined by the equation*
The constant part of Xe, he sets equal to a quantity L, so that his final
eqmtion for Y becomes*Y” = loj ro - Uj L - >-o4?r J
If we now plot Y against the slope of the curve will be 5040
Kid we may find t.
T may be found according to the above equation for each line, and
then averaged over each aultiplet. Tihon this was done for six multiplets
to the Pe I arrays 3d?4s - Sd^dp and Sd^ds^ - 3d®4s4p the following values
of and Y were found*Table 8
Multiplet > Y
a5F - ySpo 0.96 3.84
asF - y®D° 1.60 5.28
asF - y % ° 0.96 3.74
a5? - z68° 0.95 5.81
asD - z5F° 0.048 4.64
a % - zbi0 0.034 4.69
Bhen this material was plotted, the slope gavo an excitation temperature
of 5540° A. From the Fo I spectrum Henzel, using the material of Allen,
(% obtains a tmperature of 41B€^^S0® (P.E.)
For the same array, Menzel had four multiplets. A temperature
determined from than corns out at about 3040®, but since the points are *14l Menzel, Donald H., Ap. J., 87, 81, 1938.
51
badly scattered it does not have much significance.
When it became necessary to combine the points on these two arrays
into one curve of growth, a very useful table was found that had been derived
by Kingly 0f noun^ Wilaone He had experimentally determined the relative
intensities of a number of the heavier lines of Fe I. By plotting these
experimental intensities against the theoretical relative intensities, two
45° curves were found for the two arrays. The separation between the two
curves was 1,18 in the logarithm. This was therefore assumed to be the
relative intensity of the one array with respect to the other, so that by
making this correction to the array they could both be plotted on the same
relative intensity scale.
When this was done the heavy black points of Figure 8 were found.
LOG X
Figure 8. The Two Fe I Arrays 5d74s - 5d74p and 5d64s2 - 3d64s4p plotted on the Harvard Curve of Growth.Filled Circles z points determined by sum rule and Goldberg1s
relative intensitiesOpen circles • points determined by arbitrarily moving multiplets
onto curve.
15. King, Robert B., Ap. J., 87, 24, 1958.
In this figure the two arrays are superimposed on the curve of growth deter
mined at Harvard by Menzel**. the open circles are some lines of multlplete
the relative intensities of which were not treated theoretically by
Oeldberg, and so > Jvh had to be arbitrarily moved over onto the curve.
These points extend the Harvard curve of growth up considerably, but
they do not add anything to the knowledge of the damping constant, since
the arrays do not contain any lines on the flat part of the curve of
growth to orient the heavier multlplete. A theoretical discussion which
may be made later may decide definitely the relative intensities of those
lighter multlplete here arbitrarily treated. In that event this work
should be repeated.
In a recent paper King* 17 has published the absolute f values for
twelve lines of Fe I. These lines were members of two multlplete,
a5p - gSpo gad a®D - z^D°. Using these values he was able to calibrate
his relative f scale, and he obtained the equation
absolute f - 1.85 x 10”* x relative f.
Knowing the absolute f values, it was possible to determine the number
ef Fe I atoms in unit column with square centimeter cfoss-section of the
solar reversing layer. -
Two methods were used. In the first, knowing log J7 for each line
considered, we were able to go to the Harvard curve of growth (Figure 8)
and obtain log I*. Then knowing log S for each line, and the absolute. . . - ■ ' - - . • Z* , \ ■■ - „ ■ -
17. ling, lobert B., Ap. J., 95, 78, 1942.
S3.
f values for twelve of the lines we had measured, we were able to determine
the relationship between these quantities. The following table gives the
data that were use*i
Table 9. ,
Multiple* Line f(abs) S gf log gf 3
asD - *5F° 5706.6 0.62 0.0021 7 0.0147 8.167 83719.9 1.34 0.0130 9 0.1170 9.068 4
3722.6 0.60 0.0033 6 0.0166 6.117 23737,1 1.18 0.0127 7 0.0889 6.949 33746.6 0.98 0.0117 5 0.0686 8.767 2
. •' ■ 3746.9 0.45 0.014 1 0.014 8.146 0
3748.6 0.76 0.0121 5 0.0363 6.660 1
a®D * s®D° 3824.4 0.48 0.00194 9 0.01746 8.242 4
3866.4 0.60 0.0030 7 0.0210 8.322 3V . 3859.9 1.18 0.0074 8 0.0666 8.824 4
. J ■3878.6 0.54 0.0029 6 0.0146 8.161 2
3886.3 0.86 0.0044 7 0.0308 8.489 5
Figure 9 is a plot of log S against the absolute log gf.£ a
From this curve we were able to derive the following equations
S grg- + J.JO - tOftus, knowing log S f__ for eadh line, we were able to deteraim
£aleg gf, and since we know that g « 2j +1, we can find log f.
34.
r ! T ' T 'T "
1.5
1.0(Z)
05
Figure 9. The Relationship Between Log S 8 and L(% gf (absolute)£e
Open oirvles s lines in multiplet a°D - ii5F°Closed circles = lines in multiplet a^D - r^D0.
New the equation for Xq
X -rTe g.™ c 'fir V X
may be put in a convenient form by substituting:J~ -^ CLTr Cv*c
- - /= 2 X 3 f x J 0 SICWe then get: p-— ,
x . - //5"x /d-6 a / -t " A/ ^
In the case under consideration the mean As 3720 A, T ■ 4400°^ and ■ 56. When these are substituted, our equation for *f becomest
/<x N ~ f - /q q X 0 "t //.34Thus, since we know log Xc, we can find log Nf, and knowing log f
we can find log N
& given traasitio b , so that In order to know the total number of Fe I atoms,
me have to multiply each N by an appropriate factor B, which, is an expression
for the way in which the atoms divide themselves among tho different
possible energy levels at a given tmaperature f. It is a ratio, being the
reciprocal of the probability of finding a given atom in a given energy
level•
whore g£ a statistical weight of the lower energy level
% „ its excitation energy measured from the grotmd state
s f * the excitation temperature of the reversing layer.
For oomputational purposes, this equation may be put in a more convenient
the lines originating frees the few lowest levels contribute anything to
tiie summation, so that the result is very easily found to be
Since yzb is known for each line, we may evaluate log B, which when
added to Log H, gives log N0, or the logarithm of the total number of Fe I
atoms in the elemental column, this was dons for 34 lines, and the results
V9
where % * excitation potential in volts
& - 5040
% e n this summation is evaluated for Fe I, it is found that only
Therefore we have finally
log B a 1*4 - log g -f- 7^^
36
are tabulated as follows* la Table 10.
f In this table the source of log £ Is indicated. If it was derived
from, the absolute values of King, it was designated by an A; if by the
relative values of King, by an H, and if by the graphical method, tying in
log S and the log gf, it was designated by a 0.
The mean of the M0*s comes out to be
4.25 x 1018 a 0.31 atoms
The second method available is to use the UhsSld equation for the
damping portion of the curve of growth. King has evaluated it on the
assumption that the damping constant was ten times classical, and that the
excitation temperature was 4400°K. He obtains the equation
H u t * ( Q f
where IH equals the quantity II previously used. This equation is more
7 convenient in the logarithmic forms .
loy N H • Zt-t/ + Z /of - lojfi Since everything cm the right is known, log *H can be evaluated,
which when added to log B gives log He. This was dene and the results
shown inTable 11 were obtained.
The average H0 obtained by this method was
5.86 x 1018d! 0.25 atoms
Using 46 lines in this region and in the visible region of the spectrum.
King obtained the value, for H0t
log * 4.3 x lO18* 0.18
The difference between the results obtained by the graphical and algebraic
methods should be duo mtirely to the inclusicm of in the equation of
Unsold. But in the sun this constant turns out to be 0.95, so that the two
5
Multiple* Line106 X losS",
(oorr.to array A)
log B
a®P « *G@o 5689.1 -4.28 1.25 1.535608.9 -3.57 1.77 2.075651.6 -5.46 2.06 1.645647.8 -3.64 2.18 1.49
a5D • s8P° 5649.2 -4.44 -0.71 0.465679.9 -3.86 6.48 0.465722.6 -3.70 0.60 0.805757.1 -3.47 1.18 0.615746.6 -3.60 0.98 0.803748.5 -3.67 0.76 1.04
a®D - *80° 5824.4 -4.18 0.48 0.453866.4 -3.84 0.60 0.613869.9 -3.58 1.18 0.463886.3 -3.68 0.86 0.61
esF - y8?0 5727.6 -3.85 1.36 1.643745.3 -3.90 1.18 1.823768.2 -3.66 1.78 1.643765.0 -3.69 1.58 1.823767.2 -3.68 1.48 2.073787.9 -5.98 1.18 2.073796.0 -3.76 1.56 1.82
»5p - w 6do 5790.8 -4.51 1.66 5.05e8F - y8P° 5841.0 -5.87 1.68 2.53e8H - y8flo 5869.2 -4.60 2.21 3.01
5875.8 -4.71 2.12 3.125895.9 -5.02 0.71 5.123890.0 -4.75 0.72 5.25
A8? _ ySpC 5820.4 -3.48 2.07 1.335826.9 -5.64 1.91 1.495640.4 -5.70 1.48 1.825849.9 -3.84 1.18 2.075865.6 -4.05 1.18 2.073872.6 -5.70 1.54 1.823878.0 -3.96 1.36 1.64:
sourcelog f A a aba, leg JU log If log If log Ho SetxlO18)
R a rel.G a graph. ^ 6
8.92 R 2.87 14.28 17.51 18.64 4 49.09 R 4.24 16.80 16.71 18.78 6.08.70 R 4.68 16.04 17.54 18.98 9.88.60 & 4.49 16.86 17.86 18.86 7.15.76 1 2.62 13.88 18.15 18.58 3.87.10 I 3.84 16.20 18.10 18.66 5.67.61 A 4.15 16.49 17.98 18.78 6.08.10 A 4.66 16.02 17.92 18.65 5.48.07 A 4.56 16.72 17.66 18.46 2.68.08 A 4.21 15.67 17.49 18.65 3.47.29 A 5.14 14.60 17.21 17.66 0.67.48 A 5.83 15.19 17.71 18.52 2.17.87 A 4.86 16.21 18.34 18.79 6.27.64 A 4.19 16.56 17.91 18.62 5.58.51 R 3.82 16.18 16.87 16.51 3.28.31 R 5.71 16.07 16.78 18.68 3.88.87 R 4.48 16.84 16.97 18.61 4.18.83 R 4.17 16.65 16.70 18.62 3.38.90 1 4.19 16.65 16.68 18.TO 8.08.60 R 5.62 14.88 16.56 18.45 2.88.56 R 4.00 16.56 17.01 16.85 6.88.40 0 2.56 13.72 16.52 18.86 2.29.13 a 3.76 16.12 18.99 18.62 3.38.80 6 2.40 15.76 14.96 17.97 0.98.78 0 1.67 15.05 14.26 17.87 0.27.88 G 0.56 11.92 14.54 17.66 0.67.47 G 1.60 12.96 16.49 18.72 6.28.72 1 4.64 16.00 17.28 18.61 4.18.67 a 4.60 18.86 17.16 18.68 4.88.60 a 4.18 16.49 16.99 18.81 6.68.60 a 3.85 15.19 11.69 16.76 6.88.42 R 8.40 14.76 16.54 16.41 2.68.18 R 4.14 18.60 17.81 19.14 15.88.05 R 5.59 14.96 16.90 18.64 8.6
Table 10
Tabl« 11.
line 2 log log *f w* 22.81+21og_3_
log Hq So
5589.1 ' -8.66 r ' 14.26 18.66 4.63608.9 -7.14 15.67 18.66 4.55631.5 -6.92 18.89 18.63 6.88647*8 -7.08 15.73 18.72 6.33649.2 -8.88 13.93 18.63 4.38679.9 -7.70 15.11 18.46 2.95722.6 -7.40 15.41 18.70 5.08757.1 -6.74 16.07 18.88 5.85746.6 -7.20 15.61 18.34 2.28746.5 ■ ’ - -7.34 -V 18.47 ■ 18.43 - ' 8.78624.4 -8.32 14.49 17.65 0.48866.4 -7.68 15.13 18.26 1.88889.9 -6.76 ; 16.05 18.63 4.38886.5 , -7.36 16.45 18142 2.68727.6 -7.70 15.11 18.44 2.83743.3 -7.80 15.01 18.62 3.55758.2 -7.10 15.71 18.46 3.05768.8 -7.58 15.43 18.42 2.63767.2 -7.36 - : ■ ' 15.45 ■ • 18.62 4.23787.9 -7.96 14.65 18.42 2.63796.0 -7.62 15.29 18.76 6.83841.0 -7.74 15.07 16.47 3.05820.4 -6.98 15.85 18.46 2.93825.9 -7.08 15.73 18.68 ' ' ' 3.63840.4 : -7.40 15.41 18.73 5.45849.9 -7.68 15.13 18.70 i.O3865.5 -8.10 14.71 18.36 2.23872.5 -7.40 15.41 19.06 11.03878.0 -7.90 14.91 18.60 3.2
89.
results should be essentially equal. The difference is therefore entirely
due to the scatter of the determinations of the equivalent widths.
In conclusion one may say that in this thesis we have been mainly
concerned with a production of a table of equivalent widths in the near-
ultra-violet region of the solar speetrum, and have made a statistical
study of the observations, with emphasis upon the -problem of determining
the true meaning of a Rowland Intensity. Finally, we have used seme of the
observations of the heaviest iron lines to extend the Harvard curve of
growth into the damping region, and simultaneously made a determination of the c
excitation temperature end the absolute number of Fe I atoms present per
elemental volume in the sun* s reversing layers
I wish to express my appreciation for the assistance given this work
by the Physios Department and the Steward Observatory of the University of
Arizona. In particular I wish to thank.Dr. 0. i. W. Mulders, of Mount
Wilson, vho took the plates; Dr. E. F. Carpenter, who kindly consented to
our using the Moll micro photometer; and in Dr. F. E. Roach, who as director
of this thesis was a constant inspiration.
40.
©Uneflld, A.
Mensel, ttm&ld E
E lng, Robert B & Ar&ur S,
Mantel, Donald H.
3
Tbaokeray, A. D.
Oeldberg, Leo
Goldberg, Leo
White, H. B.
Blitter, Leon
libliogri^y
Physik der Btarnataosph&ren, Pt. S. Berlin, 1958.
. Equivalent Width and the Temperature of the SolarT O T .---------
R e la tiv e f-V a lu es fo r L ines o f Fo I and Ti I ,' Ap . X, 0, m ,The Theoretical Interpretation of Equivalent
breadths of Absorption Lines/Tp. J., o4,m ; m e '------------------ —
Intensities of Blended Absorption Lines,Ap. J., 'ft, 4 M , IbSs.
Relative Multiplet Strengths in LS Coupling,• iP . j :, it, i. --------Roto on Absolute Multiplet Strengths, Ap. J.,
Introduction to Atonic Spectra.McGraw-Mill Book do., hew fork, 1954.
The Temperature of the Solar Reversing Layer from Relative Intensities of the ■Rotational Lines of Cyanogen. Library, Unlv. of Arizona, aTS5”Ap7 J . , 9 1 , 421 , 1940.
41APPENDIX
Table 2.
'0
3
W. L. R. I. W (i
8S85e859 1 2154*259 -2 234.531 2 4434.919 3 6335.415 4 6435.727 3 %36.024 -1 936.568 7 16436.964 -11 837.244 1 2137.497 2 3257.738 .3 3237.904 4 8038.258 1 4838.560 2 48
38.796 1 1740.127 . 5 6840.716 3 10841.096 7 21642.091 6 23242.256 3 1942.672 -1 4343.266 2 4443.390 2 3843.683 3 5444.230 1 3344.635 S 6444.913 -2 1845.196 4 5545.513 0 2045.646 6 13245.830 3 7546.207 1 3146.543 -1 846.710 -1 2747.027 0 S47.800 5 4148.191 6 8748.462 -1 5649.010 2 34
r 6. I.Local True
0.77 0.8 0.680.83 0.92 0.760.78 0.72 0.570.82 0.69 0.480.72 0.60 0.430.78 0.60 0.470.81 0.89 0.720.81 0.41 0.350.80 0.94 0.760.83 0.82 0.6S
0.70 0.73 0.610.56 0.76 0.480.85 0.50 0.420.79 0.64 0.300.81 0.65 0.530*86 0.83 0.710.89 0.58 0*810.94 0.43 0.410.92 O.S7 0.340.90 0.37 0.33
0.57 0.78 0.450.87 0.74 0.660.85 0.70 0.S90.88 0.68 0.580.92 0.62 0.66
0.94 0.70 0.700.96 0.62 0.600.88 0.88 0.780.90 0.67 0.610.70 0.88 0.620.93 0.45 0.410.94 0.85 0.620.94 0.65 ■ 0.610.96 0.91 0.880.96 0.90 0.87
0.87 0.94 0.830.64 0.63 0.410.87 0.42 0.340.90 0.79 0.710.92 0.67 0.60
W. L. R. I . H (*4) r e .Local
I .True
3549•243 r 22 0.92 0 .8 0 0 .7349.572 0 6 0 .9 0 0 .9 8 0 .8 649.626 -1 ' 5 8 .9 9 0 .9 4 0.9349.873 3 64 0.96 0 .5 6 0.5260.223 1* 31 0 .9 0 0 .8 3 0 .7 4
50.600 ' 4 ' 54 , 0 .8 6 0.66 0 .4 960.799 -2d 4 0 .88 0.96 0.8451.113 1 83 0 .9 0 0.75 0.6451.634 4 119 0 .9 2 0 .5 5 0 .4 461.660 1 8 0 .7 2 0 .8 9 0 .6 4
61.968 1 48 0.92 0 .6 4 0.5952.11352.434
2 ‘ 54 0 .9 7 0 .6 4 0.660 23 0.96 0 .7 7 0.7362.726 1 9 0.53 0 .9 0 0 .8 1
62.846 6 159 0 .9 4 0.59 0.3752.992 1 7 0 .5 7 8 .9 : 0.6063.164 -1 7 0.81 0.92 0 .7 753.484 3 61 0.80 0.56 0 .4 463.747 6 80 0.78 0 .5 1 0.3964.123 6 64 0 .8 2 0.51 0.4154.511 ' ■ -3 70 0.72 0 .6 6 0 .4 064.649 1 9 0.68 0 .8 6 0 .6 564.938 9 381 0 .93 0.82 0 .2 665.466 2 40 ■ 0 .88 0 .6 8 0 .6 166.948 -2d? 6 0.92 0.84 0 .6 7
56.804 4 220 0 .8 6 0 .3 1 0.2667.366 -1 7 0 .8 8 0.92 0 .6 468.073 1 20 0 .7 8 0 .7 8 0 .6 058.633 8 508 1.00 0 .2 6 0 .2 258.784 1 26 0.61 0 .7 5 0 .4 6
59.080 1 28 0 .78 0.72 0.5669.617 5 71 0 .8 8 0.50 0 .4 459.924 0 18 0 ,82 0 .7 6 0 .6 260.077 -1 15 0.82 0 .8 2 0 .8 760.417 -2 2 0;82 0.94 0.7860.898 4 50 0 .7 8 0 .5 4 0.4861.583 1 49 0 .91 . 0.68 0.5861.768 3 34 0.70 0.62 0.4481.904 1 16 0.74 0 ,7 8 0 .S862.097 OH 6 0 .8 2 0 .9 3 0.76
W.L. B. I. W (a4) r C.Local
I.True
3562.271 1 26 0.96 0.72 0.6962.927 ON 28 0.91 0.79 0.7663.160 -2N 11 0.96 0:89 0.8663.404 -21 5 1.00 0:94 0:9463.612 -1 11 o;S4 0.86 0.82
63.790 -2* 9 0.98 0.90 0.8864.127 4 59 0.90 0.82 0:4764.626 3 49 0.71 0.55 0.4064.797 -1 4 0.62 0:94 0.5864.987 4 60 0.58 0.58 0.8065.687 4 80 0.84 0.76 0.2666.839 0 8 0.54 0.94 0.61§6.978 1 16 0.62 0.78 0.4066.176 2N 22 0.39 0.80 0.3166.384 10 264 0.71 0.80 0.21
66.690 . 1 19 0.51 0.81 0.4167.048 2 80 0.89 0.48 0.4267.378 1 48 0.88 0.61 0.6867.697 < 80 0.83 0.42 0.8667.945 -1 14 0.87 0.84 0.7568.249 -1 12 0.79 0.88 0.7068.449 3 44 0.77 0.68 0.4468.629 -1 4 0.80 0.92 0.7468.830 3 62 0.80 0.52 0.4268.984 4 52 0.69 0.52 0.8669.885 6 129 0.68 0.86 0.2069.511 4 18 0.38 0.78 • 0.2570.988 0 7 0.69 0.91 0.6271.234 5 SS 0.89 0.59 0.4871.408 -1 3 0.76 0.9# 0.7871.690 2 SO 0.58 0.71 0.4271.876 6 200 0.77 0.32 0.2572.322 -3 2 0:76 0.98 0.7472.479 4 188 0.78 0.84 0.2872.752 -1 8 0.84 0.89 0.76
78.068 IN 37 0.98 0.69 0.6873.408 2 48 0.88 0.87 0.8074.086 0 9 0.60 0.85 0.5174.264 0 86 0.91 0.75 0.6274.417 1 54 0.98 0.55 0.55
44
W. L. a . i .
3574.808 074.968 676.122 575.265 376.566 2
75.766 -175.979 4
,76.530 . 476.767 2
, 78.864 1
77.064 -277.246 177.466 177.876 578.101 1
78.219 -178.395 " 478.694 1079.569 -2 179.665 , 1
,79.836 280.088 -180.217 IS80.413 180.543 IN
80.928 681.201 SO81.666 281.818 281.942 1
82.206 582.552 282.572 282.699 385.540 6
83.698 385.912 384.318 -284.621 284.662 6
r C. I .L eeal , True
0 .80 0 .81 ■ 0 .650 .69 0 .5 6 0 0 80 .6 7 0 .75 0 .4 20 .6 5 0 .7 0 0 .5 70 .9 0 0 .58 0 .5 4
0 .98 0 .8 0 0 .7 60 .9 4 0 .4 8 , 0 .4 40 .9 7 0 .5 6 0 .5 60 .98 0 .4 4 0 .4 40 .6 2 0 .8 4 0 .6 2
0 .9 6 0 .9 2 0 .8 80 .9 4 0 .7 2 . 0 .6 70 .9 4 0 .7 2 0 .6 80 .85 0 .4 0 0 .3 80 .68 0 .8 6 ; 0 .5 8
0 .70 0*95 0 0 80 .68 0 .6 8 0 .3 90 .68 0 .3 7 0 .250 .82 0 .9 4 0 .7 80 .7 7 0 .7 9 0 .6 0
0 .70 0 .73 0 0 80 U 2 0*95 0 0 80 .68 0 .8 3 0 0 90 .48 0 .8 7 0 .4 20 .42 0 .9 2 , 0 .3 8
0 .2 7 0 .78 0 .2 11 .00 0 .1 6 0 .1 60 .5 1 0 .8 0 0 .2 50 .52 0 .8 5 0 .2 70 .39 0 .8 2 0 .8 4
0 .59 0 .7 5 0 .2 80 .68 0 :60 0 .5 40 .44 0 .9 0 0 .3 70 .62 0 .S 2 0 .550 .59 0 .5 4 0 .3 2
0 .6 0 0 .59 0 .560 .5 6 0 .6 5 0 .3 60 .71 0 .9 4 0 0 70 .4 6 0 .7 6 0 .410 .61 0 .5 4 0 .21
W (mA)
! 1644
, 182885
1675102
8210
5242889112
51266422SO3
16IS6
221686
171117
18478
746848416
18149
45
W. L. B. I .
3884.801 684.966 . 6
.86 .171 . 588.619 286.716 6
,86 .119 4.86 .868 -186.646 486.761 386.991 8
87.430 387.761 587.944 688.125 -288.247 0
88.326 -188.623 488.926 289.115 489.462 2
89.633 689.768 eat89.969 . - i90.096 i i90.469 2
90.663 - -191.009 . . 191.366 291.489 292.028 2
92.478 192.679 592.900 093.083 093.496 9
93.796 -293.998 -2%94.639 694.877 396.116 1
r 6. I.h&atl True
0 .4 0 0 .6 7 0 .2 70.42 0.67 0.420 .2 2 0 .8 3 : 0 .1 70.50 0 .8 4 0 .2 80 .43 0 .4 0 0 .1 5
0 .49 0.42 0 .2 10.66 0.92 0 .5 60 .6 3 0.89 0 .3 50 .59 0 .6 6 0.260 .52 0 .3 3 . 0 .15
0 .60 0 .4 8 0 .2 80 .6 8 0 .4 8 0.840 .8 0 0.42 0 .250.58 0 .96 0 .5 60 .5 8 0 .8 0 0 .4 6
0 .59 0 .6 6 o .e o0.80 0 .4 8 0 .2 50 .59 0 .6 3 0.621.00 0.41 0 .2 60.57 0.54 0.30
0 .4 6 0.49 0 .2 4O .iS 0 .48 0 .2 80.54 0 .89 0 .4 80 .6 6 0 .7 0 0.390.74 0 .3 0 0.23
0 .7 6 0 .8 5 0 .6 60.86 0 .6 0 0 .6 20.74 0 .8 6 0.430 .7 6 0.89 0 .4 40 .9 0 0 .4 6 0 .4 1
0 .8 4 0 .6 2 0 .6 20.81 0.49 0 . #0.78 0.64 0.600 .7 3 0 .7 3 0.540.76 0.23 0.18
0 .7 4 0 .9 0 0 .6 60 .79 0.81 0 .6 40.76 0 .4 2 0.320 .7 7 0 .48 0 .3 60 .8 2 o.m 0.48
W (ml)
24261710. 16884
. 54828. 227
. 6868. 77216
. 510060189
. 48
43. 66
62211012383936
. 64
36662921247• 820
. 866342
w. L. B. I. W (mA)
3595.309 2 46! «“2 10
95.880 1 2696.056 4 4696.206 1 4896.610 0 1697.048 Sd? 7997.718 8 16898.272 1 4498.721 1 ~ 39
98.940 2 . ’ 4899.146 2 6299.382 -2* 899.632 8 54
8699.971 1 88
8600.172 -SB 400.740 5 SO01.199 ■2 801.429 -2 h01.665 0 3201.928 1 5402.069 5 6702.286 4 4802.470 3 9702.679 • -8 32
08.098 1 1903.211 5 12105.981 1 4604.278 1 4504.ST9 2 84
04.705 1 4004.984 -2 406.085 ' -1 1106.202 6 1206.917 1 5406.040 -2 606.879 0 1706.856 1 IS07.580 -2 607.684 3 49
r C. I .Local T rw
0.85 0.52 0.440.94 0 .8 6 0.800 .8 4 0 .6 6 6.6®0 .69 0 .6 8 0.860 .92 0.52 0 .4 8
0.94 0 .8 0 0.740 .9 8 0.44 0 .4 10 .9 0 0.50 0.270.96 0.60 0 .6 80.87 0 .5 7 0.500.75 0.67 0.420 .88 0.48 • ei«0.87 0.90 0 .6 60.91 0.60 0 .4 50 .9 0 0.60 0 .5 4
0 .9 5 0.94 0 .360 .9 4 0.48 0.460.98 0.90 0 .890 .92 0 .8 8 0 .8 10.89 0.68 0.570 .9 0 0.68 0 .4 60 .78 0.41 0.820 .69 0 .4 8 0 .8 80.67 0.42 0 .2 80.93 0.66 0.620.64 0.76 0.480.89 0.56 0.520.98 0 .5 5 0 .4 96.94 0.62 0.586 .7 9 6 .6 0 0.480.89 0.46 0 .4 00 .7 6 0 .9 1 0 .4 40.52 0.88 0.500 .3 4 0.86 0.290 .7 6 0.62 0 .49
0.76 0.91 0 .690 .8 0 0 .76 0 .6 10.68 0.61 0 .6 20.69 0 .W 0.660 .8 7 0.60 0 .45
47.
w. L. a . i . W (m
3608.011 ~2 4308.166 4d? 4408.498 3 5008.870 20 97209.529 5d? 57
09.473 2 : 7009.769 -21 1010.167 5 17710.297 2 1010.461 4 78
10.703 3 7611.061 2 3411.186 1 1611.460 0 1511.689 - i 9
, 11.724 2 4211.896 -1 1012.076 4 7012.520 -2 8
-r) 12.745 6d? 164
12.942 3 3415.110 2 8615.460 2 3113.606 2 2313.810 4 . 110
14.119 2 . 56, 14.662 2 S3
19.777 2 1819.938 1 1220.033 0 16
20.248 2 ' : . 2620.489 3 . 7220.880 1 6421.468 6 5921.726 2 . 36
22.010 ■ ' 6 72n 22.666 -2 8
: 23.193 I l l23.461 2 4723.786 4 60
r C. I .Local fn w
0 .7 3 0 .6 6 0 .4 80 .6 0 0 .6 3 0 .3 20 .4 4 0 .7 2 • o .3 11 .0 0 0 .1 9 0 .19 .0 .6 0 0 .6 0 0 .3 0
0 .81 0 .6 2 0 .4 20 .81 0 .9 1 0 .7 40 .8 0 0 .3 0 o;240 .88 0 .8 2 0 .220 .53 0 .4 6 0 .2 4
0 .8 6 0 .8 2 0 .4 00 .78 0 .6 7 0 .4 40 .78 0 .7 2 0 .6 60 .9 0 0 .7 7 0 .6 90 .89 0 .6 2 0 .7 4
0 .89 0 .6 9 - 0 .520 .86 0 .8 4 0 .7 20 .89 0 .4 3 0 .380 .9 0 0 .9 4 0 .8 60 .96 0 .4 0 0:31
0 .79 0 .6 8 0 .4 80 .94 0 .4 6 0 .4 30 .8 4 0 .6 2 0 .820 .72 0 .7 5 0 .6 20 .73 0 .4 9 0 .5 4
0 .89 o.m 0 .530 .89 0 .6 6 0 .490 .5 6 0 .7 7 0 .4 40 .61 0 .8 6 0 .6 30 .72 0 .9 1 0 .6 8
0:74 0 .7 0 0 .6 00 .89 0 .5 3 0 .4 60 .88 0 .6 3 0 .880 .6 3 0 .6 7 0 .3 60 .7 6 0 .6 1 0 .46
0 .8 0 0.4® 0 .3 70 .9 6 0 .9 1 0 .8 60 .9 2 0 .4 6 0 .4 00 .79 0 .6 6 0 .4 40 .79 0 .4 9 0 .39
48
W. L. R. I. W (mA) r C.Local
I.True
3623.918 1 6 0.59 0.90 0.5324.119 5 60 0.64 0.53 0.3424.305 3 36 0.66 0.61 0.4024.964 1 11 0.65 0.84 0.5525.148 5 55 0.75 0.51 0.3825.502 1 31 0.96 0.72 0.6925.754 —2 10 0.94 0.88 0.8226.110 0 43 0.98 0.67 0.6526.188 1 33 0.94 0.67 0.6326.740 2 42 0.96 0.61 0.6827.062 2 40 0.94 0.62 0.5927.814 4 63 0.92 0.46 0.4228.099 2 50 0.90 0.64 0.4928.280 -2N 4 0.88 0.95 0.8428.600 -1 12 0.85 0.86 0.7128.708 2 77 0.96 0.56 0.5428.829 2 72 0.95 0.56 0.6429.007 -3 4 0.89 0.92 0.8229.353 -2N . 12 0.95 0.90 0.8429.738 1 35 0.90 0.65 0.5829.906 1 19 0.78 0.76 0.5830.028 1 24 0.84 0.72 0.6230.235 0 12 0.75 0.86 0.6430.356 4 46 0.72 0.47 0.3430.779 3 97 0.58 0.40 0.2430*986 2 18 0.41 0.75 0.3031.476 15 1257 1.00 0.21 0.2132.300 -1 7 , 0.68 0.90 0.6232.561 3 47 0.78 0.62 0.4132.841 1 46 0.80 0.82 0.5033.513 33,653
-Id? 18 0.78 0.84 0.65-2 5 0.79 0.92 0.7335.836 4 65 0.86 0.42 0.8634.711 4 53 0.62 0.65 0.3334.953 3 57 0.66 0.62 0.3435.198 2 26 0.58 0.68 0.5935.469 4 44 0.71 0.59 0.8835.829 -1 10 0.88 0.89 0.7836.239 2 91 0.89 0.42 0.5737.001 2 63 0.64 0.49 0.41
49
W. L. S. I. W(mA) r 6 .Local
I.True
3637.256 1 36 0.82 0.63 0.5237.555 ' -1 12 0.95 0*66 0.8257.738 0 34 0.94 0.68 ' 0 . 6437.874 4 35 0.71 0.64 0.4588.506 3 140 0.90 0.36 0.35
38.606 -3 4 0.98 0.98 0.9838.906 -2 14 0.19 0.87 0.8639.031 0 19 0.95 0 .8 0 0 .7639.286 1 40 0.96 0.64 0.64$9,806 2 4$ 0.93 0.88 0 .6 4
’ 40.396 6 89 0.92 0 .4 6 0.4240.646 -2 4 0.92 0.94 0 .8641.035 1 28 0.96 0.71 0.6841.336 4 75 0U92 0.48 0.4441.460 1 14 0.68 0.79 0 .64
41.647 ' 1 21 0.86 0 .70 0.8041.966 -1 12 0.89 0.83 0.7342.282 -o r 6 0.90 0.92 0.8242.399 ' -2 5 0.86 0.92 0 .8042.538 -S 2 ' 0 .87 0.97
■ . . ;/ 0.8442.683 7 ISO 0.62 0.45 0.2848.962 -2 12 0.89 0.84 0.7444.418 5 82 0.84 0.46 0.4044.795 3 56 0.72 0 .61 0.3644.979
'0 6 0.66 0.89 0.52
46.083 2 38 0.74 0.67 0.4245.291 3 94 0 .74 0 .4 7 0.3445.498 3 74 0.90 0.47 0*4245.828 4 47 0.89 0.47 0.4246.098 -1 14 0 .80-.. - - 0.82 0.6646.1*7 1 SO 0.89 0.63 0.5946.619 2 28 0.82 0.65 0.5446.989 2 SO OiTS 0,66 0.4847.096 0 12 0i78 0 .86 0.8447.429 4 34 0.50 0*64 0.32
47.852 12 1042 1.00 0 .20 ’ O.to46.531 0 16 0 .76 0.79 0.6148.999 1 29 0.82 0.65 0.5349.299 4 152 1.00 0.38 0.3449.512 6 72 0.69 0.42 0.29
50
W* L. B. I. W (mA) r (Local
8649.699 9 0.71 0.8549.838 1 24 0.69 0.6860.038 4 66 0.68 0.4960.286 5 63 0.71 0.4850.639 2 67 0.96 0.4961.475 7 92 0.77 0.8861.665 1 16 0.67 0.8051.801 4 31 0.68 0.6252.261 -1 12 0.94 0.8652.562 3 62 0.95 0.50
68.863 1 26 0.86 0.7053.502 5 69 0.79 0.4853.762 2 52 0.79 0.6154.447 -1 10 0.88 0.8664.699 2 42 0.86 0.60
65.004 2 47 0.94 0.6065.220 -1 10 0.84 0.8466*356 3 8 0.61 0.6856.662 3 96 0.98 0.4256.862 -3 7 • 0.91 0.9056.220 3 101 0.97 0.4066.368 1 38 0.89 0.7656.549 -2 6 0.98 0.9256.966 0 18 0.91 0.7767.138 2 44 0.89 0.54
67.424 1 82 0.98 0.6667.712 IK . 43 0.92 0.6767.906 3 49 0.74 0.5568.100 1 74 0.98 0.4858.661 1 32 0.96 0.64
59.525 6 57 0.86 0.4959*783 5 69 0.84 0.4860.212 —1 29 0.94 0.7460.637 2 25 0.86 0.6760.779 2 28 0.92 0.65
61.039 -2* 9 0.93 0.9061.373 3 48 0.98 0.5661.958 3 44 0.98 0.5462.241 5 79 0.91 0.4562.365 -3 3 0.88 0.94
I.True
0.60 0.47 0.34 0.34 0.47
0.270.460.350.800.48
0.S80.880.480.760.52
0.570.700.580.400.82
0.390.640.850.700.48
0.610.690.410.460.61
0.420.410.700.680.60
0.880.640.800.400.88
51.
W. L. i. I.
3662.842 468.69968.968 264.098 . 64?64.829 ; -2*
65.029 -1*68.725 -165.65166.251 366.540 1
66.645 ■ , -166.771 . 368.98^ SHd?67.262 . 4 ■67.751' !
. ,. ' . 'i
67.997 468.218 368.660 - 1 168.970 169.245 4;
69.527 469.687 169.840 -3*70.818 4.:71.277 o
71.625 071.688 371.948 -372.126 -272.517 -5
72.466 -272.715 573.088 373.227 OH78.427 -2
78.684 -173.889 274.414 276.(XX) -375.295 1
r C. I.L@e#l True
0.96 0.47 0.440.94 0.80 0.760.66 0.76 0.61'0.9# 0.36 0.350.85 0.84 0.72
0.95 0.76 0.721.0# 0.79 0.780.95 0.94 0.870.82 0.62 0.420.90 0.58 0.620.79 0.81 0.680.60 0.62 0.490.93 0.46 0.440.90 0.48 .0.480.98 0.92 0.900.97 0.46 . . 0.4#0.92 0.88 0.490.98 0.84 - 0.780.84 0.62 0.520.74 0i51 0.580.70 0.62 0.570.90 0.66 0.580.90 0.92 01840.95 0.60 0.470.99 0.72 0.71
0.99 0.69 0.680.96 0.66 0.5*1.00 0.96 0.961.00 0.90 0.901.00 0.96 0.96
0.99 0.85 0.840.99 0.57 0.680.99 0.51 0.510.93 0.74 0.680.92 0.82 0.78
0.94 0.82 0.770.88 0.62 0.540.94 0.80 0.660.98 0.94 0.920.95 0.74 0.70
W(mA)
701615
13412222035648
113568TO668441127495427461228044874
1148682714
148534S26
W. L. B. I.
3678.460 -175.690 176.977 -276.323 > s76.563 2
77.319 478.10178.235 lid?78.870 479.003 2
79.113 -2 179.362 179.540 179.686 179.924 9
80.390 2^0.666 380,803 480.945 381.231 2
81.27281.664 , 381.886 082.626 -1*82.671 OH
83.046 • 383.093 483.481 -3 .83.624 284.124 7dt
3685.197 lOd?3716.181 2
15.477 ■ 416.917 316.155 -31
16.452' i7
16.700 -317.188 -117.308 217.837 0
r • . C. I.Local' True
0 .9 4 0 .8 8 0.8©0.97 0 .6 8 0 ,6 80 .0 4 0.88 0 .8 40 .9 6 0 .4 8 0.410 .8 6 0 .6 9 0.690.93 0 ,4 1 0 .390.72 0.94 0 .6 80.78 0 .7 4 0 .5 80 .92 0 ,4 6 0.420 .8 7 0 .6 2 0 .4 6
0.74 0 .9 4 0 .7 00.84 0.72 0.600 .7 1 0.81 0 .5 80 .5 8 0 .7 8 0 .4 41 .0 0 0 .3 3 0 .2 7
0 .7 8 0.84 0 .5 00 .8 2 0 .4 8 0 .4 80 .5 0 0 .6 4 0 .3 20.82 0 .5 2 0.420 .8 5 0.60 0 .51
0 .8 8 " -0,86 0 .8 6 0 .4 80.82 0.81 0.660 .6 6 . 0.96 0 .6 80 .73 0.84 0 .6 0
0 .7 8 0 ,3 8 0 .2 70 .7 8 0 .3 7 0 .28 "0 i7 4 0.96 0 .7 00 .7 4 0 .6 8 0 .5 10.70 0.40 0.320 .90 0.89 0 .3 40 .59 0 .7 0 0.390.78 0.4# 0.320.73 0.61 0 .4 40 .78 0.94 0 .7 3
0 .79 0 .4 8 0 .3 70 .82 0 .9 8 0 .790 .9 3 0 .9 4 0 ,890 .9 0 0 .8 9 0.640 .91 0 .8 7 0 .7 9
52i
W(nA)
12SS9
545S
805
267078
3221216
514
5261265533
564®12
418
124116
2SO100160
29127
414
10414
259
53
3
"3k
W. L. B. I.5717.956 -21
18.153 OH18.413 418.952 119.949 40
21.279 321.687 4d?21.952 322.050 222.258 1
22.590 625.611 125.846 024.094 124.587 6
24.576 124.851 125.160 125.508 025.500 3
26.025 026.667 026.922 4d?27.100 327.549 127.656 427.820 228.044 228.554 OH28.404 -128.675 228.956 Id?29.341 029.526 -129.815 330.014 -150.394 330.758 150.952 551.161 -1
W (xnA) r
3 0.9128 0.8838 0,7842 0.67
2104 1.00
10 0.4628 0.6557 0.6218 0.8912 0.66736 1.0010 0.7611 0.7916 0.8266 0.80
22 0.8029 0.8220 0.823 0.8336 0.8510 0.87IS 0.86
101 0.6060 0.6618 0.54
525 1.0024 ' - 0.4514 0.6914 0.7921 0,92
37 0.8843 0.878 0.984 1.0050 0.928 0.90
134 0.8847 0.8048 0.785 0.77
C. I.Local True0.96 0.880.78 0.750.66 0.460.64 0.430.30 0.50
0.82 0.370.75 0.850.67 0.420.74 0.440.84 0.48
0.88 0.290.66 0.650.92 0.730.80 0,660.58 0.48
0.71 0.670.72 0.600.72 0.610.98 0.790.63 0.58
0.92 0.790.83 0.720.43 0.340.52 0.340.85 0.45
0.80 0.300.74 0.880.80 0.550.86 0.680.85 0.78
0.89 0.820.68 0.600.90 0.680.94 0.980.56 0.S2
0,88. - 0.780.46 0.400.58 0.440.60 0.420.95 0.78
W. L. R. I. W (mA) r C. I.Local True
5751.263 0 6 0.69 0.91 0.6451.583 3 46 0.89 0.55 0.4931.625 -1 5 0.84 0.92 0.7831.729 -1 2 0.85 0.96 0.6231.952 0 4 0.62 0.92 0.6632.037 2 25 0.76 0.66 0.5032.408 6 73 0.70 0.49 0.3432.754 2 29 0.69 0.64 0.4453.197 1 18 0.27 0.86 0.2735.332 7d? 213 0.58 0.34 0.20
33.494 1* 14 0.30 0.90 0.3234.137 1 61 0.41 6.91 0.3854.876 40 2575 1.00 0.29 0.2935.336 4 21 0.34 0.76 0.2738.966 0 29 0.55 0.84 0.46
37.143 30 1269 1.00 0.27 0.2738.314 3 65 0.69 0.48 0.3438.612 1 12 0.70 0^0 0.5639.000 -1 2 0,65 0.94 0.7939.120 2 45 0.83 0.5# 0.4639.230 3 94 0.77 0.35 0.2739.327 1 8 0.55 0.86 0.4739.531 3 53 0.82 0.S3 0.4439.785 1 23 0.89 0.74 0.6440.066 3 39 0.93 0.60 0.S6
40.247 3 83 0.89 0.60 0.4541.067 4 54 0.96 0.67 0.6241.481 1 34 0.91 0.66 0.6041.647 4 71 0.86 0.47 0.4042.148 1 36 0.86 0.68 0.58
42.625 3 79 0.92 0.60 0.4842.952 1 81 0.78 . 0.66 0.6143.370 . 6 469 1.00 0.20 0.2243.781 1 22 0.70 0.71 0.«343.890 2 29 0.74 0.64 0.47
44.112 4 76 0.81 0.S1 0.4144.568 1 42 0.83 0.64 0.6545.576 8 943 1.00 0.29 0.2945.912 8 311 0.66 0.39 0.2646.050 0 6 0.29 0.88 0.29
55
w L. B. I. W (mA) r jC. I.Local free
5746.246 1 9 0.68 0.87 0.5146.477 2 . ; - 54 - 0.64 0.61 0*3946.576 1 ■ . ■ 42 0.7* 0.66 0.4846.924 3 90 0.74 0.44 0.5547.227 0 ' 10 0.74 0.86 0.6447.560 -1 1 0.60 0.67 0.7747.664 1 28 0.74 0.70 0.6248.002 1 30 0.44 0.76 - 0*3448.275 10 801 1.00 0.81 0.5148.508 1 6 0.34 0.92 0.3248.679 1 17 0.47 0.76 0.3648.968 2 74 0.57 . 0.60 0.2249.497 20 2470 1.00 0.19 0.1949.940 0 6 . 0.46 0.91 0.4260.506 1 12 0.56 0.86 0.4750.6W : i 16 0.66 0.81 ' 0.4860.874 2 19 0.66 0.78 0.4951.092 1 18 0.68 0.76 0.5261.226 OK 7 o . n 0.90 0.6451.694 1 28 0.77 0.70 0.5451.826 1 58 0.82 0.62 0.5062.417 5 50 0.82 0.56 0.4662.062 4 66 0i83 0.47 0.4052.994 1 18 0.80 0.74 0.6865.144 2 ' 26 0.81 0.66 0.5455.542 1 SO 0.84 0,66 0,6055.622 6dl 86 0.84 0.49 0.4264.541 -IK 5 0.91 0.93 0.8464.607 ... 3 • 55 0.88 0^0 0.4466.156 ' 0 6 0.98 0.92 0.9066.464 IK 20 0.96 0.76 0.7266.575 -1 11 0.94 0.90 0.8656.074 - 3 46 0.98 0.64 0.5366.945 : 4 63 : 0.88 0.62 0.4657.167 1 14 0.81 0.82 0.6657.460 2 28 0.66 0.63 0.4157.686 4 66 0.68 0.62 0.8658.247 15 1048 1.00 0.17 0.2769.501 12d? 239 0.81 0.86 0.3359.475 0 - 5 0.61 0.96 0.67
W. L. R. I . W(nA) r C.Local
I.True
S759.587 1 12 0.72 0.81 0,6860.057 6 67 0.80 0.49 0.4060.226 1 11 0.80 0 .8 5 [email protected] 4 62 0.81 0.50 0.4081.822 7 146 0.79 0.40 0.5161.692' IN 11 0.83 0.76 0.6361.876 5 46 0 .88 0.61 0.5262.212 2 68 0 .8 0 0 .4 6 0*4862.620 1 15 0.90 0 .7 9 0,7063.010 2 28 0 .79 0.74 0.6865.673 1 6 0 .3 6 0.91 0.3268.805 10 775 1 .0 0 0 .2 9 0.2964.115 1 7 0.46 0 .9 0 0.4264.223 1 10 0.65 0 .8 5 0 .4 664.386 —IN 5 0 .7 0 0.96 0.6665.306 0 •‘■'6 0.86 0.93 0.7665.663 6 140 0.96 0*41 ■ 0.3565.712 1 56 0.89 0 .5 4 0.4966.096 2 40 0 .9 0 0.60 0.5466.469 -1 2 0.78 0 .9 6 0.7B66:668 3 38 0.66 0.63 0.8666.822 ’ 1 16 0.62 0.77 0.4867.206 8 788 1 .00 0 .2 9 0.2967.652 0 15 0.60 0.92 0 .6 668.036 3 47 0.82 0.64 0.4468.250 2 27 0.77 0.71 0.6268.408 0 6 0.78 0.90 0.7068.785 1 82 0.80 0.76 0.6269.021 ON 7 0.82 0.93 0.7769.465 5 33 0.78 0.66 0 .8 2
69.996 4 42 0.88 0.60 0.4270,171 -1 26 0.68 0 .9 6 0.6670.309 2 81 0 .69 0.68 0 .4 070.415 2 21 0.87 0.74 0.4270.601 1 13 0.60 0.84 0.6070.974 2 22 0 .6 6 0.76 0.5171.499 1 18 0.70 0.78 0.6471.660 2 27 0.71 0.70 0 ^ 272 *686 2 48 0.82 0.67 0.48'72.953 Old? 14 0.86 0.89 0.77
17
3
3
w. L.3775,566
75*70173,89274,33874.664
74.85475.58075.86276.06176.200
76,46376.561 77.076 77.354 77.458
78.06878.16578.52978.51778.705
78.80079.02979.20979.45380.708
81.19381.61781.94082.12182.465
82.61583.19183.561 83.53785.820
85.90284.25484.60686.23685.709
H. I. W (nA) r 0.Looel
1 17 0.80 0.753 48 0.82 0.68
-1 3 0.86 0,963 52 0.88 0.541 32 0.84 0^44 100 0^6 0.5©7 101 0.90 0.421 21 0*86 0.722 38 0.82 0.67OK 4 0.87 0.943 62 0.92 0.481 41 0.94 0.592 -44- 0.95 0,571 38 0.9© 0.623 60 0.91 0.53
2 28 0.76 0.840 4 0.77 0.923 37 0.8© 0.6#2 47 0.78 0.673 44 0,78 0.68
1 46 0,92 0,64-1 ' 5 0.96 o.»g1 27 0.90 0.684 106 0.88 0.463 61 0.87 0.68
5 60 0.97 0.611 45 0.91 0.622 40 0.92 0.6®1 38 0.87 0.602 82 0.81 0.63
1 48 0,98 0.66-1 4 0.91 0.982 40 0.91 0.806 88 0.83 0.40
" 110 0.60 0.88
-1 15 0.88 0.80••o- 10 0.96 0.8f0 17 0.93 0.810 26 0.89 0.791 39 0.81 0.68
I.
0,610.460.820.480.54
0.480.380.620.470,81
0.480.560.620.560.48
0.480.710.470.440.43
0.500.890.620.400.60
0.600.670.620.580.50
0.640.860.540.540.70
0.700.820.760.700.47
Yl. L. a. I. W(ffiA) r 6. I.1«OC8l1 True3785.792 1 20 0.68 0.70 0.4885.954 5 46 0.72 0.66 0.4086.044 1 13 0.50 0.78 - 0.6986.177 4d? 37 0.68 0.62 0*6686.381 1 14 0.59 0.78 0.4786.684 5 105 1.00 0.44 0.3687.168 1 71 Oils: 0.62 0.4#87.893 9 397 1.00 0.42 0.3888.441 0 14 0.83 0.84 0*7088.703 2 ' 28 0.77 0.68 0.5488.863 1 , 14 0.68 0.82 0.6689.186 3 38 0.75 0.68 0.4689.421 21 38 0.67 0.60 0.3489.579 1 31 0.76 0.62 0.4689.824 1 28 0.6® 0.69 0.4890.100 5 73 0.79 0.61 0.3190.225 m 48 0.63 0.61 0.3290.493 1 31 0.74 0.67 0.5090.659 1 26 0.73 0.67 0.4991.112 0 18 0.88 0.60 0.7091.382 1 19 0.87 0.80 0.6691.511 2 31 0.86 0.62 0.6491.751 1 32 0.87 0.66 0.6792.160 3 33 0.79 0.62 0.4992.349 1 34 0.79 0.70 0.6892.688 2 29 0.61 0.65 0.4092.834 2 50 0.75 0.68 0.5093.360 1 16 . 0.65 0.71 0.3793.487 2 21 0.64 0.70 0.3893.607 4 43 0.63 0.S8 0.4093.878 2 44 0.80 0.61 0.4994.349 4 71 0.85 0.49 0.4294.775 1 26 0.64 0.68 0.4396.014 8 664 1.00 0.33 0.5596.446 0 2 0.52 0.94 0.4995.540 1 51 0.70 0.64 0.4595.902 0 2 0.72 0.97 0.7296.017 0 6 0.71 0.66 0.6096.109 0 6 0.64 0.90 0.8896.188 0 15 0.72 0.62 0.80
59
w. L. 1. I.
5796.393 006.498 096.806 196.889 29T.141 0
97.624 537.722 197.956 298.259 098.625 6
@8.905 099.263 1*4?
5799.560 73800.521 0*00.648 1
00.862 001.116 001.373 101.686 301.817 2
01.992 202.154 -102.287 203.092 103.260 1
03.484 004.016 804.288 004.614 104.795 2
06.181 605.747 OH06.221 206.377 006.447 0
06.720 8d?07.183 607.646 $07.989 108.136 1
r C. I.Weal True
0.70 0.94 0.660.71 0.92 0.640.54 0.90 0.490.64 0.66 0.420.88 0.79 0.460.69 0.62 0.380.49 0.88 0.42O.GO 0.69 0.350.45 0.95 0.420.56 0.48 0.26
0.31 0.92 0.660.32 0.91 0.461.00 0.12 0.520.84 0.86 0.720.86 0.62 0.700.89 0.88 6.7#0.88 0.84 0.710.68 0.79 0.540.68 0.67 0.530.54 0.64 0.34
0.76 0.49 ■ 0.370.78 0.92 0.720.84 0.66 0.460.74 0.64 0.470.94 0.67 0.64
0.92 0.76 0.700.96 0.46 0.430.98 0.91 0.8#0.91 0.64 0.691.00 0.47 0.470.96 6.34 0.530.96 0.91 0.640.76 0.66 0.400.77 0.78 0.600.80 0.69 0.60
0.84 0.36 0.300.80 0.38 0.8©0.78 0.39 0.300.81 0.67 0.640.76 0.64 0.49
WCnA)
5664919
es142922161
48
11621219
9ITITU24
50.:.4871632
207663963
1T46
8916IT.112§61172841
59
W. L. 8. I. Tf (mA) r C.Local
I.True
3808.288 1 S3 0.92 0.68 0.5408.624 0 14 0.90 0.79 0.7206.756 3 76 0.8# 0.40 0.3609.061 1 49 0.97 0.52 0.6009.688 4 57 0.62 0.59 0.87
10.056 -Id? 8 0.94 0.94 0.8810.296 -la? 10 0.96 0.90 0.8710.902 0 4 0.74 0.91 0.6811.045 i 48 0.68 0.66 Qim11.500 i 44 0.92 0.66 0.63
11.382 0 4 0.77 Oi#6 0.6611.809 2 14 0.66 0.62 0.4611.896 2 152 0.99 0.38 0.3612.064 0 25 0.81 0.81 0.6012.260 -1 12 0.90 0.88 0.77
12.460 —2 6 0.94 0.96 0.8913.264 0 5 b.eo 0.94 0.5513.396 2 75 0.69 0.66 b.5413.493 0 8 0.68 0.87 0.4913.642 2 63 0.66 0.60 0.42
13.894 2 68 0.67 0.49 0.3814.124 0 15 0.80 0.84 0.6414.623 4 . 104 0.76 0.46 0.3014.786 1 37 0.69 0.62 0.4216.853 15 620 1.00 0.29 0.29
16.347 3 30 0.46 0.64 0.2916.470 1 . 8 0.56 0.87 0.4816.747 1 19 0.72 0.73 0.6816.924 1 37 0.78 0.62 0*4817.384 0 , 17 0.96 0.60 0.7417.649 3 84 0.78 0.47 0.3617.846 o , 18 0.84 0.74 ‘ 0.6218.246 1 63 0.88 0.67 0.5018.547 1 24 0.76 0.66 0.4618.477 o . 11 0.78 0.81 0.64
18.622 1 26 0.80 0.67 0.6419;065 lid? 39 0.84 0.66 0.6619.276 1 34 0.66 0.71 0*4619.496 2 58 b.se 0.68 0.3819.690 INd? 7 0.44 OiS2 0.41
1 7 ' 1 9 7
60
W . L. a. I. W (nA) r e.Local
X.Truo
5820.438 26 1249 1 .0 0 0.20 0.2021.188 4 63 0 .6 6 0 .8 4 0 .3 021.496 -1 4 0.68 0 .9 3 0.6821.730 IN 12 0 .68 0 .8 5 0 .4921.642 4 11© 0.78 0 .4 6 0.8221.939 0 27 0.60 0.81 0 .4 022.266 0 42 0 .8 6 0.67 0 .5 822.660 -1 6 0 .8 6 0 .6 9 0.7722.868 Id? 64 0.98 0 .5 1 0.4723.218 0 11 0 .88 0 .8 3 0 .7 5
23.368 -IN 2 0*62 0 .9 4 0 .7 723.516 4 70 0 .81 0 .4 1 0 .5 323.897 1 . 36 0 .6 6 0 .59 0.3224.084 1 36 0 .4 8 0 .6 4 0 .3 024.314 2 16 0 .2 6 0 .7 9 0.2924.464 6 222 0 .66 0 .9 4 0 .2324.576 1 2 0 .2 6 0.94 0*2224.928 1 24 0.62 0.74 0.4826.410 2 12 0 .4 0 0.88 0.8425.893 20 1104 1 .0 0 0 .1 8 0.1626.420 1 11 0.48 0.64 0 .4 128.627 IN 29 0.87 ©.TO 0.4026.864 2 86 0 .6 4 0 .5 3 0 .3 427.086 0 4 0.68 0.92 0.6327.303 1 26 0.67 0.79 0.4627.834 8 368 0.66 0 .25 0 .1 650.078 0 18 0 .6 4 0.77 0.6130.377 0 16 0.74 0 .8 6 0 .6 430.492 0 4 0 .68 0.61 0 .6 330.611 o 28 0 .59 0 .7 2 0.4830.766 2 22 0.82 0 .7 0 0.8630.869 2 40 0.62 0.67 0.8631.039 3d 40 0.60 0 .6 4 0 .3 851#200 -Id? 4 0 .6 4 0.96 0 .6 031.702 6 69 0.46 0.67 0.2632.890 3N 19 0.40 0 .7 7 0.8133.086 1 19 0 .3 6 0 .79 0 .5 433.319 4 56 0.63 0.61 0 .2 734.236 10 1432 1 .0 0 0.16 0 .1 634.731 0 3 0 .4 6 0 .9 4 0 .4 3
61.
%
W. L. K. I . W (mA) r I .Local f r w
3335«163 0 19 0 .4 0 0.62 0 .3 8- 86•092 2 38 0 .5 5 0.60 , 0.33- S6#5$9 . - 3 45 0 .5 7 0 .5 5 . 0 .3 1. 56 •808 1 41 0 .6 3 0 .6 4 0.5836.771 1 26 0 .58 0 .6 9 0 .4 1
36.922 1 21 0.50 0 .7 6 0.4437.143 2 39 0 .58 0 .6 0 0 .3 437.426 OUd? 9 0.50 0 .9 0 0 .4 537.637 Id t 13 0 .42 0 .0 6 0.3637.828 0 22 0 .3 5 0.86 0 .3 0
37.900 0 41 0 .3 8 0.66 0 .2 558.998 O 4 0 .4# 0 .9 4 0 .4 639.268 3 52 0 .55 0 .4 5 0 .2 539.441 0 7 0.02 0.90 0.4639.627 2 35 0 .56 0.65 0 .3 6
39.787 2 38 0 .5 5 0.56 0 .3 240.107 0 7 0.55 0 .9 2 0.5140.449 8 764 1 .0 0 0.18 0.1840.758 ur 13 0^39. 0 .8 6 0 .3 441.080 10 611 1 .00 0.24 0.2441.282 i 22 0 .38 0 .7 6 0.2941.462 0 11 0 .86 0.82 0 .4 641.782 24? 55 0*67 0.57 o . s s42.086 58 0.74 0.44 0 .3 342.219 04? 7 0.69 0.92 0 .6 4
42.646 0 17 O.M 0 .7 9 0 .7 042.908 1 7 0.80 0 .79 0 .4 742.992 3 141 0.75 0.41 0 .5 243.268 4 58 0 .72 0 .4 5 0 .3 345.485 ON 11 0.75 0 .8 7 0.6543.717 25 82 0 .7 4 0 .S 1 0 .3 844.000 2 47 0.74 0 .5 # 0.4044.239 44? . • 58 0 .7 8 ©.SO 0.5944.450 O', § 0.80 0.87 0.6944.576 0 6 0.84 0 .8 8 0.7544.727 -IN 2 0 .96 0 .9 6 0 .9 244.894 0 30 0.95 0 .7 1 0 .6 845.022 1 21 0 .71 0.78 0 .5 246.176 3 59 0 .7 5 0 .4 2 0 .2 945.472 84? 69 0.69 0 .4 4 0 .8 0
62
W. L. a . I . W(mA) r 1Local
5846.702 1 27 0.71 0.6646.995 2 67 0 .84 0.6046,290 1 82 0.64 0 .6 546.419 2 56 0.64 0 .6 646.644 1 44 0.67 0 .5 6
46.811 6 37 0.51 0.6546.952 1 68 0 .88 0.4747.828 1 100 0.88 0.4647.875 1 102 0.98 0 .4 448.299 2 51 • 0 .88 0 .5 5
48.555 -1 28 0.87 0 .8 548.615 -1 31 0.87 0.8248.849 11 56 0.82 0 .7249.008 3d? 89 0 .8 5 0.4949,369 IS 67 0 .81 0 .89
49.645 1 25 0.64 0 .6 849,759 Oli IS 0 .4 4 0.8449.979 10 656 1.00 0.2050.167 ISd? 25 0 .5 4 0 .7 550.668 -1 9 0.56 0.8960.655 0 9 0 .4 4 0 .8 850.828 4 192 0.83 0.3150.962 0 10 0 .45 0.8161,295 2Sd? 54 0 .72 0.5261.658 . o so 0 .79 0 .6 9
61.860 -1 9 0.92 0.6662.219 1 30 0.66 0.6162.409 . 2Sd? 65 0 .8 6 0 .4 552.661 4 139 0 .91 0 .4 462.711 -1 7 0 .71 0.9252.914 -1 10 0.92 0 .8 683.049 -1 11 0 .78 0.6653.206 Id? 37 0.76 0 .6953.545 OH 20 0.65 0.7455.486 2d? 65 0.70 0 .5 0
53.754 0 17 0 .7 5 0 .8154.061 0 20 0.72 0 .7S54.213 0 54 0.64 0 .6 564.572 2 48 0*55 0 .5 464.575 2Sd? 38 0 .S 6 0 .6 5
I.True0.460.420.670.670.68 .
0.280.590.440.440.460.720.710.540.560.42
0.460.410.200.800.50
0.46 0.26 0.460.420.54
0.780.560.58.0.500.65
,0.79 . 0.78.0*62. 0.480.860.690.560.410.600.68
65
W. L. 1 . I .
3354.856 156.126 -158.818 . 255.686 155.853 4
56.028 156.383 856.666 2H56.925 067.166 157.888 057.447 -157.669 64?57.894 158.184 1*58.805 758.474 058.691 058.691 2N58.867 1166.919 169.225 359.924 2060.485 060.497 0
60.626 3E60.850 061.026 061.169 4X4?61.346 361.982 IX62.496 262.595 163.070 163.403 3X63.756 363.870 063.978 064.113 164.307 3
r C. I.Local True
0 .7 4 0 .7 4 0 .5 41 .0 0 0 .9 1 0.920 .8 3 0 .4 8 0 .4 00 .7 8 0 .4 8 0.860.61 0 .5 6 0 .3 4
0 .5 3 0 .7 6 0.411 .00 0 .1 9 0 .1 90.4® 0 .7 1 0.850.80 0.89 0 .680 .8 4 0.69 0.670.98 0.91 0 .8 40.93 0.96 0 .8 90 .8 2 0.49 0.400.76 0 .6 8 0.620.61 0.62 0.620 .7 7 0 .4 6 0 .2 70 .6 0 0 .9 4 0 .4 80 .4 6 0.97 0 .4 50.46 0 .7 9 0.400 .5 0 0 .6 8 0 .3 4
0 .6 4 0.47 0 .3 00 .52 0 .6 0 0 .3 31 .00 0.17 0 .1 70 .46 0 .8 5 0 .3 90 .41 0 .8 8 0 .5 4
0.53 0 .7 0 0 .5 30.59 0 .8 8 0.490 .5 8 0 .8 6 0.4®0 .5 0 0 .6 2 0.910.48 0 .6 2 0.290 .8 4 0 .8 1 0 .6 80 .8 2 0 .5 4 0 .4 40 .78 0.69 0 .5 00.89 0 .6 8 0.590.94 0.54 0*460.65 0.46 0.310 .8 2 0.92 0 .6 30 .71 0.67 0.610 .9 0 0 .6 6 0 .6 10.89 0 .5 6 0 .4 9
W (mA)18492TO5218
565297
SO
828880141441
16m
6484
16881616
44137
34311454262662
6948
8239
64
W. L. R. I. W (ml) r e. I.Local True
5864.494 1 34 0.85 0.74 0.6164.876 5*d? 46 0.94 0*56 0 .6 566.006 0 3 0.68 0.93 0.6466.163 3 32 0*76 0.62 0.4865.655 7 344 1.00 0.25 0.23
65.992 5Hd? 68 0 .80 0.55 0.4466.447 1 49 0.98 0.66 0.6566.566 0 24 0 .96 0.72 0.6866.724 0 8 0.65 0.85 0.6966.828 2 92 0 .93 0.59 0.42
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68.241 0 IS 0 .71 0.73 0.5368.411 1 28 0 ,78 0.65 0.6168.745 1 46 0.62 0.64 0.5269.175 1 22 0.63 0.71 0.48694315 Oldt 56 0.68 0.62 0.42
69.561 3 101 0.74 0 .32 0.8469.924 IS 38 0.75 . 0 .67 0.4270.161 IE 42 0.67 0.56 0.88:70.567 0 16 0.61 0.79 0.4870.485 1 34 0 .6 0 0.70 0.42
70.889 1 18 0.48 0 .7 7 0 .8 771.594 2d? 51 0.62 0.58 ■ 0.3071.665 0 4 0.52 0.92 0.4871.760 2 63 0 .61 0.42 0.2671.905 0 24 0.79 0.70 0.56
72.064 IE 45 0.78 0.56 0.4372.612 6 782 1 .00 0.21 O O l72.954 2 38 0.82 0 .58 0.3675.155 2 77 0.65 0.42 0.2775.577 1 38 0.78 0.60 0.47
75.769 4 m 0.78 0 .30 0.2473.961 4 72 0 .72 0.35 0.2674.526 2 57 0.68 0 .52 O O O74.778 2 58 0.97 0,51 0.4975.087 2 67 0 .92 0 .67 0.64
65
W. L. B. 1.
3876.292 2Nd?76.782 276.053 676^12 076.422 0
76.488 076.680 176.847 476.980 4XdY77.200 IN
77.346 177.453 077.837 078.029 878.582 7dt
78.681 278.840 079.196 179.678 179.661 0
79.966 130.040 080.192 080.396 280.679 1
80.796 181.004 181.309 281.593 181.877 2
82.087 182.302 282.613 182.691 182.849 1
85.641 084.371 284.611 184.846 085.153 2
r 6. I.Local True
0.91 OeS® 0.510 ^ 1 0.51 0.47Cl .97 0.28 0.260.96 0.82 0.790.88 0.70 0.61'
0.92 0.70 0.640.90 0.73 0.660.90 0.46 0.400.88 0.4# 0.390.62 0.72 0.5#
0.7# 0.88 0.610.72 0.68 0.480.38 0.89 0.431.00 0.19 0.190.76 0.22 0.17
0.20 0.82 0.220.3# 0.68 0.400.61 0.62 0.420.91 0.69 0.640.86 0.67 0.50
0.72 0.67 0.400.73 0.68 0.500.62 0.91 0.560.76 0.50 0.380.96 0.48 0.43
0.91 OJit 0.480.79 o.m 0.42 ■0.71 0.53 0.370.84 0.43 0.380.84 0.31 0.26
0.64 0.58 0.280.60 0.38 0.230 ^ 4 0.58 0.280.46 0.62 0.280.46 0.61 0.28
0.98 0.82 0.760.82 0.87 0.300.86 0.67 0.170.86 0.87 0.760.76 0.4© 0.30
W (mA)
6651
1051235
S?19576923
10328
438398
IT17743854
61565781025575729690
M52443738
149442989
W. L» S. I. V? (mA) r c*Local
I.True
3885.621 4 67 0.73 0.4# 0.3386.758 1 15 0.64 0.79 0.6085.935 0 12 0.68 0.87 0.4786.296 15 817 1.00 0.20 0.2086.806 3 22 0.S1 0.74 0.59
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96.474 1 23 0.81 0.71 0.6696.785 0* 14 0.97 0.65 0.8297.462 2 58 0.92 0.48 0.4197.650 0 3 0.90 0.94 0.8098.396 2 46 0.81 0.60 0.48
98.514 o 12 0.79 0.84 0.6699.038 5 75 0.99 0.43 0.42
3899.144 2 44 0.82 0.56 0.443900.226 0 6 0.84 0.92 0.76
00.545 5 140 0.86 0.50 0.26
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02.452 . 18 17 0.77 0.79 0*8002.632 28 20 0.64 0.76 0.4804.078 0 20 0.80 0.76 0.60©4.652 0 13 0.91 0.82 0.7204.792 3 68 0.82 0.46 0.57
05.011 1 11 0.65 0.86 0.5706.191 2 10 0*55 0.85 0.4706.907 3 31 0.62 0.88 0.3406.502 2 56 0.69 0.61 0.4206.766 4 69 0.88 0.45 0.38
06.966 1 16 0.88 0.76 0.8607.116 oKd? 6 0.86 0.92 0.7807.480 3d? 55 0.92 0.46 0.4507.674 1 20 0.89 0.75 0.6407.776 1 14 0.77 0.80 0.61
07.942 5 87 0.95 0.56 0.5508.276 1 34 0.90 0.70 0.6208.415 0 • 4 0.85 0.95 0.7808.560 0 10 0.87 0.86 0.7508.764 4 68 0.84 0.44 0.5708.950 1 71 0.99 0.62 0.6109.887 -0 16 0.98 0.81 0.8009.504 **1 5 0.92 0.92 0.8409.670 4 54 0.88 0.46 0.4009.859 5 ' 96 0.79 0.64 0.45
10.558 2 58 0.96 0.52 0.5010.556 2 50 0.77 0.67 0.4410.669 0 9 0.78 0.86 0.8810.861 4 62 0.81 0.52 0.4111.005 5 34 0.79 0.57 0.45
11.182 0 25 0.96 0.74 0.7111.419 Old? 5 0.98 0.96 0.9511.705 1 21 0.99 0.74 0.7511.827 2 22 0.82 0.69 0.6611.911 2K 27 0.82 0.67 0.64
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MASTER CAROUNIVERSITY OF ARIZONA
LIBRARY