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.

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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 0.70@0.538 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

67.216 5 65 0 .8 0 0.39 0 0 967.629 1 67 0.94 0 .47 0.4567.776 1 14 0.66 0.80 0,6167.951 2 34 0 .6 4 0 .6 7 0 .1768.152 0 14 0.70 0.82 0.58

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

87.061 7 239 1.00 0.32 0.3287.892 -1 6 0.68 0.92 0.8388.043 0 7 0.80 0.92 0.7488.626 6 81 0.82 0.54 0.3488.831 2 25 0.66 0.70 0.47

89.678 2 50 0.68 0.80 ■ 0.3489.931 1 51 0.64 0.67 0.3790.198 11 21 0.84 0.76 0.4890.401 2 31 0.66 0.61 0.4090.570 IN 31 0.73 0.68 0.48

90.851 3 66 0.74 0.44 0.8391.200 11 . 39 0.79 0.63 0.5091.385 0 5 0.78 0.89 0.7091.613 11 23 0.80 0.70 0.5891.783 0 14 0.76 0.80 0.81

91.936 4 93 0.82 0.39 0.3292.316 0 18 0.88 0.76 0.6792.593 2 46 0.92 0.80 0*6693.404 4 147 0.87 0.28 0.2393.922 2 21 0.66 0.68 0.38

94.104 5 195 0.98 0.24 0.2494.495 11 24 0.96 0.74 0.7294.988 3 64 0.96 0i*4 0.4295.244 2 7 0.52 0.86 0.4696.141 0 28 0.84 0.72 0.60

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

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