A Hi£h-1 «»pytral

Analysis Of the Bal Star

HD 204075 (i Capricomi)

Bureau

of

Standards

4
i


UNITED STATES DEPARTMENT OF COMMERCE Maurice H. Stans, Secretary

NATIONAL BUREAU OF STANDARDS Lewis M. Branscomb, Director

A High-Dispersion Spectral Analysis of the

Ba II Star HD 204075 (

C, Capricorni)

Jack L. Tech

Institute for Basic Standards

National Bureau of Standards

Washington, D.C. 20234

U, S' National Bureau of Standards, Monograph 119 ,

' » * Nat. Bur. Stand. (U.S.), Monogr. 119, 174 pages (March 1971) CODEN: NBSMA

Issued March 1971

For sale by the Superintendent of Documents, U.S. Government Printing Office, Washington, D.C. 20402 (Order by SD Catalog No. C13.44:119), Price % 3.2.5
NATIONAL Bmm OF STANDARDS

MAY 1 7 1971

Library of Congress Catalog Card No.: 70-607151
Acknowledgments

This investigation could not have been completed without the continued guidance and en- couragement of my teacher and friend. Prof. C. H. Payne-Gaposchkin. I only hope that the work

adequately reflects the benefits I have derived from my frequent appeals to her experience and

good counsel in matters of scientific judgment and stellar spectroscopy.

I am indebted to Prof. Leo Goldberg not only for his active interest and frequent advice throughout this investigation, but also for arousing my interest in stellar abundances and for introducing

me to the theory of the curve of growth through his supervision of my earlier study of the solar chromium abundance.

I am grateful to Prof. J. L. Greenstein for suggesting the problem and for lending me the highdispersion plates of ^ Capricorni on which the analysis is based. His hospitality at the California

Institute of Technology and his instructing me in the use of the direct-intensity microphotometer

are very much appreciated.

My colleagues in the spectroscopy laboratory at the National Bureau of Standards, especially

Dr. Karl G. Kessler, were unstinting in their support of this work. I am greatly indebted to Dr. William C. Martin for such support, for many useful discussions, and for constructively criticizing

parts of the manuscript. Charles H. CorUss has patiently endured my constant demands on his wide experience in the field of laboratory /-values. His contributions are gratefully acknowledged.

My training in the critical identification of spectral lines has been provided by Dr. Charlotte

Moore-Sitterly. Her generosity in critically reading the manuscript and in helping to resolve a number of problems that arose in this work is deeply appreciated. Her great interest in the analysis of

^ Capricorni led to many fruitful discussions and to a corresponding improvement of the work.

I would like to thank Drs. A. A. Nikitin and N. P. Penkin for valuable conversations and helpful

instruction during my stay in the Astronomy Department of the State University of Leningrad under

the auspices of the cultural exchange program with the Soviet Union.

Many lively discussions with Drs. Gerald Newsom, Andrea Dupree, Roger Kopp, Paul

Blanchard, and Frances Wright were also of great help to me.

Finally, I should like to acknowledge the careful typing of the original manuscript by Miss

Judith Grabusnik and the meticulous assistance given by Mrs. Ruth Peterson in many phases of

the technical clerical work.

This NBS Monograph is a partially revised and updated version of a doctoral thesis presented

earlier to the Department of Astronomy at Harvard University. The work was supported in part

by fellowship grants from the National Science Foundation.

Ill

Contents

Page Acknowledgments Ill

1. Introduction 1

1.1. General remarks 1 1.2. The barium stars 2

1.3. The problem 3

2. Observational material and measurements 4

2.1. Basic data for ^ Capricorni 4

2.2. The plates 4

2.2.1. Description 4

2.2.2. Wavelength measurements 4

2.2.3. Microphotometry 5

2.3. Equivalent widths 5

2.3.1. The primary equivalent widths 5

2.3.2. Derivation of equivalent widths from the measured central depths 8

2.3.3. The treatment of weak lines 10

2.4. Comparison with other measurements 11

2.5. Estimation of the error 11

3. Line identifications and gf-values ^ 18

3.1. The identification of spectral lines 18

3.1.1. General principles 18

3.1.2. Literature sources used in making line identifications 19

3.1.3. The identification of A. 4608.74 19

3.1.4. A nonsense curve of growth for tantalum (Ta I) 22

3.2. Theg/^values 23

3.2.1. The use of gf-values in this study 23

3.2.2. Sources of g/"-values 23

3.2.3. Wavelength-dependent corrections to the gf-values of NBS Monograph 53 24

3.2.4. Comparison of the NBS intensity estimates for neodymium with those of King (1936) 27

3.3. A relation for converting NBS intensities of unclassified lines to gf-values 29

4. Curve of growth analysis 31

4.1. The differential method 31

4.2. The stellar line strengths 34

4.3. Conversion of NBS g^-values to line strengths in e Virginis 35

4.4. Theoretical curve of growth for ^ Capricorni 46

5. Comments on individual spectra 48

5.1. Introduction 48

5.2. The spectra 48

5.2.1. Aluminum 48

5.2.2. Barium (Ba I) 48

5.2.3 Barium (Ban) 48

5.2.4. Cadmium 49

5.2.5. Cerium 49

5.2.6. Dysprosium 49

5.2.7 Europium 52

5.2.8. Iron(Fel) 52

5.2.9. Lanthanum 52

5.2.10. Lithium 52

5.2.11. Magnesium 53

5.2.12. Molybdenum 53

5.2.13. Neodymium 53

5.2.14. Nickel 53

5.2.15. Oxygen 53

5.2.16. Praseodymium 53

V
5.2.17. Ruthenium 53

5.2.18. Samarium 54

5.2.19. Scandium 56

5.2.20. Silicon 56

5.2.21. Strontium 56

5.2.22. Sulfur 56

5.2.23. Technetium 56

5.2.24. Titanium (Till) 56

5.2.25. Vanadium 56

6. Atmospheric parameters for ^ Capricorni 57

6.1. The excitation temperatures 57

6.2. The ionization equilibrium 68

6.3. The Carter effect 68

6.4. Gas velocities in the atmosphere of ^ Capricorni 73

6.4.1. Thermal velocity 73

6.4.2. Microturbulence 76

6.4.3. Macroturbulence 77

7. The chemical composition of ^ Capricorni 79

7.1. The abundances 79

7.2. Use of ^ Capricorni as a comparison star 82

8. Discussion and summary 86

8.1. The accuracy of the abundances 86

8.2. Discussion 86

8.3. Summary 88 Appendix

A.l. Sample differential curves of growth 89

A.2. Sample absolute curves of growth 107

A.3. Table A, the line list arranged by wavelength 123

A.4. Table B, the line list arranged alphabetically by spectrum 146

A.5. References 169

List of Tables

Table Description Page

2.1. Fundamental data for HD 204075 4

2.2. Observational material for { Capricorni 4

3.1. Sources of ^/-values 24

3.2. Mean ratios of original NBS intensity estimates for lines observed in each of two different exposures

3.3. Comparison of NBS intensity estimates for neodymium with those of A. S. King

4.1. Coefficients for the polynomials representing the normalized stellar curves of growth

4.2. Conversion of NBS g/-values to line strengths in e Virginis '^^

5.1. NBS ^/-values for recently classified lines of Ce II 49

5.2. NBS gf-\a\ues for recently classified Lines of Nd ii 53

5.3. Suggested revision of Warner's Sm ii identifications > 5000 A 54

6.1. Differential excitation temperatures of ^ Cap relative to the sun and to e Vir 58

6.2. Adopted excitation temperatures 61

6.3. Determination of differential electron pressures for ^ Cap relative to the sun and to e Vir 68

6.4. Mean excitation potentials for Fe I lines used in the construction of the solar curve of growth shown in figure 6.10... 73

6.5. Doppler velocities derived from individual curves of growth 76

7.1. Parameters used in the determination of relative ionization equilibria 79

7.2. First ionization potentials and partition functions used in the calculation of ionization corrections to the relative abundances 80

7.3. Logarithmic abundance ratios 81

7.4. Abundances derived from NBS g-Z-values converted to line strengths in e Virginis 81

7.5. Logarithmic abundances in ^ Capricorni relative to iron 81

8.1. Physical parameters for ^ Capricorni 88 A The line list arranged by wavelength 123 B The line list arranged alphabetically by spectrum 146

VI
A High-Dispersion Spectral Analysis of the

Ban Star HD 204075 ( ^ Capricorni)

Jack L. Tech

A double differential curve of growth analysis, using both the sun and 6 Virginis (G9 II^III) as comparison stars, has been performed for the Ban star ^ Capricorni. The observational material consists of equivalent widths, central depths, and half-widths for 1100 spectral lines measured on direct- intensity tracings of plates obtained by J. L. Greenstein at the coude focus of the 200-in telescope. The

plates cover the spectral regions 3880-4825 A and 5100-6720 A at reciprocal dispersions of 2.3 and

3.4 A/mm. respectively. Line identifications given in earlier lists for barium stars have been critically re-examined. Three lines have been attributed with reasonable certainty to dysprosium, which has not previously been observed in barium stars. The atmospheric parameters derived for ^ Cap are:

Oqxc '• 1-13 -1.28

flion : 0.99 + 0.13

log 2a : -2.5 -1.10

i-'muro 3.5 km/s -0.03

fmaero : 5.5 km/s

Atmospheric abundances have been derived for 37 elements. The results obtained with respect to the two comparison stars are in good agreement. The barium star exhibits essentially solar abundances

for most elements lighter than germanium, but overabundances by factors of about two are indicated

for carbon and lithium. With the exception of europium, all observed elements heavier than germanium

are found to be overabundant in ^ Cap. Improved NBS #r/-values, converted to the system of line strengths in € Vir. have yielded exceptionally well-defined curves of growth for several rare earths. Overabundances by factors of about eight or nine have been found for the 5-processed rare earths, as well as for dysprosium, which is generally considered to be r-processed. The abundances derived for the rare earths are greater by about a factor of three than those derived for the same star by Warner

(Mon. Not. Roy. Astron. Soc. 129, 263 (1965)).

Key words: Abundances of elements in stars: Ball stars Capricorni); curve of growth: equivalent

widths: identification of spectral lines: ionization in stars: oscillator strengths; temperature in stars; turbulence in stars.

1. Introduction

1.1. General Remarks

In recent years considerable importance has been

attached to obtaining accurate determinations of

chemical abundances in the atmospheres of stars of abnormal composition. Abnormality in this context is ordinarily defined in terms of the solar composition taken as standard. The atmospheres of the

great majority of cool dwarfs like the sun are found

to exhibit more or less solar abundances, which suggests that their composition is essentially that of the

interstellar medium from which the stars were

formed. The development of theories of stellar evolution and of the formation of chemical elements

through nucleosynthesis has relied heavily upon the

characteristics of stars departing from the normal

(Burbidge et al., 1957; Burbidge andBurbidge, 1957;

Seeger et al., 1965).

There are several widely studied classes of stars

for which striking abundance anomalies have been

reliably established. Extreme metal deficiencies

characterize the older stars of Population II (Aller

and Greenstein, 1960) and certain high-velocity

stars (Koelbloed, 1967). The magnetic Ap stars separate into subgroups distinguished by different types

of compositional anomalies. Among the elements

most affected are Sr, Y, Zr, Cr, Fe, Mn, O, and the

rare earths, especially Eu. The origin of the ab- normal abundances in these stars is not well understood, but has been related to the loss of angular

momentum during pre-main-sequence contraction,

and to surface nuclear processes generated by

strong magnetic fields (Cameron, 1967).

The CH stars (Wallerstein and Greenstein, 1964)

show multiple characteristics that also appear in1
dividually in other groups of stars — high carbon

abundance, metal deficiencies, and enhancement of

certain rare earths. The occurrence of nuclear activity has been spectroscopically verified in the case of

S-type stars, in which Merrill (1952) identified lines of technetium, whose longest-lived isotope thus far detected has a half-life of only about 200,000 years.

1.2. The Barium Stars

The barium stars form one of the most important

groups of abnormal stars. They are distinguished by

the unusual strength of the Ba II resonance doublet

at \X4554 and 4934 A. These stars played a central

role in the early development of theories of element

synthesis (Burbidge and Burbidge, 1957). Bidelman

and Keenan (1951) first recognized the Ba II stars as formmg a special class and pointed out their characteristic spectroscopic features. They are giants of

spectral types G and K and spectroscopically re- semble stars of type S in showing extraordinarily

strong lines of ionized barium and certain other heavy

elements, but technetium has not yet been identified

in these stars. For their spectral type, the Ba II stars also exhibit unusually strong lines of Sr II (X4077

and \4215) and a striking enhancement of the G

band (due to CH). Miss Maury (1897) very early

recognized the unusual strength of Sr II and Ba II in the star ^ Capricorni.

Intermediate-band photometry by Bond and Neff

(1969) reveals a broad absorption centered near X4000 A in the spectra of Ba II stars. The similarity of this opacity feature to that observed in the carbon

stars of type N strengthens Mrs. Gorden's (1968)

argument that the barium and N-type stars are re- lated, perhaps differing from each other only in surface temperature.

The most notable characteristic of the Ba II stars from the point of view of element formation is the

great enhancement of lines in the spectra of elements

such as strontium, barium, zirconium, samarium,

cerium, lanthanum, neodymium, and yttrium, whose

most abundant isotopes are formed predominantly

by slow neutron capture (s-process). Garstang (1952) was the first to call attention to the great richness of

lines of the singly ionized rare earths in the spectrum

of I Capricorni. The overabundances found for these

elements in the atmospheres of Ba ll stars is inter- preted as strong evidence that products of interior nuclear reactions have been brought up to the sur- face through convective mixing. The determination

of accurate chemical abundances in these stars.

therefore, is of great importance to the further re- finement of current ideas concerning element

formation.

Warner has listed the basic data for twenty known

Ba II stars. In addition to the five stars reported in the original announcement by Bidelman and

Keenan, fifteen other Ba ll stars have been identified, chiefly by Bidelman, the Cowleys, Warner,

and Wallerstein (Warner, 1965a) More recently,

Bidelman identified the G8ll star ^ Cygni as also belonging to this group, but its Ba ll star characteristics are comparatively mild (Chromey et al., 1969).

The small number of stars now definitely established as Ba II stars may considerably misrepresent

their actual frequency and evolutionary importance.

H. E. Bond, for example, has informed the writer

that he has tentatively identified about 75 stars showing Ba ll characteristics on his set of objective

prism plates taken at the Cerro Tololo Observatory

in Chile.

Several workers have studied the chemical composition of Ba II stars, the most extensive investigation being that by Warner (1965a), who has derived

relative abundances for nine southern Ba II stars. The star HD 46407 was studied differentially with

respect to k Geminorum in the classic work by the

Burbidges (1957). This star was also included in the work of Warner, who found smaller overabundances of the 5-process elements than found by the

Burbidges. Warner traced the discrepancy to underestimated equivalent widths in the earlier work.

Cowley (1968) derived differential abundances

for HR 774 relative to the standard star tt^ Orionis

that are in good agreement with those derived by

Nishimura (1967) for the same star relative to e Virginis. Danziger (1965), from a differential study

of HD 116713 and HD 83548 relative to a Bootis,

found significantly larger overabundances for the

rare earths than those obtained by Warner for the same stars. Unsold (1969) compares in detail the

results of these two investigations and emphasizes

how easily systematic differences in abundance

determinations can result from the use of slightly different values for the general atmospheric

parameters.

Chromey et al. (1969) have analyzed the mild

Ba II star ^ Cygni differentially with respect to

e Virginis. Relatively small enhancements were

found in the abundances of the 5-processed ele- ments. From evidence that the enhancement of heavy elements occurs earlier in the main-sequence

2
phase of these giants, the authors conclude that the Ba ll stars do not form a discrete group, but

that the development of the typical Ba ll star features progresses in a continuous fashion for

stars evolving along this path.

1.3. The Problem

The brightest known barium star (me = 3.9), ^ Capricorni (HD 204075), is also the earliest in spectral type, hsted as G5-Ba2 in the scheme proposed

by Warner (1965a). This star was studied quaUtatively by Garstang (1952) and Greenstein (1954)

and quantitatively for the first time by Warner.

Because of the great interest in the barium stars,

it was considered of some importance to make an

accurate study of one of them at higher dispersions

than heretofore available. This would eliminate some of the problems caused by the severe blending

that results from their spectroscopic richness in lines of the singly ionized rare earths. J. L. Greenstein emphasized to the writer the importance of such an analysis of ^ Capricorni and generously

offered the loan of high-dispersion spectrograms

of this star taken by him at the coude focus of the

200-in Palomar telescope.

It is the purpose of the present investigation to derive the physical parameters and chemical

composition of the atmosphere of ^ Capricorni from

this observational material.

3
2. Observational Material and Measurements

2.1. Basic Data for ^ Capricorni

The basic data for HD 204075, as given in the

comprehensive summary of Ba il stars by Warner

(1965a), are hsted in table 2.1. The UBV photometric

indices obtained after applying his estimated cor- rection for CN absorption to the original values are given in parentheses.

Table 2.1. Fundamental data for HD 204075

a (1950) 21" 23.8'" Rad. Vel. (kni/s): + 3.3 6 (1950) -22° 38' V; 3.74

m,- 3.9 B-V: 1.00 (0.92) Spectral type G5-Ba2 U-B: 0.57 (0.67) M (7yr) 0.024

As with all the known barium stars, the proper

motion and velocity of HD 204075 indicate that it belongs to intermediate Population I. Bidelman

assigned (, Cap to luminosity class II—III, but Warner

concluded that it is closer to II. From a study of H and K emission, Warner also derived an absolute

magnitude of Mi, — — 3A for the star and estimated

its mass to be about 4>Mq.

Table 2.2. Observational material for Capricorni

Plate number Date Emulsion

(Eastman

Kodak)

Wavelength

range

Reciprocal

dispersion

(i) {A/mm)

Pc 3469 9-19-57 IIa-0 3700-5100 9.2

Pb 4768a 9-23-59 IN 6430-8150 6.8 Pb 4768b 9-23-59 I-N 8150-8800 6.8

Pc 4775 9-24-59 I-N 6250-8650 13.6

Pc 6001 6-30-61 IIa-0 3700-5100 9.2

Pa 5994a 6-29-61 IIa-0 3880-4300 2.3 Pa 5994b 6-29-61 IIa-0 4300-4825 2.3

Pa 6000a 6-30-61 103a-F 5100-5850 3.4 Pa 6000b 6-30-61 103a-D 5850-6720 3.4

2.2. The Plates

2.2.1. Description

As stated earlier, the high-dispersion spectrograms of ^ Capricorni were obtained by J. L. Greenstein at the coude focus of the 200-in telescope. A

summary of the plates is given in table 2.2.

2.2.2. Wavelength Measurements

All the spectrograms were measured by hand on

the comparators in the Spectroscopy Section of the

National Bureau of Standards. A total of 10,000

individual settings were made on lines in the spectral

range 3880 to 8700 A. This figure includes at least two measurements for each line. A versatile computer program, CWLT5, was written to aid in the

reduction of these measurements. This doubleprecision program for polynomial fitting by least squares has also been used repeatedly in other

phases of reduction and analysis of the data. As

applied to wavelength determinations in stellar spectra, input to CWLT5 consists of three sets of

data cards: (1) comparator readings and standard

wavelengths for lines measured in the iron comparison spectra on each plate; (2) comparator

settings and laboratory wavelengths for a few identi- fied lines in the stellar exposure; and (3) comparator settings for the remaining, unidentified,

lines in the stellar exposure. For sets (1) and (2), the program finds the least-squares polynomial

of lowest degree that adequately fits the input wavelengths as a function of the corresponding comparator readings. When CWLT5 is used as a general

X — Y fitting program, set (2) is omitted. The

difference in the wavelengths calculated by the two

polynomials for the fines in set (2) represents the

Doppler shift of the stellar spectrum. The mean

Doppler shift is calculated and used in the determination of the "laboratory" wavelength for each

stellar fine of set (3) after its "observed" wavelength

has been calculated by the polynomial representing the iron comparison spectrum. In the calculation

of the polynomials and the value of the correction

for radial velocity, the program automatically

rejects any lines that depart by more than a pre- scribed number of standard deviations from the mean fit, presumably as a result of poor measure-
ment or incorrect identification. As a final check,

the program plots the residuals of the fit for a visual

"appraisal of the quality of the measurements.

A comprehensive line list including identifica- tions and estimated visual intensities for ^ Cap is being prepared from this material. The final list will probably contain about 3500 discrete absorption

lines. A need has long been felt for such a reference

description for Ba II stars (Cowley, 1968). In the

present investigation the complete line list was

used only to resolve questions associated with

the identification of those hnes for which equivalent

widths were measured.

2.2.3. Microphotometry

Only plates Pc 3469, Pa 5994a-b, and Pa 6000a-b

are of photometric quality. The calibration plates were obtained by Greenstein with a wedge-slit

grating spectrograph. Using the wedge-silt calibrations, the writer made tracings of these five plates

j by use of the direct-intensity recording microphotometer at the California Institute of Technology.

Several important regions of the plates were traced

. twice under different conditions. The scale of the

' charts ranges from 0.6 to 1.2 angstroms per inch.

A sample region, reduced, is shown in figure 5.3.

2.3. Equivalent Widths

2.3.1. The Primary Equivalent Widths

Line crowding and strong absorption by the CH

t and CN molecules make it extremely difficult to find unblended lines or to locate the continuum

level shortward of 4300 A. Except for a few hnes

considered of great importance to the analysis,

therefore, the measurements have been restricted

to the spectral regions 4316 to 4819 A and 5102 to

j 6710 A. For brevity, spectral lines measured in

; these two regions are distinguished by referring

I to them as "blue" and "red" Unes, respectively,

i Ahhough the gap between 4800 and 5100 A is

' covered by the charts for plate Pc 3469, this region

has been omitted from the abundance analysis

because of the considerably lower dispersion.

I The charts were divided into 32 sections correI sponding to the several pieces of broken plate

Pa 6000a and to the natural stopping points in the

tracing process caused by (1) occasional checking

of the clear plate reading, (2) changes in the photographic calibration of the plate, and (3) periodic

adjustment of the vertical scale of the tracings.

For each succeeding section, the plate was backed

up to provide a region of overlap with the preceding

section.

The continuum was located on the tracings by

drawing a straight line through the high points

found in regions about 20 A wide. A comparison of

these tracings with those in the Utrecht Solar Atlas

(Minnaert et al., 1940) helped to identify windows

in the spectrum. The continuum level for each chart

section was drawn independently without reference

to that of the preceding section for the overlap

region. Special care was also given to avoid the

underestimation of continuum level that Unsold

(1955) warns is a common mistake of beginners.

After the continuum had been established over

the entire chart coverage, the lines to be measured

were selected by marking a point in their profiles

to serve as a starting point for the tracer point of

the planimeter. Lines whose profiles were incomplete because of partial blending with adjacent lines were sketched in at this time. Only lines that had

the appearance of being relatively unblended were

selected. A few good hnes in each chart section were then

identified to serve as the standards required by the

computer program CWLT5 in calculating wavelengths for the remaining lines. The equivalent widths of all selected hnes were measured by use of a precision polar planimeter

in the usual way. Equivalent widths measured by

planimeter are called the "primary" widths to distinguish them from equivalent widths derived

later from measurement of central depth alone. The data recorded for each line included (a) an

indication Q of the quality of the line on a scale from 1 (poor) to 5 (excellent); (b) the width in milHmeters of the profile at half-intensity; (c) the positions of the continuum and vertex of the line on

the chart scale; and (d) the chart section number.

The judgment of quality index was based on the extent to which the profile had to be completed by

hand, on the suspicion of any blending, and on the

general appearance of the line. The information for each line was punched on

cards as input to a special adaptation of CWLT5

whose output for each fine consisted of the

wavelength (in A), half-width (in mA), central

depth (Re), and equivalent width (in both mA and

the form log W/k). At the same time, the ratio of

measured equivalent width to that estimated by the

product of half-width and central depth was cal- culated for each line. Every line for which this

5
Figure 2.1. Relation between equivalent width and central depth for lines with wavelengths shorter than 5000 A.

6
Figure 2.2. Relation between equivalent width and central depth for lines with wavelengths longer than 5000 A.
ratio departed greatly from unity was remeasured

as a check. A number of errors in recording or keypunching were thus detected. The residuals

of a polynomial fit of measured half-widths to the

central depths were also plotted. All lines falling far off the mean curve were later checked for the

possibility of being broad blends.

To avoid any bias in line selection, only at this stage of the reduction was a comparison made with

the line identification lists as described in section

3.1.2. About 50 of the measured lines turned out

to be unusable because it was not possible to identify

their chemical origin. Also, more than 100 lines had

to be rejected as being unresolved strong blends.

Table A in the Appendix lists the measured quantities and relevant spectroscopic information for some 1100 Hues used in the remainder of this investigation.

2.3.2. Derivation of Equivalent Widths From

the Measured Central Depths

After obtaining a reliable set of primary equivalent

widths directly from the line profiles by counting

squares or, as here, by planimetry, it is possible to augment the number of measurements by abbreviated methods and to improve the primary set by

statistical smoothing. Both of these applications

have been made to the measurements in ^ Cap.

The method most frequently used for augmenting

a primary set of measurements is to establish a functional relationship, often involving the wavelength, between the central depths and equivalent

widths of the small primary set to enable the derivation of equivalent widths for additional lines simply

by a measurement of central depth alone. Values

derived in this way are here called the "/^c-widths."

The technique has been used with success (Warner,

1964b) in investigations involving a large number

of lines in several stars, where practicality rules out

direct planimetry for all lines of interest. An improved set of equivalent widths can be

obtained (Wright, 1948) by averaging the primary

widths themselves with the semi-independent values

returned through the functional relationship derived

between central depth and equivalent width. For

certain types of blending the /?c-width of a line may even be a better approximation to the actual

line absorption than is the directly measured width.

This would be the case, for example, when two

lines forming a blend are close enough in wavelength to produce a broadened profile, but not so

close as to have completely additive central depths.

Thus, an average with the 7?c-width can partially

eliminate from the original planimeter values any

contribution caused by unrecognized blending.

The primary equivalent widths {W) measured

in ^ Cap are plotted against central depth (Re) in figure 2.1 for wavelengths shorter than 5000 A

and in figure 2.2 for those longer than 5000 A. The

relation between the two quantities is well-defined

in each of the two regions. The mean curves drawn

were derived from a least squares parabolic fit to the points and were constrained to make W = 0

when Rc = 0. The equations of these curves are

blue region: r = 205 Rc + 173 (mA) (2.1)

red region: r-252 Rc + 23S R'^ (mA). (2.2)

A slight improvement in the standard deviation of the fit can be made by plotting fF/X, rather than W,

against Rc. More importantly, however, it is found

that by choosing WjX the fitted equations describe

so nearly the same curve that no significant compromise in the analytical representation is made

if both spectral regions are treated together. The

combined plot, omitting lines of quality Q <2 for k > 5000 A, is shown in figure 2.3. The mean curve drawn in this figure represents adequately the dis- tribution of points for i?c ^ 0.60. Its equation, with

both W and A. expressed in angstroms, is

(r/\)x 10^ = 400 + 460 (2.3)

For values of Rc in the range 0.10 ^ /?c ^ 0.60,

the semi-independent /?(-widths calculated by this formula have been averaged with the primary

equivalent widths listed in column (10) of tables

A and B. This average was used in the calculation

of the quantity log (JF/A.) listed in column (11)

of the same tables. The above formula has been used also to derive

equivalent widths for some lines not measured by

planimeter. These are distinguished from the planimeter measurements by assigning a value zero to the chart-section number given in column (13) of tables A and B. The fines in this category include

(a) those whose importance was recognized only

after the original planimeter measurements had

been completed, and (b) lines of certain elements

represented by an insufficient number of primary

measurements to define an accurate curve of growth.

8

Most of the lines in both these groups failed to have

planimeter measurements because their profiles

could not be confidently sketched to completion owing to blending with adjacent lines. Their relatively

undisturbed central depths, however, could be

measured with some assurance.

2.3.3. The Treatment of Weak Lines

Several considerations demonstrate that the

primary equivalent widths of weak lines {Rc < 0.15) are too small. First, the use of these measurements

in curves of growth gives a distinct curvature to the "straight-line" portion. Second, the plots in figures 2.1 and 2.2 show the weak lines falUng

progressively farther to the left of the mean curve

as Rc decreases. Third, the primary values are

significantly less than the estimate derived by the

"triangle-rule," whose reliability is well established

in the literature. One formulation of this rule describes the equivalent width of faint lines in terms of the product between central depth and

half-width, namely.

W=ARcH. (2.4)

For faint hues, the half-width can be regarded as a constant equal to the limiting Doppler half-width

(as Rc^O) found below. The factor A partially

offsets the inadequacy of the triangular representation of line profiles and is best determined empirically. The need for this factor is caused in part by

the inability of a triangle to account for the absorption in the wings of the line and for the rounding at the line center. As determined from the measurements, the factor ^ is a function of central depth. Its value ranges

from about 1.00 for Rc < 0.20 to about 1.10 for Rc = OJO. The average value over the entire range

is A = 1.06. It is not surprising that A is found to depend upon Rc, because the quadratic expression

found above relating Rc and W can be regarded as

just an extension of the triangle rule to include

stronger lines. For faint lines the quadratic term can

be neglected and the formula for the /?(.-width

reduces to

(at 5000 A) W= 0.20 Rc (in A). (2.5)

The coefficient of Rc in this expression agrees well

with the limiting Doppler half-widths found below.

It is noteworthy that our empirically derived factor, .4 = 1.06, corresponds to that predictable for weak lines of Gaussian profile. In the usual notation

(Unsold, 1955), for pure Doppler broadening the

equivalent width of a line. ^= (2.6) J

0 {1-exp {-Toe-^'')}dv,

can be approximated for small optical thicknesses

by

To. 2A\« 2 But from the definition of optical depth.

or

/, = /°e-x~/°,(l-Tx)

I°-h

To 7° Rc

Hence, using eq (6.19), we obtain

V

//i?c= 1.064 HRc

(2.7)

(2.8)

(2.9)

(2.10)

As further justification for preferring the triangle

values, it is well known that the measurement of small areas by planimeter is inherently imprecise.

Also, a check of the tracings reveals a consistent

underestimation of the limiting half-width when

filling in incomplete profiles for faint lines. For

weak fines having Rc < 0.15, therefore, the planimeter measurements have not been averaged with

the /?c-widths, which alone were used in the calculation of log (r/\).

To summarize, the equivalent widths used in the

calculation of log (W/k) are derived in four different ways:

Type Value taken for W

(a) Rc > 0.60 the original planimeter measure- ment

(b) 0.15 ^ Rc the unweighted average of the

< 0.60 planimeter measurement and

the /?r-width

(c) Rc < 0.15

and

(d) lines not measured by

planimeter

the /?c-width.

10
2.4. Comparison With Other

Measurements

The only other measurements in the spectrum of

^ Cap with which a comparison can be made are those pubhshed in Warner's study of southern

barium stars (1964b). His measurements were made

at reciprocal dispersions of 6.8 A/mm (blue) and

13.6 A/mm (red). The equivalent widths measured

in the present investigation are plotted against those

of Warner in figure 2.4 for A. < 5000 A and in figure 2.5 for \ > 5000 A. The comparison is restricted

to those fines judged in the present work to be least blended. In the blue spectral region the agreement

between the two sets of measurements is quite

good, at least for these selected fines. There is no evidence of any serious systematic difference over the range of equivalent widths shown, but the

present measurements tend to be smaUer than

Warner's for weak lines. This may be related to his choice of the wing factor^ = 1.15, which is perhaps

too large for weak lines, or to a difference in the

choice of continuum.

In the red region, the two sets of measurements

are in poor agreement. Besides the sizable scatter revealed in figure 2.5, there is also a striking

systematic difference. On the average, Warner's

values are almost 50 percent larger, but individual

fines have equivalent widths differing by factors up to 6. Apart from this single comparison, there

is no evidence for a systematic discrepancy in the

present data between the two spectral regions. For

example, such a systematic error should give rise

to a relative displacement of fines from the two

wavelength regions when plotted together on a curve

of growth. Warner was led to treat the two spectral

regions independently because of such an apparent

discrepancy in their absolute scales. A test has been made to ascertain whether an

important residual difference in scale between the

two regions exists in the present data. Figure 2.6 shows an absolute curve of growth for iron based

on the gf-values tabulated by Corliss and Tech

(1968). A differential curve of growth based on solar

line strengths obtained by reading the Utrecht

equivalent widths into the Pierce-Aller solar curve

of growth is shown in figure 2.7. In neither figure

is an appreciable systematic difference observed

between measurements made in the blue (< 5000 A,

circles) and the red (> 5000 A, crosses) spectral

regions. In these curves of growth the values used

for the absolute and differential excitation temperatures are those derived in section 6.1. Warner's

measurements for the same fines are similarly

plotted in figures 2.8 and 2.9. On the basis of the

scatter shown in these plots, it appears that the

origin of the unsatisfactory comparison in figure 2.5

lies chiefly in Warner's data.

It is difficult to attribute the disagreement in equivalent widths solely to the well-known dispersion effect (Unsold, 1955), which predicts that larger equivalent widths will be derived from lowerdispersion plates because of greater chances for unrecognized blending. This may explain the more widely scattered points in the plots, but it is improbable that nearly all fines would be affected

in this manner, especially in the red where the fine crowding is not great. A difference in cafibration

and in tfie choice of continuum must play a large

role.

2.5. Estimation of the Error

It is virtuaUy impossible in a work of this kind to formulate a quantitative measure of error. The

greatest error is probably associated with the location of the continuum, but for reasons cited later,

the choice of continuum level is considered to have

been physically realistic. Duplicate measurements

of the equivalent widths for lines in the regions of

overlap between sections of the tracings were

usually in agreement to within about 5 percent and

rarely differed by more than 10 percent. Values of

the central depths and half-widths for these lines always agreed to within 0.02 in Rc and about 15

percent in HW. The individual measurements for these lines were averaged and assigned the section

number of the longer wavelength section to the line. The half-widths of the lines could not be measured

to better than 1 mm, which corresponds to about

30 mA on the average chart scale. Averaging the primary equivalent widths with

the semi-independent values calculated from the

relation established above between Rc and W has

probably improved the measurements. From the

consistency of the data, the small scatter of many

of the curves of growth, and the comparison made

in section 2.4 with the independent measurements

by Warner, an estimate can be made with some

assurance that the probable error in the values

tabulated here for log {Wlk) is less than about

±0.10.

11

398-978 0 - 71 -2
mS (Warner, 196^b)

Figure 2.4. Comparison of equivalent widths measured in this investigation with those of Warnerfor lines with wavelengths < 5000 A.

12
m& (Warner, 1964b)

Figure 2.5. Comparison of equivalent widths measured in this investigation with those of Warnerfor lines with wavelengths > 5000 A.

13
I

o

in

Fe I

*«. Maw** +

o

o

1 1 1 1 r -3-00 -2.00 -1-00 0.00 1.00 2.00 3.00

Log(gfX)-ex

Figure 2.6. Absolute curve of growth for iron.

Circles, A < 5000 A; crosses, k > 5000 A.

14
o

-Log X' (0)

Figure 2.7. Differential curve of growth for iron based on solar line strengths.

Circles, X < 5000 A; crosses, X > 5000 A.

15
o

Fei

+ + (4 +^

+ ++ T-

+

o

O

ID

"-3.00 -2.00 -1.00 0.00 1-00 2.00 3

Log(gfX) - ex

Figure 2.8. Absolute curve of growth for iron.

The equivalent widths used in this plot are talten from the work by Warner (1964b). Circles, K < 5000 A; crosses^ K > 5000 A.

16
o

Fei

+0 +*

0+ o 9

O

to

"^'.00 eToo 5 '.00 4'. 00 3 '.00 2T00 r.oo

/ -Log (0)

Figure 2.9. Differential curve of growth for iron using solar line strengths.

The equivdeni widths are taken from the work by Warner (1964b). Circles, K < 5000 A; crosses, K > 5000 A.

17
3. Line Identifications and gf-\alues

3.1. The Identification of Spectral

Lines

3.1.1. General Principles

No matter how sophisticated the method used, it

is evident that a determination of chemical abundances in a stellar atmosphere can have physical

meaning only to the extent that the spectral lines used in the determination are correctly identified as to chemical origin and spectrum. The importance

of meaningful line identifications is being stressed

throughout this study.

The starting point in any attempt at line identi- fication is always the observed wavelength, adjusted

to compensate for the Doppler shift and other physical effects, if necessary. Wavelength coincidence

within a realistic tolerance between the observed

line and the postulated identification must be com- mon to all identifications but in itself does not provide a conclusive criterion as to the origin of the

observed line. This point is often overlooked. The

observed stellar wavelength serves basically as negative evidence that simplifies the problem by

allowing the investigator to exclude from consideration the vast majority of spectral lines known from

independent laboratory investigations.

A stellar spectrum generally represents a superposition of a variety of atomic and molecular spectra. In the present analysis of ^ Capricorni, for example,

the spectra of about 50 different chemical species

have been identified. If reference cannot be made to a list of accurate line identifications for a similar

star, the intelligent approach to unraveling such a superposition of spectra is to compare element by

element the laboratory wavelengths of pertinent

spectra with the stellar line list. This procedure is less susceptible to errors than the alternative one

of comparing the stellar lines individually with some

comprehensive collection of laboratory wavelengths

of many spectra. The latter approach has led to many errors of line identification in the literature. To be reliably productive, this approach requires

that a sound enough familiarity with the stellar spectrum and the physical conditions in the star has already been acquired to permit a refined

judgment. It may also be useful in the identification

of those lines remaining unexplained after the first method has been exhausted.

In comparing a simple laboratory spectrum with

that of the star, it is necessary first to account for the behavior of the resonance lines. If the resonance

lines, or the strongest and most sensitive lines in the range of the stellar observations, are unac- countably absent in the stellar spectrum, any

coincidences between stellar lines and the subordinate lines of the laboratory spectrum are very

likely to be accidental. In the case of very complex

spectra, whose total intensity is distributed among

many lines of similar intensities, the probability of accidental coincidence of a stellar and laboratory

wavelength becomes quite large, and other factors must be considered along with wavelength agree- ment. These include the excitation potentials, the

results of comparisons of relative line intensities

in the stellar and laboratory spectra, the wavelength tolerance, the line shape, and the general

quality of the line lists. Implicit in the eventual judgment about the

chemical origin of a given absorption feature in a

stellar spectrum is the reservation, of course, that the judgment may be incorrect. Even when the

investigator is confronted with conflicting evidence,

however, the probability can ordinarily be con- sidered high that the assigned origin of a line is actually the physically correct one provided the

weight of the evidence favors it. In certain cases,

as in the identification of Ha in many stars, this probability of correctness can approach unity. In other cases, when the evidence is ambiguous or when the line for some reason cannot be compared

for consistency with a group of related lines, for example with other lines of the same multiplet, the

process of line identification will often be quite

subjective. For weaker Unes especially, there

always remains the possibility that the stellar line may be a blend.

Under such circumstances, the acceptance of

abundance results from any atmospheric analysis

must necessarily be cautious. For example, an independent study of sources of data now available

for hafnium spectra raises some doubt as to whether

hafnium contributes significantly to any of the lines assigned to Hf II and used to derive a hafnium

abundance in a recent analysis of e Virginis. The

same is true in the case of Cdl and, to a lesser

extent, of Gd II. Pr II, and some other spectra in that

18
work. It is admitted, however, that some other

observer might be able to marshal evidence in persuasive support of those identifications. The

purpose of this argument is only to stress the important point that the reliability of derived chemical

abundances can never be greater than the reliability of the line identifications, and that errors in this phase of the analysis severely compete in magnitude

with other sources of error. This is especially true when the number of stellar lines observed for a given

chemical species is small. The point is well illus- trated in connection with the later discussion of

ruthenium in ^ Cap.

3.1.2. Literature Sources Used in Making

Line Identifications

In the main, only two important sources have

been used to assist in the identification of spectral

lines observed in C, Capricorni. These are the Second

Revision of the Rowland Table (Nat. Bur. Stand.

(U.S.), Monogr. 61, 1966) and the Tables of Spectral

Line Intensities (Nat. Bur. Stand. (U.S.), Monogr. 32,

1961). The first of these is probably the most useful

single reference for line identifications in stars near

spectral type G. The authoritative solar identifica- tions contained in that work document the results of

critical evaluations by C. E. Moore and others and

are appropriately conservative. The severe deficiency of the solar spectrum in fines of the rare

earths, however, represents a crucial limitation to the application of the Rowland Table to line identi- fications in barium stars, where the enhancement of

lines of certain rare earths is a feature that helps

to define the class. In this respect, the NBS Intensity Tables, currently one of the best sources for wavelengths in the first and second spectra of the

rare earths, offer a most useful and necessary sup- plement to the Rowland Table. The Intensity

Tables are correspondingly deficient in lines of the

lighter elements and the iron group, but in the case

of only one rare earth spectrum (Ce II) does it ap- pear that the spectrum of ^ Cap has exceeded the

sensitivity Hmit of those tables. The usefulness of NBS Monograph 32 in analyzing a stellar spectrum is significantly increased by

the inclusion of line classifications and of relative intensities on a fairly uniform scale. Since the arc temperature to which these intensity measurements

correspond is 5100 K, the stated relative intensities

(at least over limited spectral ranges and within a

single spectrum) serve as a rough guide to those

observed in the spectra of stars having reciprocal

excitation temperatures (5040/7^x0) near the typical

value ^*xc = l-00- If the stellar temperature departs

appreciably from this value, a rough mental con- version of the intensities can be made by paying

attention to the excitation potential of the line. This

feature was an enormous aid in the treatment of the

rare earths in the barium star (0exc^l-13). It often

provided the only additional evidence required be- yond simple wavelength coincidence to confirm a

line identification or to recognize a blend. It is possible that too much reliance has been placed on

these intensities, but their general utiHty in this respect has been amply proven.

In general, the intensity estimates included in most laboratory analyses of atomic spectra must be

used with great caution in making identifications

in stellar spectra. The rough intensity estimates

Hsted in the MIT Wavelength Tables (Harrison et al., 1939), for example, are not homogeneous and can

be very misleading. The best criterion for relative intensity comparisons is to be had from laboratory

estimates by a single experienced observer, such as those contained in the many contributions by A. S. King or the NBS Intensity Tables.

Several other references used extensively in making line identifications in ^ Cap include the

Revised MuUiplet Table (Nat. Bur. Stand. (U.S.),

Tech. Note 36, 1959), the line lists for e Virginis by

Cayrel and Cayrel (1963) and for barium stars by

Warner (1964b), the MIT Wavelength Tables,

individual papers in the literature, and some un- pubhshed laboratory line lists.

3.1.3. The Identification of X 4608.74

The identification of a line measured at 4608.74 A

on the tracings of ^ Cap has been selected as an

illustration of the procedure. The line is well isolated

and is of good quality. Its observed central depth

and equivalent width are Rc = 0.20 and = 47 mA,

respectively. The Revised Multiplet Table contains no line sufficiently near the observed wavelength

to provide an identification. The Rowland Table

lists an unidentified weak line {W = 4 mA) at 4608.71 A, but since the line observed in ^ Cap is ten times stronger, the coincidence in wavelength

is tentatively assumed to be fortuitous. Experience

with other lines has shown generally closer agree- ment in equivalent widths between corresponding

unidentifiable features in ^ Cap and the sun. The

only possibility found in NBS Monograph 32 is a Mo I fine with intensity 2.5 at 4608.71 A having a low excitation potential of 2.50 eV. This identifica19
o

in

Tax

-Log X' (solar)

Figure 3.1. A nonsense differential curve of growth for ''tantalum'^ in ^ Capricorni.

As explained in the text, the lines used actually belong to ten different spectra but approximately coincide in wavelength with known Ta I lines. Note the reasonable fit of these

points to the theoretical curve of growth adopted for the star. This plot should be compared with that of figure 3.2.

20
-3.00 -2.00 -1,00 0.00

Log(gfX)-0X

3 .00

Figure 3.2. An absolute curve of growth constructed by use of the same "'tantalum" lines as in figure 3.1.

The ^/-values are taken from ihe w.jrk of Corliss and Bozman (1962). The sc-atter caused by bad line idenlificalions is considerably more pronounced than in the differential curve t>f firowth.

21
tion for the line is given in Warner's list for ^ Cap,

but a rough check for intensity consistency casts doubt upon its correctness. The strongest lines of

Mo I near this wavelength in Monograph 32 are masked in ^ Cap by lines of different chemical

origin, but the line at 4621.38 A with intensity 8

provides a good test, because its excitation potential

(2.28 eV) is comparable with that of the line under

discussion. On the basis of the relative laboratory

intensities its central depth would be expected to be about 0.40, but no line absorption is present at that wavelength on the tracings. Several other

nearby Mo I hues to be expected on the assumption

of the above identification are also absent. The

identification of the observed stellar line as Mo I must, therefore, be rejected.

Unless such a line for some reason were con- sidered of strategic importance, the expenditure of

additional effort to identify it would probably not be

justifiable, except as an example.

An examination of this wavelength region on the

tracings of rj Pegasi (G2 II-III) suggests that the hne

might belong to the spectrum of one of the rare earths enhanced in (, Cap. The line is not present in

rj Peg, even though the spectra of the two stars apart

from these rare earths are quite similar. The MIT

Tables, listing a cerium line of unknown ionization

stage (I or II) at 4608.75 A, offers some support for

this conclusion, but the absence of this line from

NBS Monograph 32 raises serious doubt. The

strength of the observed stellar line would definitely

require it to be above the sensitivity threshold of

the cerium list in that work. An appeal to the un- published cerium lists of Martin and Corliss, and

of Albertson, confirms the Ce II identification, however, and the contradictory evidence of Monograph

32 is resolved by a check of the original spectrograms used for that work — the line is present with

intensity 4 on those plates, but was accidentally

omitted from the measurements. Finally, from the

list of Ce II energy levels provided by Goldschmidt

(1968) the classification of the line has been deter- mined, and a ^-value calculated for it. The identi- fication as Ce II appears to be correct, and the hne

has been included in the curve of growth for Ce II.

3.1.4. A Nonsense Curve of Growth for

Tantalum (Ta I

)

A forceful demonstration that even random line identifications can lead to apparently reasonable

results is provided by the following example, which

illustrates, also, one of the major hazards in applying

the method of differential analysis to stellar atmospheres.

A nonsense curve of growth has been constructed

for tantalum in ^ Cap by selecting from the final hst of observed Hues all those that approximately

correspond in wavelength to known tantalum hues

(Ta l). The coincidences in wavelength are fortuitous,

and the observed hues are properly attributed to ten

different spectra in table A. In associating these

lines with tantalum, general intensity considerations were also taken into account in the sense that wavelength coincidences with very weak Ta I lines were

disregarded. Differential excitation corrections

depending on the actual tantalum excitation potentials were made in the usual way to solar line strengths. The latter were obtained by reading the

Utrecht equivalent widths for the corresponding solar

lines at those "tantalum" wavelengths into the

Pierce-Aller curve of growth. It is emphasized again

that these are not tantalum hues, either in the sun

or in the barium star. But the resultant differential curve of growth, shown in figure 3.1, has little scatter and appears to be quite well established. By fitting to the points the theoretical curve adopted later for

^ Cap, one might conclude that the tantalum abundance in the barium star differs very little from that

in the sun. The predicted shift for equal abundances

with respect to hydrogen in the two objects is 0.75. The observed horizontal shift of the observed curve

to the theoretical one is 0.69. The curve of growth for the same lines, con- structed by using the g/"-values given for Tal in NBS Monograph 53, is shown in figure 3.2. A comparison of the two curves leaves little doubt that the

differential abundance derived above for "tantalum"

has no physical meaning.

It is a well-known observation, commonly

attributed to poor laboratory /-values, that curves of growth constructed by use of stellar line strengths

tend to show less scatter than those constructed

by use of laboratory oscillator strengths. In view

of the above curves for "tantalum," this result is not entirely surprising. In fact, several of the

differential curves of growth constructed here for

^ Cap show noticeably more scatter than do the

corresponding absolute curves. Misidentified lines

will ordinarily not stand out in differential curves of

growth because the differential curves of many

spectroscopically conspicuous elements fall quite

close on the horizontal axis if the excitation temperatures and relative chemical abundances in the two

objects are nearly the same. The more prominent

22
scatter of misidentified lines on absolute curves of growth is caused partly by the greater involvement

of (a) the absolute abundances of the individual

elements in the star, (b) the relative partition functions of the elements, and (c) the excitation potentials of the individual hnes plotted, the latter being

virtually suppressed in a differential analysis

because of the commonly small differential excitation temperatures. This is clearly shown by table

7.3, giving the predicted horizontal shifts of differ- ential curves of growth for equal chemical

abundances in the barium and comparison stars studied here. For example, the predicted shifts for the neutral elements in the iron group are

essentially identical, as are the shifts for all the

singly ionized atoms. Some elements having ionization potentials significantly different from the

average depart from this rule — neutral zinc, for example.

For equal abundances, then, the differential curves of many elements will actually coincide

within the error of observation, as can be seen by

superimposing the sample curves of growth shown

in section A.l of the Appendix. In such circumstances, the correctness of the fine identifications

becomes almost irrelevant to the appearance of the empirical curves of growth, as demonstrated

above for tantalum. It is a great weakness of the

differential method that mistakes in spectral line identifications are often inconspicuous.

A good example in this connection is offered

by the work of Cowley (1968). who examined point

by point aU those lines that showed a wide scatter from the absolute (but not the differential) curve of

growth that he constructed for Fe I in the Ba II star HR 774. He demonstrated that in nearly every

case the dominant contributor to the line had very

likely not been properly chosen.

This discussion argues strongly that even in a

differential analysis the use of relative or absolute

gf-values is very desirable whenever possible, if only as an additional check on the line identifications. Such recourse undermines one of the important advantages often cited for the differential method, namely its independence from laboratory

/-values, but its many other advantages remain

intact and persuasive.

3.2. The gf-Values

3.2.1. The Use of gf-Values in This Study

As explained in section 3.1.4, the use of absolute

gf-values in this differential study has been confined

for the most part to the resolution of questions

connected with spectral line identifications and to the recognition of blends. But in certain instances

gf-values have been used also as a means to improve

abundances determined from inadequately populated differential curves of growth. For several

spectra, in particular those of the rare earths, the

total number of good lines observed in the barium

star greatly exceeds the number in common with

the line lists of the comparison stars. Only two of

the 61 lines of neodymium measured in ^ Cap appear

also in the list for e Virginis, for example. The situa- tion with respect to the sun is somewhat more

favorable, but the rare earth lines used in the

analysis are generally quite weak in the solar spec- trum because of the differences in opacity, electron pressure, and chemical abundance. The difficulty in accurately measuring such weak solar lines greatly increases the scatter in the differential curves of growth for these elements with respect

to the sun. Under such circumstances, more reliable differ- ential abundances can be obtained by a suitable

conversion of the available ^/-values to the system

of line strengths in the comparison star. The details of this conversion are given in section 4.3. This procedure obviously permits a better utilization of the experimental material. A similar approach was used by Wallerstein and Greenstein (1964) in their differential study of two CH stars with respect

to e Virginis. With the exception of Nd II, however,

the present results for the conversion of several

spectra to the system of e Vir do not agree entirely

with those obtained by Wallerstein and Greenstein.

This discrepancy has been discussed privately with

Wallerstein, but joint efforts to pinpoint its origin were not successful.

3.2.2. Sources of g/-VaIues

The ^/-values used in this investigation are listed

in column (7) of the main table A; they were taken

from the sources given in table 3.1. In the few cases

(except Fe II) where gf-values for a single spectrum were taken from more than one tabulation, a comparison of values in common showed the data to be

very nearly on the same scale, and no corrections

for scale were applied. The small corrections sug- gested by Warner (1967) to the gf-values for Sc II and Ti II given by Corliss and Bozman (1962) are, however, included. For Fell, a correction

+ 0.75 ±0.18 (std. dev.) was required to bring the

23
values of log (gf \) of Groth (1961) onto the same

scale as those of Warner (1967). This correction was

derived from 53 good lines common to both tabulations. No significant dependence on wavelength or

line intensity was noted.

Table 3.1. Sources of gf-values

op. Sn Ref. op. Ref. op. l\cl

Al I [11 Ge I [41 Sc I [41 Ba 1 (21 La II [41 L^J Sc II [41 Ba n [2] Li I [11 Si I [3, 9] C I fll Mgi [31 Si II [31 Cai [3] Mn I [4] Sm II [4J Ce n [4] Mo I [41 Sn [8,41 Co I [4] Nai [31 Til [41 Cri [4] Nbi [41 Tin [4,10,111 Cr II [10, 11, 12| Ndii [41 Vi [4] Cu I [51 Nil [71 Wi [41 Dy II [41 Oi [1] Yi [4] Eu II [4| Pbi [4] Yii [41 Fe I [61 Pril [41 Zn I [41 Fe II [11.121 Ru I [41 Zrl [41 Gd II [4] Si [31 Zr 11 [4]

References

[1] Wiese, W. L., Smith, M. W., and Glennon, B. M., Atomic

Transition Probabilities. Vol. I, Nat. Bur. Stand. (U.S.), Nat. Stand. Ref. Data Ser., 4 (1966). [2] Miles, B. M., and Wiese, W. L.. Nat. Bur. Stand. (U.S.), Tech. Note. 474(1969).

[3] Wiese. W. L., Smith, M. W., and Glennon, B. M.. Atomic

Transition Probabilities, Vol. II. Nat. Bur. Stand. (U.S.), Nat. Stand. Ref. Data Ser., 22 (1969). [4] Corliss, C. H., and Bozman, W. R., Nat. Bur. Stand. (U.S.), Monogr. 53(1962).

[S] Kock, M., and Richter, J., Z. Astrophys. 69, 180 (1968). [6] Corliss. C. H., and Tech. J. L., Nat. Bur. Stand. (U.S.), Monofir. 108(1968).

[7] Corhss, C. H., J. Res. Nat. Bur. Stand. (U.S.), 69A (Phys.

andChem.),87(1965).

[8] Eberhagen, A., Z. Phys. 143, 392 (1955). [9] Miller, M. H.. and Bengston, R. D., Astrophys. J. 156, 393

(1969). [10] Yamashita, Y., Publ. Domin. Astrophys. Obs. 12, 455

(1967). [II] Warner, B., Mem. Roy. Astron. Soc. 70, 165 (1967). [12] Groth, H. G.,Z. Astrophys. 51,231 (1961).

3.2.3. Wavelength-Dependent Corrections to the g/-Values of NBS Monograph 53

It has been necessary to make wavelengthdependent corrections to the ^/-values for some

spectra given in the compilation by Corliss and

Bozman (1962). Despite a number of well-known

shortcomings, this work remains the only source of

experimental gf-values for many spectra. As pointed

out in the discussion of samarium in section 5.2.18 and as shown in figure 3.3, a horizontal shift between

the blue and the red lines appeared in the absolute

curve of growth constructed for Sm II in i, Cap. The

possible causes of such a systematic discrepancy

are many and complex. The observed shift may yet

be attributable to the identifications or to the measured equivalent widths, but it appeared important

to start by examining the gf-values themselves. A

possible cause for the observed discrepancy

emerged.

The gf-values given by Corliss and Bozman in NBS Monograph 53 are based on relative emission

intensities measured for 39,000 spectral lines of 70

elements by Meggers, Corliss, and Scribner (Nat. Bur. Stand. (U.S.), Monogr. 32, 1961). C. H. CorHss

has generously put at the disposal of the author the

original record books containing these intensity

estimates. The intensities represent visual estimates on spectrograms exposed to an arc fired between

copper electrodes diluted with 0.1 atomic percent

of the element under investigation. They were cali- brated against the simultaneously exposed copper

lines and are claimed to be on a uniform scale. Because of the spectrograph design and the varying

sensititivity of the photographic emulsions used,

it was necessary to make five different sets of ex- posures in order to cover the wavelength region from

2000 to 9000 A. The breaks, or overlap regions,

between the various exposures occur on the average

at 2800, 3800, 4800, and 6800 A. In reducing the

measurements, duplicate intensity estimates for

fines observed on both exposures in the regions of overlap were simply averaged, but an examination

of the original data reveals in some cases a systematic, not a random, variation between the two sets of spectrograms. These systematic effects are probably related to a variability in the burning of

the arc and in the vaporization of the elements from

the copper electrodes from one exposure to the

next. In any case, it would seem more appropriate

to correct for these systematic variations not by

averaging the overlap regions but by adjusting the

different sets of exposures either to the intensity

scale of an arbitrarily selected one or to some

average scale. In table 3.2 the intensity ratios found between

exposures for a number of spectra of immediate

interest in this investigation are tabulated. Only

the overlap regions at 4800 and 6800 A are important

for this study. No difference was found between the

calculated intensity ratios for the first and second

spectra of the elements considered. In some cases, however, the ratio appears to be dependent upon the

fine intensity. For example, the ratio for lanthanum

24
Figure 3.3. Absolute curve of growth for Sm II in ^ Capricorni.

As explained in the lexl, a systematic error in the ^/-values of Corliss and Bozman is believed to contribute to the systematic horizontal shift between lines with wavelengths

jireater than 5000 A ^c^osses} and less than 5000 A {circles).

25
Table 3.2. Mean ratios of original NBS intensity estimates for lines observed

in each of two different exposures

Element Range of No. of Intensity Standard Intensity Intensity Correction to overlap lines ratio deviation range dependence log {gfK)

(A) Ce 4680-4931 72 1.79 0.40 1-28 Y -0.18

6612-7000 37 1.74 .45 0.3-6 N -.42

Co 4663-4843 9 2.83 .61 0.6-4 N (-.30) 6678-6873 4 1.64 .27 0.4-2 N (-.50)

Cr 4646-4923 24 0.98 .25 3-100 Y .00 6661-6979 5 1.34 .33 1-2.5 N

Dy 4698-4894 18 1.50 .30 3-19 N -.15

6639-6930 24 1.16 .19 0.6-22 N -.21

Ell 4840-4912 4 1.00 .27 5-12 N .00 6645-6915 13 2.74 .45 0.6-100 N -.40

Gd 4728-4894 34 0.97 .14 2-45 N .00 6568-6887 28 1.44 .20 0.7-8 N -.15

La 4602-4861 40 0.81 .17 2-60 Y + .12 6650-6959 11 1.20 .18 1-13 N + .04

Mn 4701-4845 10 1.15 .14 2-90 N -.05

0 AO/I Q 1 o.UU

Mo 4595-4869 44 0.60 .14 1.6-90 Y + .30 6650-6992 32 2.18 .78 0.2-7 Y -.13

Nd 4670-4945 71 1.88 .45 1.2-26 N -.30

6650-6907 28 1.83 .31 0.8-5 N -.56

Ni 4714-4919 8 0.66 .16 1.8-12 N (+.18) 6643-6915 4 2..34 .89 0.5-1.6 N

Pr 4687-4785 16 0.75 .12 5-30 N

4785-4926 25 1.70 .39 1.2-13 Y

6595-7021 19 1.67 .45 0.6-7 Y

Sc 4670-4910 18 1.41 .31 2.5-110 Y -.15

6737-6836 5 1.10 .09 3.5-7 N .00

Sm 4674-4930 53 1.98 .29 1.4-65 N -.30

6569-6910 42 1.11 .23 1.4-22 N -.35

Ti 4722-4886 27 1.10 .20 1.6-40 Y -.05

6575-6944 13 1.46 .20 1-8 N -.20

V 4670-4905 33 0.92 .19 1.4-50 N .00 6605-6871 12 1.33 .31 0..5-5 Y .00

Zr 4627-4894 39 1.02 .17 2-200 Y .00 6678-6855 17 1.31 .25 0.6-9 N -.10

26
o at the 4800 A break varies from about 1.0 at 1 = 2

, to 0.6 at 7 = 60. Also, the ratio found for praseo-

! dymium changes abruptly from less than 1.0 to greater than 1.0 in the middle of the 4800 A overlap

region. A thorough analysis of these additional

complexities is beyond the scope of this investigation, but is being pursued in connection with the

revision of NBS Monograph 32 now in progress by

C. H. CorHss and the writer. The successive columns of table 3.2 give the

j relevant chemical element, the exact spectral region

of overlap, the number of lines common to the differj ent exposures in the overlap region, the mean

intensity ratio at the break in the sense intensitylongward/intensity-shortward, the standard deviation from the mean, the range of (shortward) in- tensities in the region of overlap, an indication of

any intensity dependence (Y=yes, N=no), and the

correction to log {gf A) recommended to place all values between the breaks on a scale consistent

with that at 4500 A. The intensities in NBS Monograph 32 for most Unes within the stated overlap

ranges represent averages from two exposures and

1 the indicated correction must be suitably adjusted.

The recommended corrections do not exactly cor- respond to the observed intensity ratios. When a dependence upon intensity is indicated, the adopted

correction was weighted toward the stronger lines.

,1 Also, the corrections for some spectra are absent

' or given with reservations (in parentheses) because

of insufficient data. The effect of the wavelength-dependent error

as it propagates to the NBS gf-values is particularly

apparent in the absolute curve of growth constructed

for Nd II in C, Cap (fig. 3.4). The average shift re- quired to bring the red lines into unsystematic

scatter about the curve defined by the blue lines

I is —0.22, in good agreement with the correction

found in table 3.2.

3.2.4. Comparison of the NBS Intensity Estimates for Neodymium With Those of King

(1936)

A possible consistency check on the above results was obtained by comparing for neodymium the arc

jl intensity estimates of Meggers et al. (1961) with

[t! those of King Q933). Because of the somewhat

I

unequal excitation conditions in the two experiments, the first and second spectra are treated

separately, and the range of excitation potentials

for lines used has been restricted. The average value

of the ratio R = Imsllii^ns was calculated from se- lected lines on each side of the break at 4800 A. The empirical exponent 0.65, derived in a pre- liminary analysis, compensates for the nonlinearity

of King's intensity estimates and ehminates the

intensity dependence of the ratio R. The value

found for this exponent is in good agreement with

Russell's (1925) observation that in many multiplets

the square roots of King's intensities are pro- portional to the LS theoretical intensities. The

results for neodymium spectra are given in table

3.3.

Table 3.3. Comparison of NBS intensity estimates

for neodymium with those of A. S. King

D _ ^NBS ^ T0.65 •King

Range Spectrum No. of lines («) Std. Dev.

iA) 4350-4670 Ndl 20 0.85 0.13 Ndll 67 1.29 .27

4910-5320 Ndl 29 1.91 .37 Ndii 39 4.29 .55

It is seen that the NBS intensities tend to become

larger with respect to King's intensities as the

4800 A overlap region is crossed. This is in general

agreement with the results given above, but it is emphasized that no firm conclusions can be drawn

owing to a lack of knowledge about the photographic

details in the King experiment.

It is noteworthy that among the rare earths only

lanthanum shows an intensity ratio less than unity

at the 4800 A break. The discrepancy discussed by

Wallerstein (1966) in the solar La/Ce abundance

ratio appears to be related to this fact. Using NBS

gf-values, Wallerstein found that the La/Ce ratio

in the sun was anomalously high in comparison

with that observed in chondritic meteorites. A

partial re-analysis of Wallerstein's data carried

out in the light of the above results resulted in an

appreciable reduction of that discrepancy.

The validity of applying the stated corrections

outside the overlap regions in which they are explicitly found cannot be easily established. Judging

from the available evidence and from the manner

in which the original intensity estimates were cali- brated, it appears that the extrapolation is required.

But until a more definitive analysis of these sys398-978 0 - 71 -3
Figure 3.4. The curve of growth for Nd II defined by the blue lines (< 5000 A, circles) lies to the left of that defined by the red lines {> 5000 A, crosses).

This has been tentatively attributed to a systematic error in the ^-values of Corliss and Bozman. but a systematic error in the measured equivalent widths may also contribute.

28
matic effects can be made, the indicated corrections have been adopted only for Eu. Dy, Nd, Sm,

La. and Ce. which seem well estabUshed and are

of greatest importance in the present study. In

the meantime, it is important to call the attention

of other users of the NBS g/-values to the above re- sults and suggest that, for greatest accuracy,

astrophysical usage of these gf-values be restricted

as far as possible to lines whose original intensities he in the range 3 < / < 200. and whose range of wavelength does not cross one of the overlap re- gions noted above (at least for those elements

exhibiting abnormal behavior in those regions).

3.3. A Relation for Converting NBS

Intensities of Unclassified Lines to

gf-Values

As a final remark on the Hne intensities given in NBS Monograph 32. we derive a useful relation

that appears not yet to have been recognized, but

that is extremely useful in constructing absolute curves of growth for stars whose excitation temperature 0exc (5040/rexc) is near unity. We have

found this relation to be very helpful in identifying

rare earth hnes in ^ Cap.

The collection of gf-values by Corliss and Boz- man. although based on the NBS Intensity Tables,

included only those Unes from the latter tables

whose energy classifications were known, roughly

60 percent of the total. But in many cases the

remaining 40 percent of the Hnes become avail- able for constructing stellar curves of growth,

because attention is focused not so much on gf as on the quantity log (gfk) —6*^^x^ for which a reasonable approximation can be found even with- out knowing the Hne classification. Here x is the

lower excitation potential of the line expressed in electron volts. The NBS arc intensities provide gf-values through

the expression

gf==C{ulNp)Ik^e (3.1)

where C is an empirical normaHzing function that converts relative values of gf to absolute values, u is the partition function, A'^ is the percentage of

atoms of the element in the given stage of ionization,

and p is the persistence of the atoms in the arc stream. The other symbols have their usual meanings. The values of C, N, p, and T can be found in the introduction to the work of CorHss and Bozman.

After multiplying both sides of eq (3.1) by the wavelength, converting to logarithms, and subtracting

^excX' we find

log (g/-A)-0*x = 4 1og\ + log/

+ C' + a0^'-^£„-0*X (3.2)

where a = 1.2398 X lO""* eV/cm"^ The wavelength

is here expressed in angstrom units and the upper

energy level E„ in cm~^ We have also set

C' = log {ulNp)+ log C. (3.3)

In the original reduction, Corliss and Bozman

adopted for log C an empirically determined function

that was the same for all spectra and that depended

on Eu- A detailed investigation by Warner and

Cowley (1967) indicates that the function varies

from spectrum to spectrum, however. In the case

of Fel, for example, the constant value log

C = — 16.61 appears to be most appropriate.

The last two terms of eq (3.2) can be put into a more convenient form by setting

and by using the relations

and

X = ocEi,

n = 1.0003

10«

iE„ - E,) =

nX.

(3.4)

(3.5)

(3.6) where Ei is the energy of the lower level of the

transition, and n is the approximate dispersion of

air. We then have

aO^^'Eu - d*x = ad^'^^En - aid''"' + Ae)Ei = a9^''{Eu-Ei) -Adx (3.7)

Since the temperature of the NBS arc is 5100 K, we have ^^''^ = 0.99, and eq (3.1) becomes, finally.

log igfk) -0*x = 4 log X + log/ +

12300

+ C - A^x (3.8)

29
where the difference is just

Ae=dt,,-0.99. (3.9) For unclassified lines, the unknown correction

term — A^x reasonably approximated by

adopting for x ^ value most suitable to the given

wavelength and element. For the sun, where = 0.03 (6®, = 1,02) one might arbitrarily

choose X ~ 2 eV for unclassified lines. The maximum error in calculating log (g/A) — 0®x by the

above formula is then only 0.09 over a range of 5 eV, well within the accuracy of the NBS intensities

themselves. As a practical matter, those workers

who use the NBS /-values from magnetic tape in computer applications might consider the advantages of having the NBS Intensity Tables on tape

instead. Equation (3.8) not only makes the unclassified lines available in many cases for constructing

Note Adde

The recent, very important measurements of Fe I /-values at the Kiel Institut fiir Experimentalphysik^'-, the National Bureau of Standards^, and

elsewhere leave little doubt that a temperature

error was present in the early measurements of

King and King^' ^. This temperature error has

been propagated to a number of other collections

of experimental /-values that directly or indirectly

used the data of King and King for purposes of cali- bration. Such a propagated temperature error occurs also in NBS Monographs 53 and 108, which

have served as sources of /-values for several

spectra in the work presented here.

It must be explicitly pointed out that the stellar analysis given in the present work is a differential one, and the results do not significantly depend on

the /-values. The restricted use of /-values here —

mainly to assist in line identifications — has been

explained in sections 3.1.4 and 3.2.1. As a test of the effect the temperature error has on our absolute curves of growth, we have reconstructed the curve of growth for Ce II shown in figure 4.4 after applying the temperature correction derived below.

The shape of the curve was negligibly affected;

it is merely shifted in the direction of smaller

abscissae by — 0.97.

It is apparent from eq (3.1) and the subsequent

analysis that A log(g/) = A^X" + AC' (3.10)

1 Garz, T., and Kock, M., Astron. & Astrophys. 2, 274 (1969).

2 Richter, J., and Wulff. P., Astron. & Astrophys. 9, 37 (1970).

•''Bridges, J. M., and Wiese, W. L., Astrophys. J. 161, L71

(1970).

' King, R. B., and King, A. S., Astrophys. J. 82, 371 (1935).

5 King, R. B.. and Kng, A. S., Astrophys. J. 87, 24 (1938).

curves of growth, but also reproduces the NBS

g/values themselves (by setting 6* = 0.00). Unhke

the gf-values, moreover, the line intensities are not

subject to revision as the partition functions are improved or as the normalizing function C of eq

(3.1) becomes better understood. Also, evidence is accumulating that the temperature of the NBS arc may actually be closer to 7000 K than to the adopted

value 5100 K (Corliss, private communication).

If this should prove to be the case, the above

analysis remains intact, of course, but some

modification would be necessary. For example, the

value of the quantity C in eq (3.8) would require an

adjustment to reflect the different degree of ionization corresponding to the higher arc temperature,

and the application of the equation to unclassified

lines would have to be restricted to stars having

excitation temperatures near 0^*^ = 0.72.

In Proof:

where A log (g/) is the error in log (gf) resulting

from an error Ad in the adopted arc temperature.

Not for all lines, but for the vast majority of them,

the temperature error present in the aforementioned

NBS monographs unquestionably dominates any

systematic errors owing to departures from LTE and

other causes. Monograph 108 is a tabulation of

/-values from several sources and any assumed

temperature error would, of course, be that of

a "fictitious" arc. Since the values in this compilation were cahbrated against the NBS arc used

in the preparation of Monograph 53, the temperature error in the two works should be approximately the same, however.

From a least-squares comparison of Monograph

108 with the Kiel /-values only, we find A0 = — 0.25,

corresponding to a temperature for the NBS arc

of 6810 K, compared with the previously adopted

value 5100 K. Application of this correction to the

NBS values gives a standard deviation of ±0.i6

between the two sets of log (g/)-values. Even

without a knowledge of the element-dependent

quantity AC in eq. (3.10), it would seem that useful relative /-values, for statistical purposes

only, could still be obtained by applying eq (3.10)

to the data of Monograph 53. We cannot here give

further study to this recommendation, but such an

investigation, including the relationship to the

temperature error of the so-called normalization

function C, might be worthwhile because of the

likelihood that many spectra included in that monograph, especially those of the rare earths,

will not be re-observed in more precise experiments in the near future.

30
4.1

4. Curve of Growth Analysis

The Differential Method

The atmosphere of ^ Capricorni has been studied

differentially with respect both to the sun and to the

G9 II—III giant e Virginis. analyzed in detail by

Cayrel and Cayrel (1963). The method of differential analysis used here, imphcit in the pioneering work of

Adams and Russell (1928), has been extensively

developed by Greenstein (1948, 1949) and by Pagel

(1964).

The theory of stellar atmospheres has now reached

such a successful stage of development that the

analysis of a stellar spectrum should, ideally, be

based on a rehable model atmosphere calculated

for the star. The widespread availabihty and use

of electronic computers has essentially eliminated

any computational objections to such a refined

depth-dependent analysis. But, as pointed out by

Cowley and Cowley (1964), the difficulty is not merely computational. Uncertainties in the experimental data (the equivalent widths, the laboratory

/-values), and in the stellar parameters (effective

temperatures, surface gravities), as well as the

theoretical problems associated with the treatment

of blanketing, turbulent atmospheres, and departures from local thermodynamic equilibrium, make

it doubtful whether a calculated model offers accuracy in abundance determinations as great as the complexity and labor of such a treatment would

suggest.

In particular, for the rare earths that are of great

interest in Ball stars, there is considerable uncertainty both in the absolute scale of the one set of

available /-values and in the relevant partition functions. Also, in an atmosphere with high macroturbulent velocity (as in ^ Cap) there is some doubt

whether a physically meaningful temperature dis- tribution with depth can be assigned. In any case, experience has shown for several stars —e Virginis,

for example — that the results of analysis in the

single-layer approximation are in very good agree- ment with those obtained for the same stars by

detailed analyses based on model atmospheres.

For comparison with the results derived in the

present monograph, the writer is currently carrying

out a depth-dependent analysis of C, Capricorni. A

model atmosphere was developed for this purpose

from the grid maintained by Gingerich and his co- workers at the Smithsonian Astrophysical Observatory. The analysis is not yet completed, but the

preliminary results indicate only minor differences

with the differential study presented here. The curve of growth for spectral lines can be

viewed quite generally as a saturation curve giving

the equivalent width as a function of total oscillator strength. In the Milne-Eddington formulation, the

abscissa of the curve of growth is defined by the

fine strength parameter r),,. where (Unsold, 1955;

Aller, 1963)

log r7o = log7V, + log {gfX)-dxr.s-loguiT) — log z; — log Ax + const. (4.1) Here A'^,- is the abundance of the element in the rth stage of ionization, Xr,s is the excitation potential

of the lower level s of the transition, g is the statis- tical weight of the level, 0 = 5O4O/rexc, "(T") is the

partition function, and k\ is the continuous absorption coefficient. In the analysis, the small variation

of the opacity over the wavelength range of the

observational material can be ignored. Differentially, for two stars of similar temperature, the small dif- ferences in values for the partition functions are not important, and one may write

[Vo] = [Nr]-MXr,s-[v]-[k] (4.2)

where the bracket notation introduced by Heifer

et al. (1959) is used. By this convention the bracket

[Q] is defined as the logarithmic difference in any

physical quantity Q between the star under study

and the comparison star. That is.

[Q] = log ^(star) — log (^(standard)

Qistar)

log

^(standard)'

(4.3)

By normalizing the theoretical curves of growth such

that the values of abscissa log A" = log 170 + const, and

ordinate log {WjK) coincide for weak lines, the

microturbulent parameter v is eliminated from the

analysis (Cayrel and Jugaku, 1963), and one may

write

[Z] = [yV.]-A0Xr,. - W- (4.4)

In the differential curves of growth given here for

^ Cap, values of log {WJ\) are plotted against

31
32
o

o

in

(P.8.00 7.00 6.00 5.00 4.00 3.00 2.00

-Log X

/

Figure 4.2. Differential curves of growth for nickel with respect to the sun (circles) and to e Virginis (crosses).

33
log X* — A6(£^ — *)xr,s where is the normalized

stellar line strength obtained from the theoretical curve for the comparison star (sun or e Vir) and

AdU~*) = di,,-d*^^. (4.5) By eq (4.4), the horizontal displacement required to

shift the empirical curve into coincidence with the

adopted theoretical curve immediately gives the

logarithmic abundance ratio of the element for the

given stage of ionization in the stars in terms of the

difference in opacity,

[X] = [Nrlk]. (4.6)

Finally, the apphcation of corrections to be dis- cussed later for differences in opacity and ionization

equilibrium between the two stars gives the total ratio of stellar abundances for the given element.

There are several advantages to performing a double differential analysis by using two comparison

stars. Comparison of two differential curves derived

from the same spectral lines helps in the recognition

of bad blends or poor measurements. For example,

a widely discrepant point in both empirical curves can usually be traced to blending in the barium star. Also, many lines measured in ^ Cap do not appear

in the line list for e Vir, but are available for use

in the differential curve relative to the sun. The

double analysis thus permits a fuller exploitation

of the observational data for the barium star. In accordance with the analysis of the Cayrels,

the chemical composition of e Virginis is assumed to be identical to that of the sun. As a byproduct of

the double differential analysis, however, one can

in fact derive the relative abundances also for e Virginis. The horizontal shift between any two dif- ferential curves plotted for some spectrum in (, Cap

is simply

A logZ - [X] - [X] = [Nrik] ,_0

-[Nr/k]^-,. (4.7)

By expanding the brackets, it is seen that the parameters for the barium star cancel out, and

Mog X=[Nrlk],-e. (4.8)

The differential curves of growth for Ca I and Ni I in ^ Cap using the stellar line strengths discussed

in the next section are shown in figures (4.1) and

(4.2). The observed values of A log X are 1.37 and

1.23 for Nil and Cal, respectively. The corresponding values predicted in the detailed analysis by the

Cayrels on the assumption of equal abundances for

e Vir and the sun are 1.38 and 1.12.

4.2. The Stellar Line Strengths

The solar line strengths, log X(Q), used in constructing the differential curves of growth for 4 Cap

were obtained by entering the Pierce-AUer curve

of growth with solar equivalent widths from the

Second Revision of the Rowland Table (Nat. Bur. Stand. (U.S.), Monogr. 61, 1966) and reading off the

corresponding value of the abscissa. Similarly, the

line strengths \ogX{e) for differential curves relative

to e Virginis were obtained by use of the equivalent

widths and theoretical curve of growth for e Virginis

given by Cayrel and Cayrel (1963). In both cases, the theoretical curves were normalized to have

equal ordinate (log [WIK]) and abscissa (log X(*))

for weak lines. To avoid the errors and the labor of evaluating

graphically both sets of comparison line strengths

for the 1100 spectral lines measured in I, Cap,

computer-oriented polynomials have been calculated

to represent each theoretical curve in the form

logZ =/(logr/A). Since the values of log {WqIK)

and log (WtlX) were included on the punched cards

containing the measurements in I, Cap, the evaluation of the corresponding log X{*) could be rapidly

accomplished.

The theoretical curves of growth for the two comparison stars were indirectly reconstructed. The

Pierce-AUer curve of growth was obtained by using

the solar equivalent widths and solar Hne strengths

Usted by the Cayrels in their line list for e Vir. The

curve for e Vir was similarly reconstructed from the

values of log ^(e) given by Wallerstein and Greenstein (1964) in their Hne Hst for two CH stars. The analytical representation for each curve was

obtained by fitting the corresponding set of points

to a polynomial by means of the general least- squares program CWLT5 mentioned earher. It was

necessary to divide each curve into three sections,

because a simple polynomial representation for the

entire curve is not possible to the desired precision.

Table 4.1 Hsts the coefficients of fifth-degree polynomials describing each section. The coefficients are stated in exponential format, in which the sign

and integer following each number represent the

exponent of the power often by which the preceding

number is to be multiphed. (In this convention, for example, 1.2345 + 3=1.2345x 103). Nowhere does

the error in the calculation of log X exceed 0.02 by

use of these expressions.
T.\BLE 4.1. Coefficients for the polynomials rep- resenting the normalized stellar curves of growth

logxn^^ air

i = 0

Sun e \ irgims C, Capricomi

-6.50«y«4.85 -6.50 «y« -4.85 -6.50Sy«-4.60

-Oo

fll a.

ai

<Li as

+ 9.054776210 +2

+ 7.295101356 +2

+ 2.343845144 +2 + 3.769455460 +1 + 3.030168531 +0

+ 9.739678650 -2

+ 7.592728450 +2

+ 6.216381693 +2

+ 2.032155776 +2 + 3.330008853 +1 + 2.729582146 +0

+ 8.949677628 -2

+ 1.500322741 +3 + 1.325361840 +3 + 4.674737809 +2

+ 8.244279540 + 1 + 7.261594589 +0 + 2.554781086 -

-4.85 « yS -4.45 -4.85«y«-4.45 -4.60«y«-4.20

Oo

Oiat

Oi

Oi

as

-2.969210028 +5

-3.157713154 +5

-1.342551273 +5

-2.852608896 +4

-3.029173506 +3

-1.286112672 +2

+ 7.322789597 +5 + 7.829199288 +5 + 3.348216960 +5 + 7.159176686 +4 + 7.653391012 +3 + 3.272402327 +2-2.269867716 +5

-2.528140610 +5

-1.125246254 +5

-2.501961990 +4

-2.779276587 +3

-1.233999502 +2

-4.45«yS-3.50 -4.45 =s y«-3.50 -4.20«y«-3.50

ao

atat

as

atas

+ 1.722082789 +4

+ 2.152726622 +4

+ 1.075557085 +4

+ 2.684783907 +3 + 3.348264877 +2 + 1.669141190 +1

+ 1.782950880 +4

+ 2.311731158 +4

+ 1.197860158 +4

+ 3.100207120 +3

+ 4.007339284 +2

-2.069643167 +1

-1.411797999 +4

- 1.773508229 +4

-8.874656647 +3

-2.210547953 +3

-2.739442329 +2

-1.350177854 +1

We stress that no physical significance is attached

to these analytical expressions, which were used

solely as an expedient labor-saving device. Although

the adopted polynomial representations yield the

desired accuracy, no claim is made that the best

representations for the curves have been found.

For later use, the coefficients representing the

normahzed curve of growth for ^ Capricorni as described in section 4.4 are also listed in table 4.1.

4.3. Conversion of NBS gf-Values to

Line Strengths in e Virginis

As pointed out in section 3.2.1, the spectra of

certain rare earths are more completely developed

in ^ Cap than in e Vir as a result of the greater abundances in the barium star. For example, only two of more than 60 Nd II hnes measured in ^ Cap are also contained in the hne hst for e Vir. Some other lines of Nd II that were in fact observed in the comparison

star could not be used in the differential curves of growth, either because the degree of blending was

different in the two objects or because the spectral

range of the present observations did not include

them.

In order to use the extensive observational material to better advantage, therefore, the NBS

gf-values for several spectra have been converted

to the system of e Virginis by a method that is essentially a reversal of the familiar one by which

estimates of /-values are obtained from observed

stellar Hne strengths. This indirect procedure gives

fairly rehable differential abundances from the gfvalues without making any demands on the correct- ness or consistency of their absolute scales.

If the curve of growth constructed for e Vir by use

of gf-values has the same shape as the theoretical curve derived by the Cayrels (1963), one can write

with sufficient accuracy

logX{e) = log{gfX)-d{e)x + 8 (4.9)

where 8 is a constant that differs from spectrum to spectrum and effectively shifts the corresponding

gfX curves of growth to the normahzed theoretical curve for the comparison star. Values of the quantity

8 have been determined that are appropriate to six rare-earth spectra for which the differential curves

of growth for ^ Cap are not sufficiently populated to yield reliable abundances. Within each spectrum, an unweighted average was taken of the 8-values

obtained by applying eq (4.9) to all but a few badly

blended Unes in the hst given for e Vir. A slightly

different treatment of the Pr II spectrum was

required, because the Pr II Hnes measured in e Vir

are so badly blended that httle confidence can be

accorded a 8-value derived from those hnes. The

S-value cited for Pr II in table 4.2 was therefore

obtained by first applying eq (4.9) to the more

numerous solar Pr II lines and then adding the

shift +1.06 predicted from the model atmosphere

analysis by the Cayrels. The individual residuals

indicate the probable error in the determination of

the 6-values to be less than about ±0.20. The

results are given in table 4.2.

Table 4.2. Conversion of NBS gi-values to line strengths in e Virginis

lofZ(e)=log igfk)-die)x + 8

Spectrum 8

Cell -7.00 La n -6.26

Ndll -6.53

Prn -7.43

Sm n -6.95

Yn -5.46

35
o

o

O

"'9.00 8.00 7.00 6.00 5.00 4.00 3-00

-Log X

/

Figure 4.3. Differential curves of growth for singly ionized cerium relative to the sun (circles) and to e Virginis (crosses).

36
o

U3

CeiL

4 -1 .00 0 .00 1 .00 2 .00 3 .00 '.00

Log(gfX)-0X

Figure 4.4. Absolute curve of growth for singly ionized cerium.

(Circles, K < 5000 A; crosses, \ > 5000 A.)

5.00

37
o

o

<£>

O

"b.OO 8.00 7.00 6.00 5.00 4.00 3

-Log X'

Figure 4.5. Differential curves of growth for singly ionized lanthanum relative to the sun (circles) and to e Virginis (crosses

38
o

La IE

o

o

-2.00 -1.00 0.00 1.00 2.00 3.00 4.00

Log(gfX)-0XFigure 4.6. Absolute curve of growth for singly ionized lanthanum.

(Circles, K < 5000 A; crosses, K > 5000 A.)

39
40
Figure 4.8. Absolute curve of growth for singly ionized neodymium.

{Circles, \ < 5000 A; crosses, K > 5000 A.)

41
o

o9 ^

O

"^9.00 8-00 7.00 6.00 5.00 4.00 3.00

-Log X'

Figure 4.9. Differential curves of growth for singly ionized samarium relative to the sun (circles) and to e Virginis (crosses).

42
-1.00 0.00 1.00 2.00 3.00 4.00 5.00

Log(gfX)-0X

Figure 4.10. Absolute curve of growth for singly ionized samarium.

(Circles. K < 5000 A; crosses, X > 5000 k.)

398-978 0-71-4

43
Figure 4.11. Differential curves of growth for singly ionized yttrium relative to the sun (circles) and to e Virginis (crosses).

44
-3 .00 -2 .00 -1 .00 0.00 1 .00 2.00

Log(gfX)-0X

Figure 4.12. Absolute curve of growth for singly ionized yttrium.

(Circles, A < 5000 A; crosses, K > 5000 A.)

45
Now, in the differential curve of growth, the

abscissa is

log X' (e) = log X(e) - A0(^ - e)x. (4.10)

But by eq (4.9), this is equivalent to

\ogX'{e) = \ogisfk)-die)x + 8-A0U-€)x

(4.11) or logZ'(e) = log(gA)-6'(Ox + 8. (4.12)

The absolute curves of growth constructed for 4 Cap can, therefore, be treated in the same way as the differential curves in the derivation of relative abundances, provided the correction factors S are applied to the relative abundances obtained from

the observed shifts of the absolute curves. Since

these absolute curves of growth tend to be very well

defined, the determination of the abundance shifts can be accomplished with exceptional reliability.

The analysis is carried out in section 7.1. The absolute and differential curves of growth for five of these

spectra are shown in figures 4.3 to 4.12. The absolute curve of growth for praseodymium can be found in the Appendix.

4.4. Theoretical Curve of Growth for

C, Capricorni

Fundamentally, every fine of every atom in a

stellar atmosphere has a unique curve of growth —

there is no "universal" curve. To simphfy the analysis of (, Cap, some one theoretical curve of growth

must be selected that most nearly describes the

shape of the many empirical curves constructed

here for this star. Hunger (1956) has examined the most common

theoretical curves of growth based on simple stellar models (Milne-Eddington, and Schuster-Schwarzschild) and on simple mechanisms for line formation

(pure scattering, pure absorption). He concludes

that the differences between these curves are so

small, i.e., comparable with the errors in the physical data to which they are applied, that the choice

of one curve over another matters little in the analysis of a stellar atmosphere in this approximation.

As a mean theoretical curve. Hunger recommended

the use of that for pure absorption in the M-E

approximation or of that for coherent scattering

and the S-S model.

With various values assumed for the damping

constant, all the major theoretical curves based on

simple models (Wrubel, 1949; Hunger, 1956; van

der Held, 1931) have been compared with the empirical curves of growth for ^ Cap. The best-fitting curve was not the same for all spectra. Some of this variation could, however, be traced to the effects of blends or to the influence of systematic errors in the stellar line strengths (sec. 6.3) on the shape of

the empirical curves. The theoretical curve that

offers the best fit to the majority of the empirical curves of growth for ^ Cap, and the one that has

been adopted, is that for pure absorption in a MilneEddington atmosphere (Hunger, 1956). The quantity

Rc, the limiting central depth for strong fines in a given spectral region, appears in the expression for both the ordinate and abscissa of this curve. In most

of the following it can be assumed without significant error that /?c= 1. For example, the ordinate of the

theoretical curve is log {WI2Rcb), where 6, the

Doppler width, is given by

Since the ordinate is log {Wl\) in the empirical

curves, the vertical shift between the empirical and

theoretical curves of growth immediately gives the

velocity parameter v discussed in section 6.4.2. The shape of the upper part of the curve of growth

is governed by the choice of damping parameter.

For ^ Cap, the value of the damping parameter

log 2a = log (r/Awz>) (4.14)

was empirically found to be log (2q:)= — 2.5 from

a comparison of the theoretical curve with those of the empirical curves for which the damping region

is reasonably well defined. At 5000 A the classical

radiation damping constant is 7^1 ~ 0-889 X 10^ (AUer, 1963). The observed damping r= 1.4 X 10^ s"'

in ^ Cap is thus about 60 percent larger than the

classical value. The normalized theoretical curves of growth for both ^ Capricorni and e Virginis are shown in figure

4.13. The shapes of the two curves are practically

identical and can be made nearly to coincide by

sliding the curve of ^ Cap down the linear portion

to compensate for the difference in velocity parameters for the two stars. The curve shown in figure 4.13 for ^ Capricorni

has been drawn on all the empirical curves plotted

in this study.
o

o

o

o

m

i

o

o

o

o

I/}

IT)

O

O

O

LO

THEQRETICRL

CURVES

upper curve: ^^T Cap

lower curve : e Vlr

"^6.50 5.50 4.50 3-50 2.50 1 .50 0.50

-Log X

Figure 4.13. Normalized theoretical curves of growth for ^ Capricorni and e Virginis.

The curve for i Cap is thai calculated by Hunger (1956) for pure absorption in a Milne-Eddington atmosphere {log 2a =— 2.5). The curve for t Vir is taken from the study by

Cayrel and Cayrel (1963).

47
5. Comments on

5.1. Introduction

Some of the results derived later in this investigation of HD 204075 are closely associated with certain

early judgments and spectroscopic details about the

individual spectra studied. The writer has, for example, proposed energy transitions for a number

of previously unclassified lines of the singly ionized

rare earths and has derived new gf-values for them

from the arc emission intensities given by Meggers

et al. (1961). Further, the identifications adopted for many hnes differ from those as assigned by Warner

(1964b) for this star and, in a few cases, differ also from the solar identifications for the corresponding

lines as given in the Second Revision of the Rowland

Table (Moore et al., 1966). The interpretation of

Sm II in ^ Cap has a bearing on a possible systematic

error in the measurement of equivalent widths and

also leads to a major revision of some of the gfvalues in the work by Corliss and Bozman (1962).

Some of the above considerations require ex- planation or justification and ultimately affect the

derivation of chemical abundances and physical

parameters for ^ Capricorni. In the next section the

most important individual comments are given for the various spectra, arranged alphabetically by

element. To avoid unnecessary repetition, certain

other results not derived until later in the study are

freely quoted in the presentation of this basic

background analysis.

5.2. The Spectra

5.2.1. Aluminum

The Al I 45 — 5/) doublet at 6697 A offers the only

lines suitable for an abundance determination.

Although the 4^ — 6p doublet at 5558 A falls within

the range of the observational material, it must be

excluded from the analysis; one of its members is a severe blend with three Fe I transitions, and the

other is masked by a Ce II line.

5.2.2. Barium (Ba 1)

Since the primary measurements in I, Cap re- vealed no lines of Bal, the tracings were subsequently examined at the predicted positions of

about 20 strong Ba I lines. Most of the lines in the

list were either not present or were masked by lines

ndividual Spectra

otherwise identified. For example, the strong line of Ba I at 5535.5 A is masked by a hopeless blend of

Nd II, Ce II, and Fe I. Also, the moderately strong

hue at 5826 A attributed to Ba I by Warner almost

certainly belongs to Nd ll. Central depths have been measured for several

remaining features, most of which appear not as

distinct lines but only as parts of broader continuum

depressions. At two of the measured wavelengths

(5971.70 and 6595.33 A), unidentified weak hnes

appear also in the solar spectrum. It may be unsafe

to attribute any of these features in ^ Cap to Bal,

but the measured equivalent widths can be regarded

as useful upper bounds. In any case, the presence

of Ba I in 4 Cap has not been unambiguously

established.

5.2.3. Barium (Ba II) Only four Ba II lines occurred in the primary list. Since they are all strong lines falling on the damping

portion of the curve of growth, an effort was made to locate fainter lines that might help to define the

weak portion of the curve of growth more positively.

An examination of the microphotometer tracings at the positions of all Ba ll hnes hsted in the Revised

Multiplet Table yielded only two additional lines. One of them, at 4524.93 A, occurs as one of three

dips in a broad profile caused by blending with

adjacent lines of Ti ll (4524.73 A) and Fe I (4525.15 A).

By using the correlation between central depth and

equivalent width discussed in section 2.3.2, equivalent widths were derived for all three lines. The

reliability of the Ba ll measurement was then tested

by demonstrating that the Fe I and Ti ll lines,

measured in the same way, fit acceptably onto their already well-populated curves of growth.

The second line, a weak feature at 6379.94 A,

probably corresponds to a similar line observed in the solar spectrum. The measurement of this line

in ^ Cap yielded an equivalent width of 19 mA. No

identification is attached to the line in the Revised

Rowland Table, but Warner has provisionally

identified it in ^ Cap as belonging to Ball. On the

basis of a new compilation of oscillator strengths

for Ba II (Miles and Wiese, 1969) the fine would be

roughly 30 times too strong to be attributed to Ba ll. The line may be a blend having Mn I as a contributor.

48
5.2.4. Cadmium

If present in C, Cap, the strong red line of cadmium

at 6438 A would fall in a portion of the tracings very

i favorable for its detection, but the continuum at that

position is undisturbed. A Une with equivalent width

Ij 101 mA was measured at 4678.16 A. but it probably

\ corresponds to a moderately strong unidentified

I feature at the same wavelength in the solar spectrum

rather than to Cdl.

5.2.5. Cerium

Twelve Ce II hnes for which /-values were pre- viously unavailable have been measured in ^ Cap.

Recent progress in the analysis of Ce II by Z. Goldschmidt (1968) has made it possible to calculate new gf-values for these lines by using her new level values in conjunction with the hne intensities

given in NBS Monograph 32. A new g/value has

also been calculated for the hne at 5359.50 A, in accordance with its revised classification by Goldschmidt. By using her level values, tentative classifications have been found for three additional

hnes not included in her hst. The results are given

in table 5.1. The values cited for the quantity log

(g/X) do not incorporate the corrections suggested

in section 3.2.3 of the present study.

The Ce II curve of growth constructed by use of

the NBS gf-values (fig. 4.4) shows httle scatter and

provides evidence that the Ce II lines measured in

i C, Cap are relatively unblended. Only the lines at 4604 and 5610 A depart significantly from the mean

i curve. The large half-width measured for the latter

^ Table 5.1. NBS gi-values for recently classified

lines of Ce II

Wavelength Intensity Energy levels Low EP log (NBS) (sA)

(A) (cm-') (eV) 4413.19 8 9198-31851 1.14 3.01 4484.83 12 90.54-31345 1.12 3.15 4608.76 3 11388-33080* 1.41 2.81 4659.40 4 9779-31235 1.21 2.73 4686.81 6 8804-30135 1.09 2.78

4702.01 6 65.50-27812 0.81 2.50

47.53.65 2 10314-31345* 1.28 2.47

.5.347.81 3.5 .5969-24663* 0.74 2.10

.5359..50 2.5 14387-33040 1.78 2.99

.5468.37 15 11310-29.592 1.40 3..38

.5.556.97 6 14517-.32.508 1.80 3.36

59.59.69 3.5 13118-29893 1.63 2.93 6143.36 4 13676-29949 1.70 3.05

*Tentative classification suggested by the writer.

hne suggests that it is a blend, probably with C2.

According to the Pr II curve of growth, the Pr II line of the same wavelength would not significantly

contribute to the observed hne. The hne at 4604.18 A

appears to belong predominantly to Sm II.

5.2.6. Dysprosium

The three Dy II lines measured on the tracings of

^ Cap have provided the first abundance determination for dysprosium in a barium star. Surprisingly, a large overabundance is indicated. Dysprosium is a predominantly r-processed rare earth and had been

expected to show (like europium) a relatively normal

abundance in these stars. Even though the dysprosium abundance has been derived from only

three hnes, the determination is regarded as fairly

reHable.

Unfortunately, two of the measured Dy ll lines occur in the unfavorable spectral region below

4300 A, where hne crowding is severe. To establish

the general correctness of the adopted continuum

in the vicinity of the Dy ll lines, several nearby

lines belonging to other spectra were also measured

and shown to fit reasonably on their already well- populated curves of growth.

Figure 5.1 shows a comparison of the microphotometer tracing of ^ Cap (solid line) with that of r\ Pegasi (dashed hne) in the spectral region near

o 4070 A. As already mentioned, the spectrum of 17 Peg (G2 II-III) is quite similar to that of ^ Cap

except for the enhancement of lines arising from

elements such as cerium and neodymium, for which

definite overabundances in the barium star have

been derived. It is seen that the Fe I hnes are of comparable intensity in the two objects, but those of

Wl, Ndll, Cell, Zrl, Zrll, and Dy 11 are all en- hanced in ^ Cap. The second Dy ll hne in this region,

at 4103.34 A, is similarly enhanced with respect to the corresponding line in 17 Peg. The fact that Dy ll behaves hke Ce II and Nd II in this respect is in- terpreted as qualitative evidence that the over- abundance derived for dysprosium in ^ Cap is real. The third Dy ll hne, at 5169.71 A, falls in the wing

of an adjacent strong blend of Fe I and Fe II. The

measured equivalent width is therefore not very

accurate but is considered to be a good upper limit. The location of this hne on the differential curve of

growth with respect to the sun (fig. 5.2) is not consistent with the two other Dy II lines and adds

considerable uncertainty to the abundance deter- mination. This line alone suggests an almost normal

49
50
8 .00- 7 .00 6-00 5 .00 4.00 3 .00 2 .00

-Log X'

Figure 5.2. Differential curve ofgrowth for dysprosium relative to the sun (circles).

The absolute curve of growth {triangles) constructed by use of gf-values has been superimposed on this figure.

51
dysprosium abundance in ^ Cap. However, a more

detailed examination has shown that the Dy ii identification given in the Revised Rowland Table for

this line is almost certainly incorrect. By use of

^/-values, it was found that A 5169 is an order of magnitude too strong to fit the mean solar curve of

growth defined by nine other Dy ii lines. C. E. Moore

has pointed out to the writer that she earlier re- garded this line as a blend with Fe II. In figure 5.2 the absolute curve of growth for Dy ll in ^ Cap has

been superimposed on the differential curve. It is seen that, when gf-values are used, the line at 5169 A

does not depart significantly from the theoretical curve fitted to the stronger lines.

5.2.7. Europium

Only three europium lines, all belonging to Eu ll, have been measured in the spectrum of ^ Cap. In

deriving the europium abundance from the differ- ential curve of growth with respect to the sun,

greatest weight has been assigned the unblended

line at 6645 A. The equivalent width of the line at 4129 A in ^ Cap is somewhat uncertain because of

the difficulty in making accurate measurements in that part of the spectrum. SHght blending with a weak Ce II line is also suspected.

The solar line strength for the remaining Eu ll line, at 6437 A, is definitely too large. According to the

Revised Rowland Table, the solar line has an unidentified contributor on its long wavelength side. This is confirmed also by the ratio of the g/"- values for XX 6645 and 6437. Both lines fall on the linear part

of the curve of growth and have essentially the same

excitation potential.

5.2.8. Iron (Fel)

Because of the large number of iron lines measured in ^ Cap, it is unnecessary to examine all the identifications in detail. A few undetected blends

or misidentifications will not significantly affect the curve of growth or the resultant relative abundance

for iron. However, several Unes originally identified

with iron have been reassigned to other spectra on

the basis of their wide divergences from the iron curve of growth. In this category are the lines at 5804 A (Nd II), 5680 A (Ce ll), and 5805 A (La ii).

5.2.9. Lanthanum

The La ll Hne at 6526 A offers a good example of

a case where an equivalent width derived from

central depth is more reliable than that measured

by planimetry. The half-width (469 mA) of this line

is far in excess of that expected from its central

depth (0.50). The reason for this is that the line is flanked on each side of its profile by somewhat

weaker lines of Si I. The Si I contributions broaden

the line, but are sufficiently separated in wavelength

that they do not seriously affect its central depth.

The equivalent width derived from its central

o depth is 184 mA, whereas that found by direct

planimetry is 260 mA.

5.2.10. Lithium

Weak absorption at the position of the Li I reso- nance doublet was measured in ^ Cap to have an

equivalent width of 29 mA, which is about 25 percent

the value obtained by Warner. At lower dispersions,

blending with an unidentified feature at A.6707.45 (Fe?) often interferes with the accurate measure- ment of the lithium absorption (Bonsack, 1959;

Rodgers and Bell, 1968), but on the tracings of ^ Cap the broad lithium doublet is well separated

from that feature. In the light of the discussion of samarium below, Warner's identification of A6707.45

as belonging to Sm II (Rodgers and Bell, 1968) is subject to serious doubt.

In table A the Utrecht measurement is quoted

for the equivalent width of the lithium doublet in the sun, but in the derivation of the differential abundance of lithium in ^ Cap preference has been

given to the value log (^o/A) = — 6.15, as found by

Greenstein and Richardson (1951).

Warner (1965) has derived a useful relation giving

the abundance of lithium relative to the sun when

the line is unsaturated and H^ is the dominant

source of opacity. He shows that

1 A^*(Li) , r*(Li)

ro(Li) -4.93(7-1) (5.1)

where 7 = 0*^10?^.. By assuming that

0^ ' ^lon (5.2)

and using the values obtained below, it follows that

(5.3)

which, as expected for the reasons cited by Warner,

is somewhat smaller than the value +0.33 de- rived below on the assumption of an isothermal

atmosphere.

52
5.2.11. Magnesium

I The weaker Mg I Hnes at 6318.72 and 6319.22 A

have fairly good profiles on the tracings. Since the

other unblended Mg I lines are so strong, these two

fainter hnes are quite valuable in fixing the shoulder

, of the Mg I curve of growth.

5.2.12. Molybdenum

Ahhough five lines have been attributed to Mo I in table B, these identifications must be considered

I o

j as tentative. Only the line at 6030.66 A shows an

i undisturbed profile. The measured equivalent

! widths for the hnes at 4411 and 5506 A, which ap-

' pear as side distortions on the profiles of adjacent

j strong lines, are not entirely trustworthy.

5.2.13. Neodymium

j The recent analysis of Nd II by Wyart (1968) has

I' made it possible to calculate ^/-values for 13

: previously unclassified hnes of Nd II that have been

; observed in ^ Cap. Also, the gf-\a\ue and excitation

potential of the fine at 5745 A have been changed

I from the NBS values to conform with Wyart's

! revised classification for this fine. Tentative classifi-

! cations have been found for two Hnes not included in the work by Wyart. The new data are summarized

in table 5.2. The values cited for the quantity

log (gfk) do not reflect the corrections suggested

j in section 3.2.3 of the present study.

Table 5.2. NBS ^-values for recently classified

lines of Nd II

Wavelength Intensity

(NBS)

Energy Levels Low EP log

j (.4) (cm-i) (eV) 4563.22 20 1470-23378* 0.18 2.08

i 4S17.18 3.0 5986-26739 .74 1.76

! 4818.96 2.0 3802-24547 .47 1.31

! 5385.88 12 5986-24547 .74 2.28 5744.76 5 10883-28286 1..35 2.47

{ 5753.51 3.0 1650-19026 0.20 1.12

! 5769.86 4 10887-28214 1.35 2.38 6009.30 1.6 .3067-19703 0.38 1.01 6382.06 2.5 11581-27246 1.44 2.23

1 6385.20 7 9358-25014* 1.16 2.40

I 6428.64 2.0 1650-17201 0.20 0.91 6549.52 1.6 513-15777 .06 .67

j 6550.19 1.6 2585-17848 .32 .93

j 6591.43 1.2 1650-16817 .20 .69

*Tentative classification suggested by the v^riter.

5.2.14. Nickel

A Hne measured at 5347.79 A was initially at- tributed to Ni I, but the nickel curve of growth for ^ Cap does not permit this identification. The Hne is too strong by about 400 percent to fit on the curve of

growth. A Hne at 5347.81 A is listed as Ce I in NBS

Monograph 32, but an examination of the unpublished cerium line lists of Martin and of Albertson

reveals a peculiarity in the behavior of this line that suggests it may be a blend of Ce I and Ce II. Its strength in the spectrum of ^ Cap supports that conclusion. The measured equivalent width of

42 mA, as weU as the Hne intensity given in NBS

Monograph 32, must represent the Ce II component

of this line.

5.2.15. Oxygen

Weak Hnes observed at 6300.32 and 6363.80 A have

been identified as the forbidden 2p^ ^P-^., i — 2p4 ^D.^ transitions of [O l]. The first of these is badly blended

on the longer wavelength side of its profile, but the

line at 6363 A is well isolated on the tracings. The

solar equivalent widths for these lines are taken

from the work of Goldberg, MiiUer, and Aller (1960).

Unfortunately, the green forbidden Hne at 5577 A is masked by strong Co absorption in ^ Capricorni.

5.2.16. Praseodymium

Unfortunately, praseodymium is a very difficult element in barium stars. Many of the available Pr ll lines are badly blended, often with lines belonging to other enhanced spectra, including CH. Even at high

dispersion such blending inflates the measured

equivalent widths of most of the Pr ll Hnes available

in the blue region. Each of the three moderately

strong lines that would help to estabHsh the shoulder

of the Pr II curve of growth is a blend with Ce II. These lines, at 4408, 4413, and 4510 A, have here

been given less weight in the determination of the

praseodymium abundance. The solar line strengths

obtained for the Hnes at 4570.61 and 4612.07 A have

also been given less weight, because it is doubtful

whether these lines in the solar spectrum actually

belong to Pr ll.

5.2.17. Ruthenium

The Ru I lines most likely to be present with any

intensity in the range 4000 to 4800 A all coincide

with strong lines otherwise identified. The strongest

expected line falls exactly on the 4554 line of Ba II. If ruthenium were sufficiently abundant, the lines at
4584 A and 4709 A would seem to have the best

chance of detection on the tracings. These wavelengths place them in relatively isolated positions on the tracing, but still in the wings of adjacent lines. Figure 5.3 shows that there are slight dips in the

continuum at these wavelengths, but these may not be real. Although the identifications are relatively

insecure, the derived equivalent widths would at least represent maximum values for these lines. When plotted on a A.-curve of growth, the points

for these lines appear reasonably situated, but this may be fortuitous. The abundance obtained for ruthenium is not markedly different from that ob- tained by Warner. Of the three lines used by Warner

in deriving a ruthenium abundance, however, we

feel that one is a strong Fe II line, one is an un- blended CH line, and the third is a Cr ll line blended

with C2. The final derived ruthenium abundances,

therefore, cannot be directly compared.

5.2.18. Samarium

It is obviously impractical and undesirable to set forth at length the individual complexities that each

of the more than 40 spectra observed in ^ Cap has

presented. It is perhaps justifiable, however, to explore in some detail the problems encountered in the treatment of Sm II, mainly because of its bearing on the need suggested earlier for a recalibration of

the extensive collection of /-values by Corliss and

Bozman(1962).

The original measurements included Sm II lines

Q only shortward of 5000 A, many of which are

seriously blended. It was expected that the deter- mination of the samarium abundance could be

improved by finding some other suitable lines in the red. Although Warner (1964b) includes six red

lines in his samarium analysis, it now appears

doubtful whether any of those lines contains a

significant Sm II contribution. This group of lines

is summarized in table 5.3. A survey of the tracings yielded eleven weak lines

in the range 5300 to 6700 A that may belong to Sm II. The measured central depths and derived equivalent

widths must be considered as upper limits, because

most of the lines are weak features without distinct

profiles. When plotted on an absolute curve of growth with gf-vedues from NBS Monograph 53,

these lines fall very much below the mean curve

defined by the blue lines, as shown in figure 3.3. The samarium abundances implied by the lines in the two spectral regions differ by a factor of more

than two. Efforts to improve the data have thus made

matters even worse, but fortunately this dilemma

can be resolved and leads to consequences of some

importance, as described below.

Table 5.3. Suggested revision of Warner's (1964b)

Sm II identifications > 5000 A

Wavelength -iog(r/\) Probable Note

(Warner) identification

5719.12 4.88 Prn + Ndn

5779.25 4.84 Fe I 1 5867.79 4.98 Ca I 2 6389.87 5.02 Ndn 3 6628.88 5.34 Ce n 4 6754.68 5.25 Smu? 5

Notes

1. No line is present at this wavelength on the higher dispersion

tracings used here. The measurement must refer to the Fe I line at 5778.78 A.

2. The samarium line of this vvfavelength belongs to Sm I.

3. On our plates a line was measured at 6390.00 A, which agrees

with a laboratory wavelength of Nd n. The samarium line at 6389.87 A would have been partially resolved, if present.

4. Although a Ce I line is listed at this position in several laboratory sources, a check with the unpublished cerium observations of Martin leaves little doubt that there is a Ce n line of nearly the same wavelength, thus explaining its appear- ance in ^ Cap.

5. This line falls beyond the range of the present measurements.

The possibility emerges, then, that there does

indeed exist a systematic error in the present material that has resulted in underestimated equivalent

widths for the red, as previosuly indicated by the

comparison with Warner's measurements in figure

2.5. However, this argument would still not be consistent with the differential curves of growth, which

show no conclusive wavelength dependence. In any

case, the extent of the shift observed in Sm ll con- siderably exceeds that suggested by the comparison

with Warner or that allowable by an alteration of the

adopted continuum. A second possibility is that the

blue section of the curve of growth is substantially

raised by the effects of blending. Some of these

lines are severely blended, but it is regarded as unlikely that all of them are thus affected. Further attempts to resolve this discrepancy in Sm II led to an examination of the /-values themselves and to the conclusion that they contain a

calibration error. The nature of this error has already

been discussed in section 3.2.3. In particular, ap- plication of the correction suggested by that discussion brings the results for Sm ll in the two wavelength regions into satisfactory agreement.

54
Ru I Ru I

4584.44 & 4709.48 A

1=0.0 _____

Figure 5.3. Microphotometer tracing of the spectrum of £, Capricorni in the vicinity of two Ru I lines.

55
5.2.19. Scandium

The first spectrum of scandium is represented in

^ Cap by a very unsatisfactory group of weak lines whose equivalent widths could be only poorly

measured. The Sc I line at 5700 A is strongly blended

with Cu I. The observed line is assigned to both

spectra, but Cu I appears to be the dominant component. Certain intensity anomalies indicate the

presence of blending in some of the remaining Unes. For example, both in the sun and in ^ Cap (but not

in e Vir) the pair of hues 6210/6239 A show an

intensity relation opposite to that observed in laboratory sources, even though the lines have the same excitation potential. The same situation is observed for the pair 5355/5356 A, the second

member of which is not present on the tracings

of C Cap.

5.2.20. Silicon

A weak hne appearing at 5675.73 A in the spectra

of both t, Cap and the sun is considered hkely to have the same chemical origin in the two objects.

Charlotte Moore tentatively identifies it in the

Revised Rowland Table as belonging to Si I. Since

this hne departs significantly from the mean sihcon curve of growth for ^ Cap, the correctness of the

identification becomes more doubtful, but the Hne

has been retained in our list.

5.2.21. Strontium

Although sparsely populated curves of growth

cannot be expected to yield trustworthy stellar abundances, a consistent result from a double

differential analysis of the type used here gives

shghtly increased confidence in abundances derived

from just a few lines. The strontium abundance in ^ Capricorni is based

solely on the resonance line of Sr I at 4607.33 A. The

solar Une strengths for the three remaining lines measured in the barium star must be given low

weight because of the inherent difficulty in measuring such faint Unes in the solar spectrum. The Sr I Une Usts for e Vir and ^ Cap have only three lines

in common, the two weaker of which appear to be

blends in e Vir. Apart from these considerations, the three weak

Unes given in the Sr I list for C, Cap are themselves

so seriously blended as to be unsatisfactory for use

in the determination of the strontium abundance.

The intensities of other nearby lines of CN indicate

that a significant fraction of the measured Sr I X6508

absorption is due to a coincident CN line. The Une at 6550 A belongs predominantly to Sm II, and that at 6504 A is a broad blend of Sr I with V I and Pr II. Other lines from Sr I and Sr II were considered too strong to be of any use or too hopelessly blended to yield even approximately reUable equivalent widths.

5.2.22. Sulfur

The relative intensities observed in ^ Cap for the

S I pair of Unes 6046/6052 A are in the same order as those given in the Revised Multiplet Table, but are reversed in comparison with those observed in the sun or in e Vir.

5.2.23. Technetium

From the new Tc I analysis by Bozman, Corliss,

and Tech (1968), a group of about 25 Unes judged

most Ukely to be present in the spectrum of ^ Cap

was selected. A careful examination of the complete

Une Ust for (, Cap (3883-8700 A) did not yield any

positive evidence for the presence of Tc I in this spectrum.

5.2.24. Titanium (Till)

Unfortunately, the stronger lines of Ti II in the

Ust are aU affected by blending, mainly with lines of

Ce II. We have given less weight to these lines in

fitting the curve of growth.

5.2.25. Vanadium

Among the lines of V I measured are some rather

bad blends with Gdll, Ndll, and CH. Less weight was given to these recognized blends in fitting the curve of growth and deriving the vanadium

abundance.

56
6. Atmospheric Parameters for ^ Capricorni

6.1. The Excitation Temperatures

Measurements in the line spectrum of ^ Cap

permit a direct spectroscopic determination of the mean excitation temperature. In the approximation

used here, a Boltzmann correction accounting for the differing populations of the atomic energy levels appears as an additive term in the expression for the abscissa of the curve of growth and effectively

reduces all curves to that for resonance lines. In

absolute curves of growlh the quantity plotted along

the abscissa is

^ logX'^iog {gfk)-e,,,x (6.1)

and in differential curves.

logZ'=logZ-AeexcX- (6.2)

The stellar hne strength, log X, is obtained by

reading the equivalent width observed in the standard comparison star into its empirical or theoretical curve of grow1:h. The quantity A^exc is given by

^^exQ — ^exc ((, Cap)— ^exc (standard) (6.3)

and X is the excitation potential of the lower level

of the transition.

If the range of excitation of the hues plotted is sufficiently restricted, as by using Unes belonging

to the same multiplet, the Boltzmann correction

remains effectively constant. The quantities 0exc or A^exc can therefore be determined in the following

way L\ller, 1963). Separate curves of growth are prepared for hnes in each of several small excitation ranges. The horizontal stufts required to bring the

j separate curves into best coincidence or onto an

average fit with some theoretical curve will, accordI ing to the above expressions for log X' , he hnearly

j related to the mean excitation potential of the Hnes

I used in the separate curves. The gradient of this linear function is taken as defining the mean

excitation temperature.

The procedure just described has several important drawbacks. To obtain an accurate mean temperature, it is necessary to have measurements of

high quahty for a large number of unblended lines

! covering a sizable range of excitation. Lsing such

II observational material for Arcturus, for example,

Griffin and Griffin (1967) constructed numerous

partial curves of growth whose relative shifts •Yielded remarkably well-defined excitation temperatures for Ti I and Fe I. More commonly, it is neces- sary to take rather large (~ 1 e\ ) ranges of excita- tion in order to populate the individual curves of growth satisfactorily. This is true even for neutral

iron, which has a well-developed spectrum in many

stars of interest. In a star with dexc~ 1.00, this leads

to a horizontal spread due to temperature alone

of 1 dex in the individual absolute curves of growth.

The derived temperature can also depend markedly both on the way in which the available lines are separated into excitation ranges and also on

the way in which the horizontal shifts are made to bring the curves into "best" visual coincidence.

Lsing the same observational material for Fe I in e A ir. Griffin and Griffin (1967) and Ca}Tel and Cayrel

(1963) obtained Aeexc = 0.13 and A0exc = O.18,

respectively, for the differential excitation temperature of e \ ir relative to the sun. In an attempt to overcome these difficulties, the

following method has been adopted for obtaining

spectroscopic temperatures. A preliminary estimate

of ^exc OT A^exc is choscn and the quantity logX' is computed for each of the observed lines of a given

element. A least-squares cubic or quartic polynomial

is then calculated to give the best representation of log X' as a function of log (W''jk). The standard

deviation cr of the points from this mean curve in a direction parallel to the logZ'-axis is affected by

the choice of temperature. By iterating the calculation for several values of ^exc around the initial estimate, a series of cr-values is obtained that describes the variation in the scatter of the curve of growth as a function of assumed temperature. A

graph of this function is found to be a smooth one

with a unique minimum. The mean temperature is taken to be that value for which cr is least. Virtues

of this method are as follows: (a) each hne is treated separately with its correct excitation

potential rather than in a group with other hnes

covering a finite range of excitation; (b) the method

gives dispassionately reproducible results; (c) a system of weights can be apphed to the hnes with

httle additional effort. For example. Unsold (1955)

recommends that higher excitation hnes should be more heavily weighted, because any error in the

I
choice of temperature will have more effect on the

positions of these lines in the curve of growth than on lines of lower excitation. In the application of the

minimum-sigma method this was approximately

achieved because, in general, there are more medium and high excitation lines than low. Trial

calculations with a system of weights equal to the

excitation potentials did not produce significantly

different results. A major disadvantage of this method is that great care must be exercised in assuring that no widely

discordant lines are used in the analysis. In general,

lines on the flat or damping portions of the curve of growth should also be excluded. Such lines will dominate the value of the standard deviation and

mask the smaller excess caused by using a slightly

incorrect temperature. In addition, it must be

established that the mean curve from which the

deviations are calculated really does represent the

distribution of points adequately.

As a test of this procedure, the mean excitation

temperature for iron in e Vir has been determined

with a rather different group of lines from that used by the Cayrels in their determination of the

temperature. The lines used are those measured

in ^ Cap that also appear in the Cayrels' line list for e Vir, about 180 in all. The use of solar line strengths obtained from the Pierce-AUer curve of

growth gave a differential temperature of 0.19, as shown in figure 6.1. By use of the /-values given by

Corliss and Tech (1968), an absolute temperature

of 1.21 was also derived (fig. 6.1). The differential temperature relative to the sun is in good agreement

with the value 0.18 derived by the Cayrels and 0.17

by Nishimura (1967) for e Vir. For later use, an absolute temperature determination based on about 300 Fe I lines observed in ^ Cap

was similarly made for the sun. The solar equivalent

widths used are those taken from the Revised Rowland Table and listed in Table A. The analysis,

shown in figure 6.2, yields the value 0exc(O) ^ 1-02,

which is in agreement with a value predictable from

the above results for e Vir, namely,

0exc(O) = 0exc(e)-A^exc(e-O) = l. 21-0.19=1. 02.

(6.4)

Values for 0exc(O) currently quoted in the astro- physical literature range from about 0.98 (Cowley

and Cowley, 1964) to 1.06 (Warner, 1964a).

The absolute temperature of C, Cap has been de- rived from about 300 Fe I Unes for which /-values

were available. The minimum-sigma criterion yields

^exc(D~l-13, as shown in figure 6.2. Since the same group of lines was used in deriving the solar temperature, the vertical separation in this figure

between the plots for the sun and for ^ Cap reflects the difference in the contributions of the equivalent

widths and of the length of the transition portions of the respective curves of growth to the total scatter. Differential temperatures for ^ Cap with respect

to both the sun and to e Vir have been similarly

determined from lines of Fel, Nil, Til, and Cri.

These are the only spectra with a sufficient number

of measured lines and wide enough range of excita- tion potentials to be useful for this purpose. The

value obtained for A^exc(4~e) may be poor in the case of Cr I because the requirements just stated are only marginally satisfied. The V I curve of growth

is sufficiently populated, but the lines differ very

little in excitation. A summary of the results is presented in the following table. Table 6.1. Differential excitation temperatures of

I, Cap relative to the sun and to e Vir

Spectrum No. of

lines Aeexc(«-e) No. oflines

Fe I 0.10 328 -0.09 189 Nil .09 45 -.09 24 Til .09 45 -.08 34

Ci-I -.01 35 -.14 21

As has been discovered in other stellar analyses

(Cayrel and Cayrel, 1963), the lines of CrI require a

significantly different excitation temperature from

that of other neutral spectra in the iron group. A

satisfactory explanation has not yet been proposed

for the effect. It seems improbable that chromium

should be excited in different layers of the atmos- phere from other elements of similar ionization

potential. The ad hoc appeal to such selective strat- ification of elements remains unconvincing in the

absence of a reasonable mechanism to produce it. A nonequilibrium population of the low odd levels near 3.00 eV, or differential damping effects (Sandage and Hill, 1951) between lines from lower

odd and lower even levels would also influence the

determination of the excitation temperatures. It may be relevant in this connection that the term

structure in CrI is such that there is an unusually

large number of level differences that very nearly

repeat and lead to doubly or triply classified lines. This problem does not, in general, affect the lowlevel lines. 58
0.24

0 .23

0.22 -

0 .2

0.20 -

0.19 -

0 .1 8

Aa(£-0)=O.I9

I

a(€) = l.2l

0.00 0.10

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0.20 0.30

I.I 0 1.20

0.26

0.25

0. 24

0.23

0.22

0.21

0.20

0.40 Aa

1.30 1.40 Q

Figure 6.1. Determination of absolute and differential excitation temperatures for e I' irginis.

(Abscissa, assumed temperature: ordinate, standard deviation of horizontal scatter in the curve of growth for neutral iron.)

398-978 0 - 71 -6 59
60
0.22

0.21 -

0.20

0.17

0.19 -

0.18 -

Figure 6.3. Determination of mean excitation temperature from ion lines observed in ^ Capricorni.

(Abscissa, assumed temperature; ordinate, standard deviation of the horizontal scatter in the composite curve of growth.) i The mean excitation temperature obtained from

spectra of singly ionized atoms (^pxc) '^^^ found to be slightly higher than that from neutral spectra

). The determination was made in the following

way. About 200 lines representing 14 singly ionized

elements were combined into a single curve of

growth using an estimated ^J^p = ^^'i^^ . Differential

shifts related to their respective abundances were

then applied to the individual elements in such a way

that the sum of the deviations of the points for each

element from the mean multi-elemental curve was

zero. The procedure was iterated through a succession of mean calculated curves and sets of shifts to the point where the shifts remained constant. Having

thus applied individual shifts to bring all ion spectra

onto a single curve of growth, only the value of

0^xc then varied to provide a minimum-sigma

test. The result using g/- values is shown in figure 6.3. The above analysis fixes the temperature of ^ Cap

almost exactly midway between those of the sun and

e Vir. The finally adopted values are as follows, each

with an estimated error of ±0.03. The differential excitation temperatures are assumed to be the same

for both neutral (n) and ion (i) spectra.

Table 6.2. Adopted excitation temperatures

1.02 = 4940°± 140

o"^,iC) = 1.13 = 4460° + 120 OLM) = 1.07 = 4710°± 130

Sexc(e) = 1.21 = 4165°± 100

Aeexc(?-O)= + 0.10

A0exc(^-e)=-O.O9

61
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The effect thai the choice of temperature has on

the scatter in the curves of growth for iron is shown

in figures 6.4 to 6.9, which compare absolute and

differential curves using the excitation temperatures

derived above with those using temperatures dif- fering by ±0.15 from the adopted values. As the

temperature departs from the adopted values, the

scatter becomes worse, and a clear separation of the

points according to excitation potential emerges.

It is important to note that the scatter in the damping

portion of the differential curve relative to the sun is less for A0 = + 0.25 than for the adopted differential temperature. This is related to the Carter effect discussed in section 6.3.

6.2. The Ionization Equilibrium

To obtain the total abundance of an element from

the observed differential shifts in the curves of

growth, the differential ionization equilibrium must

be known. Writing the Saba equation for both the

barium star and the comparison star, and subtracting, gives in the bracket notation of section 4.1

{Nr^.lNA [P.] - A^ionXr-l [^ion] (6.5)

where Xr is the ionization potential, ^ion is the ioniza- tion temperature, Pe is the electron pressure, and

\_]Slr+\INr^ is the horizontal shift between curves of

growth drawn for some element observed in two

stages of ionization.

Ideally, A^jon and \_Pe\ = A log Pe would be deter- mined simultaneously by plotting against ionization

potential the relative shifts found for several spectra

observed in two stages of ionization. The range of

ionization potentials is so small for such spectra

observed in ^ Cap, however, that a meaningful

simultaneous determination is not possible. The

usual assumption was therefore made that A0ion =

A^exci and the value of \_Pe\ was derived from the

observed shifts between differential curves of growth

for the neutral and singly ionized stages of the six elements given in table 6.3. Although only the differential values are important

in the determination of relative chemical abundances, the absolute values of P| and can be

estimated by taking 0g„=O.89 and log P®= 1.30 at a representative optical depth of 0.35 (Aller and

Pierce, 1952). This gives log P| = + 0.02 and

ef„„ = 0.99. A value of = 0.98 would be obtained

if 0fgn were approximated by taking 6^^ = 9^\,^ —0.15,

Table 6.3. Determination of differential electron pressures for ^ Cap relative to the Sun and to e Vir

Element wt. X

Sun 6 Vir

[N*IN°] [A'+/A'°]

7/ re 0 7.87 0.37 -1.26 0.68 0.12

Ti 6.82 ,52 -1.30 .44 .26 Cr 6.76 .33 -1.11 .45 .15 Sc 6.54 .40 -1.15 .54 .14 Zr 6.84 .62 -1.40 .50 .21 Y 6.38 .81 -1.55 .75 -.09

[/'e] 5^ =-1.28

Adopted:

[Pe]?-. =+0.13

as has been suggested by the work of Preston (1961)

and others.

6.3. The Carter Effect

The differential curve of growth shown in figure 2.7 for Fe I in ^ Cap relative to the sun shows on the

damping portion of the curve a systematic displacement between the blue and the red lines. This

displacement can be traced to the solar line strengths. In his study of Fe I in the sun. Carter (1949) found

that lines absorbed from odd energy levels ("odd"

lines, for brevity) were systematically stronger on

the damping portion of the solar curve of growth than were lines having the same /-value but absorbed

from lower even levels. He attributed this separation by parity to differential damping in the solar atmosphere or to a preferential population of odd

states during recombination from Fe II. Sandage and

Hill (1951) noted a similar effect for Cr I in the sun. The process is still not well understood.

The Carter effect is shown in figure 6.10, which is a solar curve of growth based on gf-values taken from

NBS Monograph 108. The separation of the odd and

even lines is quite striking for values of log {WjX)

greater than about —4.80. The strong separation

does not continue into the linear portion of the curve.

It is apparent that solar line strengths obtained for odd lines on the damping portion of the curve will be

overestimated relative to those for even lines. This

overestimation will be transmitted to differential curves of growth constructed with solar line strengths

as a reversed Carter effect. That is, the odd fines

will fall to the right of the even lines on the damping

portion of the differential curve. This is clearly seen

68
o

Fe I (sun)

+ 7* +

a + o + + # +

++

p a ffl

o: odd-even transitions

+• even- odd transitions

CD-3 .00 -2 .00 -1 .00 0.00 1 .00 2.00 3 .00

Log(gfX)-9X.

Figure 6.10. Absolute curve of growth for neutral iron in the sun. A distinction is made between odd-even transitions (circlesi and even-odd transitions (crosses). 8= 1.02.

69
o

in

Fe T

+ ---^+ +

m 0

<» +/ + + OOf /

r +

/* +

+ / + +

0: odd-even transitions

even-odd transitions

6 .00 5-00 4 .00 3 .00 2 .00

-Log X'(0)

1 .00

Figure 6.11. Differential curve of groivth for neutral iron in ^ Capricorni.

A distinction is made in this plot between odd-even Icircles) and even-odd {crosses) transitions. Notice tlie reversed Carter eflFect on the damping portion of the curve.

70
o

m•_ I I I I L CO

o

o

0*. odd-even transitions

+: even-odd transitions

o

"^-3.00 -2.00 -1.00 0.00 1.00 2.00 3.00

Log(gfX)-0X.

Figure 6.12. Absolute curve ofgrowth for neutral iron in ^ Capricorni,

Notice the absence of any significant Carter effect. {Circles, odd-even transitions; crosses, even-odd transitions,)

71
o

Fe I

o". odd-even transitions

+• even-odd transitions

^6.00 5-00 4 .00 3-00 2 .00 1 -00

-Log X' (e)

0 .00

Figure 6.13. Differential curve of growth for neutral iron relative to e Virginis.

Circles, odd-even transitions; crosses, even-odd transitions.

72
in figure 6.11, where the differential curve for ^ Cap

is now constructed with a distinction made between

odd and even lines. Comparison of this plot with that

of figure 2.7 shows, moreover, that the odd fines generally have wavelengths greater than 5000 A,

thus explaining the apparent wavelength separation

in figure 2.7. That no significant internal Carter

effect is present in ^ Cap itself is apparent from

figure 6.12 and figure 6.13, in which the even-odd

distinction is made in plots using gf-values and fine strengths from e Vir, respectively.

The curve shown in figure 6.10 differs considerably from those obtained for Fe I by Kuli-Zade (1968),

who also used NBS gf-values. In that investigation

the bifurcation of the fines according to parity was

present not only on the damping portion but was

found to extend over the entire solar curve of

growth. That result can, however, be traced to the use of an inappropriate mean solar excitation temperature. The effect the selection of excitation

temperature has on the parity distribution in the

solar curve of growth is indicated by the following

argument.

Let us examine the mean excitation potentials for

lines of each parity in the damping and Doppler

regions of the solar curve of growth. The mean level of line formation for higher excitation fines will be at greater optical depths than for lower excitation

lines. The effects of pressure and coUisional damping

will also be correspondingly greater. Averaging the

excitation potentials for just the Fe I fines used in our figure 6.10 yields the results shown in table 6.4.

Table 6.4. Mean excitation potentials for Fe I lines used in the construction of solar curve of

growth shown in figure 6.10.

The number of lines used in forming the individual averages is given in parentheses.

Region <X> odd (x) even A<x) odd-even

eV eV eV

Entire curve 4.07 (173) 2.53 (143) 1.54 Damping portion log (r/A)>-4.90 3.91 (76) 1.96 (65) 1.95

linear portion and

shoulder log < - 4.90 4.18 (101) 2.99 (78) 1.19

On the damping part of the curve there is a 2 eV

difference in the mean excitation potentials for even and odd lines, almost twice that for the remainder of

the curve. From the point of view of line excitation,

table 6.4 suggests that the damping portion defined

by the odd lines, rather than by the even lines, cor- responds more closely to the linear portion of the curve when a mean excitation temperature is used

because of the more equivalent average excitation

energies.

The mean excitation temperature would normally

be derived by minimizing the scatter for the fainter

fines on the curve of growth, as this is the more useful region for abundance work. If a temperature so derived were decreased (^exc increased), the odd

fines on the average would be shifted farther to the

left than the even lines (owing to the excitation dif- ferential), the odd-even displacement being greater on the damping portion. The effect is shown in figure

6.14, which has the appearance of the curves re- ported by Kuli-Zade. The odd-even separation can be

reversed, however, simply by adopting a mean

excitation temperature that is too high (fig. 6.15). In general, if a mean excitation temperature 6 pro- duces minimum parity separation, a temperature

6' = 6 + AO wiU yield an average parity displacement

of 1.5 A.0 along the abscissa of the curve of growth.

On the damping portion of the curve, the corre- sponding displacement wiD be about 2 AO.

In one sense, then, the Carter effect can be

interpreted as simply a manifestation of the AdamsRussell effect (Adams and Russell, 1928), which

describes the observation that in some stars ^exc (or A^exc) is a function of excitation potential. The

phenomenon appears as a curvature in the plot (see

sec. 6.1) of relative shifts of partial curves of growth

against excitation potential, or as a grouping of points by excitation potential in a curve of growth

constructed by use of some mean temperature. On

this basis, it would be expected that a star showing

the one effect would also show the other. We note, finally, that the tendency in e Vir for the

low-level fines to indicate a greater microturbulent

velocity than the high-level fines (Cayrel and Cayrel,

1963, figs. 7-9) is intimately related to the reversed

Carter effect transmitted by the solar fine strengths

and to the distribution of excitation energies cited

in table 6.4.

6.4. Gas Velocities in the Atmosphere

of ^ Capricorni

6.4.1. Thermal Velocity

On the assumption that the gas kinetic temperature in the atmosphere of ^ Capricorni is equal to the

73
o

Fe I (sun)

g: odd-even transitions

+• even-odd transitions

-3 .00 -2 .00 -1 .00 0 .00 1 .00 2 .00 3 .00

Log(gfX)-eX.

Figure 6.14. Enhancement of the Carter effect in the solar curve ofgrowth by use of an incorrect mean excitation temperature (i9= 1.22).

Circles, odd-even transitions; crosses, even-odd transitions.

74
o

Fe i: (sun)

+ + e

+ +

+ +«•

8>te 5 a

* +O (9+

+ + o + <s

0". odd-even transitions

+• even-odd transitions

-3 .00 -2 .00 -1 ,00 0-00 1 -00 2 .00

Log(gfX)-0X.

3 .00

Reversed Carter effect in the solar curve of growth caused by use of an inappropriate excitation temperature (0 = 0.82).

Circles, odd-even transitions; crosses, even-odd transitions.

398-978 0 - 71 -5 75
excitation temperature derived in section 6.1, the

purely thermal velocity is given by the relation

For the iron group, this gives

vt~ 1.2 km/s. (6.7)

6.4.2. Microturbulence

From the theoretical curves of growth for simple

steUar models, the curve for pure absorption in the

Milne-Eddington approximation has been found to represent most satisfactorily the empirical curves

of growth for ^ Capricorni. As discussed in section

4.4., the theoretical curve with damping constant

log (2a) = — 2.5 has been used. The ordinate of the

theoretical curve (Hunger, 1956) is log {JVI2bRc)

,

where Rc is the Umiting central depth for strong

lines, and b, the "Doppler width," is given by

b^^\D = voXlc. (6.8)

The rms Doppler speed vo, or velocity parameter,

includes purely thermal gas motions and small-scale

turbulence (microturbulence) according to the

relation

v'o-vf + v'^,,,,. (6.9)

The quantity vo was determined from the observations by shifting the empirical curves of growth both

vertically and horizontally until the best fit to the

theoretical curve was achieved. The value derived

for Vo depends to some extent upon the theoretical curve with which the observations are compared,

but the differences are small (Hunger, 1956).

Since the quantity log (Wlk) is plotted along the

ordinate in the empirical curves of growth, the

velocity parameter vo is obtained from the vertical

shift A log (WlX) according to the relation

Alog(r/\)=log(r/X) -log (WI2bRc) (6.10) or

logt;o = Alog(r/X) + 10.20 (6.11)

where the value Rc=0.95 observed for Mg I A.5183.60 has been taken as a representative limiting central

depth. The variation of Rc with wavelength is not

significant in comparison with the errors inherent in

fitting the empirical curves of growth.

Table 6.5 lists the velocities derived from those

spectra whose curves of growth are sufficiently'

populated to allow reasonably accurate determinations. The average values for vo as derived from

absolute curves of growth and differential curves

with respect to the sun and to e Vir are in good agree- ment. There is a tendency for lines of singly ionized

spectra to give a higher microturbulent velocity

than those of neutral spectra, as in supergiants

(Wright, 1948j, but Sell is a notable exception. A

more careful examination shows that the higher

velocities derived from Ti II and Fe II are probably

related to blending in the stronger observed lines., In any case, the variations in the derived velocities amount to only ±0.10 on the ordinate of the curve

of growth, which is about the error in making the

fit. In view of the marginal significance of the variations, a single value of vo has been adopted for aU

spectra,

Alog(r/\)=-4.63 (6.12)|i

log =5.57 ±0.05 (6.13)

j;o = 3.7 ±0.4 km/s. (6.14)

Table 6.5. Doppler velocities derived from indi- vidual curves of growth

Spectrum

Source of Line Strengths

€ Vir c un -A log (r/x) Vo — A log {Wl\) Vo -A log

Vo

kmis kmjs kmjs

Fel 4.63 3.7 4.67 3.4 4.65 3.5 Ca I 4.70 3.2 4.68 3.3 4.71 3.1 Cri 4.62 3.8 4.68 3.3 4.63 3.7 Mn I 4.63 3.7 4.70 3.2 4.65 3.5 Ni I 4.74 2.9 4.58 4.2 4.66 3.5 Ti I 4.59 4.1 4.66 3.5 4.60 4.0 Na I 4.66 3.5 Ce n 4.61 3.9 4.52 4.8 4.48 5.2 Fe u 4.49 5.1 4.60 4.0 4.52 4.8 Ndn 4.58 4.2 4.56 4.4 Sm n 4.55 4.5 Tin 4.54 4.6 4.65 3.5 4.51 4.9 Sc u 4.65 3.5 4.61 ' 3.9

(Average) 4.61 3.9 4.64 3.6 4.60 4.0

Adopted: A log ( r/\) = - 4.63

1)0 = 3.7 km/s.

76
Using eq (6.9), we finally obtain

l'micro= V[(3.7)2-(1.2)2] (6.15)

i'micro~3.5±0.5 km/s. (6.15)

'{The microturbulent velocity in ^ Cap is therefore

I^bout twice that observed in the sun or in e Vir

:ijCayrel and CayTel, 1963).

6.4.3. Macroturbulence

As is characteristic of giant stars, the Hnes in the

i^pectrum of ^ Cap are quite broad. The measured

' lalf-widths amount typically to 0.20-0.40 A. Doppler

Pproadening is almost whoUy responsible for the

Pialf-widths of weak and moderately strong lines. 'Since half-widths were measured for nearly all hnes

^sed in this investigation, it is possible to obtain a very good determination of the Doppler width, and

nence the macroturbulent speed.

If a MaxwelHan distribution of velocities is as- sumed, the relative intensity in a hne broadened

only by the Doppler effect is

I Vtt AXd

(6.17)

where (AX/AXo) is the Doppler shift in units of the

shift corresponding to the most probable speed vpIThe exponential term reaches its maximum value,

inity, at the hne center and decreases to one-half

his maximum value at a distance A\h from the hne

center, where A\// is defined by

(6.18)

The Doppler half-width. Da, of the line (total width

;it half-intensity) is therefore given by

Dx = 2A\H = 2.Vh72A\D=l-665 A\d. (6.19)

After substitution in the Doppler formula, the total iDoppler velocity is found to be

vd^ —

=o.60l;x-.

A A

(6.20)

The Doppler half-width, Dk, is deduced from the

ixperimental data by extrapolating the observed

lalf-widths to very weak lines. The ratio HjK, where

j¥ is the observed half-width, is plotted against

pentral depth in figure 6.16. The correlation is not

strong. To reduce the number of points to be plotted.

aU lines with a quahty Q <2 have been omitted for wavelengths greater than 5000 A and Rc > 0.12. The

weak hnes of poor quality have been retained in order to demonstrate a possible underestimation of

half-widths for such hnes. In general such weak

lines had incomplete profiles that were approximately sketched in to allow measurement by

planimeter.

With H and X expressed in angstroms, the result

for both regions is H X 10^ = 415 + 350Rc ± 35 (p.e.). (6.21)

The extrapolation to Rc = 0 gives the Doppler half- width and Doppler width

at 4500 A /)x = 0.19 ±0.02 A, AXd = 0.11 ± 0.01 ^

(6.22)

at 6000 A Z)a = 0.25±0.02 A, A\z) = 0.15±0.01 A

The corresponding Doppler velocity from eq (6.20) is

7.4 ±0.6 km/s. (6.23)

In deriving this velocity, the contribution of the apparatus profile to the total line width has

been neglected. The results of measurement of a dozen Hnes on the tracings near 6300 A caused by

O2 absorption in the earth's atmosphere suggests an upper limit of 0.15 A for the instrumental half- width of these hnes. On the assumption that both

the Doppler and the instrumental profiles are Gaussian, the squares of their respective half- widths must be added to give the square of the

half-width of the folded profile. A partial instru- mental correction to the above velocity can be

made with only a small residual error by adopting

^instr'^O-lO A as a mean value for the entire

range of wavelengths. The final Doppler velocity

then becomes

2;d = 6.6 ±0.6 km/s. (6.24)

The total Doppler velocity is related to the

thermal (vt) and the turbulent (^) velocities by

Vp = vf +

If the assumption is made that

. -|- ^ = 'micro ''macro' ^;^;

the macroturbulent velocity is found to be

J^macro=5.5± 1 km/s.

(6.25)

(6.26)

(6.27)

77
o

oo

o

o

to

s 1 ee»

• r: t

e / em*

a • h * 9

e + e e/ e « f S 0

o

in

CL. lUQo

-loci:

CJcn

o

o

o'

o

o

200

0: X < 5000 A

+• X > 5000 A

400 600 I QOO" 1000 1200

Figure 6.16. Relation between half-width and central depth.

Circles. K < 5000 A; crosses, K > 5000 A. 78
7. The Chemical Composition of C, Capricorni

7.1. The Abundances

Having visually fitted the adopted theoretical curve of grov^fth as well as possible to each of the

empirical curves, and thereby found the relative horizontal shifts, the determination of differential chemical abundances in ^ Cap with respect to the sun and to e Vir is straightforward. In none of these

stars is second ionization important. Attention can

therefore be confined to the neutral and singly

ionized stages.

Now, for a given element in ^ Cap and one of the

comparison stars (*) we can write

jyL A^* /V^ yv?

or N*

log ^= log ^- log ^ + log (7.2)

In the bracket notation, this becomes

[N] = [Nr]-[NrlN]. (7.3)

In this expression, is the total number of atoms

per gram of stellar material, and Nr is the number

of them in the rth stage of ionization. The last term

is the logarithmic ratio of the fraction of atoms found

in the rth stage of ionization in the two stars and is calculated directly from the ionization equation by

using the appropriate known values of Tjon and Pe. We seek the quantity [N]

.

By eq (4.6). the first term on the right side of

eq (7.3) is given by the difference in opacities and

the horizontal shift of the empirical curve of growth

onto the theoretical one. That is,

[yV.] = [A]. (7.4)

Combining eqs (7.3) and (7.4), we obtain

[N] = [X]+[k]-[NrlN]. (7.5)

This is the basic relation by which the relative total abundances [A'^] in ^ Capricorni have been

determined.

The reasonable assumption is made that absorption by H" represents the dominant opacity source

in these stars. The formula given by Koelbloed

(1953) can then be used for the calculation of the

logarithmic difference [A]

[A] = 1.75A0ion+ [/^e]. (7.6)

Using the values for A^ion and [Pe] found in section

6.2 we obtain

[A]i_0- 0.18 - 1.28 = - 1.10 (7.7) and

[A]4_,=- 0.16 + 0.13 = -0.03. (7.8)

The absolute parameters necessary to evaluate

[NrIN] by the Saha equation can be obtained by

adding the differential parameters derived earlier

to the solar values adopted in section 6.2 for a representative optical depth of 0.35. These parameters are listed in table 7.1. The values derived for [NrIN] depend primarily on the differential parameters and are not sensitive to the absolute values

used in the Saha equation.

Table 7.1. Parameters used in the determination

of relative ionization equilibria

Sun A(^-0) C Cap e Vir

0.89 + 0.10 0.99 -0.09 1.08

log Pe 1.30 - 1.28 + .02 + .13 -0.11

To solve Saha's equation,

log

^= - 0/ + 2.5 log T - 0.48

iVo + log log P., (7.9)

it is also necessary to know the partition functions

u(T). The same values were used for all three stars and were taken mainly from the tabulation by

de Galan (1968) for an average temperature

r=5200 K. The partition functions for some rare earths are not well known because of the fragmentary state of the spectral analyses. The values

estimated by Corhss and Bozman (1962) for some of

these ions have been adopted here, but for Cel,

Cell, Ndl, Ndll, Smi, and Smll the new energy

levels from unpubhshed analyses in progress by

W. C. Martin, Z. Goldschmidt, J. F. Wyart, and
others have been used to calculate new partition

functions according to the relation

"(n = 2 gse-^^l'^'^, (7.10)

s = 0 Table 7.2. First Ionization Potentials and Partition Functions Used in the Calculation of Ionization Corrections to the Relative Abundances

(r= 5200 K)

Element I. P. u°{T)

(eV)

T ; O 1 l.U

L. 1 1 OA 1 l.zo y.l ^ o o.y 0 13.61 8.9 4.0 Na 5.14 2.1 1.0 c

lU.OO

Ayr.* Mg 7.o4 1.0 2.0

A 1 Al 5.98 5.9 1.0

Si 8.15 9.5 5.7 Ca 6.11 1.2 2.2 Sc 6.54 12.2 23.2

Ti 6.82 30.9 56.5 V 6.74 49.0 44.5 Cr 6.76 10.8 7.3 Mn 7.43 6.5 7.8 Fe 7.87 28.5 44.2

Co 7.86 34.4 30.4 Ni 7.63 31.2 11.1 Cu 7.72 2.4 1.0 Zn 9.39 1.0 2.0 Ge 7.90 7.7 4.5

Sr 5.69 1.3 2.2 Y 6.38 12.1 16.3 Zr 6.84 35.5 46.8 Nb 6.88 54.9 44.8 Mo 7.10 11.6 7.9

Ru 7.36 35.3 24.5 Ba 5.21 2.7 4.3 La 5.58 27.0 30.3 Ce.. 5.65 188.0 190.0 Pr 5.42 80.0 87.0

Nd 5.49 85.0 103.0 Sm 5.63 37.8 61.6 Eu 5.68 9.2 15.7 Gd 6.16 51.0 78.0 Dy 5.93 90.0 100.0

Ta 7.88 18.0 23.7 W 7.98 13.4 14.6 Pb 7.42 1.6 2.1

80

where gs is the statistical weight 2J + 1 of the level whose energy is Eg, k is Boltzmann's constant, and

T is the adopted ionization temperature. The values = used here for first ionization potentials and partition

functions are tabulated in table 7.2. By setting [A^ = 0.00 in eq (7.5), we calculated

for each observed curve of growth the quantity

[xy^iNrim-m (7.11)

which represents the predicted horizontal abundance shifts on the assumption of equal total abundances in the barium and comparison star. The actual logarithmic abundance ratios are then

given by the difference between the observed

and predicted shifts. That is, m= [^] - [X] (7.12)

The results are presented in table 7.3. The

successive columns give the spectrum from which

the abundance was derived, the predicted and ob- served shifts relative to the sun, the corresponding

quantities relative to e Vir, and finally the derived

abundance ratios. The abundances of the elements in the iron

group tend to be systematically lower in the barium

star than in e Virginis, but the effect is quite small. A similarly small, but now positive, difference is found for the differential abundances relative to the sun. This latter result supports an argument

by Warner (1964a), who estimated that a dif- ferential analysis of a cool giant relative to the sun will yield abundances systematically too large

by ~ 0.05 to 0.10 dex because of differences in the

temperature structure of their atmospheres.

The apparent sodium deficiency in ^ Cap relative

to e Vir is probably a reflection of the corresponding

excess of sodium found by the Cayrels in e Vir. In general, the abundances in ^ Cap relative to the sun and to e Vir are in excellent agreement.

The abundances of Ce, La, Nd, Pr, Sm, and Y

relative to e Vir have also been determined from

the curves of growth constructed by use of NBS

^/-values. As discussed in section 4.3, it was

necessary to apply correction factors 8 to convert

the observed shifts of the absolute curves to the

system of fine strengths in e Vir. The abundance

results for these elements, given in table 7.4, tend to be somewhat smaller than those derived

directly from the stellar line strengths. The results

in table 7.4 have been averaged with the dif-
Table 7.3. Logarithmic abundance ratios

Table 7.4. Abundances derivedfrom NBS ^-values

converted to line strengths in e Virginis

Pred.

shift„ Obs.

shift.

0.48

1.10

1.10 0.45

.71

.54

.82 1.17

1.10 0.55

.59 1.10 0.62

1.10 0.61

.62 1.11 0.69

.74 1.12

0.75

.75

.76

.99 .78

.50

.57 1.10 0.62

1.10

0.63

.66

.69 1.10

1.10

1.10

1.10 1.10

1.10

1.10

1.10

1.10 0.77

0.69

0.81 1.45

1.05 0.63

.69

.73

.92 1.17

1.38 0.64

.83 1.23 0.70

1.22 0.64

.75 1.08 0.72

.80 1.17

0.79

.79 1.02 0.98

.96

1.59

1.48 2.29

1.41 2.03

0.92

1.41 1.18 2.50

2.09

2.17

1.91 2.06

1.99

1.26

1.48

1.95 1.14

1.41

Pred.

shiftj

-0.42

.03

.03 -.40

-.60

-.47

-.47

.23

.02 -.48

-.52

.03 -.55

.03 -.54

-.54

.04 -..58 -.59

.08

-..56 -.52

-.52

-.24

-.52

-.45

-.51

.03 -.55

.03

-.55 -.56

-.57

.03

.03

.03 .03

.03

.03

.03

.03

.03

.12 .05

Obs.

shiftj

-0.05

-.65

-.74

-.50

-.50

.20 .59

.38

.16

.48 .04

.57

.59 .14

.76 .64 .04

.58

.58

.71 .04

.49

.49 1.24 0.36

.86

1.40 0.96

.96

.68 1.01 0.80

+ 0.33 + .35 -.05 + .18 -.02

+ .19 + .10 .00 + .28 + .09

+ .24 + .13 + .08 + .12 + .03 + .13 -.03 + .03 + .06 + .05

+ .04 + .04 + .26 -.01 + .18

+ 1.09 + 0.91 + 1.19 + 0.79 + .93

+ .29 + .75 + .49 + 1.40 + 0.99

+ 1.07 + 0.81 + .96 + .89 + .16

+ .38 + .85 + .37 + .72

(-0.08)

(-.25) -.14

-.03

-.03

-.22

-.11

+ .14 + .13 + .07 -.07

-.03

-.05

-.18

-.18

-.05

-.04

-.02

-.06

-.19 + .20

+ .94 + 1.00 + 1.21 + 0.91 + .83

+ 1.37 + 0.93

+ .93 (+.65) + .98 + .77

Predicted Observed

Element shift shift —

8

Ce +0.03 0.93 0.90 La +.03 .85 .82 Nd +.03 .95 .92 Pr +.03 .98 .95 Sm +.03 .78 .75 Y +.03 1.06 1.03

Table 7.5. Logarithmic abundances in ^ Capricorni relative to iron

Element

[Af(El)/Af(Fe)] This study Estimated error

(see text) [N{E\)IN(Fe)] Warner

Li +0.27 0.4 -4-1 Q +.29 .3 n —.11 . o Na +.12 3 Mg -.08 .35 +.07

Al +.07 .35 +.04

Si .00 .2 s +.03 .3 Ca —.01 .2 .00 Sc +.15 .2 -.05

Ti +.04 .2 +.14 V .00 .2 +.04 Cr —.04 .15 + 10 Mn —.08 .15 -.08 Co .00 .15 -.05

Ni —.02 .15 +.03 Cu +.03 .25 Zn +.09 .3 -.10 Ge +.12 .3 -.15

Sr +1.01 .3 +.18

Y +1.06 .25 +.70

Zr +0.86 .35 +.60 Nb +.23 .4 Mo +.69 .2 +.47 Ru +.43 .3 +.45

Ba +1.38 .5 +1.00 La +0.93 .3 +0.36 Ce +.98 .2 +.55 Pr +.88 .3 +.57 Nd +.97 .25 +.26

Sm +.82 .25 +.31 Eu +.10 .3 +.10 Gd +.32 .3 +.05 Dy +.79 .4 W +.31 .5 +.61 Pb +.66 .5 +.31

81
ferential results in deriving final values for the

relative abundances in ^ Cap.

The final description of the chemical composition of ^ Capricorni is presented in table 7.5. The

values given for the abundances have been nor- malized to iron by taking [jV(Fe)] = 0.00. By giving

the abundances relative to iron, the small sys- tematic effects mentioned above are ehminated,

and the averages of the results obtained from the

two comparison stars become more meaningful.

The separate abundances derived for the same

element observed in two stages of ionization have

also been averaged. In all cases there is excellent

agreement between the two determinations.

The assumption has been made, of course, that the atmospheres of e Virginis and the sun have

identical compositions. The detailed analysis by

the Cayrels has shown this assumption to be correct except possibly for sodium. The abundance de- rived for sodium relative to e Vir has, therefore,

been disregarded in the preparation of the final table. The same is true for carbon and praseo- dymium, whose abundances relative to e Vir were

based on only one and two Unes, respectively.

7.2. Use of ^ Capricorni as a Comparison Star

In comparing a barium star with the sun or a normal giant, one encounters the problem, owing

to differences in opacity and abundances, that many

of the rare earth lines strong enough to have been

measured in the comparison star are already so strong in the barium star as to fall on the unfavorable

flat portion of the curve of growth. Moreover, the

weakness of the solar comparison lines of these

elements makes their equivalent widths difficult to measure accurately and undoubtedly contributes

to the large scatter in several of the differential curves of growth. The weaker rare earth Unes found

in I, Capricorni do not appear in the comparison

stars at all.

It might be argued that differences among barium

stars themselves could be more reliably established

by selecting a member of their own class as the

comparison star for a differential analysis. It is not suggested that ^ Capricorni, the brightest known

barium star and logical candidate, is at present

suitable for this purpose. It is highly desirable

that independent measurements of equivalent

widths from additional sets of plates, preferably

o o including the spectral region from 4800 A to 5100 A,

first be obtained and perhaps a detailed depthdependent analysis performed.

As an example, however, several differential curves of growth have been constructed for the

Ba ll star HD 116713 relative to ^ Cap. The equivalent widths for HD 116713 are taken from the work

of Danziger (1965).

The stellar line strengths were obtained by

reading the equivalent widths measured in the

present investigation into the normalized curve of growth adopted for ^ Capricorni in section 4.4. The differential excitation temperature was found

by the minimum-sigma method discussed in section

6.1 to be A^exc(HD 116713 - ^) = 0.11 ± 0.04. The

results for Fe I, Ca I, and Sm II are shown in figures

7.1 through 7.3. For the illustrations, the blue and

red lines have been combined into a single curve of growth by compensating for the logarithmic differ- ence of 0.15 in log V found by Danziger between the

two regions. The theoretical curve of growth fitted to these plots is that adopted for ^ Capricorni.

Differential curves drawn for several other spectra were not quite so smooth as these, but were completely acceptable. The analysis will not be pursued

here, but it is of interest to note that the curve for Sm II is almost normalized, suggesting nearly equal

abundances if Warner's result is adopted that the

electron pressures in the two stars are essentially

the same.

82
o

o

CO

o

LTD cn

Fe I

HDl 16713

6 .50

0: X < 5000 A

+• X > 5000 A

5 .50 4 .50 3 .50 2 .50 1 .50 0 .50

-Log X/(^Cap)

Figure 7.1. Differential curve of growth relative to ^ Capricorni for neutral iron in the barium star HD 116713.

Circles, k < 5000 A; crosses, K > 5000 A.

83
oo

o

in

o

o

CD

OQ ir>

O i/i

1 o

LO

O

HDl 16713

O: X < 5000 A

+• X > 5000 A

8 .00 7 .00 6 .00 5 .00 4.00 3 -00

-Log X'(5Cap)

Figure 7.2. Differential curve of growth relative to C, Capricorni for neutral calcium in the barium star HD 116713.

Circles, \ < 5000 A; crosses, \ > 5000 A.

84
o

o

Sm in

HD116713

—

i

1

11

I

(9

/ ® o

o

—

/

®

/ ®

.^''^ / /

® / /

®

O: X < 5000 K

+: X > 5000 K

3-00 7.00 6 .00

I ! 5.00 4.00 3.00 2

-Log x'(^Cap)

Figure 7.3. Differential curve ofgrowth relative to I, Capricorni for singly ionized samarium in the barium star HD 116713.

Circles, K < 5000 A; crosses, K > 5000 A.

85
8. Discussion and Summary

8.1. The Accuracy of the Abundances

Experience has shown that the errors accumulating in any atmospheric analysis, no matter how

carefully performed, usually produce an uncertainty by a factor of about two in the derived

abundances. As pointed out by the Burbidges

(1957), a quantitative evaluation of the actual

error in this kind of work presents difficulties not

easily surmounted.

An error in the value adopted for A^exc affects mainly the abundances derived from neutral

lines. In the case of ^ Cap, an error of ±0.01 in the value adopted for A^exc will produce a logarithmic abundance uncertainty of about ±0.06 for most observed spectra. It is seen from eq. (7.6) that an error in [Pe] is wholly transmitted to the

opacity difference [k], which, in turn, is transmitted

to the abundances obtained from ions. Since

[Pe] depends on the product of ^dion and the aver- age ionization potential for the observed elements

(~ 7 eV), an error of ±0.01 in the value of A^jon

will generate uncertainties of about ±0.07 in abundances derived from ion spectra — aU the rare

earths, for example. Since neither A^exc nor Afljon can be expected to be correct to better than ±0.02,

the uncertainty in the abundances can easily

become ±0.20 on a logarithmic scale. Quite apart from errors in the differential parameters, the random errors involved in fitting theoreti- cal curves of growth to the empirical curves severely

limit the reliability of the derived abundances.

In fact, it has become increasingly the practice

in work of this kind to estimate errors in the abundances chiefly by a consideration of the maximum

reasonable variation in fitting the curve of growth

itself. This variation depends on a number of factors,

including the total number of lines used and whether

the lines fall on the linear or flat portions of the curve of growth. For spectra with few observed

hnes, the probable validity of the line identifications assumes dominating importance and must also be taken into account in any error estimate. It

is not being overly cautious to distrust any abundance determination based on fewer than five or

six good lines. The estimates of error stated in table 7.5 have

been made with all the above considerations in mind. In view of the general consistency of the

data and the small scatter in most of the curves

of growth, we might reasonably judge the overall accuracy of the abundances to be within the factor

of two expected of the method.

8.2. Discussion

The specific abundance abnormalities exhibited

by barium stars have been treated in detail by the

Burbidges (1957). Their basic account remains

essentially unchanged despite the minor modifications required by more recent estimates of neutron

capture cross-sections (Seeger et al., 1965). Briefly,

it is thought that the originally solar-type material

in the interior of the barium star was subjected at some stage in its evolution to a source of neutrons

that produced heavy elements from seed nuclei

through the process of slow neutron capture. In

this 5-process of element formation, each capture is followed by /S-decay to a stable isobar. Some of the

5-processed stellar material is then brought to the

spectroscopically observable surface layers through

convective mixing, thus accounting for the abund- ance anomalies found in these stars relative to the sun, which has undergone a different history.

Among the lighter elements, carbon and lithium

show overabundances in ^ Capricorni by about a

factor of two. The result here for hthium differs considerably from the factor of ten obtained by

Warner (1965a), but the discrepancy is solely

attributable to the difference in measurements of

equivalent width for the resonance doublet of Li I at 6707.84 A. The small overabundance (+0.12) obtained for sodium is probably real and appears to be typical

of barium stars. Danziger (1965) found somewhat

larger overabundances (+ 0.45) for sodium in HD

116713 and HD 83548. It is tempting to interpret

the simultaneous excess of carbon and sodium

observed in barium stars as evidence of the carbon

"flash" discussed by Reeves (1966). Such a flash leads to a very rapid neutron flux that preferentially

enhances these two elements. Since this postulated

carbon flash almost simulates an r-process, the large

dysprosium excess found in ^ Cap might also be

explained as a product of this stage of the stellar history. However, the normal abundance found for r-processed europium would stiU remain a mystery.

86
The abundances of the elements from magnesium

to germanium do not indicate any important deviations from the normal solar composition. In view of the error estimates, little significance can be

attached to the shght overabundances ( —hO.lO)

obtained for zinc, germanium, and scandium. It is of interest, however, that the result for scandium seems to be more or less typical of barium stars (Burbidge and Burbidge, 1957; Warner, 1965a).

The most abundant isotope of scandium is 5- processed from Ne, but according to the discussion

by the Burbidges the production of a great excess

of scandium would not be expected owing to the

depletion of the neutron supply through the much

greater capture cross sections of the iron-peak

elements and their products.

The elements strontium, yttrium, and zirconium

are similar in that they all have magic-number

nuclei and about the same atomic weight. It has

been argued (Heifer et al., 1959) that the relative overabundances of these three elements should,

therefore, be nearly equal if the 5-process is the

dominant mechanism by which the elements have

been formed. Within the experimental uncertainty,

the abimdances derived for these elements in ^ Capricomi are indeed nearly the same, all of them

being overabundant by factors of 8 to 10 relative

to the standard solar composition. The abundance

for strontium is the most unreliable of these three

elements, but the uncertainty is not sufficient to explain the difference by a factor of seven between

the present result and that of Warner for the star. In contrast, the abundances derived for yttrium and

zirconium in the two investigations are comparable.

The close agreement between the results here

and those of Warner for molybdenum, ruthenium,

tungsten, and lead is rather encouraging in the hght

of the paucity of hnes observed for these elements

and the differences in hne identifications for the

first two elements. Overabundances of these

elements in ^ Cap by about a factor of two are

certaintly indicated.

The small overabundance obtained for niobium

is probably real. There remains some doubt about

the hne identifications for niobium, but the over- abundances found in this investigation and in those

of Danziger (1965) and the Burbidges (1957) suggest

that the enhancement of niobium is a general characteristic of barium stars. The result obtained here for the barium abundance should not be taken too seriously, because

the measured lines are far too strong to obtain accurate abundance shifts. As expected however.

barium is certainly overabundant in ^ Cap — by

about a factor of 10 to 30. The results for the 5-processed elements confirm

the general impression given by a visual inspection

of the stellar spectrum and are similar to the results obtained for barium stars by other workers. Among

the rare earths, lanthanum, neodymium, praseo- dymium, cerium, and samarium are overabundant

by a factor of eight or nine. The overabundance

obtained for gadohnium is much smaller.

It is frustrating that dysprosium has not yet been

measured in other barium stars. If the line identi- fications are correct, a substantial overabundance

of this rare earth is indicated in ^ Capricorni. This

result is of some interest, because if conflicts with

the expectation that the dysprosium abundance in barium stars should be, hke that of europium,

essentially normah Neither element is predominantly

5-processed by current estimates. In many respects, this independent study of ^ Cap at higher dispersion agrees well with that of

Warner for the same star. The most important

diff^erence is the relative amounts by which the

5-processed rare earths in the barium star are found

to be overabundant with respect to the solar composition. It is noteworthy that the corresponding

abundance ratios found by Danziger (1965) — after compensating for the metal deficiency of Arcturus,

his comparison star — are also larger than those

derived by Warner for the same two barium stars by about the factor of three found here in the case

of l Capricorni. As pointed out by Cayrel and Cayrel

de Strobel (1966) and by Unsold (1969), part of this discrepancy might be explained on the basis of the

differences in the physical parameters derived for the stars. The temperatures and electron pressures

determined by Warner and Danziger for their

common stars diff"er significantly, for example, but

that is not the case for (, Cap. Some of the abundance

differences appear too large to be accounted for solely on this basis. Other effects, perhaps of a systematic nature, may be operative. For example,

the striking difference of 0.7 dex found in the two

investigations for the logarithmic abundance of

neodymium relative to iron in ^ Cap appears to be

incompatible with the reliability generally claimed

for the diff'erential method of abundance analyses.

A detailed investigation of this problem is beyond

the scope of the present work, but will be dis- cussed further in connection with the model

atmosphere analysis of ^ Cap currently in progress

by the writer.
8.3. Summary

A differential curve of growth analysis for the

barium star ^ Capricorni has been performed.

Both the sun and e Virginis have been used as comparison stars. The spectrograms used in the

analysis were obtained by J. L. Greenstein at the

coude focus of the 200-in telescope. The reciprocal

dispersion was 2.3 A/mm in the blue and 3.4 A/m

in the red spectral regions. Table A presents

identifications, half-widths, central depths, and

equivalent widths for the 1100 spectral hues

measured in this investigation.

The physical parameters derived for ^ Capricorni

are collected in table 8.1. Table 8.1. Physical parameters for L, Capricorni

^exc 1.13 - 1.28 0.99 + 0.13

log 2a -2.5 - 1.10

^micro 3.5 km/s [A] J-.: -0.03

^macro 5.5 ktn/s

The atmospheric abundances for 37 elements

are given in tables 7.3 and 7.5. The resuhs with

respect to the sun and to e Virginis are in excellent

agreement. The barium star exhibits essentially

solar abundances for most elements through ger- manium. Overabundances by factors of about two

are indicated for carbon and lithium, however. The

smaller overabundances found for sodium and

scandium may be real, but the values are within

the estimated error of the determinations. There

may be a slight manganese deficiency.

With the exception of europium, all elements

heavier than germanium are found to be over- abundant in C, Cap. Large overabundances have

been found for the 5-processed elements, as well

as for dysprosium, which is generally considered

to be r-processed. Although the writer has reasonable confidence in this result for dysprosium, the

reliability of the determination is seriously affected

by the difficulty in making positive line identifica- tions and by the few lines upon which the deter- mination is based.

The extent by which the rare earths are found to be overabundant — by factors of about eight or nine — is greater than that found by Warner for the same star. Similar results obtained by Danziger

for two of the barium stars also studied by Warner

suggest that the average scale of Warner's abundances for these elements may be too small.

88
Appendix

A. 1. Sample Differential Curves of Growth

A number of the differential curves of growth constructed for the analysis of ^ Capricorni and

not already displayed in connection with discussions in the main text are collected in this section.

They are here presented in alphabetic order according to spectrum. Each plot contains differential curves of growth with respect to the sun (circles) and to e Virginis (crosses).

7 .00 6.00 5 .00 4.00 3 .00 2 .00

-Log X'

Figure A.1-1.

89
90
6 .00 5.00 4.00 aToO 2^00

-Log X'

1 .00

Figure A.1-3.

398-978 0 - 71 -7 91
Figure A. 1-4.

92
o

in

Fe T

^6.00 5-00 4.00 3-00 2 .00 1 .00 0.00

-Log X'(€)

Figure A. 1-5. Differential curve ofgrowth with respect to e Virginis only.

Corresponding curves for Fe I with respect to the sun have already been shown and discussed in the main body of the text.

Circles. X < 5000 A; crosses. X > 5000 k.

93

f

I
94



98
Figure A. 1-11.

99
100
Figure A.1-13.

101
o

in

-Log X'

Figure A.1-14.

j

I

102

104
Figure A.1-17.

105
7 .00 6 .00 5.00 4.00

-Log X'

3 -00 2 .00

Figure A.1-18.

106
A.2. Sample Absolute Curves of Growth

This section presents some of the absolute curves of growth constructed for the analysis of

I Capricorni by use of the ^/-values discussed in section 3.2. Such curves for additional spectra

have already been displayed in connection with discussions in the main body of the text. The plots

here are arranged in alphabetic order according to spectrum. In each plot a distinction is made

between Hnes with wavelengths greater than 5000 A {crosses) and less than 5000 A {circles). The

absence of systematic grouping of hnes by wavelength suggests that the continuum level adopted in the measurement of equivalent widths was fairly consistent throughout the spectral range studied.

-3 .00 -2 .00 -1 .00 0.00 1 .00 2 .00 3.00

Log(gfX)-eX.

398-978 0 - 71 -8

Figure A.2-1.

107
-2 .00 -1-00 0.00 1 .00 2 .00

Log(gfX)-0X.

3.00 4 .00

Figure A.2-2.

108
Figure A.2-3.

109
o

o

O

LO"^-5-00 -4.00 -3-00 -2.00 -1 -00 0.00 1 -00

Log(gfX)-9X.

Figure A.2-4.

110
-1-00 0.00 1-00 2.00 3.00 4.00

Log(gfX)-0XFigure A.2-5.

Ill
Figure A.2-6.

112
-3.00 -2.00 -1.00 0.00 1.00

Log(gfX)-eX.

z.oo 3.00

Figure A.2-7.

113
114
o

Ni X

o

o

T \ 1 r -3.00 -2.00 -1 .00 0.00 1.00 2.00

Log(gfX)-eX.

Figure A.2-9.

115
Figure A.2-10.

116
o

-1 1 1 1 -6.00 -5 .00 -4.00 -3. 00 -2.00 -1.00 0-00

Log(gfX)-ex.

Figure A.2-11.

117
o

o

03

O

T

1 1 1 r -1.00 0.00 1.00 2.00 3-00 4.00

Log(gfX)-eXFigure A.2-12.

118
Figure A.2-13.

119
Figure A. 2-14.

120
Figure A.2-15.

121
0.00 1 .00

Log(gfX)-eX.

Figure A. 2-16.

122
A.3. Table A, the Line List Arranged by Wavelength

Tables A and B contain the results of measurement of 1100 atomic spectral lines in the spec- trum of ^ Capricorni. Table A lists the data by increasing wavelength, whereas table B groups the

hnes according to spectrum. The information given in the two tables differs only in the contents

of columns 5 through 7. The description of table A is given below.

Description of Table A

Column 1 Column 2 Column 3 Column 4 Column 5

Column 6 Column 7 Column 8 Column 9 Column 10 Column 11 Column 12

Column 13:

the spectral identification of the measured line the laboratory wavelength in angstrom units the multiplet number of the line as listed in the Revised Multiplet Table (Moore, 1959) the excitation potential (in eV) of the lower level of the transition — log (Wf)lk), the solar equivalent width of the line as listed in the Second Revision of the Rowland Table (Moore et al., 1966) — log ( WJK), the equivalent width of the line as observed in e Virginis (Cayrel and Cayrel, 1963)

log igfk), obtained from the sources hsted in table 3.1 of section 3.2.2 the measured Une width at half-intensity, in mA

the central depth

the primary equivalent width, in mA

the value of — log (JF/A.) obtained after the adjustments discussed in section 2.3.4 an estimate of the general quality Q of the measurement on a scale of 1 (poor) to 5 (excellent). A quality Q =0

has been assigned to a few lines. These represent very strong blends whose primary equivalent widths have been distributed, according to estimated simple ratios, over the contributors to the absorption in the calculation oflog(r/\).

the chart section on which the line was measured, as discussed in section 2.3.1

398-978 0 - 71 -9 123
Table A

Spect

Wavelength

Mult EP

— Log -Log Log

i pf\ \ \gj A)

HW Rc W

-Log Q A'

Ce II 4053.51 36 .00 5.76 2.78 256 .62 194 4.32 2 0

Pb I 4057.81 1 1.32 5.40 3.96 227 .41 98 4.62 1 0

Fe I 4059.71 767 3.55 4.76 3.36 242 .52 135 4.48 2 0

Nd II 4059.97 63 .20 5.83 2.63 242 .52 135 4.48 2 0

Fe I 4067.99 559 3.21 4.49 3.96 261 .65 206 4.29 2 0

Ce II 4068.84 82 .70 6.07 3.24 253 .59 161 4.40 2 0

Nd II 4069.27 20 .06 5.68 2.60 251 .58 157 4.41 2 0

Fe I 4070.78 558 3.24 4.64 3.65 254 .60 165 4.39 2 0

Zr II 4071.09 54 1.00 5.38 247 .55 146 4.44 2 0

Ce II 4072.92 .33 2.67 A'J 243 .52 1

'5 C 135 A AO 4.4o 2 0

Dy II 4073.12 .54 5.91 3.42 233 .45 111 4.56 2 0

W I 4074.37 6 .37 5.35 2.98 225 .39 92 4.65 1 0

Fe I 4091.56 357 2.83 4.83 2.37 231 .43 105 4.59 3 0

Ce II 4093.96 .53 2.63 236 .46 115 4.55 2 0

Ca I

A t\C\ A C\ A 4094.94 25 2.52 A Z' 1 4.61 2.92 246 .53 140 A AH 4.47 2 0

Fe I 4098.18 558 3.24 4.56 3.52 258 .61 189 4.34 2 0

Si I 4102.94 2 1.91 4.59 .71 261 .63 198 4.32 2 0

Dy II 4103.34 .10 5.53 3.18 246 .53 140 4.47 2 0

Nd II 4109.45 10 .32 5.02 3.20 111 .74 246 4.22 2 0

Ce II 41 17.29

^7 A .74 2.93 221 .39 93 4.65 2 0

Ce II 4117.59 1.32 3.51 240 .48 123 4.53 2 0

Fe I 4120.21 423 2.99 4.63 3.23 256 .59 163 4.40 2 0

Ce II 4120.84 112 .32 5.50 2.88 262 .63 198 4.32 2 0

Co I 4121.33 28 .92 4.52 3.58 275 .72 237 4.24 2 0

Eu II Ally.13 1

f\f\ .00 4.88 3.31 III . 15 Z4z 4.23 z u Gd II 4130.37 19 .60 5.57 3.71 241 .48 123 4.53 2 0

Nd II 4133.35 19 .32 5.57 2.47 251 .55 148 4.44 2 0

Fe I 4139.94 18 .99 4.68 .78 254 .57 156 4.42 2 0

La II 4315.90 41 .40 5.98 1.28 377 .38 157 4.74 0 27

Gd II 4316.05 A43 .66 5.59 2.97 ill .38 157 A HA 4.74 0 27

Ti II 4316.81 94 2.05 5.06 4.71 2.57 267 .50 135 4.50 2 27

Zr II 4317.32 40 .71 5.52 2.16 251 .61 167 4.41 2 27

Ca I 4318.65 5 1.90 4.57 3.43 283 .67 225 4.28 2 27

Sm II 4318.94 27 .28 5.64 2.86 308 .53 172 4.43 1 27

Fe I 4319.45 214 2.61 5.52 1.13 209 .20 43 5.01 1 0

Cr I 4319.64 96 2.89 5.46 3.46 210 .20 43 5.01 1 0

Ti II 4320.96 41 1.16 4.84 1.37 288 .72 237 4.26 1 0

La II 4322.51 25 .17 5.56 2.00 251 .60 167 4.40 3 27

Sc II 4325.01 15 .60 4.57 3.27 302 .81 280 4.19 3 0

Fe I 4325.76 42 1.61 3.74 4.00 628 .86 587 3.87 3 27

Ti I 4326.36 43 .83 5.29 2.74 226 .31 73 4.77 1 0

Sm II 4329.02 15 .18 5.56 2.73 282 .45 129 4.54 2 27

V I 4330.02 5 .00 5.09 2.41 237 .38 95 4.66 2 0

Ni I 4331.64 52 1.68 4.89 2.27 314 .56 179 4.41 3 27

Zr II 4333.28 132 2.41 3.53 298 .45 145 4.52 2 27

Ce II 4336.26 89 .70 6.24 3.14 232 .53 132 4.49 4 27

Fe I 4337.05 41 1.56 4.56 2.49 294 .75 251 4.24 3 0

Fe I 4343.70 517 3.05 4.79 2.55 265 .56 160 4.43 1 0

Fe I 4347.24 2 .00 5.03 246 .43 112 4.59 2 0

Fe I 4348.94 414 2.99 4.87 2.26 235 .42 108 4.60 4 27

124
Table A

opcct

Wavelength

\liilt -»1 HI I EP — Log —Log

(B^./X)

Log

(g/"X)

IHWi rr l\R

c

W

-Log CtV /V

4349.79 59 .70 5.76 3.22 220 .53 135 4.49 4 27

Cr T 4357.52 198 3.37 5.06 213 .27 67 4.83 3 27

Nd II 4358.17 10 .32 5.06 2.66 278 .64 202 4.33 3 0

Sm II 4362.04 45 .48 5.94 2.68 298 .52 167 4.45 2 27

Ce II 4364.66 135 .50 5.56 3.29 251 .60 172 4.40 2 27

Fe I 4365.90 415 2.99 4.96 2.21 188 .35 75 4.74 2 27

Ce II 4375.92 134 .50 3.06 301 .77 260 4.43 0 27

Fe I 4376.78 471 3.02 4.93 2.37 219 .41 90 4.65 2 27

Fe I 4377.80 645 3.27 5.05 2.31 204 .28 59 4.85 3 27

V I 4379.24 22 .30 4.60 4.12 226 .63 157 4.45 3 27

Zr II 4379.78 88 1.53 3.45 251 .63 183 4.38 3 27

Ce II 4382.17 2 .68 5.74 3.47 314 .61 195 4.35 1 27

Fe I 4383.55 41 1.48 3.64 4.15 627 .90 630 3.84 2 27

Fe I 4388.41 830 3.60 4.63 3.84 277 .62 194 4.36 3 0

Fe I 4389.24 2 .05 4.82 251 .60 165 4.41 1 28

V I 4389.97 22 .28 4.72 3.69 279 .63 198 4.35 1 0

Ti II 4391.03 61 1.23 5.11 1.61 445 .74 350 4.60 0 28

Ti II 4394.06 51 1.22 4.79 4.47 2.17 307 .71 241 4.26 3 28

Ti II 4395.85 61 1.24 4.86 4.58 1.98 290 .70 228 4.28 2 0

Y II 4398.02 5 .13 4.98 2.40 382 .81 325 4.13 2 28

Ce II 4399.20 81 .33 5.90 2.86 282 .60 181 4.39 2 28

Ti II 4399.77 51 1.24 4.58 4.39 2.56 301 .77 260 4.23 3 0

Zr II 4403.35 79 1.18 2.54 286 .67 215 4.31 2 0

Fe I 4404.75 41 1.56 3.69 3.89 643 .87 613 3.86 3 28

V I 4406.65 22 .30 4.75 3.39 282 .56 171 4.42 4 28 Pr II 4408.84 4 .00 5.64 2.81 293 .71 233 4.28 2 0

Mo I 4411.57 2.08 5.99 4.30 220 .24 54 4.91 1 0

Ce II 4413.19 1.14 3.01 282 .38 109 4.63 2 28

Pr II 4413.76 26 .22 6.10 2.40 265 .53 151 4.47 2 0

Zr II 4414.54 79 1.24 5.28 2.59 301 .63 210 4.32 2 28

Sc II 4415.56 14 .60 4.71 2.81 282 .73 238 4.27 2 28

V I 4416.47 22 .27 5.09 2.80 244 .39 100 4.65 1 0

Fe II 4416.82 27 2.78 4.76 1.55 313 .72 245 4.26 2 28

Ti II 4417.72 40 1.16 4.66 4.45 2.50 338 .77 276 4.20 3 28

Ti II 4418.35 51 1.24 4.80 4.46 1.98 301 .65 222 4.30 3 28

Ce II 4418.78 2 .86 5.41 3.68 278 .61 189 4.37 2 0

Sm II 4421.14 37 .38 5.65 2.63 263 .53 151 4.47 3 28

Fe I 4422.57 350 2.84 4.58 3.43 407 .77 333 4.32 0 28

Y II 4422.59 5 .10 2.06 407 .77 333 4.32 0 28

Sm II 4424.34 45 .48 3.22 278 .61 189 4.37 4 0

Ca I 4425.44 4 1.88 4.48 3.26 276 .67 204 4.34 4 28

Fe I 4430.62 68 2.22 4.59 2.63 329 .70 260 4.23 3 28

Sc II 4431.37 14 .61 5.17 1.51 257 .47 126 4.54 2 28

Fe I 4433.22 830 3.65 4.66 3.70 276 .59 176 4.40 2 0

Sm II 4434.32 36 .38 5.47 2.89 271 .56 163 4.43 5 0

Fe I 4436.95 516 3.05 4.77 2.27 219 .48 109 4.57 4 28

Fe I 4438.35 828 3.69 5.00 2.86 307 .41 123 4.67 0 28

Fe I 4439.89 116 2.28 4.98 1.65 26^ .38 97 4.66 2 28

Fe I 4442.34 68 2.20 4.41 3.15 391 .77 307 4.16 5 28

Ti II 4443.80 19 1.08 4.55 4.36 2.95 363 .81 321 4.14 4 28

I
Table A

Spect

W ave- length

Mult EP Log

( W/ l \ \

\ tr ( j/ A. j — Log

1 JT/ l \ \ {IV (IK) Log( rrf\ \ HW Re W

— Log

{ TV/ 1 \ \ Q A'

Fe I 4445.48 2 .09 5.17 ^ 244 .38 102 4.65 5 28

Nd II 4446.39 49 .20 5.72 2.35 282 .61 194 4.36 4 28

Fe I 4446.84 828 3.69 4.80 3.28 259 .48 133 4.53 3 0

Fe I 4447.13 69 2.20 4.87 1.76 261 .49 136 4.51 3 0

Fe I 4447.72 68 2.22 4.40 3.07 329 .72 259 4.23 5 28

Mn I 4451.59 22 2.89 4.69 4.34 235 .68 187 4.38 5 28

Nd II 4451.99 6 .00 1.70 250 .53 141 4.67 0 28

V I 4452.01 87 1.87 5.31 4.35 250 .53 141 4.98 0 28

Sm II 4452.73 26 .28 5.84 2.67 267 .53 152 4.47 3 0

Mn I 4453.00 22 2.94 4.99 3.71 244 .38 97 4.66 2 0

Ti I 4453.31 113 1.43 4.88 4.04 260 .48 133 4.53 1 0

Ti I 4453.71 160 1.87 5.09 4.01 250 .32 11 4.76 3 28

Fe I 4454.38 350 2.83 4.72 3.14 283 .63 198 4.35 3 0

Mn I 4457.04 28 3.07 5.07 3.35 232 .30 72 4.79 2 0

Sm II 4458.52 7 .10 2.38 260 .48 133 4.53 3 0

V I 4459.76 21 .29 4.97 3.01 211 .38 82 4.70 4 28

Fe I 4461.65 2 .09 4.59 .94 301 .74 246 4.26 2 0

Nd II 4462.99 50 .56 5.54 2.81 275 .64 201 4.35 3 29

Fe I 4466.55 350 2.83 4.55 3.83 344 .76 282 4.20 3 29

Sm II 4467.34 53 .66 5.75 3.26 270 .54 156 4.46 2 0

Ce II 4467.54 17 .61 2.82 270 .54 156 4.46 2 0

Ti II 4468.50 31 1.13 4.57 4.36 3.06 501 .85 444 4.00 3 29

Mn I 4470.14 22 2.94 4.96 3.80 242 .36 91 4.69 2 0

Ni I 4470.48 86 3.40 4.81 4.24 282 .54 147 4.47 2 29

Ti II 4470.86 40 1.16 4.92 4.51 1.82 294 .68 202 4.35 2 29

Sm II 4472.43 .18 6.11 2.12 240 .35 88 4.71 1 0

Sm II 4475.18 .10 1.23 214 .18 39 5.06 1 0

Nd II 4475.57 .06 1.07 250 .30 73 4.79 2 29

Fe I 4476.02 350 2.84 4.47 3.79 313 .73 242 4.27 5 29

Fe I 4478.04 69 2.20 5.47 .96 213 .20 44 5.01 4 29

Fe I 4480.14 515 3.05 4.92 2.64 325 .53 180 4.43 2 29

Fe I 4481.62 827 3.69 4.99 3.14 246 .38 98 4.66 2 0

Fe I 4482.17 2 .11 4.43 .80 366 .80 319 4.15 5 29

Gd II 4483.35 62 1.06 6.48 2.95 235 .27 59 4.86 2 29

Ce II 4483.90 3 .38 5.48 3.52 282 .57 185 4.40 3 29

Fe I 4484.23 828 3.60 4.77 3.88 250 .57 155 4.44 3 29

Ce II 4484.83 1.12 6.65 3.15 244 .37 95 4.67 2 29

Nd II 4485.95 .38 1.38 250 .31 94 4.98 0 29

Fe I 4485.97 825 3.65 5.40 2.34 250 .31 94 4.98 0 29

Ce II 4486.91 57 .30 5.61 3.03 263 .64 166 4.43 4 29

Fe I 4489.74 2 .12 4.74 .25 295 .69 224 4.30 3 0

Fe II 4491.40 37 2.85 4.83 4.62 1.56 289 .65 206 4.34 3 0

Ti II 4493.50 18 1.08 5.24 4.68 .86 338 .56 188 4.41 3 29

Sm II 4499.48 23 .25 6.35 2.07 243 .36 92 4.69 2 0

Ti II 4501.27 31 1.12 4.61 4.34 2.86 469 .83 409 4.04 4 29

Mn I 4502.22 22 2.92 4.96 4.66 3.84 250 .41 102 4.63 1 29

Fe I 4502.60 796 3.57 5.33 4.80 2.38 188 .24 51 4.93 1 29

Ti I 4503.76 184 2.13 5.75 3.42 244 .13 32 5.22 2 29

Fe I 4504.84 555 3.26 4.99 2.20 244 .36 92 4.69 1 0

Sm II 4505.05 .25 1.75 218 .20 44 5.01 1 0

126
Table A

Spect Waveleri'^'th Mult EP — Log

(WJk) — Log[WJX)

Log HW Rc W

Log

[WJK) o Q

Y I 4505.95 14 1.37 6.35 3.61 212 .16 34 5.12 1 0

Fe II 4508.28 38 2.85 4.78 1.89 325 .70 249 4.26 2 29 Pr II 4510.16 20 .42 6.48 2.87 313 .55 180 4.42 3 29

Ca I 4512.27 24 2.52 5.40 4.83 216 .18 39 5.06 1 0

li I 4j 12. /J 4Z 8/1 .54 A Ql A An 4.DU 1/11 J. 41 77

1

Z / 1 CI .J J

1 c/1

1 j4 A Al 4.4 /

-JJ U Fe II 4515.34 37 2.84 4.78 4.53 1.74 298 .70 228 4.30 2 0

Fe I 4517.53 472 3.07 4.87 2.54 306 .55 166 AAA 3 29

Ti I 4518.03 42 .83 4.86 4.54 3.51 263 .54 144 4.48 2 29

Sm II 4519.63 49 .54 5.96 5.01 2.74 256 .51 141 4.50 4 29

v^c 11 L . J z J.JO 4. /D 1 70 7Q7 Z7 / .\jy M 774 zzt A 11 7z 0

Sm II 4523.91 41 .43 5.61 4.86 2.49 275 .46 122 4.56 3 29

Ti II 4524.73 60 1.23 5.40 4.70 1.59 264 .48 135 4.53 2 0

Ba II 4524.93 3 2.51 5.15 4.65 3.30 291 .65 206 4.34 2 0

Fe I 4525.15 826 3.60 4.58 4.39 3.83 297 .69 224 4.31 2 0

La II tJ ZD. 1 Z . 77/ / ^ A^ J.4J A 81 7 ^7 z. jz JUD 10A .J J

11 8^O J AH.^41J

11 7QLy

Cr I 4526.47 33 2.54 4.63 4.08 313 .65 213 4.33 3 29

Ca I 4526.93 36 2.71 4.78 4.58 3.23 256 .49 116 4.55 2 29

Ti I 4527.31 42 .81 4.83 4.54 3.38 306 .71 226 4.50 0 29

Ce II 4527.35 108 .32 3.05 306 .71 226 4.50 0 29

FC 1 HJ J

1

.Dj J J J

7 1 j.Z 1 A Q7 7Z.4Al/ 7^0 ZjU .4Al/11 71Z J 4. J J 7z 7QLy

Ti I 4533.27 42 .85 4.70 4.47 4.30 281 .67 215 4.32 2 29

Ti II 4533.97 50 1.24 4.62 3.02 500 .85 438 4.02 4 29

Ti I 4534.79 42 .84 4.75 4.51 4.07 281 .62 189 4.38 4 29

Cr I 4535.15 33 2.54 5.24 4.75 3.18 226 .24 56 4.91 1 0

Cp it v-c il 11 . JS7Z 1J.Z71J 77^ ZZJ .Z71J Jt^A A Ql 7z 0

Sm II 4537.96 45 .48 6.00 5.19 2.58 281 .51 142 4.50 3 29

Ce II 4539.07 1.37 3.20 241 .33 83 4.74 2 0

Cr I 4540.50 33 2.54 4.90 4.55 3.88 254 .41 110 4.62 1 0

Nd II 4541.27 58 .38 2.28 276 .55 163 AAA 1 0

Ti II 11 11 HJ't't.Ul AOOU 1 lA 1 .Z4 J.l 1 A A^ 4.DJ 1 ^8 1 .JO 1 1 7 J 1 Z .Dj Al 71/1 Z14 A SI 4. J J V 7QLy

Cr I 4545.96 10 .94 4.79 2.69 269 .64 186 4.39 5 29

Fe I 4547.85 755 3.55 4.79 4.58 3.67 244 .56 156 4.45 5 29

Ti I 4548.76 42 .83 4.86 4.57 3.48 250 .50 132 4.52 3 29

Ni I 4551.24 236 4.17 5.30 4.83 3.54 219 .52 128 4.98 0 29

Co IT i^e II 43 J 1 .j\J 7/1 7 Ql 7 1 Q zl 7

'57

. jZ 11 78ZO A4. A8Do AU 7QLy

Fe I 4551.67 912 3.94 5.30 4.87 2.66 203 .24 59 4.90 1 29

Ba II 4554.03 1 .00 4.46 4.24 3.83 843 .91 1068 3.63 3 29

Ti I 4555.49 42 .85 4.93 4.63 3.37 275 .54 160 4.46 2 0

Fe I 4558.11 894 3.64 5.38 2.31 234 .28 63 4.84 4 30

La II 4j jy.zo . 1

1

£i AQ D.4o 1 Q/1 1 QO 1/1 .34 7

1

/ 1 A If- 4. /D cJ 7QLy

Ce II 4560.96 2 .68 6.01 2.96 271 .51 148 AA9 3 0

Ce II 4562.36 1 .48 5.43 4.85 3.59 250 .64 159 4.46 5 30

Nd II 4563.22 .18 2.08 lie .54 161 4.45 3 0

Ti II 4563.76 50 1.22 4.58 4.35 2.80 387 .79 368 4.09 3 30

Sm II 4566.21 32 .33 5.78 5.08 2.25 234 .35 83 4.72 2 30

Fe I 4566.52 641 3.30 5.10 4.74 2.37 187 .25 52 4.92 2 30

Fe I 4566.99 723 3.41 5.43 1.94 234 .32 80 5.10 0 30

Nd II 4567.61 49 .20 6.36 1.49 219 .30 68 4.81 3 30

Ti II 4568.31 60 1.22 5.26 4.78 1.73 250 .39 96 4.66 4 30

Fe I 4568.79 554 3.26 5.06 2.08 250 .37 100 4.86 0 30

127
Table A

^pect

Wavelength

Mult iVlUlI FP -Log -Log Log

'If Vrw -Log nV /V

^JDO.OO 8Q4 ^ 6^ 5 ^6 7 ^7 750 ^7 11 00\J\J 4 96 0 30

Pr- II ri 11 4S7n HJ ft] / w.u 1 77 6 ^6 1 . -/-7 vol 14 S IQ 11 "^0 Mg I / 1 . lU 11 ,\J\J 00 4H. 70/ u LO 1

11 QQyy A ^0

r^f^ ri

11 1 .HO _) . 1 J? ?S0 ^0 RO 4 7f^ ^0

Nb I 4573.08 .27 2.83 203 .08 16 5.46 2 0

irc 1 554 3 71 S 14 4 81 7 03 71

9

27 61 4.86 30

7r T 4S7S 5 . 00\J\J 5 66 4 94 7 30 750 27 65 4 85 30

tt 4576 33 38 7 84 4^ .y91i. 4.66 1 44 343 61 224 4.31 5 30

VV T1 4577 17 4 00 5 26 2 40 234 .30 74 4.79 3 30

Sm II 4577.69 23 .25 6.06 2.26 265 40 109 4^63 1 30

Ta T 4578.55 23 2.52 4.80 4.60 3.10 281 .45 122 4.57 1 30

Tr T1 4580 06 1

0

1 \j 94 4 76 7 46 781 58 1I/O78 4 41 7Z. 30

V T 4580 39 4 02 5 04 7 52 375 .46 183 4.76 0 30

FeX & T1 4580 59 877 3 65 5 06 2 51 375 46 1 83 4.76 0 30

Ce II 4582.50 7 .70 6.06 3.11 343 .56 185 4.41 1 30

At 11 4582.84 37 2.84 4.97 4.73 1.22 293 .53 157 4.47 2 30

Ti-I- TT 1 11 4583 44 ^9 1 16 5 76 4 73 750 44 11 70Z.V/ 4.58 30

T^e i. t TT11 4583 83 38 7 81 4 57 7 41 437 .11 366 4.10 4 30

Ru I 4584.44 5 1 00 6 49 3 50 206 .10 20 5.35 1 0

Ca I 4585^87 23 2.52 4.53 3.47 281 !59 199 4^38 3 30

V I 4586 36 4 .04 5.08 2.65 312 .40 145 4.85 0 30

Fe I 4587.13 795 3.57 5 00 2.87 281 .37 110 4.65 3 30

CrV—•* IT11 4588 22 44 4.07 4.84 3.01 296 .58 195 4.39 5 30

TiA 1 TT11 4589.96 50 1.24 4.82 4.53 2.05 306 .68 229 4.30 5 30

Sm II 4591.82 14 !l8 6^49 L89 242 32 80 4.76 1 0

CrV^l TT11 4592 09 44 4 07 5 07 7 79 260 .43 118 4.59 2 0

FeJT C T1 4597 66 ^9 1 56 4 68 1 75 ^17 70 261 4H. 25 4 30

FeX W T1 4593 54 971 y 1 1. ^ 94 5 V) 4 86 7 65 781 39 106 4.83 0 30

NH1^ VJ TI11 45Q4 45 57 70 11 .''xy 49 756 Z._J VJ 32 84 4.75 30

Fe I 4595.36 594 3.30 4.88 2.73 312 .56 181 4.62 0 30

Nii~ 1 T1 4595 96 101 1 V/ 1 ^ 47 5 1 3 3 18 296 .49 151 4.85 0 30

XFeW T1 4596 06 820 3 60 4 88 2.92 296 .49 151 4.69 0 30

XFe& T1 4596 43 873 3 65 5 70 4 83 2.28 250 .23 60 4.91 1 30

FeC T1 4598 17 554 ^ 78 4H. 78/ O 4 58 7 98 271 50 145 4.50 3 0

Fe I 4598.74 819 3.69 5.58 5.02 2.05 218 .17 39 5^08 1 30

Cr^1 T1 4600 75 71Z. 11 00 4 76 4 57 7 64 783 57 174 4.42 2 0

*^e it11 4601 ^7 11 . JZ^7 7Z.OH64 7'^6 .^o 7R 68 4 8"? 3 0

Fore TI 4A07 no 1Q 1 .Dl A 88 4.oO 4. J J 11 . 11 6

D

775 Z / J

1 .J 1

11 JZ57 4 4Q J

'^0 7r I Al 1 '40UZ. 11 .o87/ D. 1 7 44.U101 71ZIO8 . 1 o 44 5 04 11 10

Fe I 4602.94 39 1.48 4.68 4.34 2.20 281 .70 225 4.31 4 30

F<i re I

1 4141U0 7 QQ J.5 4Q47 1 50 750 .z77/ 77 4'-r .y95J 0Km 30

Qm IT oITl 11 Af^C\A 1 8 'tOU'+. lo .U4 11 .DZ 67 718 zi o 7Q 74 4 80 11 '^0 r'o ce IT

II 401)4. Zl 1 .Uj 7Z. 11 6

D

71zio8 .Ly 7Q 74 4 80 11 10 cr I 40U4.JO 1 on lyu J. JZ ^ HQ 44. 7^/ D 765 ZDJ .zo 78 80 4H.7Q/ y 9 10

TsTi T 1 1 4604 99 98yo ^ 48 4 87 4.39 265 .49 132 4.53 3 30

Ce II 4606.40 .91 3jJ

286 , .59 182 4.40 3 0

Nb I 4606.77 .35 5.92 217^ -.16 35 5.12 2 0

Sr I 4607.35 2 .00 5.11 4.71 4.00 286 .59 183 4.40 2 0

Ce II 4608.76 1.41 2.81 203 .20 47 4.99 2 30

Ti II 4609.26 39 1.18 5.62 5.00 275 .34 96 4.70 3 30

128
Table A

Spect

3.VC"

1 Y\ 1 rt ri Mult EP — I Ci^ — I .Off HW Rc W

— Log Q A'

Fe I 4611.28 826 3.65 4.64 3.68 291 .62 194 4.38 2 0 Pr II 4612.07 .00 6.12 1.67 287 .23 69 4.88 2 30

Nd II 4612.47 3 .06 6.27 .95 312 .25 74 4.84 2 30

Zr II 4613.95 67 .97 5.20 4.78 277 .53 157 4.47 2 0

Sm II 4615.69 22 .19 5.73 2.09 263 .44 122 4.58 2 0

Cr I 4616.14 21 .98 4.81 4.60 2.72 289 .60 187 4.39 3 0

Cr II 4616.63 44 4.07 5.10 4.91 2.15 306 .46 149 4.52 2 30

Ti I 4617.27 145 1.75 4.97 4.72 4.38 234 .39 99 4.66 5 30

Fe I 4619.29 821 3.60 4.82 4.65 3.40 273 .50 146 4.50 2 0

La II 4619.87 76 1.75 6.27 3.47 287 .43 126 4.58 2 30

Fe II 4620.51 38 2.83 4.99 4.78 1.03 281 .51 159 4.48 4 30

Cr I 4621.94 32 2.54 5.01 3.41 278 .32 90 4.73 3 30

Cr I 4622.49 233 3.55 5.15 4.75 4.23 265 .31 93 4.73 2 30

Ti I 4623.10 145 1.74 5.00 4.64 4.07 274 .38 98 4.67 3 30

Ce II 4624.90 27 1.12 5.89 3.52 390 .62 256 4.46 0 30

Fe I 4625.05 554 3.24 4.78 4.58 3.04 390 .62 256 4.46 0 30

Co I 4625.77 176 3.71 5.82 3.65 209 .13 29 5.39 0 30

Cr I 4625.92 244 3.85 5.59 209 .13 29 5.39 0 30

Cr I 4626.19 21 .97 4.84 4.64 2.66 281 .53 167 4.45 2 30

Ce II

,4 Z* O 1 Z" 4628.16 1 .52 5.52 4.86 3.52 337 .67 226 4.31 4 30

Fe I 4630.13 115 2.28 4.88 4.59 1.84 249 .56 161 4.45 2 30 re I 4632.92 39 1.61

A /' Q 4.68 1.36 291 .61 189 4.39 2 0 re I 4635.85 AC\ 349 O A 2.84 5.02 4.70 2.21 ^ AC\ 249 .38 91 A ZT O 4.68 1 30

ll II 4636.35 38 1 1 Z" 1.16 5.52 4.90 306 .41 124 4.59 2 30 re I 4638.02 822 O Z" 3.60 4.75

"> A"^ 3.43 312 .53 174 4.45 3 30

Sm II 4642.24 36 .38 5.79 4.99 2.55 299 .47 152 4.51 2 30

Fe I 4643.47 820 3.65 4.87 4.57 3.21 281 .46 125 4.56 2 30

Y I 4643.70 4 .00 4.97 2.76 254 .38 101 4.66 1 0

Cr I 4646.17 21 1.03 4.78 4.47 3.17 374 .66 238 4.29 2 30

XT * * Ni I 4648.66 98 3.42 4.84 4.56 4.47 305 .52 161 4.47 2 30

Cr I 4649.46 32 2.54 5.37 4.85 3.03 218 .22 50 4.96 1 30

Cr I 4652.16 21 1.00 4.75 4.52 2.88 256 .61 170 4.44 5 30 re I

>l Z" Af\ 4653.49 17 .99 5.76 312 .27 90 5.00 0 30

om II 4655.13 A O

.48 1.87 227 .21 49 4.98 2 0

Ii I 4656.47 6 .00 4.93 4.53 2.52 271 .47 135 4.54 3 30

Ti II 4657.21 59 1.24 5.09 4.66 286 .57 176 4.42 1 0

Ce II 4659.37 1.21 6.19 2.73 218 .28 69 4.83 3 30

La II 4662.51 8 .00 6.02 5.00 1.68 264 .55 150 4.47 4 30

Cr I 4664.80 186 3.12 4.95 4.04 226 .34 78 4.75 3 30

Fe I 4668.14 554 3.26 4.62 3.38 280 .60 174 4.41 3 31 Na I 4668.56 12 2.10 5.08 4.63 2.37 251 .35 92 4.71 2 0

Fe I 4672.83 40 1.61 5.18 4.81 171 .22 38 5.02 1 31 Fe I 4673.17 820 3.65 4.81 1.11 311 .53 189 4.43 4 31 Ti I 4675.12 77 1.07 5.19 4.75 2.57 218 .27 66 4.85 2 31 Sm II 4676.91 3 .04 6.13 5.08 2.13 296 .37 109 4.65 3 31 Fe I 4678.85 821 3.60 4.68 4.55 3.83 289 .58 181 4.41 3 0

Ti I 4681.91 6 .05 4.86 4.54 2.68 284 .55 168 4.44 1 0

Fe I 4683.57 346 2.83 5.01 4.72 2.12 302 .37 113 4.65 2 31 Ge I 4685.84 3 2.03 5.97 2.37 216 .13 33 5.28 2 0

Ni I 4686.22 98 3.60 4.92 4.66 3.99 234 .35 90 4.71 3 31

129
Table A

Spect

Wavelength

Mult EP -Log

{Walk) — LogiWjK)

Log HW W

-Log oV N

^ TT Le II 4DoO. / J

11 Ajy no 77 D.Z / z.oy 11

A

Z /4 IQ .Ly /o A 7Q 4. ly

•1D 3

1

Zr I 4687.80 43 .73 5.80 3.66 252 .36 95 4.69 3 31 Cr I 4689.37 186 3.12 5.18 3.91 312 .36 110 4.85 0 31 Fe I 4690.15 820 3.69 4.96 4.72 3.02 254 .36 95 4.69 0

Co I 4693.19 156 3.23 5.44 4.89 3.89 181 .18 41 5.06 31 C T '407'+. 1 J 7L S7 J

<\ .jySQ J .J J

1 Q1 77A zzo . 11 Qy 414J u S I 4695.45 2 6.52 5.11 5.47 1.77 218 .14 31 5.19 0

S I 4696.25 2 6.52 5.11 5.56 1.52 226 .19 43 5.03 \ 0

La II 4699.64 .40 1.46 265 .31 79 4.77 3 32

Fe I 4700.17 935 3.69 4.96 4.71 2.82 302 .37 105 4.66 5 32

Fpc I1 4701 OS 870 D .yjy S OQ 7Z.Jo<i8 7Qf; ZZ7U .z77/ 87oz 4 80 17JZ Ce II 4702.01 .81 2.41 249 .30 89 4.76 2 32

Mg I 4702.98 11 4.34 4.16 4.33 3.09 324 .69 288 4.21 4 32

Sm II 4704.40 1 .00 6.07 4.84 1.98 243 .37 88 4.70 4 32

Fe I 4704.96 821 3.69 4.91 4.69 3.13 265 .37 101 4.67 3 32

MiIN T 1 11 78 S 77 S 71 7 QO 70fi S 1 8 z 17JZ Nd II 4706.54 3 .00 2.02 249 .56 136 4.48 4 32

Cr I 4708.04 186 3.17 4.96 4.70 4.37 249 .40 110 4.63 3 32

Ti II 4708.66 49 1.24 5.01 4.70 278 .50 148 4.50 2 0

Fe I 4708.98 889 3.64 5.10 2.88 280 .50 152 4.90 0 32

IT C 1 47nQ H / \jy .\jy OQ 871 4 80 J . 77zz 780 so 11 JZS7 4 70 0 J17z Ru I 4709.48 14 1.13 6.13 3.47 204 .05 10 5.67 1 0

Mn I 4709.72 21 2.89 4.88 4.64 3.62 249 .47 129 4.55 3 32

La II 4716.44 52 .11 2.10 218 .34 81 4.74 4 32

Cr I 4718.43 186 3.19 4.90 4.65 4.49 330 .49 171 4.48 2 32

471 Hi lyQ, 1I 7^ 1 8f^ f\ 78 ^ 77 718 Z i o 1 0 71Z

1

S IS z 17 Fe I 4721.00 409 2.99 5.00 1.98 280 .38 112 4.64 4 32

Zn I 4722.16 2 4.03 4.87 4.73 4.36 280 .55 169 4.45 5 32

Ce II 4725.09 153 .52 6.50 5.67 2.34 255 .33 87 4.74 4 32

Co I 4727.94 15 .43 5.75 .63 229 .20 47 5.01 2 0

iVlg Mo T1 47^0 n^ 1 0 4 "14 4H-OD8^1 4 f,l 1 f,! I .DZ zo /

11 77zz 4 SQ z yj Fe II 4731.44 43 2.89 4.78 4.62 1.41 291 .57 179 4.42 3 0

Ni I 4731.81 163 3.83 5.08 4.79 3.61 259 .38 103 4.66 3 0

Mn I 4739.11 21 2.94 4.93 4.67 3.56 249 .41 108 4.63 3 32

La II 4740.28 8 .13 1.92 339 .63 226 4.52 0 32

Fore Ti AlACi 'XA 4U7 ? 07 J. L I

11 .yy QQ jjy 77A zzo 4n.UZfO nu 17JZ Fe I 4741.08 688 3.33 5.16 2.10 296 .34 108 4.68 4 32

Fe I 4741.53 346 2.83 4.84 4.64 2.51 311 .52 178 4.45 4 32

Sc I 4743.81 14 1.45 5.80 5.20 4.07 212 .09 19 5.40 1 0

Fe I 4745.81 821 3.65 4.84 3.24 280 .56 166 4.44 4 32

Ce II AIAI 1 A 4/4/. 14 1 A(^ 1 .40 1 AC\ Z7D 40 11 78Zo 4 ^.0 JZ17 La II 4748.73 65 .93 6.07 5.25 2.52 286 .43 122 4.59 2 32

Fe I 4749.93 1206 4.56 5.16 4.84 3.43 242 .27 67 4.85 2 0

Na I 4751.82 11 2.10 5.50 4.98 1.58 193 .13 29 5.22 1 32

Ni I 4752.43 132 3.66 4.90 4.73 3.72 262 .39 107 4.65 2 0

Ce II 4753.65 1.28 2.38 219 .13 29 5.21 2 0

Mn I 4754.04 16 2.28 4.56 4.45 3.81 249 .64 181 4.42 5 32

Cr I 4754.74 168 3.09 4.99 249 .30 84 4.77 3 32

Cr I 4756.11 145 3.10 4.90 4.69 4.55 267 .42 118 4.60 3 0

Ni I 4756.52 98 3.48 4.80 4.63 4.14 249 .47 139 4.54 2 32

130
Table A

Spect

W ave- length

Mult EP Log Log Log HW Rc W

Log

in/ iw 0 N

V I 4758.74 51 1.22 5.64 5.11 196 .10 23 5.35 1 32

Ti I 4758.91 41 .84 6.08 5.13 174 .10 17 5.35 1 32

Ti I 4759.27 233 2.25 5.06 4.79 4.40 264 .32 82 4.76 3 32

Y I 4760.98 4 .07 6.28 2.10 228 .18 41 5.06 1 0

Mn I 4761.53 21 2.95 4.81 4.60 3.71 295 .46 146 4.53 4 32

Mn I 4762.38 21 2.89 4.66 4.52 4.28 296 .59 189 4.40 2 0

Ti II 4764.54 48 1.24 5.19 4.71 273 .45 130 4.56 2 0

Mn I 4765.86 21 2.94 4.83 4.62 3.93 239 .45 115 4.59 2 32

Mn I 4766.42 21 2.92 4.73 4.54 4.13 311 .52 163 4.47 2 32

Fe I 4768.32 821 3.69 4.84 3.00 299 .56 172 4.65 0 32

Fe I 4768.40 384 2.94 4.97 2.11 299 .56 172 4.65 0 32

C I 4770.03 6 7.48 5.47 5.56 1.40 230 .19 44 5.03 2 0

Ti I 4771.10 41 .83 5.38 224 .15 37 5.13 1 32

Zr I 4772.32 43 .62 5.83 5.25 3.11 218 .28 71 4.83 3 32

Fe I 4772.82 467 3.02 4.73 2.63 249 .58 161 4.44 5 32

Ce II 4773.94 17 .92 5.75 5.13 3.03 249 .41 107 4.63 2 32

Ti I 4778.26 232 2.24 5.48 3.70 187 .13 29 5.22 2 32

Fe I 4779.44 720 3.41 4.97 4.78 2.30 218 .28 65 4.85 2 32

Ti II 4780.00 92 2.05 4.80 4.68 286 .58 174 4.43 3 32

Fe I 4780.81 633 3.25 5.68 5.23 1.47 218 .10 26 5.35 1 32

Co I 4781.43 57 1.88 5.78 5.07 2.16 202 .11 26 5.30 1 32

Mn I 4783.42 16 2.30 4.48 AAA 3.79 292 .65 209 4.36 3 32

Zr I 4784.94 44 .69 6.68 2.56 187 .12 26 5.26 1 32

Fe I 4787.84 384 3.00 5.05 A.76 1.90 249 .26 69 4.86 3 32

Fe I 4788.76 588 3.24 4.82 4.70 2.75 249 .45 125 4.57 5 32

Cr I 4790.34 31 2.54 5.48 5.07 218 .13 33 5.22 1 32

Sm II 4791.58 7 .10 6.28 1.70 229 .18 42 5.06 3 0

Co I 4792.86 158 3.25 5.08 4.85 4.44 239 .24 59 4.91 2 0

Fe I 4793.96 512 3.05 5.73 5.27 1.13 218 .09 21 5.40 1 32

Ti I 4796.21 260 2.33 5.30 4.97 3.62 218 .15 32 5.16 1 32

Nd II 4797.16 60 .56 6.28 1.95 265 .39 108 4.65 2 0

Ti II 4798.54 17 1.08 4.98 4.76 283 .50 151 4.50 2 0

Fe I 4799.41 888 3.64 5.12 2.49 273 .39 111 4.84 0 32

Nd II 4799.42 2 .00 1.10 273 .39 111 4.94 0 32

Fe I 4800.65 1042 4.14 4.82 4.59 3.42 261 .37 113 4.65 2 32

Fe I 4802.88 888 3.64 4.84 2.93 249 .37 98 4.68 3 32

La II 4804.05 37 .23 6.08 1.52 280 .48 142 4.53 2 32

Ti II 4805.10 92 2.06 4.69 2.92 311 .64 223 4.33 3 32

Zr I 4805.88 43 .69 6.38 2.64 186 .15 27 5.20 2 32

Ti II 4806.33 17 1.08 5.90 271 .21 59 4.94 2 32

Ni I 4807.00 163 3.68 4.84 4.75 3.87 279 .35 106 4.68 3 32

Fe I 4807.73 688 3.37 4.90 4.74 2.32 255 .30 82 4.78 3 32

Fe I 4808.16 633 3.25 5.20 4.89 1.83 216 .17 41 5.08 2 32

Fe I 4809.94 793 3.57 5.38 4.98 1.86 201 .12 24 5.26 3 32

Zn I 4810.55 2 4.08 4.76 4.76 4.54 276 .46 141 4.54 5 32

Nd II 4811.34 3 .06 5.70 4.96 1.76 268 JO 140 4.52 5 32

Ni I 4812.00 130 3.66 5.28 4.93 2.92 233 .22 58 4.94 3 32

Cr II 4812.36 30 3.86 5.07 4.84 1.81 259 .31 90 4.75 3 33

Fe I 4813.11 630 3.27 5.30 1.73 248 .17 45 5.06 2 33

Co I 4813.48 158 3.21 4.97 4.41 226 .25 63 4.89 3 32

131
Table

A

jpect WavelengthMult IT

O Lr

— Log— Log

(r,/x)

Log

U If HIV

D

«<-

WTV/

— Log

Q /V

Nd II 4817.20 .14 6.51 1.61 244 .26 65 4.87 2 0 C I 451 1 .5 1 cJ 7 /IS / .46 S 71 J. / 1 lis 1 . 1 J

99Q ZZ7 1 7

.1 / 1Q37

C OQ J.U7 z U

XT^ TT JNa II 4oio.yo .447/ 1 1 6 1 . ID 948 Z4o 1 8 . 1 0 4o S OI J.U3 z

1/1 34

XT^ TT INU II

J 1 UZ.4Z .Do 9 1 8 Z.lo 11 1 J 1 1 A S .4 J 1 17 13/

A S7 4. J /

•J3

9/1 Z4

XT; t JNl I J 1 UZ.7 / 4740 1 f;8 1 .Do S 08 J .Uo 44. 68Do 1 17 1 . J / 198 jZo

AA .44 1 ^1 101A S4 4. J4 9z 94Z4

Cu I 5105.55 2 1.39 4.79 4.52 2.20 319 .60 207 4.39 2 0

Fe I ^ 1 no f^f. J 1 U7.DD 11 080 Uo7 44. jU10 4.0 4 87/ 4.DD 4 66 1 6S j.DJ 989 ZoZ . 10J7 lis 1 1 J 4 6S 4.0J 9z u re 1 ^110 41 J I 1 U.^ 1 11 00 4 fil 4H. 14jH .J171 117 jj / . 70/ u 901 Z7l 44.Z9SJ 1J nu 7r TT l-X 11 J 1 1 L.Lo OSyj 1 .DD S 81 J. 01 JS . 11 SJ 9Z. 71/ 1 978 Z / o .47 40 11 JSSJ 44. JZS9 1J 94Z4 V TT I 11 S 1 1 Q 1 9 90 .yy 00 JS Sfi . JD 4 06 9Z.Ul01 J170/ 7 . JDS6 9Z 11 07 4 40 9z 94Z4

Fe I 5133.70 1092 4.18 4.49 4.61 347 .62 237 4.34 5 24

rirl OU TT11 3 1 ^v.oH 11 1 s 1 J 11 .JoS8

JS . 11 0U 9Z.7JOS 1ill77 1 1 . 1 1 01 7 s 1 1

j.ji

nu 94Z4

rC 1 SI 41 7S 1 1 4 9 49 4H. 7f. /D 4H. J7SQ 9Z. 1IH4 1S8 J Jo . JUso 11 8007 4 47 1J 94Z4

Threo T1 D3 9z.zu90

JS . ISJ J 4 04 964 ZD4 .Zo 98 76/o 44.081J 9z u

Ffi re

T1 S 1 4S 11 J 1 "4 J . 1 1 DO 9Z.ZU90

JS .u07/ 44. 71/ J 1 11 1 .J 1 90S Z7J .44SJ 114141 44. JDS6 9z u

Ti I 5145.47 109 1.46 5.14 4.81 3.52 264 .28 76 4.83 1 0 re 1 J 1 \}\i.Ly 11 00 4 f.S 4.DJ 44. 19jZ .Uj oi 141 j41 .DO 66 91S Z J J 44. j414 /I 4 9SZJ

V\\! uy TT11

J 1 yjy . 1 1 . 11 0u fi 1 1 D. 1 1 11 .40 46 91S Zj J .lU 1 0 97Z / J.Zo S 98 11 u re 1 S 1 71 f\\ If. 11 .Ho 48 4H.JSI1 9Z.H41J 147 jt / . 71/ 1

979 Z / Z 4H.ZO98 /IH 9SZJ

iVlg 1 S 1 79 f.8 z 9Z. 71/ 1

J.Dl 1 filJ1 -O6SJ 1J .J11J 670 O /U .00 88 601 D7J J.O/ 1 87J 9SZJ Fe I 5180.07 1166 4.47 5.02 4.78 3.77 253 .27 78 4.84 I 25

i>U 11 .OD 8f^ f>O.UD06 9Z. 1170 147 jnZ .J11J 11 99zz 4H.OO68 1J 9SZJ

iVlg 1 SI 81 fin

L 9z. 79/ z J1 SI .J 1 1J . JDS6 1J .JssJ 779 / / Z .7OSJ 001 7UJ 1J.76/D

AH 9SZJ Ti11 IT11 SI 8S Q1 11 .07 80 4H. OS7J 140 J*+7 .JSIJ 901 ZUl 4 44 1J 9SZJ Mii>l T1 SI 8fi SQ 90S 1J.7U00 S SI J. J 1 JS .UZ 09 9Z.7700 11 007U . 11 4H

97z / JS . 11 07 11 9SZ J Ce II 5187.45 15 1.21 5.97 5.18 3.46 304 .46 151 4.54 2 25 re 1 JS 11 o871 .yL 09 1 019 A 1 4 4. 14 S 09 J.UZ A4.D67/ 1 io J. J7 978 Z / o IS .J J 1IU7OQ 4.07 4 60 9z 9SZJ To TT

11

J

SI1 88oo.Zt94 OSyj 9Z.4j4S 6D.UZ09 1J.O87/ 901 Z7l .z97/ 870 / 4 81 4.0 1 11 9SZ J Fe I 3171 S 1 Q 1 Af^ .HO 181 JOJ 1J.U404 A SI 4. J 1 A 17 4. J / J.1 76/O 404 474 . 7S/ J 181 JOl 44.ZJ9S u 9SZJ

TiT 11 1 S 1 Q9 Q7 4 .UZ 09A 81 4.olA SI 4. J J 9Z. 76/O 11Jl70 S7 .J / 11 067D 44.4Z49 1J

AU

Ti I 5194.04 183 2.10 5.72 5.03 3.64 228 .12 26 5.26 3 25

Fe I S 1 Q4 Q4 If; 11 .JO SA

A f.9 4.DZA4.441J 9Z.U700 180 JOU .067/ 961 ZOJ 44. jU10 9z 9SZJ re 1 SI OS 47 1 009 4H.ZZ99 4H.DD66 4*+. JoS8 4H. J*T 14 104 jUH . JHS4 11 89OZ 4 46 11 9SZJ re 1 S 1 Qf^ 10 1 001 4H.ZD96 4H.oZ89 4H. 71/ J 4 07 970 Z / 7 .HZ 49 11 90ZU 4H.DZ69 11 9SZJ Fe II SI 07 S7 4047 j.Zj 1 91 4 81 4.0 1 4 6S 4.DJ 11 .OO 88 1SS J J J 61 .D 1

910 Z jU 44. ISJ J 9z 9SZJ Fe I 5198.71 66 2.22 4.78 4.51 2.22 304 .57 174 4.45 5 25 V TT I II ^90n /19 JZUU.4Z 90ZU QQ .yy CIS J. 1 J

4.07 9 /^7 Z.D / 1/11 343 70 . /U 9Q1 Z7I

A 9S 4.Zj 3 AU

11 I jzUl.lU 1 B 1lo3 9 no z.uy

C A7 J.O/ J.UD 1 so J. jU 1 QO I7U HQ .U7 1 8lo s 40 J.4U 3 9SZJ Fe I ^909 1/1 JZUZ.34 DO 9 1 Q Z.lo /I SI 4. J J A IS 4. J J 9 SI Z. JJ 149 34Z ^6 .DD 9S1 Zj3 A 11 4.31 cJ 9SZJ cr I ^9nA ^9 jZUd. jZ ZUO J. 43 S /IQ J. 47 S OS j.Uj 960 ZDU 94 .Z4 6404 4 01 4.7I 9Z AU Fe I 5207.94 880 3.63 5.44 2.52 291 .27 88 4.81 1 25

11 I O1 A "20 jZlU.iy 4 A 70 4. /o /I c 1 4. J 1 9 C9 Z.oZ 3U4 .J

J 1 87 10/

A AA 4.44 -J3 9SZJ

TT ll II jZI 1.j4 1U3O CO z.jy

C 9C J.Zj /I Q< 4.0J 9 /I9 Z.4Z 3U4 .37 1 IS 13jA fS> 4.0Z 3 9SZj

XT^ TT JNa II 44 90 .ZU

A o^ o.Ud 1 Q9 1 .7Z 110 33U Af- .4D 1 S9 1 jZA S4 4. J4 13 9SZj

L-O I 010 "TA 3ZlZ. /U 1 7n 1 /U i.jl J. jy

A QC 4.yj 4.43 901 ZU3 1 f. .10 1133 s 1 J. 10 11 9SZj

Pr II 5219.03 37 .79 6.32 2.78 240 .28 71 4.85 3 26

Ti I 5219.70 4 .02 5.32 4.79 1.82 253 .27 70 4.86 1 26

Fe I 5223.19 880 3.63 5.30 4.91 2.51 215 .20 48 5.02 2 26

Fe I 5225.53 1 .11 4.89 4.52 354 .52 168 4.49 3 26

Fe I 5228.41 1091 4.22 4.94 3.83 316 .48 152 4.53 3 26

132
Table A

Spect

Wavelength

Mult EP -Log

( W/ l\ 1 (IV r^lK) —LogI XT/ l\ \ [IT e/K) Log HW Rc W

— Log Q N

Fe I 5229.86 553 3.28 4.63 3.53 303 .55 180 4.45 4 26

Fe I 5232.95 383 2.94 4.18 4.20 4.11 392 .70 306 4.23 5 26

Nd II 5234.20 74 .55 5.82 5.06 2.43 392 .50 209 4.45 2 26

Fe II 5234.62 49 3.22 4.81 4.60 1.95 328 .61 219 4.38 2 26

Ti I 5238.56 37 .85 5.54 2.53 202 .17 38 5.11 2 26

Cr I 5238.97 59 2.71 5.52 5.05 2.83 151 .14 27 5.19 1 26

Sc II 5239.82 26 1.45 4.98 4.70 3.22 303 .53 179 4.47 5 26

Fe I 5253.48 553 3.28 4.85 4.65 2.92 303 .45 135 4.58 4 9

Nd II 5255.51 43 .20 5.88 1.99 354 .55 230 4.40 2 9

Fe II 5256.89 41 2.89 5.47 4.98 303 .29 89 4.79 4 9

La II 5259.38 21 .17 5.14 1.22 285 .36 107 4.69 3 0 Pr II 5259.74 35 .63 6.24 5.44 2.89 286 .37 111 4.68 3 0

Ca I 5260.39 22 2.52 5.27 4.94 1.82 291 .18 52 5.03 2 9

Ca I 5261.71 22 2.52 4.73 4.58 2.99 303 .50 155 4.52 4 9

Fe I 5263.31 553 3.26 4.64 3.53 349 .57 223 4.40 3 9

Fe II 5264.80 48 3.33 5.07 4.81 1.46 303 .44 147 4.57 1 9

Fe I 5266.56 383 3.00 4.32 4.27 3.81 384 .68 285 4.27 5 9

Fe I 5267.28 1146 4.37 5.32 265 .15 39 5.14 1 9

Fe I 5269.54 15 .86 4.04 3.96 2.37 518 .82 441 4.08 3 9

Cr I 5272.01 225 3.45 5.40 4.96 3.84 258 .21 55 4.98 2 0

Ce II 5274.24 15 1.04 5.91 5.13 3.24 286 .45 139 4.57 5 9

Nd II 5276.88 81 .86 6.55 2.24 265 .35 102 4.71 4 9

Fe I 5277.31 584 3.27 5.85 253 .11 27 5.30 1 9

S I 5278.96 4 6.86 5.91 1.62 241 .12 29 5.26 1 0

Fe I 5281.80 383 3.04 4.51 4.40 3.47 329 .60 212 4.39 5 9

Ti I 5282.38 74 1.05 5.38 4.90 2.29 278 .14 39 5.19 2 9

Fe I 5283.63 553 3.24 4.40 3.92 404 .66 283 4.27 3 9

Fe II 5284.09 41 2.89 4.90 4.74 1.24 312 .50 166 4.50 2 0

Fe I 5285.12 1166 4.43 5.33 4.95 3.40 253 .18 51 5.04 1 9

Fe I 5288.53 929 3.69 4.98 2.97 298 .35 111 4.69 4 9

Y II 5289.82 20 1.03 6.33 1.49 278 .45 136 4.58 5 9

La II 5290.83 6 .00 6.02 5.21 1.18 281 .36 114 4.68 5 9

Nd II 5293.17 75 .82 5.72 2.87 399 .53 217 4.43 2 9

Fe I 5295.32 1146 4.41 5.29 324 .18 53 5.03 1 9

Ti I 5295.78 74 1.07 5.72 5.02 2.48 253 .11 29 5.30 1 9

Cr I 5296.69 18 .98 4.75 4.53 2.36 283 .53 157 4.50 5 9

Ti I 5300.01 74 1.05 5.40 5.04 253 .13 31 5.22 1 9

Cr I 5300.75 18 .98 4.98 4.64 1.76 341 .37 127 4.65 1 9

La II 5303.54 36 .32 6.33 1.60 298 .42 130 4.61 1 9

Cr II 5305.85 24 3.83 5.33 4.99 1.72 291 .31 90 4.77 3 9

Nd II 5306.47 .86 6.73 2.11 265 .24 60 4.93 2 9

Fe I 5307.37 36 1.61 4.79 4.50 1.26 303 .54 175 4.47 5 9

Cr II 5308.44 43 4.07 5.28 4.98 1.95 253 .28 76 4.84 3 9

Cr II 5310.70 43 4.07 5.58 5.23 1.66 252 .17 43 5.09 1 0

Sm II 5312.23 .33 1.03 232 .06 14 5.59 1 0

Cr I 5312.88 225 3.45 5.45 5.04 3.66 239 .10 24 5.35 2 0

Cr II 5313.59 43 4.07 5.18 4.96 2.20 329 .40 129 4.62 3 9

Fe I 5315.07 1147 4.37 5.19 4.91 3.20 256 .19 49 5.03 1 0

Nd II 5319.82 75 .55 5.68 2.46 374 .53 187 4.46 5 9

Y II 5320.80 20 1.08 6.03 1.41 277 .30 86 4.79 1 0

133
Table A

Spect

Wavelength

Mult tr — Log

(r,j,/\) — Log

iWJk)

Log I I TT/ — Log Q

A/" /V

re I sio 1 11 J jZl . 1

1

1 1 DJ 4 4^ S 09 44,087/ fA7 J .DZ 784 Zo4 ^4 . j4 11 01Ul 4 77 7z nu re I

II1I ?Z 7 78 44. 9S"J 4 fi9 1 7f. 1 . / D 791 Z7

1

.4411

11 74Z4 44.0Zfi7 4 Q

r>»- TT rr II ^J')') 78 J jZZ. /o .4o 48 D.44^J 7Z. J4S4 791 Z^l ^7 11

11 ^J 44.D / Qy re I -J J Z't . 1 7 J J J

^J .Z711 44.ZW70 44.Z171 44.ZU70 jD / .Do A8 ZDJ) 44. "^O JU 4 Q

Fe II 5325.56 49 3.22 5.07 4.83 .98 283 .41 136 4.60 3 9 re 1 J JZD. 1 J 407 ^ 07 s 77 "^79 77 7"? 4 91 11 Qy re 1 7Q 1 1 47 4H.H411 J .\jy J . i u 71 S 09 11 7/ S 40 11 qy Pr I J J Ly * 1 ^ Q4 7 91 4H. 83OJ 4 fiS ftO 7S^ 97y 1 4 70 0 qy

Fl=> re T

1 S^9Q QQ J J L^y *yy 1 078 4 07 4 . QSyj J .Hy 4Q jyy .DO 38 1 SS 4 S9 J qy Ce II 5330.58 13 .87 6.25 5.33 2.81 303 .37 113 4.67 2 9

Cn T ^331 46 39J y 1 78 J5 . JJ55 7 33 765 Z.VJ_' 70 J50\J 5 07 11 qy Fpr c t1 J D J ^.yyj 3f« 1 56 4 74 1 37 379 D L.y .JO 58 770 4 40 1 qy Cr TT J J JH-.OO 4 07 4 90 7 07 7S3 ^J _J .J31k 91 4 77 7Z. qy Ti11 TT11 S^^^^ Rl 11 .Jo SR 4'4-. RR00 4 ^i7 7 OS .\J\J Z. 1 u 4 9z. Fe II 5337.73 48 3.23 5.18 298 .35 113 4.69 2 9

Ti T 1 i 1 S338 33 35 83 5 61 5 06 316 . 11 J3 38 5 72 1X qy Fpr c t

1

1 1 1 1 UiL 4 4^ S 77 S 71 740 1 1

. 1

1

74Z-t S "^0 J . JU 11 qy Fp t .J J 17 . ;7*T J J J) 4 57 4 44 3S4 67 730 Z.-J v 4 37 J 9y Fpr c t

1 37 1 .U 1 4 47 7 14 366 . 73/ J 797 4 75 XJ 9y Co I 5342.70 190 4.02 5.27 4.96 4.77 324 .19 61 4.99 2 9

Cr t 5345 81 11 80 11 .yjyj 00 4 70 4 4S 7 74 J3791 y 65 267 4.30 4 9

Ce TT 5347 81 74 1 97 765 1 6 47 5 1

1

11 qy Cr T 5348 37 1 8 1 00 4 76 4 54 7 44 778 56 174 4 46 4 9

Ca T ^^49 47 33 7 71 4 77 4 fi4 314 49 1 64 4 51 0

Co I 5352.05 111 3.58 5.41 4.93 4.47 254 .17 44 5.09 2 0 Prn TT11 ^357 41 48 61 73 7 71 760 70 53 J5 .\J011. 2 0

Fpr c t1 J D jj .jy 11 n^^7 UDZ 4 1 0 4 RS .yjj 74Q 4 50 0 qy Pp TT Vw-C 11 1

J

.00 RR ^ 70 .\jj 74Q 4 4S 0 qy

1 J J . / ^ 1 9

1 J u. u ^J . 7Q/ y 7^Q OQ 71 S 40 7 0

Nd II 5356.98 80 1.26 6.43 2.73 316 .34 114 4.70 2 9

Tp TT11 11 . 78/ 0 7 81 778 z. / 0 1

6

47 J5 ,\jy 09 qy NH TT S'^f>1 17 . JU 1 43 760 Z.V/V/ . 70ZrW J53J 5 01 0

>Jrl TT JS^^>1 jDl .JSI1 74 .Do ^^8 J.S 78/

0

7 '^S ^41 .J J 11 93yJ 4 4^^ 1

0

t S^A4 88 1 1 Af\ 1 1*+D 4 44 4*+.Dl f\\ 4 M ^1D i\j 110181 4 4S 1

0

Fe I 5365.41 786 3.57 4.84 3.37 309 .48 163 4.52 2 10

Fpre t1 3 jD / .'t / 1 1*40 A 41 4.4

1

A ^T, 4. J J 44. 77/

Z

jvy ^19 .JS7/ 70S ZUJ 4 47 1

0

1 u reFp tI jjKyy.yj 1 140 4.:? / A4.4Al/ A A') 4.4Z /I4.0U80 J41 .01 Al 7^1 Z J 1 44. ^7J /

11

11 0yj re I r> J / 1 .4y 1 c

1

J

.yo /I4. ZD /I 1 1 4.11 7 1 "J Z. 1

J

4JA^l/ .oU 80 4UZ 407 A4. 11 ^J 44 qy Fa T re I ji 1 i. i\j 1 loo 4.4 /I M/

/I Q^^ 1j.y01/ "lOO ^4 .04 11 09\jy 44. 71/ 1 J

11 0u La II 5377.08 95 2.30 6.13 5.33 3.41 270 .25 69 4.89 1 0

jvin I J J / /.DJ 4Z "J 8/1 S 08 A4. 7A/O A4.ZU70 774 Z /4 .z77/ 1 D 44.0-' 8S 7 re I CT-VQ CO yzo A Q8 4. 70 /I 7^ 4. / J 7 QS "^1 1 J 1 1 41 .4

1

11 77z / 44.DZ67 1.J 1lU0

L. I j3oU.34 i i /.Do J.3Z 7 0'\ ^41 j41 7*; .Z J 8800 44.o484 11

11 0u Fa T re I j3o3.3 / 1 14D /111 4. J 1

/I /IT 4.4Z /I /l"? 4.4 J/t QO j41 .O J ZJO 4. JD 7z 1lU0

IT iNU 11 J 30J.07 . 74/ 4 0. JO 1

1 ,yo 98 798 ^4 11 08uo 4 71 11 101 yj Fe I 5389.46 1145 4.41 4.78 4.66 4.12 329 .46 158 4.54 2 10

Fe I 5391.49 1062 4.15 4.85 3.65 405 .47 205 4.48 5 10 Mn I 5394.67 1 .00 4.86 4.50 .46 329 .44 154 4.56 4 10 Fe I 5395.25 1143 4.44 5.43 5.09 291 .16 51 5.07 1 10

Fe I 5397.13 15 .91 4.35 4.24 1.85 392 .77 341 4.20 2 10

134
Table A

Spect

Wavelength

Mult — Log — Log Log

(gf^) p — Log nV

re i S3Q7 60 841 3.63 5.35 4.95 256 .17 44 5.09 2 0

tT/^ T r^c 1 J J yo. cy 1 145 4.44 4.85 4.72 4.00 341 .41 146 4.59 3 10 Mn T -J J yy.^y49 42 3.85 5.14 4.87 3.90 324 .20 64 4.96 1 10

Fp t 5400 51 1 145 4.37 4.68 4.31 329 .56 209 4.42 1 10 Y II 5402.78 35 1.84 5^65 2!85 303 J3 170 4^48 4 10 Fe T 5403.82 1029 4.07 4.95 4.70 3.77 300 .40 126 4.63 1 0

Cr T 5405.00 191 3.37 5.73 5.20 3.52 243 .10 24 5.35 1 0

Fe I 5405.35 1162 4.39 5.10 4.83 3.89 275 .27 77 4.85 2 0

Fe I 5405.78 15 .99 4.31 4.31 1.98 405 .77 348 4.19 2 10 Fe I 5406.77 1148 4.37 5.16 4.93 278 .21 61 4.96 3 10 Fe I 5409.14 1147 4.37 4.98 3.42 341 .49 176 4.69 0 10 Ce II 5409.22 23 1.10 3.21 341 .49 176 4.69 0 10

Cr I 5409.79 18 1.03 4.55 4.41 3.03 329 .66 251 4.33 2 10 Fe I 5410.91 1165 4.47 4.51 4.56 4.78 331 .56 199 4.43 3 0

Fe II 5414.09 48 3.22 5.24 5.03 .95 278 .34 104 4.72 1 10

Fe I 5415.20 1165 4.39 4.41 4.48 4.94 329 .62 224 4.38 3 10

Nd II 5416.38 80 .86 6.73 1.92 266 .22 60 4.96 3 0

Fe I 5417.03 1148 4.41 5.17 4.96 3.18 298 .20 61 4.98 1 10 Ti IT 5418.80 69 1.58 5.04 4.76 1.63 329 .50 179 4.49 2 10

Mn I 5420.36 4 2.14 4.84 4.50 2.52 316 .40 137 4.61 5 10

Fe II 5425.27 49 3.20 5.05 4.93 .95 299 .39 123 4.65 2 0

Ti I 5426.26 3 .02 5.99 5.13 1.25 201 .09 16 5.40 2 11 Fe I 5429.70 15 .96 4.28 1.95 556 .77 465 4.07 4 11 Nd II 5431.54 80 1.12 6.08 2.53 342 .27 98 4.79 4 11 Mn I 5432.55 1 .00 5.07 4.60 .03 330 .34 112 4.70 2 11 Fe I 5432.96 1143 4.44 4.88 355 .41 147 4.59 2 11 Fe I 5434.53 15 1.01 4.47 4.35 1.77 387 .71 294 4.27 5 11 Ni I 5435.87 70 1.99 5.07 4.71 1.85 268 .34 101 4.73 3 11 Fe I 5436.59 113 2.28 5.17 4.76 1.02 285 .31 91 4.77 1 0

Nd II 5442.27 76 .68 1.84 304 .32 100 4.75 3 12 Co I 5444.59 196 4.07 5.59 5.20 4.43 164 .08 15 5.46 1 12 Fe I 5445.05 1163 4.39 4.65 4.62 4.41 334 .53 204 4.45 4 12

Fe I 5446.92 15 .99 4.36 1.84 404 .78 360 4.18 1 12 Nd II 5447.56 1.04 1.80 290 .25 73 4.88 2 12 Ti I 5453.65 108 1.44 6.13 5.29 2.60 178 .07 13 5.52 1 13 Co I 5454.57 195 4.07 5.62 5.26 4.34 178 .09 16 5.40 1 13 Mn I 5457.47 4 2.16 5.70 5.18 1.69 178 .08 15 5.46 1 13 Ti I 5460.50 3 .05 5.81 4.97 1.37 251 .13 33 5.22 1 0

Fe I 5460.91 464 3.07 5.89 5.26 250 .12 30 5.26 1 0

Fe I 5461.54 1145 4.44 539 5^01 3.10 241 .20 52 5.01 2 13 Ni I 5462.49 192 3.85 5.14 4.89 3.49 329 .29 100 4.77 1 13 Fe I 5462.97 1 163 4.47 4.77 4.63 4.22 304 .51 162 4.51 1 13 Fe I 5463.28 1 163 4 43 4.67 4.62 4.37 279 .54 170 4.48 1 13 Fe I 5466.40 1 144 4 37 4.86 4.72 3.72 304 .46 155 4.55 3 13 Fe I 5466.99 784 3.57 5.28 2.49 248 .25 64 4.91 1 13 Ce II 5468.37 24 1.40 6.19 5.42 3.20 273 .36 109 4.70 2 13 Mn I 5470.64 4 2.16 5.08 4.56 2.39 293 .33 114 4.71 2 13 Ti I 5471.20 106 1.44 5.93 5.19 2.90 252 .13 35 5.19 1 0

Ce II 5472.30 24 1.25 6.26 3.04 303 .38 133 4.64 1 13 Fe I 5473.91 1062 4.15 4.84 4.67 3.70 303 .45 160 4.55 1 13

135
Table A

Spect

Wavelenjjth

Mult EP

— Log

{W@lk)

-Log Log HW Rc W

-Log Q

Nd II 5474.76 .99 6.56 1.84 227 .21 54 4.99 2 13 Ni I 5476.94 59 1.83 4.52 3.16 360 .69 285 4.28 2 0

La II 5482.27 4 .00 .82 252 .29 78 4.83 1 13 Sc I 5484.62 16 1.85 6.26 4.07 235 .04 9 5.78 1 0

Nd II 5485.70 79 1.26 6.34 2.69 328 .36 119 4.68 4 13 Fe I 5487.16 1143 4.41 5.23 4.91 3.11 270 .28 81 4.83 1 13 Fe I 5487.76 1025 4.14 4.79 3.71 428 .49 222 4.45 2 13 Fe I 5488.14 1183 4.61 5.48 5.02 247 .17 45 5.15 0 13 Ti I 5488.20 265 2.40 5.48 5.02 3.90 247 .17 45 5.15 0 13 Ti I 5490.15 107 1.46 5.48 4.95 3.21 214 .14 30 5.19 1 13 Fe I 5491.84 1031 4.19 5.70 5.25 138 .08 11 5.46 1 13 La II 5493.45 4 .13 .72 332 .36 119 4.87 0 13 Fe I 5493.51 1061 4.10 5.20 2.95 332 .36 119 4.87 0 13 Fe I 5494.47 1024 4.07 5.34 4.97 2.80 201 .15 32 5.19 1 13 Ni I 5494.89 231 4.10 5.48 5.13 3.33 189 .08 14 5.46 1 13 Fe I 5496.57 1281 4.91 5.79 5.33 249 .11 27 5.30 1 0

Fe I 5497.52 15 1.01 4.63 4.41 1.25 402 .73 337 4.21 5 13 Fe I 5501.47 15 .96 4.68 4.47 1.08 389 .65 277 4.30 4 13 Cr II 5502.05 50 4.17 5.38 5.16 2.14 271 .23 62 4.94 2 13 Mo I 5506.49 4 1.33 6.00 3.69 281 .27 78 4.85 1 0

Fe I 5506.78 15 .99 4.66 4.41 1.30 404 .66 285 4.29 3 14 V I 5507.75 129 2.36 6.34 5.70 3.70 121 .05 6 5.67 1 14 Y II 5509.91 19 .99 5.46 2.05 379 .65 265 4.32 4 14 Ca I 5512.98 48 2.93 4.77 4.63 3.45 328 .45 167 4.54 2 14 Ce II 5516.08 1.61 2.70 273 .16 42 5.12 2 14 Mn I 5516.77 4 2.18 5.13 4.59 2.30 354 .28 107 4.77 2 14 Y II 5521.59 27 1.74 6.00 2.46 349 .46 180 4.52 2 14 Sc II 5526.81 31 1.77 4.86 4.67 3.77 328 .63 217 4.41 5 14 Y I 5527.54 12 1.40 3.49 258 .15 39 5.15 2 0

Mg I 5528.39 9 4.34 4.28 4.33 3.11 354 .72 292 4.28 2 14 Co I 5530.78 38 1.71 5.60 4.94 2.14 264 .18 48 5.06 2 0

Mo I 5533.01 4 1.33 5.90 3.52 280 .26 75 4.87 1 0

Fe II 5534.86 55 3.24 4.94 4.69 1.55 354 .52 208 4.45 1 14 Fe I 5543.18 926 3.69 4.96 4.66 2.99 327 .38 138 4.63 4 15 Fe I 5543.93 1062 4.22 4.94 4.77 3.49 383 .37 142 4.63 1 15 Y II 5544.61 27 1.74 5.84 5.33 2.46 318 .48 172 4.52 1 15 Y II 5546.03 27 1.75 5.93 2.34 339 .52 194 4.47 2 15 Fe I 5546.51 1145 4.37 5.02 4.81 3.52 250 .31 89 4.78 1 15 Fe I 5547.00 1061 4.22 5.28 4.92 2.89 224 .22 52 4.99 1 15 Nd II 5548.47 73 .55 6.35 1.48 345 .27 102 4.79 1 15 Fe I 5553.59 1161 4.43 5.14 3.41 315 .30 98 4.77 3 16 Fe I 5554.90 1183 4.55 4.74 4.12 306 .45 146 4.57 2 16

Ce II 5556.97 1.80 3.18 253 .17 45 5.09 1 16

Fe I 5560.23 1164 4.43 5.10 3.55 251 .28 76 4.85 2 16

Fe I 5562.71 1163 4.43 5.03 3.70 324 .38 135 4.64 1 16

Fe I 5563.60 1062 4.19 4.78 4.56 3.66 293 .49 154 4.54 5 16

Fe I 5569.63 686 3.42 4.54 4.46 3.82 378 .64 280 4.30 2 17 Mo I 5570.46 4 1.33 5.93 3.18 348 .19 66 4.98 1 17 Fe I 5572.85 686 3.40 4.43 4.36 4.03 504 .67 342 4.21 2 17 Fe I 5576.10 686 3.43 4.69 4.58 3.44 328 .59 251 4.37 4 17

136
Table A

Spect

Wavelength

Mult EP — Log — Log Log HIV Rc r

— Log

{IV JK) Q

P/» T J J / / .UJ 1 "^1

4

5 03 5 63 5 24 202 1 0 22 5 35 11 1

7

1 / Mi T SS78 7"^ 47 1 68 J5 .\jO 08 4 70 1 4Q 353 45 11 68UO A 54 11 7/ Co T J J O i .7Q7/ A. 1 1 52 4 79 4 61 3 04 331 51 11 81O 1 4'~r 49 0

Fe I 5584.77 782 3.57 5.24 4.83 2.56 296 .33 102 4.74 2 0

Fe I 5586.76 686 3.37 4.36 4.36 4.09 378 .68 286 4.29 5 17 5588.76 21 2.52 4.60 4.49 3.96 378 .64 267 4.32 5 17 Ni T 5589 38 205 3.90 5.35 5.05 3.28 240 .17 40 5.12 2 17 Ca T 5590.12 21 2.52 4.81 4.66 3.04 353 .49 186 4.50 3 17 Fe II 559L38 55 3^27 5^90 5^60 256 !l2 31 5^26 2 0

Ni I 5592.28 69 1.95 5.05 1.97 353 .44 176 4.54 3 17 Ni I 5593.74 206 3.90 5.12 4.90 3.56 358 .30 98 4.77 2 17 Fe T 5598.30 1 183 4.65 4.83 4 33 479 .64 326 4.43 0 17 5598.49 21 2 52 4.68 3.53 479 .64 326 4.43 0 17 Ca I 560L28 21 2.52 A.15 4.51 3^06 366 ^53 218 4.44 2 17 Fe I 5607.66 1058 4.15 5.63 5.11 262 .15 39 5.15 2 0

Fe I 5608 98 1 108 4.21 5.82 5.14 256 .12 31 5.26 1 0

Ce IT 5610 26 26 1.05 6.05 2.56 378 .42 169 4.56 2 17 CeV-^ W IT11 5613.69 32 1.42 2.57 278 .19 50 5.04 1 17 Nd II 5614J0 87 1.04 L79 353 !27 101 4^95 0 17 Ni I 5614.78 250 4.15 5.15 3.85 252 .23 68 4.93 1 17 Fe I 5618.65 1107 4.21 5.13 4.85 3.54 278 .30 91 4.79 1 17 Fe I 5619.60 1161 4.39 5.29 4.94 3.26 341 .28 101 4.79 1 17 Fe I 5624.55 686 3.42 4.60 3.57 353 .57 226 4.41 2 17 Ni I 5625.33 221 4.09 5.18 4.91 3.66 285 .26 76 4.87 2 0

Fe I 5633.97 1314 4.99 4.92 4.81 4.61 353 .39 147 4.61 1 17 Fe I 5635 85 1088 4.26 5.27 4.92 3.34 271 .19 52 5.03 1 0

Fe I 5636.71 868 3.64 5.52 5.03 2.56 264 .15 40 5.15 1 0

Fe I 5638.27 1087 4.22 4.88 3.77 325 .44 153 4.57 3 17 Sc II 5640^97 29 L50 5'l6 4.74 2^58 312 A5 155 4^56 2 17 Fe I 5641.46 1087 4.26 4.95 4.72 3.62 321 .35 117 4.69 2 17 Ni I 5641.88 234 4.10 5.37 5.05 3.39 262 .17 48 5.08 2 19

Si I 5645.61 10 4.93 5.21 2. 10 280 .24 74 4.90 2 19

Co I 5647.23 112 2.28 5.71 5.06 2.69 265 .12 31 5.26 3 19

Ti I 5648.57 269 2^49 5.15 5^23 3^92 204 .11 25 5.30 2 19

Fe I 5650.01 1314 5.10 5.23 4.97 4.34 274 .20 56 5.01 2 0

Fe I 5650.71 1314 5 08 5.22 4.93 4.14 294 .23 72 4.91 4 19

ITFpC t1 Sf^SI 47 11 1 f^^ 1 U 1 A Al JS .\JO 08 1

4

D 1 J5 .vy19 11 n

II1I 08yjo A lf\ S ^7 A Q8 ^ ^0 1 7 5 05 1 7 Fe I 5653.89 1159 4.39 5.20 4.91 3.39 305 .21 69 4.95 2 19

Sc II 5657.87 29 1.51 4.95 4.72 3.08 306 .55 193 4.46 4 17

Ff» T Sfifi7 1 087 4 1 8 4 7Q 4 1 S 9Q7 L^y 1 47 1 57 4H.J55J 7 11 8o Cr T j.t J JS .L\. 91 4 QO 711, . 11 Qy 51 5 04 "1 11 8o

«;i T JUDJ. J J 4 Q? J . 1

J

4 88 7 1 8 74 8Qoy 4H.O85J

"1 70

JDDO.DO J.S 41HI 94S 4? 5 1 7 11 8o Sc II 5667.16 29 1.50 5.36 4.86 2.40 297 .40 125 4.64 2 18 Sc I 5671.81 12 1.45 5.61 5.04 4.11 261 .13 34 5.22 2 0

Si I 5675.73 5.62 5.67 253 " .18 49 5.06 1 21 Fe I 5679.02 1183 4.65 4.99 4.83 4.14 283 .31 90 4.79 3 21 Ni I 5682.20 232 4.10 5.04 4.85 3.95 328 .26 93 4.83 1 21 Na I 5682.63 6 2.10 4.74 4.53 3.08 303 .49 167 4.52 1 21

137
Table A

J,o pCCt

Wavelength

Mult iVl U1

1

EP — Log -Log

(WJk)

Log HW -Log V

Ce II 5683.76 1.42 2.50 252 .15 36 5.17 1 21 Sc II 5684.19 29 1.51 5.19 4.85 2.67 327 .46 160 4.55 2 0

Si I 5684.48 11 4.95 4.96 4.82 2.53 310 .37 120 4.68 2 0

Fe I 5686.54 1182 4.55 4.90 4.19 353 .39 151 4.61 1 21 Sc I 5686.84 12 1.44 5.68 4.01 260 .12 31 5.26 2 0

Na I 5688.19 6 2.10 4.67 4.48 3.33 346 .55 204 4.44 2 0

Nd II 5688.52 79 .99 2.50 318 .41 137 4.62 1 0

Ti I 5689.47 249 2.30 5.71 5.18 3.83 240 .13 31 5.22 1 21

Si I 5690.42 10 4.93 5.03 4.87 2.32 366 .26 92 4.83 4 21 Fe I 5691.51 1087 4.30 5.18 3.44 278 .28 76 4.85 4 21 Ni I 5694.99 220 4.09 5.14 3.80 278 .27 87 4.83 2 21 S I 5696.63 11 7.86 6.21 246 .05 12 5.67 1 0

Fe I 5698.05 867 3.64 5.61 5.14 262 .13 34 5.22 2 0

V I 5698.53 35 1.06 5.22 3.64 434 .31 133 4.70 2 21 Sc I 5700.23 12 1.43 5.58 3.94 303 .25 78 4.88 3 21 Cu I 5700.28 2 1.64 5.58 1.42 303 .25 78 4.88 3 21

Si I 5701.10 10 4.93 5.15 4.82 2.16 303 .24 75 4.90 1 21 Fe I 5701.55 209 2.56 4.82 2.36 310 .48 178 4.52 2 21 Nd II 5702.24 .74 2.03 315 .34 115 4.71 2 21 V I 5703.56 35 1.05 5.34 4.82 3.51 279 .21 59 4.98 2 0

Fe I 5705.48 1087 4.30 5.19 4.92 3.45 273 .21 58 4.99 2 21 Fe I 5707.05 868 3.64 5.12 2.64 341 .24 90 4.85 1 21 Mg I 5711.07 8 4.34 4.73 4.64 2.21 328 .46 162 4.55 3 21 Fe I 5715.11 1061 4.19 4.89 4.77 3.48 353 .40 155 4.60 5 21 Fe I 5717.85 1107 4.28 4.96 4.76 3.75 313 .38 125 4.66 3 0

Fe I 5720.89 1178 4.55 5.61 5.19 303 .15 47 5.12 3 21 V I 5727.02 35 1.08 5.19 4.71 3.50 302 .32 100 4.76 2 0

Y II 5728.91 34 1.84 6.10 2.34 303 .42 141 4.61 4 21 Fe I 5731.77 1087 4.26 4.99 3.66 320 .35 120 4.69 3 21 Gd II 5733.86 94 1.37 7.06 2.83 258 .10 26 5.35 3 0

V I 5737.07 35 1.06 5.72 5.03 2.91 256 .09 23 5.40 1 0

Ti I 5739.46 228 2.25 5.95 5.28 3.73 252 .07 17 5.52 1 0

Nd II 5740.90 1.16 2.19 292 .27 81 4.85 2 0

Nd II 5744.77 1.35 2.17 277 .21 62 4.97 1 21 Ni I 5748.34 45 1.68 5.34 4.86 1.02 291 .26 78 4.87 1 0

Fe I 5752.04 1180 4.55 5.01 4.84 3.91 340 .29 102 4.78 3 21 Fe I 5753.14 1107 4.26 4.87 4.73 3.99 290 .43 129 4.62 1 21 Nd II 5753.53 .20 .82 328 .33 108 4.93 0 21

Si I 5753.62 5.61 5.07 328 .33 108 4.83 0 21 Ni I 5754.68 68 1.93 4.90 4.67 2.12 302 .46 151 4.57 2 21 Ni I 5760.85 231 4.10 5.31 4.92 3.72 282 .22 69 4.94 1 21 Nd II 5761.70 1.04 1.72 323 .19 65 4.99 1 21 Fe I 5762.99 1107 4.21 4.76 4.16 323 .51 187 4.49 3 21 Ti I 5766.33 309 3.29 5.83 5.36 4.56 257 .09 23 5.40 1 0

Ce II 5768.90 32 1.32 6.76 2.82 403 .43 183 4.80 0 21 La II 5769.06 70 1.26 6.36 2.41 403 .43 183 4.74 0 21 Nd II 5769.87 1.35 2.08 252 .14 35 5.19 1 21 Nd II 5770.50 1.08 1.91 302 .22 72 4.93 2 21

Si I 5772.14 17 5.08 5.09 2.40 348 .31 106 4.75 2 21 Fe I 5775.09 1087 4.22 5.08 4.83 3.60 277 .34 101 4.74 3 21

138
Table

A

Spect

Wavelength

Mult EP

— Log —Log Log

(g/"X) HW

W

— Log

(WJk)

Q .A*

Ba I D 1 1 / .OZ

Ay 1 ^8 1 .DO

A /IB 4.45 7/18 Z48 C\A .U4 1 nlU e 78 J. /8 1 nU

"1""

— -r Fe I C'7'70 Al J 1 laAl zuy 7

z. jy J. jd

A QQ 4.yo 7/17 Z4 / 1 Q .ly /IB 48 j.Uo 7z 7 1 Zl Cu I 5 /oz.li 7Z 1 CA A Q7 4.y / A Zfi 4. JD 1 QB l.yo lie JJJ A 7

.4 / Id/

A C/1 4.j4 75 AU Cr I J /OJ.I I 1 00 loo 1 17 J. jZ ^ 18 J.JO A Q< 4.yD 1 77 i. 1 L in7 jUZ 1 fi . 1 8

eij3 e ne j.Uj 7z71Zi Cr I 5787.99 188 3.32 5.21 4.84 3.88 282 11 81 4.85 3 21 Cr I CTQrv QQ 1 00 loo 1 17 J. jZ A BQ 4. ay A If. 4. jO in7 jUZ A e .4j 1 ee 1 J J A e7 4. J / 73 7 1

Zi

Ol I C7Q-3 AT

Ay

A Q1 ^ 1 8 j.loA Q1 4.y 1 7 7n z.zu 17^ jZj 77 .Z / Q7yLA a7 4.8Z 7371Zi re I J lyj.yD 1 no*; lUoo A 77 4.ZZ ^ 17 J. jZ A Q7 4.yz 1 1 1 J. 1 1

777 LI L 7n .zu (^A D4 /I Qa 4.y5 1371Zi JNa II JOU4.UZ 79 . lA/4 7 1 1 Z. 1 J

iin J ju 18 .38 1 1/1 1 34A Ae 4.0J 73 77ZZ Fe I 5804.46 1087 4.28 5.51 252 .14 41 5.19 1 22

INI I Z J4

A 1 7 4.1/ J.lo ^18 4 Qn 4.yu 1 7^ J. / J 7Qn zyu 7 1

.Z 1

A/1 D4 4.y A Q7/ 13 77ZZ

TLaO IT

II joUj. /o

A . 1 J ^ 1 n J.IU 1 in 1 . jU 7Qn zyu

A 1 .41 1 70 1 Z8A (^A 4.04 73 77ZZ Co I re I joUd. / J 1 1 8n 1 1 oU 4.D1 J.UD 1 Q1 j.yi ini jUj 78 .Z8 Q1y3 A a 1 4.61 73 77ZZ TLaO TT

II JOUO.

J 1 A4 .UU 7/.u/ m 7n . /u Zoj 77 .Z / an8U

A HA. 4.80 7Z 77ZZ Fe I 5809.25 982 3.88 5.07 4.77 2.96 290 .31 97 4.78 4 22

Mr) IT iNQ II Jol 1 .01 8^ .OO 1 CiA 1 .y4 77B 11 07/1 .Z4 77/ / A aQ 4.8y 7Z 77ZZ Co I re I CO 1 A OA Jol4.oU 1 na^ lUoo A 70 4.Zo ^ AA J. 44 ? n7 j.UZ 111 J. 1 J

7Qn zyu 1 7 . 1 / e7jZ e n7 J.U / 11 77ZZ CA ITII CO 1 c oc JOl J.OJ 1 1 7 1 1 Z 1 <Q i .JO A 7A D. /O 7 AQ z.oy 7 ^/t Zj4 .Uo 1 c 1 J e eQ j.jy 7z nU reCo II CO 1 /; -jr 1 1 7Q illy A

4.JJ 4.84

A4.DJA ni lie 31 J10 .38 111 131 4.0J 73 77ZZ Nd II 5825.87 1.08 2.11 302 .25 83 4.87 2 22

omQm II

II JOJO. 3 / 1 nn 1 .UU 1 77 1 . /Z 7 e7 ZjZ ne .Uj 1 71 Z < /;7 J.O/ 1 nu MH IT iNQ II co/n TO Jo4Z. JO 8/^ OO 1 70 1 .Zo D. jy 7 1A Z.JO lie 31 J 7 1 .Zl 7115 A QA 4.y4 7z 77ZZ Mi I IN 1 I Jo4 / .Ul /I A 44 1 f^Q 1 .Do j.4y A OQ 4.oy or\ .oU 7Q7 zy / 7f» .ZU /;7 oz A QQ 4.yy 11 77ZZ Core I1 ^^7 jjZ 1 7/^ J. ZD ^ 1 Q J. ly A Qn 4.yu 7 e 1 ZjI 1 0 .15 /IB 48 J.U / 7z 77ZZ Fe I 5852.19 1178 4.55 5.21 4.91 3.63 310 .18 58 5.03 4 22

Rq it •Da 11 JO

J J. Do 7z .ou ni J.UJ 4. Do 7 77 AAd 44y 71 . / 1 i<i 3 J 1 A 77 4.ZZ eJ 71Z3 reCo I1 JOJ J. 1 J 111/7 1 7Q A *^1 4.0 1 ^ ^1 J. jl ^ nQ j.uy 1 ^1 J.DI 777 LI 1 1 1 .13 AC\ 4U e 77 J.ZZ /I4

77ZZ Core II JO JD.Uo 1 1 70 1 1 Zo A 7Q 4.zy ^11 J. 31 A Q7 4.yz 1 10 J.JO 7B7 Z8Z 1 Q .ly e/1 j4 e ni J.U3 1 nU

v^a I JOJ / .4j Al4 / 7 Q1 z.yj 4.Dj

A </1 4. j4A nn 4.UU 30D . JD 717 Z3 / A A^ 4.41 73 71Z3

Fe I 5859.61 1181 4.55 4.90 4.73 4.11 350 .37 145 4.64 4 22 re 1 JoOZ.JO 11 1 on 1 oU A4. J J A B1 4.0J A <^B 4. Do A 7*; 4.ZJ 777 LI L IB .35 111 ill 4.Dy cJ 71Z3

L'd T n TT11 coon JOOU.OJ icJ J 71 .Z J D. jy 11 .uz n7 3Uo ma 11 .3 1 QQyy

A 771 1 7Z AU Core T1 ^881 81 JOOJ.Ol Q87 70Z 1 QA J.7D 4.A 7Q/y 1 1A J. JD 111 33 1

1/1 .34 1 7e 1 ZjA4.7n/U 73 11 IN d 1 J007.7J ^88Q 11 nn .UU 1 BQ j.oy 1 71 J. / 1 1 BQ J.oy ABe D6J 87 .5Z A/IQ D4y 1 QA 3.yo /l4 1i Ni I 5892.88 68 1.99 4.95 1.98 401 .43 191 4.63 0 1 VTo I iNa I ^eQ< Q7 J07J.7Z 1 nn .UU A n7 4.UZ 1 BB J.OO 1 <Q J. jy eQn jyu 77 . / / en7 jU/ /I n7 4.U /

/I 4 1i CIA 11 Lra II CQA/I CVl ji'U4.U/ 117 HZ 1I.6z 7 77

Z. /Z 7CC Zjj AC 1 7IZ

C A7 J.O/ 7z A Co T re I jyuj.o/ 1 1 O 1 1 lol /I c 4.6j C A 1

j.Ul

A 7A 4. /y /I A1 4.Uj 111 jjI 78 .Z8 Q1y3A 07 4.8Z 73 11 C/^ T re I C C7 552 7 7 1 3.21 C 7A 5.29 /I 07 4.83 770 378 7 A

.z9 1 1 A 1 lU >1 77 7 1 Fe I 5916.25 170 2.45 5.07 4.71 1.67 312 .32 104 4.76 3 0 re I 5927.80 1 1 T C 1 175 4.65 CIO 5.18 4.90 3.77 Zo/ COJO C A1 1 A re I 5929.70 1 176 4.55 c 1 n

5.19

A OC\ 4.89 3.52 ^oo 288 .20 COCA 1 5.01 1 A re I 5930.19 1 180 4.65 A OA 4.84 A H C 4.65 4.46 329 A A

.40 1 A139 4.63 3 0 re I 5934.66 982 3.93 A OO 4.88 A HQ 4.68 3.40 330 .40 t C 1 151 A H\ 4.61 3 1 f n 11 La II j9jd.zZ 1 A

19 1 7

.17 7 A7 7.U7

C 77 .86 70^ zy6 7 A .24 71A Q1 4.yi 7Z A

Si I 5948.55 16 5.08 4.83 4.70 2.88 354 .38 137 4.65 4 1 Gd II 5951.60 95 1.37 2.47 257 .05 13 5.67 2 0

Fe I 5952.75 959 3.98 4.94 4.76 3.22 305 .28 88 4.83 1 0

Ti I 5953.16 154 1.89 5.24 4.79 3.90 291 .21 62 4.98 1 0

Fe I 5956.70 14 .86 5.00 4.70 307 .38 113 4.69 2 1

139

398-978

O - 71 - 10
Table A

Spect

Wavelength

Mult EP -Log -Log Log HW Rc W

-Log Q A'

Ce II 5959.69 1.63 2.75 283 .16 42 5.14 1 1 Ti I 5965.83 154 1.88 5.41 4.82 3.73 377 .20 76 4.95 1 1 Ba I 5971.70 7 1.14 3.67 258 .05 13 5.67 1 0

Fe I 5975.35 1260 4.83 5.13 4.82 4.13 330 .27 88 4.84 3 2 Ce II 5975.87 30 1.33 6.78 2.81 330 .20 58 5.01 2 1 Fe I 5976.80 959 3.94 4.97 4.75 3.25 306 .34 113 4.72 2 1 Ti I 5978.54 154 1.87 5.48 4.93 3.86 306 .18 55 5.05 1 2 Fe I 5983.70 1175 4.55 4.94 4.75 3.96 318 .35 121 4.70 3 1 Fe I 5984.80 1260 4.73 4.85 4.70 4.33 283 .41 140 4.62 3 2 Fe I 5987.06 1260 4.79 4.94 4.75 4.16 330 .30 108 4.77 4 2 Fe II 5991.38 46 3.15 5.32 4.93 .82 330 .30 106 4.77 1 2 Ce II 5995.35 1.49 2.81 306 .15 48 5.12 1 2 Ni I 5996.74 249 4.23 5.50 5.12 3.24 274 .12 33 5.26 1 0

Fe I 5997.81 1175 4.61 4.95 3.59 303 .26 81 4.87 1 0

Fe I 6003.03 959 3.88 4.84 4.68 3.37 283 .42 130 4.63 3 2 Gd II 6004.57 112 1.66 2.75 258 .04 10 5.78 1 0

Fe I 6005.53 207 2.59 5.46 1.07 330 .17 53 5.07 2 2 Ni I 6007.31 42 1.68 5.48 4.92 .85 306 .18 47 5.08 3 2 Fe I 6007.96 1178 4.65 5.01 4.81 3.92 330 .32 109 4.75 2 2 Fe I 6008.58 982 3.88 4.83 4.67 3.42 306 .41 132 4.64 2 2 Nd II 6009.30 .38 .71 283 .09 21 5.40 1 2 Mn I 6013.50 27 3.07 4.84 4.61 3.63 330 .40 157 4.61 4 2 C I 6014.84 8.64 6.13 269 .09 24 5.40 1 0

Fe I 6015.25 63 2.22 6.18 5.33 266 .08 21 5.46 1 0

Mn I 6016.64 27 3.07 4.82 4.61 3.78 330 .42 151 4.60 3 2 Fe I 6019.36 780 3.57 6.08 5.32 260 .05 13 5.67 1 0

Ba I 6019.47 7 1.12 3.68 260 .05 13 5.67 2 0

Fe I 6020.17 1178 4.61 4.81 4.52 4.26 377 .48 204 4.50 4 2 Mn I 6021.80 27 3.07 4.80 4.61 3.93 306 .43 132 4.62 4 2 Fe I 6024.07 1178 4.55 4.71 4.60 4.50 283 .47 166 4.55 4 2 Pr II 6025.72 1.44 2.96 259 .11 30 5.30 2 2 Fe I 6027.06 1018 4.07 4.99 4.72 3.49 306 .35 119 4.71 4 2 Mo I 6030.66 5 1.53 6.60 3.07 271 .10 27 5.35 2 0

Ce II 6034.20 30 1.46 6.78 2.58 353 .25 85 5.00 0 2 Nd II 6034.24 1.54 6.78 2.35 353 .25 85 5.00 0 2 V I 6039.69 34 1.06 5.74 5.03 3.19 306 .11 35 5.30 1 2

Ce II 6043.39 30 1.21 6.48 5.58 2.87 306 .28 88 4.83 4 2 S I 6046.04 10 7.87 5.58 5.15 276 .12 33 5.26 1 0

S I 6052.66 10 7.87 5.74 5.44 2.71 287 .17 49 5.09 2 0

Fe I 6055.99 1259 4.73 4.92 4.73 4.16 353 .35 129 4.69 2 2 Fe I 6062.89 63 2.18 5.53 4.85 .58 286 .16 46 5.12 2 0

Ti I 6064.63 69 1.05 5.94 5.11 2.62 271 .09 24 5.40 1 0

Fe I 6065.49 207 2.61 4.72 4.53 2.75 377 .57 221 4.43 4 2 La II 6067.14 48 .77 .84 236 .10 21 5.35 1 2 Fe I 6078.50 1259 4.79 4.82 4.73 4.20 283 .37 122 4.69 2 2 Fe I 6079.02 1176 4.65 5.04 4.89 3.60 330 .23 80 4.91 2 2 Gd II 6080.65 112 1.73 2.82 2^5 .06 16 5.59 1 0

V I 6081.42 34 1.05 5.61 4.97 3.20 286 .16 46 5.12 2 0

Fe I 6082.72 64 2.22 5.25 4.82 .86 306 .24 74 4.91 2 2 Fe II 6084.11 46 3.20 5.44 5.13 .42 306 .28 85 4.84 2 2

140
Table A

bpect

Wavelength

IVlUlt iLr — Log -Log

(WJk)

Log HIT/ Ac -Log nV i\N

11 I DUoJ .ZD 6Q 11 .\JJ OS S 18 ^ . 67VJ / 106 . — 810 1 A 88 1 9Z>

VTi* T JNl I DU0D.Z7 94Q A 96 JS . 11 S

J

4 QO _> .uo _) J -J 7^ 77/ z. 4 0^ z. z. re I OU07. J /

11 197 jZ / JS .uz 09 JS .zo 98 4 Q1 4 OS ^77 .Z.V 70 7S 4 . Of^ y\j 11 V I OU7U. 1

0

14 11 .VJo 08 J.S 19JZ 4 84 711 u 1 4 00 11 Fe I 6093.66 1177 4.61 5.29 4.97 3.36 330 .13 40 5.22 1 2

r e I

111// 1 77 4 6S S 48 S 09 959 . 11 D3 35 J5 * 29ZrZ. 1 9Z> P<a tc TI yJ y 1 98 5 93 A 89 9 84 353 1

9

. 1 y 60UVJ J5 . 02VJ^ 1X 9

Cp- tt 11 . 77/ / 3J . 04V/H 93 77 4^ .y92£^ 1X 9z. Vp- re t1 0 1 uz.. 1 0 1 959 4 83 4*T. 86OU 4 73 4 95 330 _J ^ VJ 35 11 11 3-J A 72 9z« 1 Ca I 6102.72 3 1.88 4.66 4.52 2.90 330 .55 199 4.47 2 3 Fpr c t

1 61 03 1

Q

1 960 4 83 4t. 84Ot" 3 98 388 34 127 4.70 2 3 7r TT Q 1 UO.H / 1 06 11 . 7f^ / u U. 74Z,H 7S 8800 4 87 1 -J1

Tsli IN T 1 I D 1 08Uo. 11 9Z 4S 1 .uo JS .Ul 01 4 6Q 1 4Q ^10 ^8 1 ^7 4 66 11 1

I Dl 1lU.0 78/o 11.1"1 Q 4 7^ 77S . 11 0u 11z. /

11 0VJ Ni I 6111.06 230 4.09 5.23 4.95 3.30 288 .16 46 5.12 1 0

V T ^^1 1 1 6? 34 1 04 S 71 _?5 .U_J 05 9 . 96yyj 971 Z< / 1 .VJO 08 91 _/S .^VJ 46 9Zr 0

Fpr c tt11 U 1 i. J .JD HVJ .J1 . 99zz J . JU JS . 11 7/ 70f^ 70 60 S 01 9 n 7r IT 61 1 4 78 1 66 U.Ulf^l S .u67/ JJUU ^Of> .Z.77/ 81 4T" . 86OVJ 1X 1 Nii> T 1 1 6116 u 1 1 vj. 181

0

71^ 1 R

0

4 OQ 4 Q7 ^ 7^ -J J >J 70 11 04yj'-r 4 70 9 1 Co I 6117.00 1.78 5.88 5.32 1.87 269 .07 19 5.52 1 0

V T 61 1 9 51 11 .VJVJ 06 S 4Q 4 88 3 31 306 . 11 80 ^56VJ _/5 . 05VJ-J 9z> 3

K^a. 1 1 1 .oy 4 /I /I 4 40 1 '^8 J .JO 'Ml .U-> 986 zou 4 11 4 1

Si T u 1 .\J^ J .u 1 JS . 91ZJ> JS .U-7 OQ 7S0 ^jy . 11 0y S9 S OS 1-J 1

T a TT 61 96 09 VJZ7 1 7S 7 00 -JVJU 93 69Kjy _J5 . 09VJZ< 0VJ 1 Ti I 6126.22 69 1.07 5.49 4.90 2.68 306 .23 69 5.02 0 3 7r T 61 97 49 9 . 1 J 6 94 S 41 9 39 959 z,_J y 37-J / 5 1 8 2 3 FpIT C t1 61u 1 97z / . Q17

1

11 01U 1 7/ 4H. t1 4H S 1 1 J . 10ly ^^0 .z.77/ 84OH 4*T .ou 86 7 1 Ni1 T1 61 98 98 47 1 .UO S 47 4't.OO 88 . lf\ 1 u >?uu . 11 0y JOS8 5 0^ 1 3_J TL^aa TT11 61 99 56 47 11 11 .uz. fO .^u 01y 1 A 85 11 -J3 Si I 6131.57 30 5.61 5.37 5.15 292 .18 52 5.07 2 0

7r I 61 34 58 9 00 6U. 94Z.'t 5 53 1 90 915 35 ^5 . 20Z>VJ 1 3 V I 61 35 36 34 1 05 5 71 5 07 9 97 980 Z-OVJ 1

9

. 1 ^ 34 S . 26^VJ 2Z. 0VJ Fe T 61VJ 1 36VJ. 69VJ^ 11 69VJ^ 9 45 4 65 4 48 9 85 -JO 381i 59 943 4 40 1 0VJ FeX V T1 61VJ 1 J37/ . 00 69vjz> 9 90 4*+, 98!70 4 68 11 . 411

1

343 41 11 48"TO 4 69 9Z. 0\J Fe I 6137.70 207 2.59 4.68 4.44 2.84 'ill .59 236 4.41 3 3 RaIJa TT11 6141 VJ 1 H 1 . 79/ z 70 4 74 4 SO 1 71 683 . 78/ 0 695 J3 .y^ 95 4 3 OlSi T1 61 49 4Q 10 J

<N .oz 69 J.ZO96 JS .UD 06 9Q6 Z7D . 11 Qy S7 S 01 11 n

AI7r T1 610 1 41 .Zj 91 z 07 6D. J71Q S 41 J .1

1

9 1 1 Z. 1 1 9Q8 Lyo .zu 90 60DU J)S .Ul 01 7z. u Ppv^e it11 61Dl'tj. 41 16jD 11 . 70/U 9Z.o87/ 9Q4 LyH . 11 8

0

SI JS .UD 06 11 Si I 6145.02 29 5.61 5.21 5.06 302 .22 67 4.96 2 0

Fe II 4Q 94 /'J 1 fiQ ^ 74 J. Ah A QS 177 IS 11 1Qjy 4H-.Oo 68

Fpre tI 01 J 1 .DZ DZ 7 1 fi Z. 1

0

J. lo A 78 1 .Uo 981 ZOJ 11 .J J

1 1 1 111 4 74 -3 -1 Mo T iNa I

/:i C/4 01 J4.ZJ cJ Z. lU < 1^ J. JD /I 78 4. /o 7 71 Z.Zj iin 7/1 1 (\C\ lUU /t 8^ 11

-3 ol I Dl J J. 1

J

7QLy ^ A7 J.DZ /I Q1 /I 77 4. /Z iin 11 IUj /I 7^ -J i reFp tI ^1 S7 71 Dl J / . / J lUl J 4 07 ^ 1 1 J. 1 1 1 14 1S1 J J J AA 110/87 4 7S Kl J Na I 6160.75 5 2.10 5.15 4.74 2.53 ill .30 117 4.76 1 3 Ca I 6161.29 20 2.52 5.07 4.73 2.77 , 353 148 4.65 1 3 Ca I 3 1.90 AM 4.34 3.57 424 .66 - 289 4.33 3 3 Fe I 6165.37 1018 4.14 5.27 3.16 283 .24 72 4.92 1 3 Pr II 6165.95 39 .92 6.49 5.49 2.71 283 .17 54 5.07 1 3

141
Table A

Spect

W 3.VC- Mult EP Log

i W l \ \ \ Pr i; / A I

Log Log HW Rc r

Log

^ 0 Q

Ca I 6166.44 20 2.52 5.06 4.73 2.89 400 .33 126 4.71 2 3 Ca I 6169.06 20 2.52 4.86 4.62 3.24 306 .42 141 4.62 1 3 Ca I 6169.56 20 2.52 4.80 4.62 3.52 330 .49 191 4.51 1 3 Fe I 6170.52 1260 4.79 4.97 4.15 306 .39 137 4.65 2 3 La II 6172.72 4 .13 6.61 .60 330 .18 58 5.04 2 3 Fe I 6173.34 62 2.22 5.09 4.65 1.39 330 .41 152 4.61 2 3 Ni I 6175.42 217 4.09 5.23 4.86 3.72 353 .26 91 4.85 3 3 Ni I 6176.82 228 4.09 5.09 4.80 3.96 306 .30 97 4.80 4 3 Ni I 6177.26 58 1.83 5.79 4.95 .51 280 .11 31 5.30 1 0

Fe I 6180.22 269 2.73 5.19 4.77 1.71 306 .34 116 4.72 4 3 Ni I 6186.74 229 4.10 5.45 4.99 3.35 259 .17 40 5.14 2 4

Fe I 6188.00 959 3.94 5.24 4.80 282 .28 91 4.83 4 4

Co I 6189.01 37 1.71 6.01 5.06 1.94 279 .10 28 5.35 2 0

V I 6199.20 19 .29 5.89 2.42 281 .11 31 5.30 2 0

Fe I 6200.32 207 2.61 5.05 4.63 1.83 329 .41 144 4.63 4 4

Ni I 6204.64 226 4.09 5.59 3.21 294 .12 41 5.26 3 4

Sc I 6210.68 2 .00 6.49 5.29 2.22 273 .07 19 5.52 2 0

Fe 1 6213.44 62 2.22 5.01 4.67 1.64 329 .49 173 4.53 4 5 V I 6213.87 20 .30 6.32 5.12 1.88 275 .08 22 5.46 1 0

Fe I 6215.15 1018 4.19 5.19 3.27 306 .33 120 4.73 2 5 V I 6216.37 19 .28 5.32 4.79 2.40 329 .20 66 4.99 2 5 Fe I 6219.29 62 2.20 4.88 4.58 1.75 329 .50 175 4.53 5 5 Fe 1 6220.78 958 3.88 5.56 5.05 2.34 289 .14 40 5.19 2 0

Ni I 6223.99 228 4.10 5.41 3.29 306 .16 49 5.11 2 5 Fe I 6226.77 981 3.88 5.41 4.95 2.58 282 .16 45 5.13 2 5 Fe I 6229.23 342 2.84 5.28 4.80 1.68 353 .28 89 4.84 4 5 Fe I 6230.73 207 2.56 4.62 2.86 423 .62 285 4.34 5 5 Fe I 6232.66 816 3.65 4.91 3.07 400 .45 183 4.55 4 5 Si I 6237.32 28 5.61 5.02 4.83 353 .29 108 4.79 3 5 Fe II 6238.38 74 3.89 5.18 4.90 2.13 353 .41 155 4.61 5 5 Sc 1 6239.41 2 .00 6.02 5.45 1.37 285 .12 34 5.26 2 0

Fe II 6239.95 74 3.89 5.80 5.28 296 .17 51 5.09 1 0

Fe 1 6240.66 64 2.22 5.19 4.80 1.12 331 .33 114 4.74 3 0

V I 6243.11 19 .30 5.42 4.76 2.62 307 .22 69 4.96 1 0

Si I 6243.81 28 5.61 5.16 4.98 318 .27 88 4.85 2 0

Si I 6244.47 27 5.61 5.14 5.02 316 .26 85 4.87 2 0

Sc II 6245.63 28 1.51 5.32 4.87 2.74 329 .39 130 4.66 3 5 Fe I 6246.33 816 3.60 4.75 4.57 3.49 329 .49 183 4.52 3 5 Fe II 6247.56 74 3.89 5.11 4.87 2.08 376 .42 170 4.58 4 5 V I 6251.83 19 .29 5.75 2.21 288 .13 37 5.22 1 0

Fe I 6252.56 169 2.40 4.76 2.51 353 .57 212 4.45 5 5 Fe I 6254.26 111 2.28 4.74 1.82 376 .52 214 4.47 3 5 Fe I 6256.37 169 2.45 4.89 1.77 353 .51 208 4.48 3 5 V I 6256.91 19 .28 6.32 1.68 273 .06 16 5.59 2 0

Ti I 6258.11 104 1.44 5.17 3.56 282 .29 93 4.82 1 5

Ti I 6258.71 104 1.46 5.16 3.58 306 .40 144 4.63 1 5 Ti I 6261.10 104 1.43 5.19 3.44 329 .29 98 4.81 3 5 Fe I 6265.14 62 2.18 4.94 1.80 353 .50 180 4.52 5 5 Sm II 6267.28 1.17 2.23 273 .06 16 5.59 1 0

Fe I 6270.24 342 2.86 5.13 4.74 1.89 306 .36 127 4.69 2 5

142
Table A

bpect

Wavelength

Mult tr

- - Log — Log Log n W Ac ww -Log r\V

N

\r T V I OZ, /'+.D / 1

9

97 6 07 5 10 1 97 991 1 4 41 J5 .vy19 7 0u

IT DZ ly.l\j If, 98 1 SO S 44 4 98 L..^y D D J 34 1 1

Q

4 77 D u re I DZoU.DZ 11 D .ou J .uo D\j\j .HO 48 1 f\\ 1 U 1 4H.JOS^^ <J J V I /^9RS DZoJ . 11 8o 19 J . yJ S 07 1 04 .u07/ 1

1 Qy J . JZ, 0u Fe I 6290.97 1258 4.73 4.98 4J6 3.91 306 .31 96 4.79 2 5 <?m TT 1 41 9 18 974 06 1

6

^5 .J59y 11 0u VV T1

1

9

1 y 99 5 84 4 99 9 05 999 L,yy . 11 7/ _/^11 S 09 7 0u re 1

1 260 4.83 5 72 5.22 288 .12 34 5.26 0u

C 1 6797 80 62 2.22 4.99 4.69 1.49 329 .45 151 4.59 4 Js 0 I 6300.31 1 m 6!l6 288 .12 34 5J6 1 0

Fe T 6301.52 816 3.65 4.70 4.63 3.58 305 .50 182 4.52 4 5 Gd IT 6305 1 5 94 1 31 9 55 986 1

1

.11 31_J 1 5 30 2 nU 6305 67 9 02 6 76 9 31 986 1

1

.11 _J311 5 30 11 0u

"sm TT 1 0^^ 1 .uo L. 1 D OS 1 D JS .U67/

11 0u Sc II 6309.90 28 1.50 5.46 2.06 310 .22 70 4.96 2 0

Fe T 6311.51 342 9 83 5 44 4 93 1 56 995 . 11 ^5 44 5 1 5 2 0u 7r T 631 3 05 65 1 58 6 80 3 43 983 09 97 5 38 7 0u Ni T 6314 67 67 1 93 4 07 1 . yj Dz.y .H41i

1 40 4H .UH ^4 J J Fe T 631 5 39 11 01\J 1 J5 H. 1 *-r S 08 4 ^^R .Dy 1 Z,I7 4H.U^7/ J J Fe I 6315.81 1014 4.07 5.28 4.89 3.05 306 .20 62 5.01 1 0

Mp t 631 8 79 93 5 1 1 S 93 . 11 Qy ^y59 S 0^ 2 nu Mp t 6319 99 93 S 1 1 9Q^ 1 4 41*T 1 JS . 191 17 2 0u Tan 6390 39 191 y 1 7 70 _)S .-?Z. ^9 11 . ^9_7Z. 44 11 uo 4H.JOS8 1_) 0u Sc TT 6320^V/. 85O-J 98 1 50 f\ 09 S 99 1 84 "^04 1 Q JS .U0^J 2 0u Ni I 6322.17 249 4.15 5.52 5.11 3.16 2S1 .11 31 5.30 2 0

Fe I 6322.69 207 2.59 4 93 4.74 1 87 305 .41 .140 4.64 4 5 Ni I 6327 60 44 1 68 S 94 4 78 11 .\J\J 00 J LO 9S 81O 1 4 8Q 1 n Cr I 6330.10 . 94y^ 5 40 4^ ,\jy 89 1 98 305 _'U_' . 91Z. 1 61U 1 J5 . 00V/V/ 2 J Fe I 6330 86 1254 4 73 5 30 4T" . 96y\j 3 49 989 1

9

.yy ^ 1 J5 .uu 06 2 J Fe I 6335.34 62 2.20 4.79 4.57 1.94 305 .52 173 4.52 5 5 Fe I 6336 83 816 3.69 4.72 4.60 3 52 329 .46 171 4 56 J Js Fe I 6344.15 169 2.43 5.05 4.73 1.48 376 .42 182 4 80 0 J Si II 6347.10 2 8.12 5.07 4.03 322 .27 88 4.86 2 0

Fe I 6355.04 342 2.84 5 01 4 60 9 04 329 J L^y 40 147 1 / 4T" .U63J 2 J Fe I 6358.69 13 ^86 4.89 4.59 329 .45 158 4.58 2 5 Ni1" 1 T1 6360 80 999 ^,L.y 4 17 S 60 JS .\.\J 10 3 99 997 4S JS . 11 J5 2 n 7n T u JS . 7Q1 y S 44 .UU 4H, 94ZH "^1

1

.Z911 OO 4H.!70 Q8 11 n n T fiX^X ujuJ . 7Q/ y

11 .\jL D.O.J 989 zoz .Uo ns 77zz S 4^^ J .HU 1J u re t1 1 /.J J A 7Q S 41 4 Q7 4Q . 11 8o Dl JS .UH 04 11 D Nd II 6365.55 .93 1.34 235 .14 29 5.19 2 6

>Ji LSI I1 (\'\(\f, 48 9^n 4H. 11 7/ J .jy 4 OS "X AX 49HZJ . 1

J

DU Js .Uo ns 11 o rcFe TT11 DjD^-HD 40 9Z.078Q J. J J 7^8 ZJo .Z7SJ 7S 4 Q1 11 co

ol<Ii TI11 Dj / 1

.

jO L

fi 1 7 o. 1

Z

j.Dy J. / J 107 1 Q .17 jy ^ ni Z au w; T INI 1 747 4. 1 J

^ 17 J. J / 4 QQ j.DU inn 1 .ID 48 ^ 1 7 J. 1 z

11 u reFe T

1 <;-5on 7*; lUl J 4 1 Q s 9n 4 81 J.\ 41HI ins .Z77/ 01yj 4 84 /I H D Nd II 6382.07 1.44 1.93 305 .13 41 5.22 2 6

Nd II 6385.20 85 1.16 2.10 329 .18 61 5.04 1 6

Fe I 6385.74 1253 4.73 5.90 5.34 281 .07 19 5.52 1 0

La II 6390.48 33 .32 6.50 5.44 1.50 329 .40 157 4.62 2 6

Fe I 6392.53 109 2.28 5.81 5.03 .68 292 .12 35 5.26 1 0

143
Table A

Spect

3,VC" Mult EP — 1 OP" T /^ff HW Rc W

(WJk) Q

Fe I 6393.61 168 1A1> 4.74 4.52 2.71 376 .58 230 4.43 3 6

La II 6399.05 104 IM 3.28 376 .11 38 5.30 2 6

Si I 6407.27 5.87 5.39 399 .19 68 5.00 1 6

Fe I 6408.03 816 3.69 4.90 4.63 3.41 376 .45 178 4.56 1 6

Sr I 6408.47 8 2.21 6.33 5.33 4.21 311 .20 63 5.01 2 0

Fe I 6411.66 816 3.65 4.70 4.57 3.80 329 .53 191 4.50 4 6

Ni I 6414.60 244 4.15 5.63 5.19 3.46 291 .11 32 5.30 1 0

Si I 6414.97 5.87 5.15 309 .19 59 5.03 2 0

Fe II 6416.91 74 3.89 5.13 4.97 1.64 329 .32 111 4.76 3 6

Ca I 6417.69 4.44 5.85 287 .09 25 5.40 1 0

Co I 6417.82 111 2.33 5.41 2.40 284 .08 22 5.46 1 0

Fe I 6419.98 1258 4.73 4.90 4.73 4.36 305 .38 140 4.66 1 6

Fe I 6421.36 111 2.28 4.87 4.50 2.27 352 .57 207 4.46 5 6

Sm II 6426.63 1.75 2.43 280 .06 16 5.59 1 0

Nd II 6428.67 .20 7.11 .61 305 .20 69 4.99 2 6

Co I 6429.91 81 2.14 6.41 5.55 1.99 280 .06 16 5.59 2 0

Fe I 6430.85 62 2.18 4.78 4.54 2.24 375 .57 230 4.43 5 6

Fe II 6432.65 40 2.89 5.23 4.98 .76 329 .38 134 4.67 4 6

Y I 6435.02 2 .07 6.63 5.60 2.22 305 .18 54 5.07 2 6

Eu II 6437.64 8 1.32 6.03 2.72 292 .11 32 5.30 2 0

Ca I 6439.07 18 2.52 4.62 4.28 352 .62 236 4.44 5 6

Fe II 6446.43 199 6.22 6.11 5.81 279 .05 14 5.67 1 0

Ca I 6449.81 19 2.52 4.82 4.65 3.26 374 .47 187 4.54 3 0

V I 6452.32 48 1.19 6.03 5.33 2.50 281 .06 17 5.59 1 0

Co I 6455.00 174 3.63 5.77 5.23 4.09 305 .10 30 5.35 1 6

Ca I 6455.60 19 2.52 5.13 4.82 2.46 352 .27 93 4.85 3 6

Fe II 6456.38 74 3.90 5.05 4.85 2.34 375 .49 206 4.50 2 6

Fe I 6456.87 1256 4.79 5.58 5.40 302 .15 45 5.15 1 0

Ca I 6462.57 18 2.52 4.66 4.12 422 .65 305 4.50 0 6

Fe I 6462.75 168 2.45 4.97 1.81 422 .65 305 4.73 0 6

Ca I 6464.68 19 2.52 5.81 5.06 258 .14 36 5.19 3 6

Ce II 6466.90 1.77 2.63 235 .13 30 5.22 1 6

Fe I 6469.21 1258 4.83 5.09 4.80 3.99 305 .27 86 4.86 2 6

Ca I 6471.66 18 2.52 4.89 4.68 3.22 328 .45 167 A CO 4.58 3 6

Sm II 6472.34 1.38 2.07 280 .05 14 5.67 1 0

Fe I 6481.88 109 2.28 5.01 4.66 1.41 355 .38 142 4.66 2 0

Ni I 6482.81 66 1.93 5.23 4.78 1.69 258 .25 70 4.93 2 6

Sm II 6484.52 1.26 1.87 278 .04 11 5.78 1 0

Ti II 6491.58 91 2.06 5.16 305 .37 117 4.71 2 6

Ca I 6493.78 18 2.52 4.69 4.57 3.95 375 .53 214 4.47 5 7 Fe I 6494.97 168 2.40 4.60 4.42 2.95 375 .61 260 4.40 3 6

Fe I 6495.78 1253 4.83 5.19 4.96 3.83 316 .21 66 4.99 2 7 Ba II 6496.90 2 .60 4.82 3.43 656 .80 586 4.04 5 6

Fe I 6498.96 13 .96 5.18 4.75 363 .34 134 4.70 4 6

Ca I 6499.65 18 2.52 4.90 3.22 293 .42 139 4.64 5 6

Cr I 6501.21 16 .98 5.86 293 .10 29 5.35 1 0

Sr I 6504.00 8 2.26 6.64 4.07 300 .13 39 5.22 2 0

Ca I 6508.85 18 2.52 5.77 1.70 302 .14 42 5.19 2 0

Fe II 6516.06 40 2.89 5.03 1.07 352 .47 178 4.55 3 7 Fe I 6518.38 342 2.83 5.03 4.77 1.88 355 .37 138 4.68 3 0

144
Table A

Spect

Wavelength

Mult EP -Log -Log Log HW Rc W

-Log 0

Fe I 6533.94 1197 4.56 5.15 3.19 258 .19 50 5.07 1 7 Nd II 6539.94 .74 0.99 294 .10 28 5.36 2 0

Sm II 6542.76 1.46 2.22 288 .07 20 5.52 1 0

Fe I 6546.25 268 2.76 4.80 4.60 2.64 352 .53 216 4.47 2 7 Nd II 6549.54 .06 .37 258 .15 32 5.22 2 7 Nd II 6550.19 .32 0.63 234 .20 54 5.04 1 7 Sr I 6550.24 12 2.69 6.42 5.52 3.99 234 .20 54 5.04 1 7 Fe I 6551.70 13 .99 5.91 234 .08 19 5.46 1 7 Ti I 6554.23 102 1.44 5.67 5.00 1.11 351 .17 58 5.07 1 7 Ca I 6572.78 1 .00 5.40 4.76 281 .30 88 4.83 1 7 Fe I 6574.24 13 .99 5.48 4.78 281 .26 82 4.89 2 7 Fe I 6575.02 206 2.59 5.01 1.58 398 .40 175 4.60 3 7 Ni I 6586.33 64 1.95 5.27 4.81 1.57 281 .26 76 4.90 1 7 C I 6587.61 22 8.53 5.50 2.48 303 .13 39 5.22 2 0

Sm II 6589.72 1.27 2.38 287 .06 17 5.59 1 0

Nd II 6591.43 .20 0.39 295 .09 27 5.39 2 0

Fe I 6592.92 268 2.73 4.73 4.57 2.72 351 .50 202 4.51 2 7 Fe I 6593.88 168 2.43 4.87 4.64 1.79 375 .44 175 4.58 5 7 Ba I 6595.33 6 1.12 3.97 301 .12 36 5.26 1 0

Co I 6595.87 174 3.71 5.97 5.37 3.67 292 .08 23 5.46 1 0

Fe I 6597.57 1253 4.79 5.18 3.54 305 .20 66 5.00 1 7 Sc II 6604.60 19 1.36 5.26 4.90 2.28 351 .36 133 4.69 4 7 Fe I 6608.03 109 2.28 5.56 5.02 .49 304 .12 39 5.26 1 7 Fe I 6609.12 206 2.56 4.94 4.70 1.54 375 .35 133 4.70 2 7 Y II 6613.75 26 1.75 6.22 2.42 351 .39 146 4.65 4 7 Fe I 6627.56 1174 4.55 5.44 5.02 3.10 292 .16 47 5.13 3 7 Cr I 6630.02 16 1.03 6.04 5.16 187 .07 15 5.52 1 8

Co I 6632.44 111 2.28 6.12 5.20 2.60 291 .07 20 5.52 1 0

Fe I 6633.76 1197 4.56 4.98 4.82 3.69 343 .29 103 4.81 2 0

Ni I 6635.15 264 4.42 5.54 5.06 3.63 351 .13 40 5.22 2 8 Fe I 6639.71 1195 4.61 5.59 2.99 308 .14 43 5.19 1 0

Ni I 6643.64 43 1.68 4.90 1.96 328 .42 154 4.62 5 8 Eu II 6645.11 8 1.38 6.22 2.84 308 .14 43 5.19 2 0

Cr I 6661.08 282 4.19 5.82 5.41 4.23 293 .07 20 5.52 1 0

Fe I 6663.45 111 2.42 4.94 4.65 1.77 444 .43 192 4.56 2 8 Ba I 6675.27 6 1.14 3.67 291 .06 17 5.59 1 0

Fe I 6677.99 268 2.69 4.74 2.90 421 .51 211 4.50 4 8 Sm II 6693.55 1.69 2.57 294 .07 20 5.52 1 0

Ba I 6693.84 6 1.19 3.81 290 .05 14 5.67 1 0

Al I 6696.02 5 3.14 5.31 4.93 2.49 327 .18 59 5.06 1 8 Al I 6698.67 5 3.14 5.50 5.11 2.18 327 .16 51 5.12 1 8 Fe I 6699.14 1228 4.59 5.98 5.39 294 .07 20 5.52 1 0

Fe I 6703.57 268 2.76 5.32 4.87 1.30 280 .21 66 4.99 1 8

Fe I 6705.12 1197 4.61 5.20 4.90 3.39 304 .24 79 4.92 1 8 Li I 6707.84 1 .00 6.53 4.01 420 .07 29 5.36 1 8 Fe I 6710.32 34 1.48 5.75 4.96 350 .16 48 5.13 3 8

145
A.4. Table B, the Line List Arranged Alphabetically by Spectrum

With the following exceptions, the successive columns of table B are the same as described

preceding table A. Column 5: the value of the abscissa for the line on the differential curve of grovyrth with respect

to the sun

log = log — A^x

M= + 0.10

Column 6: the value of the abscissa for the line on the differential curve with respect to e Vir

logZ; = logZ.-A0X

A6» = -0.09

Column 7: the value of the abscissa for the hne on the absolute curves of growth

d" = l.lS

6' = 1.07

The stellar line strengths log Xq and logX^ are discussed in section 4.2.

146
Table B

Spect ave- length

Mult EP — Log -Log

Log

(gA)

-Ox

HW Rc W

-Log

(WIK) Q

Al I 6696.02 5 3.14 5.60 4.32 -1.06 327 .18 59 5.06 1 8 Al I 6698.67 5 3.14 5.83 4.64 -1.37 327 .16 51 5.12 1 8 Ba I 6019.47 7 1.12 2.41 260 .05 13 5.67 0

Ba I 6595.33 6 1.12 2.70 301 .12 36 5.26 1 0

Ba I 5971.70 7 1.14 2.38 258 .05 13 5.67 1 0

Ba I 6675.27 6 1.14 2.38 291 .06 17 5.59 1 0

Ba I 6110.78 7 1.19 2.89 275 .10 27 5.35 1 0

Ba I 6693.84 6 1.19 2.47 290 .05 14 5.67 1 0

Ba I 5777.62 9 1.68 2.58 248 .04 10 5.78 1 0

Ba II 4554.03 1 .00 2.84 1.12 3.83 843 .91 1068 3.63 3 29

Ba II 5853.68 2 .60 4.91 3.79 2.13 449 .71 351 4.22 5 23

Ba II 6496.90 2 .60 4.41 2.79 656 .80 586 4.04 5 6

Ba II 6141.72 2 .70 4.17 2.70 2.96 683 .78 695 3.95 4 3 Ba II 4524.93 3 2.51 5.31 3.46 .61 291 .65 206 4.34 2 0

C I 4770.03 6 7.48 6.23 4.86 -7.05 230 .19 44 5.03 2 0

C I 4817.37 5 7.48 6.49 -7.30 • 229 .17 39 5.09 2 0

C I 5380.34 11 7.68 6.07 -6.63 341 .25 88 4.84 1 10

C I 6587.61 22 8.53 6.37 -7.16 303 .13 39 5.22 2 0

C I 6014.84 8.64 7.01 269 .09 24 5.40 1 0

Ca I 6572.78 1 .00 5.40 4.15 281 .30 88 4.83 1 7 Ca I 4425.44 4 1.88 3.14 1.14 276 .67 204 4.34 4 28

Ca I 6102.72 3 1.88 4.01 2.70 .78 330 .55 199 4.47 2 3 Ca I 6122.22 3 1.89 2.94 1.66 1.24 377 .63 286 4.33 4 3 Ca I 4318.65 5 1.90 3.61 1.28 283 .67 225 4.28 2 27

Ca I 6162.17 3 1.90 2.94 1.29 1.42 424 .66 289 4.33 3 3 Ca I 4094.94 25 2.52 3.86 .07 246 .53 140 4.47 2 0

Ca I 4512.27 24 2.52 5.65 4.14 216 .18 39 5.06 1 0

Ca I 4578.55 23 2.52 4.54 3.21 .25 281 .45 122 4.57 1 30

Ca I 4585.87 23 2.52 3.47 .62 281 .59 199 4.38 3 30

Ca I 5260.39 22 2.52 5.49 4.39 -1.03 291 .18 52 5.03 2 9

Ca I 5261.71 22 2.52 4.32 3.06 .14 303 .50 155 4.52 4 9

Ca I 5581.97 21 2.52 4.51 3.24 .19 331 .51 181 4.49 3 0

Ca I 5588.76 21 2.52 3.82 2.43 1.11 378 .64 267 4.32 5 17 Ca I 5590.12 21 2.52 4.57 3.53 .19 353 .49 186 4.50 3 17 Ca I 5598.49 21 2.52 4.15 .68 479 .64 326 4.43 0 17 Ca I 5601.28 21 2.52 4.39 2.56 .21 366 .53 218 4.44 2 17 Ca I 6161.29 20 2.52 5.18 3.79 -.08 353 .37 148 4.65 1 3 Ca I 6166.44 20 2.52 5.16 3.81 .04 400 .33 126 4.71 2 3 Ca I 6169.06 20 2.52 4.72 3.30 .39 306 .42 141 4.62 1 3 Ca I 6169.56 20 2.52 4.54 3.31 .67 330 .49 191 4.51 1 3 Ca I 6439.07 18 2.52 3.91 1.43 352 .62 236 4.44 5 6

Ca I 6449.81 19 2.52 4.60 3.45 .41 374 .47 187 4.54 3 0

Ca I 6455.60 19 2.52 5.28 4.11 -.39 352 .27 93 4.85 3 6

Ca I 6462.57 18 2.52 4.07 1.27 422 .65 305 4.50 0 6

Ca I 6464.68 19 2.52 6.09 4.61 258 .14 36 5.19 3 6

Ca I 6471.66 18 2.52 4.79 3.59 .37 328 .45 167 4.58 3 6

Ca I 6493.78 18 2.52 4.19 3.01 1.10 375 .53 214 4.47 5 7 Ca I 6499.65 18 2.52 4.82 .37 293 .42 139 4.64 5 6

Ca I 6508.85 18 2.52 6.05 -1.15 302 .14 42 5.19 2 0

Ca I 4526.93 36 2.71 4.50 3.06 .17 256 .49 116 4.55 2 29

147
Table

B

Spect

length

Mult EP

— L,o<j z;

— Loe

Log

-^x

Rc

W

— Log ( IVIk)

Q

Ca I 5349.47 33 2.71 4.47 3.40 314 .49 164 4.51 1 0

Ca I 5512.98 48 2.93 4.49 3.32 .14 328 .45 167 4.54 2 14 Ca I 5857.45 A "J 47 2.93 4.07 2.76 .69 366 .56 237 4.41 3 23

Ca I 6417.69 4.44 6.32 287 .09 25 5.40 1 0

Ce II 4053.51 36 .00 5.79 2.78 256 .62 194 4.32 2 0

Ce II 4486.91 57 .30 5.67 2.71 263 .64 166 4.43 4 29

Ce II

A 1 OA 4120.84 1 1 112 .32 5.55 Z A 2.54 262 .63 198 4.32 2 0

Ce II 4527.35 1 AO 108 .32 z. /I 306

n 1 . /I ZZ6ACA

4.50 0 ^ A29

Ce II 4072.92 .33 Z.3Z A1 243 .jZ 1 c 13j

A AO 4.4o z A0

Ce II

A 1 C\C\TA 4399.20O 1 81 .33 j.yb ^ c 1 Z.jI Zoz ^ A

.oO lol

A "3A

4.3y z ^0Zo Ce II 4483.90 3 .38 5.53 3.11 282 .57 185 4.40 3 29

Ce II 4562.36 1 A 0 .48

C AC\ 5.49 y1 "5 0 4.38T AO 3.08CA 250 .64 1 CA 159AA 4.46 z5 A

30

Ce II

A'iCA CC 4364.66 135CA

.50 5.63 2.75 '1

C 1 251 ^ A

.60 172

A Af\ 4.40 2 27

Ce II Ai^ z ni 4375.92 134

CA

.50 2.52

"5

A 1 301 .11 260AA "J 4.43 0 27

Ce II

/IO"5 AO 4523.08 2 .52 5.66 /I AA 4.09 2.64 AT 297 ^ A

.69 224 /111 4.31 2 A0

Ce II 4628.16 1 .52 5.59 4.39 2.96 337 .67 226 4.31 4 30

Ce II AH'^ Z A

A 4725.09 t Zl 153 z.52 6.56C ^ 1 5.61 1 ^O 1.78 '^Z Z 255 .33

0*7 87

A 1 A 4.74 4 32

XT Ce II 4uy3.yo Z 1 .53 AiC Z3d .45 11c 1 1 J c c 4.JD z A0

Ce II

AA Z A 4467.54 17 .61 2.17 270

CA .54 156A AC 4.46 2 A0

Ce II 43oZ.l / I .68

C 0 /I 5.84 z. /4 314 .51 1 AC lyj /I '2C 4.3j 1 11 Ce II 4560.96 2 .68 6.10 2.23 271 .51 148 4.49 3 0

TT Ce II 40do.o4 82 . /o 6.16 z.4y Zj3CA

161

A A[\ 4.4U z A0

L,e II 4j3d.zd oy . /U 0.33 z.3y Z3Z

C 1 . j3 1 1") 1 3Z 4.4y /I 4 z / /"c TT L-e II AIAQ IQ 4j4y. /y CQjy . /U C Q(i J.OD Z.4 / ZZU c 1 . j3 1 3 J A Ad 4.4y 4 Z / TT Le II 1 . /U 1 c D.I J Z.3o 1 A^ 343 C/C .JO 1 oc lOJ A A\ 4.41 11 3U

Ce II 4117.29 .74 2.14 227 .39 93 4.65 2 0

Ce II

A Z Z ^ TA 4551.30 229 .74 2.14 '1 1 A 219 c^ .52 128A CQ 4.60 0 A29

Ort TT Ce II CI AHO 1 5347.81 1 A . /4 1 11 1.13 265 .16A ^ 4ZC 1 1 J.l 1 1 Ay Ce II Ann"^ Ai 4702.01 .81 1 Z A 1.54 249 T A

.30 OA©y

A nc 3Z

/"'^ TT Ce II

AA 'IO 'TO 4418.78 2 0^ .86

C CA 5.50 2.76 210 .61 1 OA i8yA in 4.3 / z A0

Ce II 5330.58 13 .87 6.35 5.16 1.88 303 .37 113 4.67 2 9

TT Ce II 5353.53 1 z 15 00 .00 2.26 366 .63 ^ /IA 24yAAC 4.4j 0 Ay

TT Ce II

A/iri/i A{\

n 1 Z.34 Zoo CO .jy 1loZA Af\ 4.4U 3 AU Ce II 4/ /3.y4 1 / 5.87 4.00 ^ AC Z.Oj Z4y A 1 .41 1 A'? lU/ A CI 4.63 Z 3Z

TT Ce II 4604.21 1 A'5 1.03 1 A/C 1.06 ^ 1 C?A

.zy /4

A OA I ^ A3U

Ce II 5274.24 15 1.04 6.04 4.86 2.13 286 .45 139 4.57 5 9

Ce II 5610.26 26 1.05 6.18 1.44

'1 ^0 378

A .42 169A Z £. 4.56 2 1 n17 Ce II 4686.75 1.09 6.39 1.52 274 .29 78 A TA 4.79 3 31 Ce II 5409.22 23 1.10 2.03 341 .49 176 4.69 0 10 Ce II 4484.83 1.12 6.76 1.95 244 .37

r\ c 95 4.67 2

•^A 29

Ce II 4624.90 27 1.12 6.03 2.32 390 .62 256 4.46 0 30

Ce II 4413.19 1.14 1.79 282 .38 109 4.63 2 28

Ce II 4659.37 1.21 6.33 1.44 218 .28 69 4.83 3 30

Ce II 5187.45 15 1.21 6.12 4.93 2.17 304 .46 151

A Z A 4.54 2 25

Ce II 6043.39 30 1.21 6.61 5.43 1.58 306 .28 88

A 0 T 4.83 4 2 Ce II 5472.30 24 1.25 6.40 1.70 303 .38 133 4.64 1 13 Ce II 4753.65 1.28 1.01 219 .13 29 5.21 2 0

Ce II 4117.59 1.32 2.10 240 .48 123 4.53 2 0

Ce II 4601.37 1.32 1.23 236 .28 68 4.83 3 0

Ce II 5768.90 32 1.32 6.89 1.41 403 .43 183 4.80 0 21

148
Table

B

Spect vV ave- length

Mult EP Log

Log

HW RcW

Q A'

Ce II 5975.87

">

A30 1.33 ^ A1 6.91 1 "?A

1.39 330

A

.20 c o 58

CA 1 5.01 2 1 Ce II 4539.07 1.37 1.73 241 .33 83 4.74 2 0

Ce II 5468.37 24 1.40 6.35 5.22 1.70 273 .36 109 4.70 2 13 Ce II 4608.76 1.41 1.30 203 .20 47 4.99 2 30

Cp tt S61 3 69 32 1.42 1.05 278 19 50 5 04 1 11 7/ Ce II 5683.76 1.42 AO

.98 252 .15 36 5.17 1 21 Ce II 4747.14 1.46 1.84 296 .40 128 4.60 3 32

Ce II 6034.20

*)

A30 1.46 /: A'^ 6.92 1 A-^ 1.02 TCI 353 c .25O c 85 c (\r\ 5.00 0 2 Ce II 4572.79 1 AO 1.48 1 z: 1 1.61 C A 250 T A

.30 OA80

AT Z' 4.76 2 1 A30

Ce TT 5995.35 1.49 1.22 306 .15 48 5.12 1 2 Ce II 4536.89 1.52 1.60 225 .23 C A 54 A Al 4.93 2 0

Ce II

CC 1 ^ AO 5516.08 1 /:! 1 1.61 AO .98 273 .16A42 5.12 2 14 Ce II C A C A Z' A 5959.69 1.63 1 A 1

1.01 283 .16 42 5.14 1 1 Ce II 6143.36 1.70 1 AC 1.05 294 1 O .18 C 1 53 C AZT 5.06 1 0

Ce II 6098.34 1.15 111 .23 11 4.92 1 2 Ce II a A cc c\c\ 6466.90 1 T? 1.77 n A .74 T> C 235 1 1 .13 1 A30 5.22 1 6

Ce II 5359.50 1.78

A 1 .91 278 .16An 47C AA 5.09 1 9

Ce II 5556.97 1 OA 1.80 1 C 1.25 253 .17

AC 45C AA 5.09 1 16 LO I 1 J

.43

C Ol 5.o2 1 A .14 229A

.20

An 47CA 1

5.01 2 A0

Co I 4121.33 28 .92 3.26 2.54 275 .72 237 4.24 2 0

t^O I c<ir\ '70 jj3U. /o 1 o JO 1 n 1 1. /I

C OA j.oUA AC 4.4d .Zl Z64 1 o .lo y1O 4o 5.U6 Z 0

CO I Ai CQ r>i i 1 1 "71 I . / 1 ^ '>A D.ZU

A CQ 4.00 A1 .Ul lly 1 A .lU '>o ZoCT c z Au

y^o I JJJ 1 .40 1 "70

1. /o

C "7C J. /j .3Z "^C c ZOJ '>A .zu CAC A^ 11 Ay LO I oil / .UU 1 'TO

1. /o ^ AO D.Uo

C A'?

— 1 A .14 Z6y A*? 1 A

ly j.jZ CO 11 A Co I 4781.43 57 1.88 6.00 4.68 .04 202 .11 26 5.30 1 32

CO I A/ITQ Q1

Q 1 ol 1 1 /t

C CI

J. 51

— .43 ZoU .Uo lb

C CA 2 A CO I 1 IZ Z.Zo j.y c m/ A CI 4.63 .1 1

265 .12 31 5.26 3 1 A

19 Co I 6632.44 111 111 T T O 2.2o 6.37 A O C 4.85 A'> .02 ^A 1 291 AT .07 A20 C C 5.52 1 0

Co I 641 /.oZ 111 111 Z.Ji

C 1

'5 5.13

— .23 2o4 AO

.Oo 22

C AH 5.46 1 A0

Co I 4813.48 158 3.21 5.05 .78 226 .25 63 4.89 3 32

Co I 40^3. ly 1 j6 i.Zi

C '7"7A '> '> 4.ZZ '>A .14 1 O 1 lol 1 o .loA 1 41 5.06 1 31 Co I 4/yz.oo 1 CO 1 JO

"3

C j.ZjC '>"7 J. 11 4.13 . 1 1

'> "3

A 239 '>A .14CA59An 1 4.91 2 A0

Co I jZIZ. /U 1 /U 1 C 1 3.51 z n

A 5.74 4.32AC .46 203 1 c .16 33 5.16 1 25

Co I j3 jZ.Uj 1 /z

'5 CO 3.5o

C T7 D.I 1 A T7 4.Z / A '> .4Z 254 .17 44C AA 5.09 2 A0

Co I 6455.00 174 3.63 6.16 4.78 -.01 305 .10 30 5.35 1 6

Co I 176 3.71 6.22

CA -.54 AA 209 .13A29CA

5.39 0 30

Co I 6595.87 174 3.71 6.37 4.96 -.52 292 .08 23 5.46 1 0

Co I 5342.70 190 4.02 5.64 4.30 .23 324 .19 61 4.99 2 9

Co I 5444.59 196 4.07 6.02 4.70 -.17 164 .08 15 5.46 1 12 Co I 5454.57 195 4.07 6.05 4 78 -.26 178 I/O 09 1 6 5 40 11 1 3

Cr I 4545.96 10 .94 4.35 1.63 269 .64 186 4.39 5 29

Cr I 4580.06 10 .94 4.26 1.40 281 .58 178 4.41 2 30

Cr I 6330.10 6 .94 5.50 4.43 .22 305 .21 61 5.00 2 5 Cr I 21 .97 4.51 3.56 1.56 281 .53 167 4.45 2 30

Cr I 4616.14 21 .98

A A''\ 4.42 3.33 1.61 289 .60 187 4.39 3 0

Cr I 5296.69 18 .98 4.23 2.89 1.25 283 .53 157 4.50 5 9

Cr I 5300.75 18 .98 4.85 3.53 .65 341 .37 127 4.65 1 9

Cr I 6501.21 16 .98 5.98 293 .10 29 5.35 1 0

Cr I 4600.75 21 1.00 4.27 2.83 1.51 283 .57 174 4.42 2 0

Cr I 4652.16 21 1.00 4.24 2.84 1.75 256 .61 170 4.44 5 30

149
Table

B

Spect

length

Mult EP

— Loe

Log -ox HW Rc

W

—Log

Q

Cr I 5345.81 18 1.00 4.07 2.16 1.61 379 .65 261 4.30 4 9 Cr I 5348.32 18 1 AA 1.00 4.27 1 A^ 2.96 1.31 278 .56 •t n A 174 A A £l 4.46 A4 9

Cr I 4646.17 21 1 A1 1.03

A 11 4.33 1C\ 2.39A 1 2.01 374 .66 238AA

4.29 2

'JA30

Cr I 5409.79 1 018 1 AO 1.03

"5 A^ 3.42 1 "7

A 1 .79 1 on 1.87

'5

A 329 .66 251 4.33 2 10 Cr I 6630.02 16 1 A1 1.03 6.17 A AA 4.90 1187 AT

.u / 15

C CO 5.52 11 8 Cr I 4526.47 33 2.54 3.95 1.21 313 .65 213 4.33 3 29

Cr I 4535.15 33 2.54

CA Z 5.45 1 OA 3.89 .31 226 .24 56AA 1 4.91 1 0

Cr I 4540.50 33 2.54

A 00 4.82 OA 1 A1 1 .Ul 254A 1 .41 1 1 A 1 lUA C"> 4.d2 1 AU Cr I 4621.y4 32 2.54 c r\c C A .54 2 /8 .32 OAyu A ni 4. /3 13

1C\ 3U

Cr I A£i ACi Ai^ 464y.4D 32 2.54 5.d2

A OA 4.2U 1 c

.Id o 1 0 218 .11 CA5U

A QC 4.yD 11 lA3U

Cr I 4790.34 31 2.54 5.75 4.62 218 .13 33 5.22 1 32

Cr I 5238.97

CA

2.71 5.81

A4.5 / — ^1 .15 1 c 1 151 .14 OT2/ CIA 5.iy 1 1Clb

Cr I A/C ^ on 2.8y c nc 5. /o .ly 0 1 A 21U OA .2U /I "J 43

C A1 5.U1 11 AU Cr I 5329.12 A A 94 A 1 2.91 A cn 4.6/ 1 A1 3.43 .31 0 c 1 253 "3 c .36 any / A nn 4. /U AU Ay Cr I An Z A HA 4 /j4. /4 168 1 An C AO 5.U8 0/(0 24y "2 A .3U 0/1 84 A nn 4. / / 13 1032

Cr I 4756.11 145 3.10 4.88 3.61 1.05 267 .42 118 4.60 3 0

Cr I A

A OA 4664.80 1 QC 186 3.12A AA c 1 .51 226 1 A .34 nQ/8A TC 4. /5 13 JA3U

Cr I Ai^QCi in 46oy.3 / 1 QC. 186 3.12 5.42 "30 .38 312 ic .3d 1 1 A 1 lU

A Q< 4.85AU 1 1

31 Cr I Anf\Q f\A 4 /Uo.U4 1 QC 186 3.1 / C A^ 5.02 1 CI 3.d3 nc\ . ly O/10 24y AC\ .4U 1 1 A 1 lU A CI 4.03 13 1032

Cr I An ^ Q Ai 4/I0.43 1 QC 186 "3 1 A3.iy

A OA 4.8y 1 A ^ 3.41 on .8y 11(\ 33U A(\ .4y 1 Tl 1/1A AQ 4.48 02 1032

Cr I 4604.58 190 3.32 5.29 3.85 265 .28 80 4.79 2 30

Cr I J /oi.l 1188 3.32 5. /I

A 1C 4.36

— A'2 .U3 Id") 3U2 1 0

.18 53

C AC 5.U5 02 0 1

21 Cr I cnon QQ 188 3.32 C AQ 5.48 A AQ 4.U8 1 1 .13 OQT 282 .2 / Q 1 81 4.55 3

0121 Cr I C-TQn QQ 1 QQ 188 3.32 A Ql 4.8 / c 1 .Dl 3U2 .45 1 <^ 155 4.5 / 3

01Zl Cr I 4j!> /.jZ 1 00 iy8 3.3 / c '^A 5.24 Til 213 .2 / D / A Q1 4.83 3 072 / Cr I 5405.00 191 3.37 6.09 4.76 -.29 243 .10 24 5.35 1 0

Cr I 5206.52 206 3.43 c 0 c 5.85

A CO 4.52 "iC(\ 26U 0 /I .24 CA64A at 4.yi 02 AU Cr I 5664.U4 203 1 /IT 3.43 C CA 5.5U 4,21 — .11 2/3 1 0 .ly C 1 51 C CiA 5.U4 13 1 Q18 Cr I 52 /2.01 225 3.45 C T c 5. /5 A 1 A 4.34 — f\C .U6 0 CO 258 0 1

.21 c c 55

A QC 4.y8 02 AU Cr I 5312.00 225 1 AZ 3.45 c 0 1

5.81 y1 AQ 4.48

— nA .24 23y 1 A .lU 0/1 24 c 1C 5.35 02 AU Cr I 4622.49 233 3.55 5.42 3.78 .22 265 .31 93 4.73 2 30

Lr I 4625.y2 ^ A

A 244 1 Q Z 3.85C AA OAO 2uy 1 1

.13 OQly

C 1Q 5.3yAUlA3U

Lr I AO 666I.U0 282 4.iy

C T7 6.2 / A CiC 4.yo

— CA .51) 2y3 c\n .U / OA2U

C CO 5.52 11 U Cr II C3 AC OC 5305.85 24 1 Q1 3.83 C *7A 5. /U A in 4.3 / — 1 TO 2.38 OQ 1

2yi 7 1.3 1

OAyuA nn 4. / / 3 Qy Cr II 4812.36 '3 A30 1 QC 3.86 C 1 1 5.31 A f\1 4.U3 — 2.32 0 CO 25y 1 1

.31 OAyu

A TC 4. /5 3 33

Cr II 4588.22 44 4.07 4.82 -1.34 296 .58 195 4.39 5 30

Cr II

AC C\C\ 4592.09 44 4.07 5.24

— A^ 2.06 260

A "5 .43 110 1 loA CA 2 AU Cr II 4616.63 44 4.07 5.38 4.18 ^A -2.20 *? Az: 306 A.46 ^ ACi 149 A4.52 2 1 A30

Cr II 5308.44 43 4.07 5.66 4.32 -2.40 253 0 0 .28 lb

A 0 A 4.o4 3 Ay Cr II 5310.70 43 4.07 6.01 4.74 -2.69 252 .17 A 'J 43 C AA 5.09 1 A0

Cr II 5313.59 43 4.07 5.51 4.29 -2.15 329 .40 129 4.62 3 9

Cr II 5334.88 43 4.07 5.57 4.16 -2.28 253 .31 91

A4. Il 2 9

Cr II 5502.05 50 4.17 5.80 4.63

— 2.32 271 .23 C"i 62

A C\A 4.94 2 13 Cu I 5105.55 2 1.39 4.40 2.78 .63 1 A 319 ^ A

.60 207

A "3A

4.39 2 u Cu I 5700.28 2 1.64 5.77 -.43 303 .25 78 A 00 4.88 3 21 Cu I 5782.13 2 1.64 4.89 3.01 .13 335 .47 167 4.54 3 0

Dy II 4103.34 .10 5.56 3.07 246 .53 140 4.47 2 0

Dy II 5169.71 .10 6.14 1.35 235 .10 27 5.28 1 0

Dy II 4073.12 .54 5.99 2.84 233 .45 111 4.56 2 0

Eu II 4129.73 1 .00 4.52 3.31 111 .73 242 4.23 2 0

150
Table B

Spect WavelengthMult EP -Log

V ' A J -Log

X,

I OCT

-Ox

HW Rc W -Log

(Wlk) Q N

Fll IT 6437.64 8 1.32 6.18 1.31 292 .1

1

32 5.30 2 0

6645 1

1

g 1.38 6.37 1.36 308 .14 43 5.19 2 0

4347.24 2 .00 4.85 246 .43 112 4.59 2 0

Fe I 5110!41 1 .00 3.61 1.46 .37 337 .70 291 4.25 3 0

Fe I 5166.29 1 .00 3.78 1.40 .03 341 .66 235 4.34 4 25

Fe I 4389.24 2 .05 4.36 251 .60 165 4.41 1 28

Fe I 4445.48 2 .09 5.10 244 .38 102 4.65 5 28

Fe I 4461.65 2 .09 3.53 .84 301 .74 246 4.26 2 0

Fe I 4482.17 2 .11 2.71 .68 366 .80 319 4.15 5 29

Fe I 5225.53 1 .11 4.55 2.91 354 .52 168 4.49 3 26

Fe I 4489.74 2 .12 4.12 .11 295 .69 224 4.30 3 0

Fe I 5269.54 15 .86 1.86 .47 1.40 518 .82 441 4.08 3 9

Fe I 5956.70 14 .86 4.88 3.83 307 .38 113 4.69 2 1 Fe I 6280.62 13 .86 5.03 306 .48 161 4.56 5 5 Fe I 6358.69 13 .86 4.63 3.29 329 .45 158 4.58 2 5 Fe I 5397.13 15 .91 2.52 1.04 .82 392 .77 341 4.20 2 10 Fe I 5371.49 15 .96 2.30 .76 1.05 457 .80 402 4.13 4 9

Fe I 5429.70 15 .96 2.35 .87 556 .77 465 4.07 4 11 Fe I 5501.47 15 .96 3.99 2.35 -.00 389 .65 277 4.30 4 13 Fe I 6498.96 13 .96 5.20 4.02 363 .34 134 4.70 4 6

Fe I 4139.94 18 .99 4.00 -.34 254 .57 156 4.42 2 0

Fe I 4653.49 17 .99 5.89 312 .27 90 5.00 0 30

Fe I 5405.78 15 .99 2.42 1.27 .86 405 .77 348 4.19 2 10 Fe I 5446.92 15 .99 2.56 .72 404 .78 360 4.18 1 12 Fe I 5506.78 15 .99 3.92 1.80 .18 404 .66 285 4.29 3 14 Fe I 6551.70 13 .99 6.03 234 .08 19 5.46 1 7 Fe I 6574.24 13 .99 5.59 4.11 281 .26 82 4.89 2 7 Fe I 5434.53 15 1.01 3.00 1.43 .63 387 .71 294 4.27 5 11 Fe I 5497.52 15 1.01 3.80 1.80 .11 402 .73 337 4.21 5 13 Fe I 4383.55 41 1.48 1.31 2.48 627 .90 630 3.84 2 27

Fe I 4602.94 39 1.48 4.05 1.36 .53 281 .70 225 4.31 4 30

Fe I 5171.61 36 1.48 3.26 .76 347 .71 272 4.28 4 25

Fe I 6710.32 34 1.48 5.93 4.52 350 .16 48 5.13 3 8

Fe I 4337.05 41 1.56 3.53 .73 294 .75 251 4.24 3 0

Fe I 4404.75 41 1.56 1.40 2.13 643 .87 613 3.86 3 28

Fe I 4592.66 39 1.56 4.05 -.01 337 .70 261 4.25 4 30

Fe I 5194.94 36 1.56 3.81 1.95 .33 380 .67 263 4.30 2 25

Fe I 5332.90 36 1.56 4.26 -.39 329 .58 220 4.40 1 9

Fe I 4325J6 42 L61 L48 2^18 628 !86 587 3.87 3 27

Fe I 4602.00 39 1.61 4.68 2.98 -.66 275 .51 152 4.49 5 30

Fe I 4632.92 39 1.61 4.06 -.46 291 .61 189 4.39 2 0

Fe T 4672 83 40 11 .\J611 5 27 4.14 171 .22 38 5.02 1 31 Fe T 5307 37 36 11 . 61vl 1 4.42 2.64 -.56 303 .54 175 4.47 5 9

Fe I 5341.03 37 1.61 3.06 .32 366 J3 297 4.25 3 9

Fe I 5202.34 66 2.18 3.43 1.32 .07 342 .66 253 4.31 5 25

Fe I 6062.89 63 2.18 5.77 4.21 -1.88 286 .16 46 5.12 2 0

Fe I 6151.62 62 2.18 5.33 4.01 -1.38 283 .33 111 4.74 3 3 Fe I 6265.14 62 2.18 4.88 -.66 353 .50 180 4.52 5 5 Fe I 6430.85 62 2.18 4.45 2.87 -.22 375 .57 230 4.43 5 6

Fe I 4442.34 68 2.20 2.84 .66 391 .77 307 4.16 5 28

151
Table

B

Spect

W 3.VC" length

Mult EP Log

X'r.

TLog

Log -ex HW Rc

W Log

Q

N

Fe I 4447.13 69 2.20 4.71 -.73 261 .49 136 4.51 3 0

Fe I 4478.04 69 2.20 5.70 -1.53 213 .20 44 5.01 4 29

Fe I 5143.73 65 2.20 5.56 4.41 264 .28 76 4.83 2 0

Fe I 5145.11 66 2.20 5.14 3.83 -1.18 295 .45 141 4.56 2 0

Fe I 6137.00 62 2.20 4.97 3.65 -1.08 343 .41 148 4.62 2 0

Fe I 6219.29 62 2.20 4.74 3.09 -.74 329 .50 175 4.53 5 5 Fe I 6335.34 62 2.20 4.48 3.06 -.55 305 .52 173 4.52 5 5 Fe I 4430.62 68 2.22 3.74 .12 329 .70 260 4.23 3 28

Fe I 4447.72 68 2.22 2.81 .56 329 .72 259 4.23 5 28

Fe I 5198.71 66 2.22 4.45 2.64 -.29 304 .57 174 4.45 5 25

Fe I 6015.25 63 2.22 6.42 5.04 266 .08 21 5.46 1 0

Fe I 6082.72 64 2.22 5.43 4.13 -1.65 306 .24 74 4.91 2 2 Fe I 6173.34 62 2.22 5.18 3.47 -1.12 330 .41 152 4.61 2 3 Fe I 6213.44 62 2.22 5.03 3.59 -.87 329 .49 173 4.53 4 5 Fe I 6240.66 64 2.22 5.34 4.07 -1.39 331 .33 114 4.74 3 0

Fe I 6297.80 62 2.22 4.99 3.65 -1.02 329 .45 151 4.59 4 5 Fe I 4439.89 116 2.28 4.98 -.93 266 .38 97 4.66 2 28

Fe I 4630.13 115 2.28 4.74 3.17 -.74 249 .56 161 4.45 2 30

Fe I 5322.05 112 2.28 4.91 3.66 -.82 291 .41 124 4.62 4 9

Fe I 5436.59 113 2.28 5.32 3.93 -1.56 285 .31 91 4.77 1 0

Fe I 6254.26 111 2.28 4.33 -.76 376 .52 214 4.47 3 5 Fe I 6392.53 109 2.28 6.07 4.59 -1.90 292 .12 35 5.26 1 0

Fe I 6421.36 111 2.28 4.72 2.57 -.31 352 .57 207 4.46 5 6

Fe I 6481.88 109 2.28 5.04 3.51 -1.17 355 .38 142 4.66 2 0

Fe I 6608.03 109 2.28 5.81 4.56 -2.09 304 .12 39 5.26 1 7 Fe I 6252.56 169 2.40 4.41 -.20 353 .57 212 4.45 5 5 Fe I 6494.97 168 2.40 3.81 1.74 .24 375 .61 260 4.40 3 6

Fe I 5141.75 114 2.42 4.41 3.16 -.59 358 .50 189 4.47 3 24

Fe I 6663.45 111 2.42 4.90 3.45 -.96 444 .43 192 4.56 2 8

Fe I 6344.15 169 2.43 5.13 3.82 -1.27 376 .42 182 4.80 0 5 Fe I 6393.61 168 2.43 4.35 2.72 -.04 376 .58 230 4.43 3 6

Fe I 6593.88 168 2.43 4.73 3.41 -.96 375 .44 175 4.58 5 7 Fe I 5916.25 170 2.45 5.17 3.74 -1.10 312 .32 104 4.76 3 0

Fe I 6136.62 169 2.45 4.03 2.35 .08 381 .59 243 4.40 3 0

Fe I 6256.37 169 2.45 4.79 -1.00 353 .51 208 4.48 3 5 Fe I 6462.75 168 2.45 4.97 -.96 422 .65 305 4.73 0 6

Fe I 5701.55 209 2.56 4.61 -.53 310 .48 178 4.52 2 21 Fe I 6230.73 207 2.56 3.91 -.03 423 .62 285 4.34 5 5 Fe I 6609.12 206 2.56 4.92 3.67 -1.35 375 .35 133 4.70 2 7 Fe I 5778.47 209 2.59 5.84 4.46 247 .19 48 5.06 2 21 Fe I 6005.53 207 2.59 5.73 -1.86 330 .17 53 5.07 2 2 Fe I 6137.70 207 2.59 4.16 1.89 -.09 377 .59 236 4.41 3 3 Fe I 6322.69 207 2.59 4.90 3.83 -1.06 305 .41 140 4.64 4 5 Fe I 6575.02 206 2.59 5.07 -1.35 398 .40 175 4.60 3 7 Fe I 4319.45 214 2.61 5.80 -1.82 209 .20 43 5.01 1 0

Fe I 6065.49 207 2.61 4.30 2.70 -.20 377 .57 221 4.43 4 2 Fe I 6200.32 207 2.61 5.15 3.33 -1.12 329 .41 144 4.63 4 4 Fe I 6677.99 268 2.69 4.37 -.14 421 .51 211 4.50 4 8 Fe I 6180.22 269 2.73 5.40 3.92 -1.37 306 .34 116 4.72 4 3 Fe I 6592.92 268 2.73 4.34 3.01 -.36 351 .50 202 4.51 2 7

152
Table B

Spect \^ ave- length

Mult EP — Log

X'r -Log

Log

-^x

HIV Rc r

-Log

( Wl\) Q N

Fe I 6546.25 268 2J6 4.57 3.14 -.48 352 .53 216 AM 2 7 Fe I 6703.57 268 2.76 5.58 4.21 -1.82 280 .21 66 4.99 1 8 Fe I 4091.56 357 2.83 4.66 -.83 231 .43 105 4.59 3 0

Fe 1 4454.38 350 2.83 4.32 -.06 283 .63 198 4.35 3 0

Fe I 4466.55 350 2.83 3.60 .63 344 .76 282 4.20 3 29

Fe I 4683.57 346 2.83 5.09 3.73 -1.08 302 .37 113 4.65 2 31 Fe I 4741.53 346 2.83 4.69 3.39 -.69 311 .52 178 4.45 4 32

Fe I 6311.51 342 2.83 5.73 4.33 -1.64 295 .15 44 5.15 2 0

Fe I 6518.38 342 2.83 5.13 3.92 -1.32 355 .37 138 4.68 3 0

Fe I 4422.57 350 2.84 3.76 .22 407 .77 333 4.32 0 28

Fe I 4476.02 350 2.84 3.18 .58 313 .73 242 4.27 5 29

Fe I 4635.85 349 2.84 5.11 3.65 -1.00 249 .38 91 4.68 1 30

Fe I 6229.23 342 2.84 5.53 4.02 -1.53 353 .28 89 4.84 4 5 Fe I 6355.04 342 2.84 5.09 3.14 -1.17 329 .40 147 4.63 2 5 Fe I 6270.24 342 2.86 5.31 3.82 -1.34 306 .36 127 4.69 2 5 Fe I 4768.40 384 2.94 5.02 -1.21 299 .56 172 4.65 0 32

Fe I 5232.95 383 2.94 2.33 .75 .79 392 .70 306 4.23 5 26

Fe I 4120.21 423 2.99 4.00 -.15 256 .59 163 4.40 2 0

Fe I 4348.94 414 2.99 4.79 -1.12 235 .42 108 4.60 4 27

Fe I 4365.90 415 2.99 5.00 -1.17 188 .35 75 4.74 2 27

Fe I 4603.95 410 2.99 5.81 -1.88 250 .27 72 4.95 0 30

Fe I 4721.00 409 2.99 5.09 -1.40 280 .38 112 4.64 4 32

Fe I 4787.84 384 3.00 5.19 3.86 -1.49 249 .26 69 4.86 3 32

Fe I 5266.56 383 3.00 2.65 .93 .42 384 .68 285 4.27 5 9

Fe I 4376.78 471 3.02 4.94 -1.04 219 .41 90 4.65 2 27

Fe I 4740.34 409 3.02 5.30 -1.42 339 .63 226 4.62 0 32

Fe I 4772.82 467 3.02 4.37 -.78 249 .58 161 AAA 5 32

Fe I 5326.15 407 3.02 5.47 329 .22 73 4.91 1 9

Fe I 5191.46 383 3.04 3.41 1.39 .32 494 .75 381 4.25 0 25

Fe I 5281.80 383 3.04 3.41 1.53 .03 329 .60 212 4.39 5 9

Fe I 4343.70 517 3.05 4.57 -.90 265 .56 160 4.43 1 0

Fe I 4436.95 516 3.05 4.50 -1.18 219 .48 109 4.57 4 28

Fe I 4480.14 515 3.05 4.92 -.81 325 .53 180 4.43 2 29

Fe I 4793.96 512 3.05 6.06 4.88 -2.32 218 .09 21 5.40 1 32

Fe I 4517.53 472 3.07 4.80 -.93 306 .55 166 AAA 3 29

Fe I 5460.91 464 3.07 6.22 4.87 250 .12 30 5.26 1 0

Fe I 4067.99 559 3.21 3.32 .33 261 .65 206 4.29 2 0

Fe I 4531.63 555 3.21 4.94 -1.16 250 .47 123 4.55 2 29

Fe I 4574.24 554 3.21 5.36 4.01 -1.60 219 .27 61 4.86 1 30

Fe I 5324.19 553 3.21 2.40 .75 .57 367 .68 265 4.30 4 9

Fe I 5909.99 552 3.21 5.59 4.06 378 .29 110 4.77 3 1 Fe I 4070.78 558 3.24 4.07 -.01 254 .60 165 4.39 2 0

Fe I 4098.18 558 3.24 3.70 -.14 258 .61 189 A.3A 2 0

Fe I 4625.05 554 3.24 4.55 2.98 -.62 390 .62 256 4.46 0 30

Fe I 4788.76 588 3.24 4.67 3.61 -.91 249 .45 125 4.57 5 32

Fe I 5283.63 553 3.24 2.91 .26 404 .66 283 4.27 3 9

Fe I 4780.81 633 3.25 6.03 4.81 -2.20 218 .10 26 5.35 1 32

Fe I 4808.16 633 3.25 5.46 4.21 -1.84 216 .17 41 5.08 2 32

Fe I 4504.84 555 3.26 5.09 -1.48 244 .36 92 4.69 1 0

Fe I 4568.79 554 3.26 5.23 -1.60 250 .37 100 4.86 0 30

153
Table

B

Spect

W 3VG- 1 (=> n trt n Mult EP Log Log

Log

-Ox

HW Rc

W Log 1 1T/I\ \ Q

Fe I 4668.14 554 3.26 3.98 -.30 280 .60 174 4.41 3 31 Fe I 5263.31 553 3.26 4.07 -.15 349 .57 223 4.40 3 9

Fe I 5339.94 553 3.26 3.49 1.91 -.06 354 .62 230 4.37 3 9

Fe I 5848.09 552 3.26 5.45 4.24 251 .18 48 5.07 2 22

Fe I 4377.80 645 3.27 5.21 -1.39 204 .28 59 4.85 3 27

Fe I 4813.11 630 3.27 5.60 -1.97 248 .17 45 5.06 2 33

Fe I 5277.31 584 3.27 6.20 253 .11 27 5.30 1 9

Fe I 4598.12 554 3.28 4.56 2.98 -.73 271 .50 145 4.50 3 0

Fe I 5229.86 553 3.28 4.03 -.18 303 .55 180 4.45 4 26

Fe I 5253.48 553 3.28 4.77 3.38 -.79 303 .45 135 4.58 4 9

Fe I 4566.52 641 3.30 5.31 3.76 -1.36 187 .25 52 4.92 2 30

Fe I 4595.36 594 3.30 4.85 -1.00 312 .56 181 4.62 0 30

Fe I 4741.08 688 3.33 5.41 -1.66 296 .34 108 4.68 4 32

Fe I 4807.73 688 3.37 4.90 3.78 -1.49 255 .30 82 4.78 3 32

Fe I 5586.76 686 3.37 2.80 1.28 .28 378 .68 286 4.29 5 17 Fe I 5572.85 686 3.40 3.04 1.27 .19 504 .67 342 4.21 2 17 Fe I 4566.99 723 3.41 5.78 -1.91 234 .32 80 5.10 0 30

Fe I 4779.44 720 3.41 5.07 3.91 -1.55 218 .28 65 4.85 2 32

Fe I 5569.63 686 3.42 3.61 2.11 -.04 378 .64 280 4.30 2 17 Fe I 5624.55 686 3.42 3.91 -.29 353 .57 226 4.41 2 17 Fe I 5576.10 686 3.43 4.28 2.97 -.44 328 .59 251 4.37 4 17 Fe I 4059.71 767 3.55 4.52 -.65 242 .52 135 4.48 2 0

Fe I 4547.85 755 3.55 4.62 2.99 -.34 244 .56 156 4.45 5 29

Fe I 4502.60 796 3.57 5.67 3.95 -1.65 188 .24 51 4.93 1 29

Fe I 4587.13 795 3.57 5.15 - 1.16 281 .37 110 4.65 3 30

Fe I 4809.94 793 3.57 5.74 4.37 -2.17 201 .12 24 5.26 3 32

Fe I 5365.41 786 3.57 4.77 -.66 309 .48 163 4.52 2 10

Fe I 5466.99 784 3.57 5.61 -1.54 248 .25 64 4.91 1 13 Fe I 5584.77 782 3.57 5.55 4.03 -1.47 296 .33 102 4.74 2 0

Fe I 6019.36 780 3.57 6.46 4.90 260 .05 13 5.67 1 0

Fe I 4388.41 830 3.60 4.06 -.23 277 .62 194 4.36 3 0

Fe I 4484.23 828 3.60 4.56 -.19 250 .57 155 4.44 3 29

Fe I 4525.15 826 3.60 3.83 1.46 -.24 297 .69 224 4.31 2 0

Fe I 4596.06 820 3.60 4.88 -1.15 296 .49 151 4.69 0 30

Fe I 4619.29 821 3.60 4.71 3.37 -.67 273 .50 146 4.50 2 0

Fe I 4638.02 822 3.60 4.50 -.64 312 .53 174 4.45 3 30

Fe I 4678.85 821 3.60 4.26 2.80 -.24 289 .58 181 4.41 3 0

Fe I 6246.33 816 3.60 4.50 2.90 -.58 329 .49 183 4.52 3 5 Fe I 4568.86 894 3.63 5.72 -1.73 250 .37 100 4.96 0 30

Fe I 5207.94 880 3.63 5.81 -1.58 291 .27 88 4.81 1 25

Fe I 5223.19 880 3.63 5.64 4.23 -1.59 215 .20 48 5.02 2 26

Fe I 5397.60 841 3.63 5.70 4.30 256 .17 44 5.09 2 0

Fe I 4558.11 894 3.64 5.74 -1.80 234 .28 63 4.84 4 30

Fe I 4708.98 889 3.64 5.34 -1.23 280 .50 152 4.90 0 32

Fe I 4799.41 888 3.64 5.37 -1.62 273 .39 111 4.84 0 32

Fe I 4802.88 888 3.64 4.77 -1.18 249 .37 98 4.68 3 32

Fe I 5636.71 868 3.64 5.90 4.45 -1.55 264 .15 40 5.15 1 0

Fe I 5698.05 867 3.64 6.00 4.65 262 .13 34 5.22 2 0

Fe I 5707.05 868 3.64 5.37 -1.47 341 .24 90 4.85 1 21 Fe I 4433.22 830 3.65 4.19 -.42 276 .59 176 4.40 2 0

154
Table B

Spect Wave1 n crt h Mult EP — Log — Log

Log -sx HW Rc W

— Log

{ Wl\ \

y yy 1 A) Q N

Fe I 4485.97 825 3.65 5.77 -1.78 250 .31 94 4.98 0 29

Fe I 4580.59 827 3.65 5.27 -1.61 375 .46 183 4.76 0 30

Fe I 4596.43 823 3.65 5.50 4.03 -1.84 250 .23 60 4.91 1 30

Fe I 4611.28 826 3.65 4.11 -.44 291 .62 194 4.38 2 0

Fe I 4643.47 820 3.65 4.86 2.93 -.91 281 .46 125 4.56 2 30

Fe I 4673.17 820 3.65 4.69 -.85 311 .53 189 4.43 4 31 Fe I 4709.09 821 3.65 4.66 -.90 280 .50 152 4.70 0 32

Fe I 4745.81 821 3.65 4.77 -.88 280 .56 166 4.44 4 32

Fe I 6232.66 816 3.65 4.96 -1.05 400 .45 183 4.55 4 5 Fe I 6301.52 816 3.65 4.33 3.23 -.54 305 .50 182 4.52 4 5 Fe I 6411.66 816 3.65 4.33 2.93 -.32 329 .53 191 4.50 4 6

Fe I 4438.35 828 3.69 5.16 -1.31 307 .41 123 4.67 0 28

Fe I 4446.84 828 3.69 4.66 -.89 259 .48 133 4.53 3 0

Fe I 4481.62 827 3.69 5.14 -1.03 246 .38 98 4.66 2 0

Fe I 4598.74 819 3.69 5.97 4.43 -2.12 218 .17 39 5.08 1 30

Fe I 4690.15 820 3.69 5.07 3.65 -1.15 254 .36 95 4.69 1 0

Fe I 4700.17 935 3.69 5.07 3.62 -1.35 302 .37 105 4.66 5 32

Fe I 4701.05 820 3.69 5.33 -1.59 296 .27 82 4.80 3 32

Fe I 4704.96 821 3.69 4.96 3.54 -1.04 265 .37 101 4.67 3 32

Fe I 4768.32 821 3.69 4.78 -1.17 299 .56 172 4.65 0 32

Fe 1 5288.53 929 3.69 5.12 -1.20 298 .35 111 4.69 4 9

Fe 1 5379.58 928 3.69 5.12 3.69 -1.22 311 .41 127 4.62 3 10

Fe I 5543.18 926 3.69 5.07 3.40 -1.18 327 .38 138 4.63 4 15 Fe I 6336.83 816 3.69 4.41 3.10 -.65 329 .46 171 4.56 5 5 Fe I 6408.03 816 3.69 4.94 3.27 -.76 376 .45 178 4.56 1 6

Fe I 5809.25 982 3.88 5.31 3.84 -1.42 290 .31 97 4.78 4 22

Fe I 6003.03 959 3.88 4.80 3.50 -1.01 283 .42 130 4.63 3 2 Fe I 6008.58 982 3.88 4.77 3.42 -.96 306 .41 132 4.64 2 2 Fe I 6220.78 958 3.88 5.97 4.46 -2.04 289 .14 40 5.19 2 0

Fe I ^ ^ ^ ^ dlld.ll 981 3.88 5.80 4.28 -1.80 282 .16 45 5.13 2 5 Fe I 5934.66 982 3.93 4.91 3.46 -1.04 330 .40 151 4.61 3 1 Fe I 4551.67 972 3.94 5.67 4.11 -1.79 203 .24 59 4.90 1 29

Fe I 4593.54 971 3.94 5.70 4.09 -1.80 281 .39 106 4.83 0 30

Fe I 5976.80 959 3.94 5.12 3.74 -1.20 306 .34 113 4.72 2 1 Fe I 6188.00 959 3.94 5.59 3.92 282 .28 91 4.83 4 4 Fe I 5883.81 982 3.96 4.66 -1.11 331 .34 125 4.70 3 1 Fe I 5952.75 959 3.98 5.06 3.79 -1.28 305 .28 88 4.83 1 0

Fe I 6096.69 959 3.98 5.58 4.14 -1.66 353 .19 60 5.02 1 2 Fe I 5329.99 1028 4.07 5.09 -1.11 399 .38 155 4.59 3 9

Fe I 5403.82 1029 4.07 5.09 3.55 -.83 300 .40 126 4.63 1 0

Fe I 5494.47 1024 4.07 5.74 4.30 -1.80 201 .15 32 5.19 1 13 Fe I 6027.06 1018 4.07 5.18 3.64 -1.11 306 .35 119 4.71 4 2 Fe I 6157.73 1015 4.07 5.40 -1.26 353 .44 187 4.75 0 3 Fe I 6315.81 1014 4.07 5.66 4.13 -1.55 306 .20 62 5.01 1 0

Fe I 5353.39 1062 4.10 4.85 -.97 366 .63 249 4.50 0 9

Fe I 5493.51 1061 4.10 5.55 -1.68 332 .36 119 4.87 0 13 Fe I 4800.65 1042 4.14 4.76 2.97 -1.26 261 .37 113 4.65 2 32

Fe I 5187.92 1032 4.14 5.24 3.41 -1.29 278 .35 109 4.69 2 25

Fe I 5487.76 1025 4.14 4.67 -.97 428 .49 222 4.45 2 13 Fe I 6127.91 1017 4.14 5.41 -1.49 330 .27 84 4.86 2 3

398-978 0 - 71 - 11 155
Table B

Spect Wavelength

Mult EP — Log -Log

K

Log

(gfk)

-dx

HW Rc W

— Log

(Wl\)

0 yv

re I DlDJ.J /

1 A1 S iUlo A4.1'+ 1 A J.OJ 1 S7 781 7/1 .Z4 77/ ZA Q7 4.yz 1 3 Fe I 6315.32 1015 4.14 5.36 3.47 -1.35 305 .39 129 4.67 3 5 Fe I 5391.49 1062 4.15 4.85 -1.04 405 .47 205 4.48 5 10 Fe I 5473.91 1062 4.15 4.82 3.41 -.99 303 .45 160 4.55 1 13 Fe I 5607.66 1058 4.15 6.07 4.54 262 .15 39 5.15 2 0 re I ^ 1 11 7rt JlJj. /V A 1 fi 1 A") J.4Z 1

1

— .1

1

1/17 34 / A7 .oz 717 A 1A 4.i4 cJ7/1 Z4

Fe I 5662.52 1087 4.18 4.68 -.57 297 .47 152 4.55 2 18 Fe I 5491.84 1031 4.19 6.15 4.75 138 .08 11 5.46 1 13 Fe I 5563.60 1062 4.19 4.65 2.78 -1.07 293 .49 154 4.54 5 16 Fe I 5715.11 1061 4.19 4.96 3.80 -1.25 353 .40 155 4.60 5 21 reFp. T1

1 ni 8 A 1 Q J. jt — 1 Af, 1 .to lOA 11 11 70ZU A 71 1z

cJ Fe I 6380.75 1015 4.19 5.56 3.93 -1.32 305 .27 93 4.84 4 6

Fe I 5608.98 1108 4.21 6.27 4.58 256 .12 31 5.26 1 0

Fe I 5618.65 1107 4.21 5.45 4.03 -1.22 278 .30 91 4.79 1 17 Fe I 5762.99 1107 4.21 4.59 -.60 323 .51 187 4.49 3 21 Vfre T1

1ixiyL 007 A 77 A 74 7 01 A.y I A1 104 jU4 S/l

. J4 1 87 1 oZ A A(^ 4.40 1 7SZj

Fe I 5228.41 1091 4.22 5.08 -.94 316 .48 152 4.53 3 26

Fe I 5543.93 1062 4.22 5.08 3.78 -1.28 383 .37 142 4.63 1 15 Fe I 5547.00 1061 4.22 5.67 4.20 -1.88 224 .22 52 4.99 1 15 Fe I 5638.27 1087 4.22 4.94 -1.00 325 .44 153 4.57 3 17 r c 1 JS77S / 1 J .\jy OQ 1 nR7 A 77 s If, j.y 1 071 —— 11.1/17 777 Z / / 14 1 oi lUl A lA 1 71Zl Fe I 5793.93 1086 4.22 5.73 4.19 -1.66 272 .20 64 4.98 3 21 Fe I 5196.10 1091 4.26 4.78 3.65 -.74 279 .42 120 4.62 1 25

Fe I 5635.85 1088 4.26 5.66 4.18 -1.47 271 .19 52 5.03 1 0

Fe I 5641.46 1087 4.26 5.11 3.62 -1.19 321 .35 117 4.69 2 17

-TC Fp t

1

II1I 08Wo A 7fi J.S 70ly A 1^ —— 1 SI 1 .J 1 10S . 11 7/ S OS 7Z11 7/ Fe I 511>\.ll 1087 4.26 5.19 -1.15 320 .35 120 4.69 3 21 Fe I 5753.14 1107 4.26 4.92 3.64 -.82 290 .43 129 4.62 1 21 Fe I 5717.85 1107 4.28 5.13 3.75 -1.09 313 .38 125 4.66 3 0

Fe I 5804.46 1087 4.28 5.96 252 .14 41 5.19 1 22 reVp t

1

1 08A A 78 S 88 J.oo A 11 4. J /1 71 1 . /

1

7QO zyu 1 7 .1 / S7jZ S 07 J.y) 1

11 77ZZ Fe I 5856.08 1128 4.29 5.72 4.19 -1.47 282 .19 54 5.03 1 0

Fe I 5109.66 1089 4.30 4.92 3.36 -1.21 282 .39 115 4.65 2 0

Fe I 5691.51 1087 4.30 5.54 -1.42 278 .28 76 4.85 4 21 Fe I 5705.48 1087 4.30 5.55 4.19 -1.41 273 .21 58 4.99 2 21 Vpre t

1 <-io-2 -17 J JOJ. J 1

1 1 A 1

1

1 OQ i.yjy 1 70 (\i 141 Ai 71^; ZJO A Ifi z1lUo Fe I 5267.28 1146 4.37 5.74 265 .15 39 5.14 1 9

Fe I 5315.07 1147 4.37 5.56 4.15 -1.74 256 .19 49 5.03 1 0

Fe I 5369.95 1146 4.37 3.33 1.61 -.14 341 .61 231 4.37 1 10 Fe I 5400.51 1145 4.37 4.33 -.63 329 .56 209 4.42 1 10 re I j4Uo. / / 4.3 / ^ < 1 J. j1 A t Q 77Q Z /o 7 1 .Zi Dl A 5

1 n Fe I 5409.14 1147 4.37 5.18 -1.52 341 .49 176 4.69 0 10

Fe I 5466.40 1144 4.37 4.90 3.62 -1.22 304 .46 155 4.55 3 13 Fe I 5546.51 1145 4.37 5.27 3.90 -1.42 250 .31 89 4.78 1 15 Fe I 5405.35 1162 4.39 5.42 3.96 -1.07 275 .27 77 4.85 2 0

Fe I 5415.20 1165 4.39 3.06 2.14 -.02 329 .62 224 4.38 3 10

Fe I 5445.05 1163 4.39 4.22 3.14 -.55 334 .53 204 4.45 4 12 Fe I 5619.60 1161 4.39 5.70 4.22 -1.70 341 .28 101 4.79 1 17 Fe I 5653.89 1159 4.39 5.58 4.15 -1.57 305 .21 69 4.95 2 19

Fe I 5295.32 1146 4.41 5.71 324 .18 53 5.03 1 9

156
Table B

Spect vV ave- length

Mult EP — Log — Log

Log

fx

HW Rc — Log

(r/x) Q N

Fe I 5326.79 1147 4.41 6.16 4.60 215 .09 17 5.40 1 9

Fe I 5367.47 1146 4.41 3.66 -.26 319 .57 205 4.42 5 10

Fe I 5389.46 1145 4.41 4.67 3.33 -.86 329 .46 158 4.54 2 10 Fe I 5417.03 1148 4.41 5.53 4.25 -1.80 298 .20 61 4.98 1 10 re I A A 1 4.41 J.DZ A ^ A 4.14 — 1 S7 1 .8 / Z /U .Zo 8151 A 81 4.0 J 1

1

1

1 J Fe I 5285.12 1166 4.43 5.76 4.24 -1.61 253 .18 51 5.04 1 9

Fe I 5321.11 1165 4.43 5.40 4.06 -1.39 284 .34 101 4.72 2 0

Fe I 5339.40 1162 4.43 6.24 4.67 240 .11 24 5.30 1 9

Fe I 5463.28 1163 4.43 4.30 3.11 -.64 279 .54 170 4.48 1 13 re 1

1 1 Ai A A'X S AQ 1 ftn 10 Q8yo A 77 1J

1 ft 1 o Fe I 5560.23 1164 4.43 5.42 -1.46 251 .28 76 4.85 2 16

Fe I 5562.71 1163 4.43 5.29 -1.31 32A .38 135 4.64 1 16

Fe I 5364.88 1146 AAA 4.06 -.38 316 .56 181 4.45 3 10

Fe I 5395.25 1143 AAA 5.88 4.49 291 .16 51 5.07 1 10 re 1 1 ItJ A AA A 88 4.00 1 S8 J.JO 1 07 .41 1i4D4A 4 SQ -3J

1lU0

Fe I 5432.96 1143 AAA 4.96 355 .41 147 4.59 2 11 Fe I 5461.54 1145 AAA 5.83 4.35 -1.92 241 .20 52 5.01 2 13 Fe I 5180.07 1166 AAl 5.28 3.81 -1.28 253 .27 78 4.84 1 25

Fe I 5373.70 1166 AAl 5.15 -1.08 300 .34 109 A.l\ 5 10

Vpr c t

1 sdi n Qi 1 1 AS A Al J. jd 7 77 —— .Z77/ 11

1

.DO 11 QQyy A 41 J 0u Fe I 5462.97 1163 4.47 4.65 3.16 -.83 304 .51 162 4.51 1 13 Fe I 5651.47 1161 4.47 6.02 4.47 262 .14 37 5.19 1 0

Fe I 5554.90 1183 4.55 4.56 -1.02 306 .45 146 4.57 2 16

Fe I 5686.54 1182 4.55 5.02 -.95 353 .39 151 4.61 1 21 r c 1

1111 78/ o ft no A (^X ini . 11 sD 47 DS .iL1 7 J1 71Zi Fe I 5752.04 1180 4.55 5.26 3.96 -1.23 340 .29 102 4.78 3 21 Fe I 5816.36 1179 4.55 4.86 3.26 -1.11 315 .38 131 4.65 3 22

Fe I 5852.19 1178 4.55 5.61 4.14 -1.51 310 .18 58 5.03 4 22

Fe I 5859.61 1181 4.55 5.02 3.61 -1.03 350 .37 145 A.6A 4 22 rc I

1I11 80oU A 81 "X A\ —— .oy 80 777 Z /Z .JO 18 1 1

1

ill A M D 71Zj

Fe I 5929.70 1176 4.55 5.58 4.10 -1.62 288 .20 58 5.01 1 0

Fe I 5983.70 1175 4.55 5.12 3.69 -1.18 318 .35 121 4.70 3 1 Fe I 6024.07 1178 4.55 AA6 2.98 -.64 283 .47 166 4.55 4 2 Fe I 6627.56 1174 4.55 5.90 4.36 -2.04 292 .16 47 5.13 3 7 re 1 474Q 1 70^ D.J J J

X .yQ71 —— 11 . 77/ z 747 Z'tZ .z77/ 67 4t.O8SJ z 0

Fe I 6533.94 1197 4.56 5.52 -1.96 •258 .19 50 5.07 1 1 Fe I 6633.76 1197 4.56 5.20 3.92 -1.46 343 .29 103 4.81 2 0

Fe I 6699.14 1228 4.59 6.46 4.91 294 .07 20 5.52 1 0

Fe I 5488.14 1183 4.61 5.96 4.34 247 .17 45 5.15 0 13 re I joUo. /3 1 1 Q(\

1 loU 4.01 J. 3 / — 1.3U .Zo yD A ei 4.81 i LL Fe I 5855.13 1179 4.61 5.99 4.47 -1.60 277 .13 40 5.22 A 22

Fe I 5997.81 1175 4.61 5.14 -1.62 303 .26 81 4.87 1 0

Fe I 6020.17 1178 4.61 4.78 2.52 -.95 377 .48 204 4.50 4 2 Fe I 6093.66 1177 4.61 5.73 4.26 -1.85 330 .13 40 5.22 1 2 Fe I 6639.71 1195 4.61 6.08 -2.22 308 .14 43 5.19 1 0

Fe I 6705.12 1197 4.61 5.60 4.11 -1.82 304 .24 79 4.92 1 8 Fe I 5598.30 1183 4.65 4.84 -.92 479 .64 326 4.43 0 17 Fe I 5679.02 1183 4.65 5.23 3.94 -1.11 283 .31 90 4.79 3 21 Fe I 5905.67 1181 4.65 5.27 3.83 -1.22 331 .28 93 4.82 3 1 Fe I 5927.80 1175 4.65 5.57 4.10 -1.48 287 .20 58 5.01 1 0

157
Table B

Spect WavelengthMult EP -Log — Log

Log -ex HW Rc W

-Log

/ TV/ 1 \ \ {Wl\) 0

Fe I 5930.19 1180 4.65 4.87 3.26 -.79 329 .40 139 4.63 3 0

Fe I 6007.96 1178 4.65 5.27 3.87 -1.33 330 .32 109 4.75 2 2 Fe I 6079.02 1176 4.65 5.33 4.09 -1.65 330 .23 80 4.91 2 2 Fe I 6094.42 1177 4.65 5.96 4.48 259 .13 35 5.22 1 2 Fe I 5984.80 1260 4.73 4.91 3.48 -1.01 283 .41 140 4.62 3 2 Fe I 6055.99 1259 4.73 5.09 3.61 -1.18 353 .35 129 4.69 2 2 Fe I 6290.97 1258 4.73 5.22 3.72 -1.43 306 .31 96 4.79 2 5 Fe I 6330.86 1254 4.73 5.75 4.23 -1.85 282 .19 51 5.06 2 5 Fe I 6385.74 1253 4.73 6.40 4.83 281 .07 19 5.52 1 0

Fe I 6419.98 1258 4.73 5.04 3.60 -.98 305 .38 140 4.66 1 6

Fe I 5987.06 1260 4.79 5.14 3.67 -1.25 330 .30 108 4.77 4 2 Fe I 6078.50 1259 4.79 4.83 3.62 -1.21 283 .37 122 4.69 2 2 Fe I 6170.52 1260 4.79 5.21 -1.26 306 .39 137 4.65 2 3 Fe I 6364.38 1253 4.79 5.89 4.24 -1.92 352 .18 61 5.04 1 6

Fe I 6456.87 1256 4.79 6.08 4.89 302 .15 45 5.15 1 0

Fe I 6597.57 1253 4.79 5.59 -1.87 305 .20 66 5.00 1 7 Fe I 5975.35 1260 4.83 5.51 3.90 -1.33 330 .27 88 4.84 3 2 Fe I 6102.18 1259 4.83 4.95 3.60 -1.21 330 .35 113 4.72 2 3 Fe I 6103.19 1260 4.83 4.89 -1.48 388 .34 127 4.70 2 3 Fe I 6293.92 1260 4.83 6.23 4.65 288 .12 34 5.26 1 0

Fe I 6469.21 1258 4.83 5.44 3.83 -1.47 305 .27 86 4.86 2 6

Fe I 6495.78 1253 4.83 5.61 4.22 -1.63 316 .21 66 4.99 2 7 Fe I 5496.57 1281 4.91 6.31 4.79 249 .11 27 5.30 1 0

Fe I 5633.97 1314 4.99 5.11 3.85 -1.03 353 .39 147 4.61 1 17 Fe I 6089.57 1327 5.02 5.75 4.10 -1.62 377 .20 75 4.96 1 2 Fe I 5577.03 1314 5.03 6.16 4.67 202 .10 22 5.35 1 17 Fe I 5650.71 1314 5.08 5.67 4.14 -1.60 294 .23 72 4.91 4 19 Fe I 5650.01 1314 5.10 5.69 4.21 -1.42 274 .20 56 5.01 2 0

Fe II 4416.82 27 2.78 4.45 -1.42 313 .72 245 4.26 2 28

Fe II 4583.83 38 2.81 3.70 -.60 437 .77 366 4.10 4 30

Fe II 4620.51 38 2.83 5.05 3.97 -2.00 281 .51 159 4.48 4 30

Fe II 4515.34 37 2.84 4.51 2.72 -1.30 298 .70 228 4.30 2 0

Fe II 4576.33 38 2.84 4.87 3.46 -1.60 343 .61 224 4.31 5 30

Fe II 4582.84 37 2.84 5.01 3.79 -1.82 293 .53 157 4.47 2 30

Fe II 4491.40 37 2.85 4.66 3.29 -1.49 289 .65 206 4.34 3 0

Fe II 4508.28 38 2.85 4.51 -1.16 325 .70 249 4.26 2 29

Fe II 4731.44 43 2.89 4.52 3.26 -1.68 291 .57 179 4.42 3 0

Fe II 5256.89 41 2.89 5.77 4.43 303 .29 89 4.79 4 9

Fe II 5284.09 41 2.89 4.86 3.82 -1.85 312 .50 166 4.50 2 0

Fe II 6369.46 40 2.89 5.86 258 .25 75 4.91 1 6

Fe II 6432.65 40 2.89 5.47 4.42 -2.33 329 .38 134 4.67 4 6

Fe II 6516.06 40 2.89 5.14 -2.02 352 .47 178 4.55 3 7 Fe II 5991.38 46 3.15 5.62 4.31 -2.55 330 .30 106 4.77 1 2 Fe II 5425.27 49 3.20 5.21 4.30 -2.47 299 .39 123 4.65 2 0

Fe II 6084.11 46 3.20 5.77 4.67 -3.00 306 .28 85 4.84 2 2 Fe II 5234.62 49 3.22 4.64 3.15 -1.50 328 .61 219 4.38 2 26

Fe II 5325.56 49 3.22 5.25 4.08 -2.47 283 .41 136 4.60 3 9

Fe II 5414.09 48 3.22 5.52 4.49 -2.50 278 .34 104 4.72 1 10

Fe II 6113.33 46 3.22 5.90 4.73 296 .20 60 5.01 2 0

Fe II 5197.57 49 3.23 4.64 3.40 -1.58 355 .61 230 4.35 2 25

158
Table B

Spect Wavelength

Lrr p —Log — Log

x:

Log

i rrf\ \ -^x

1 1 w Ac w/ — Log

(Wl\)

riV i V

Fe II 5337.73 48 3.23 5.43 298 .35 113 4.69 2 9

Fe II 5534.86 55 3.24 4.98 3.56 -1.92 354 .52 208 4.45 1 14 Fe II 5591.38 55 3.27 6.25 5.28 256 .12 31 5.26 2 0

P<a TT 48 ^ ?6 ^ 99 — ? 10 ^0^ 44 1 47 4 S7 1 q Fe II 6149.24 74 3.89 5.58 4.28 ^11 .35 139 4.68 3 3 Fe II 6238.38 74 3.89 5.50 4.18 -2.03 353 .41 155 4.61 5 5 Fe II 6239.95 74 3.89 6.22 4.82 296 .17 51 5.09 1 0

Fe II 6247.56 74 3.89 5.38 4.10 -2.08 376 .42 170 4.58 4 5 641 6 91 74 3 89 5 42 4 33 -2 52 329 32 1 1

1

4 76

Fe II 6456.38 74 3.90 5.28 4.05 -1.83 375 .49 206 4.50 2 6

Fe II 6446.43 1 c\c\ 199 6.22 6.75 5.24 279 .05 14 5.67 1 0

Gd II 4130.37 19 .60 5.65 3.07 241 .48 123 4.53 2 0

Gd II 4316.05 43 .66 5.68 2.26 311 .38 157 4.74 0 27

Gd TT 4483 35 62 1 06 6 59 1 82 235 .27 ^59y 4 86 2 29

Gd II 6305.15 94 1.31 1.15 286 .11 31 5.30 2 0

Gd II 5733.86 94 1.37 7.20 1.36 c o 258 .10 26 5.35 3 0

Gd II 5951.60 95 1.37 1.00 257 .05 13 5.67 2 0

Gd II 5140.84 115 1.58 4.76 1.26 177 .1

1

19 5.31 0 24

Gd II 5815.85 112 1.58 6.91 1.00 254 .06 15 5.59 2 0

Gd II 5904.07 112 1.62 !99 255 !05 12 5.67 2 0

Od II OUU4. J / 111 llz Loo .y 1 2jo .U4 1 AlU 11 A

J TT CjQ II 6080.65 111 112 1.73 .97 265 .06 16 C C A

5.59 1 0

Ge I A CO C OA 4685.84 3 2.03 6.20 .08 216 .13 33 5.28 2 0

La II 4662.51 8 .00 6.04 4.72 1.68 264 .55 150 4.47 4 30

La II 5290.83 6 .00 6.04 5.07 1.18 281 .36 114 4.68 5 9

T « TT La II c A '^n j4oZ.Z7 4 .00 .82 252 .29 no A 0'5 4.53 111

"5 13 La II 5808.31 4 .00 7.08 .70 265 .27 80 4.86 2 22

La II 4740.28 o

8 .13 1.78 339 .63 226 4.52 0 32

T a TT 5493.45 4 .13 .58 332 .36 119 4.87 0 13 La II 5805.78 4 !l3 4.89 L16 290 !41 128 4.64 3 22

T « TT La II ol 1 1. 11 41

"5 .13 6.62 .45 3iU COJO Z f\A 5.04 2 3 La II

A"^ C 1 4322.51 25 .17 5.60 1.82 251 .60 167 4.40 3 27

La II 5259.38 21 .17 4.95 1.04 285 .36 107 4.69 3 0

I a TT 5936.22 19 .17 7.09 5.75 .68 296 .24 73 4.91 2 0

La II 6320.39 19 !l7 6.23 5.22 1.14 360 .44 168 4.58 3 0

La II 4804.05 37 .23 6.12 1.27 280 .48 142 4.53 2 32

La II 5880.63 35 .23 6.61 .11 308 .31 99 4.77 2 0

La II 5303.54 36 .32 6.37 1.26 298 .42 130 4.61 1 9

la TT i_a 11 f\ S4 11 . 161 u 40 1 S7 4 f,! La II 4315.90 41 .40 6.04 .85 111 .38 157 4.74 0 27

La II 4699.64 .40 1.03 265 .31 79 4.77 3 32

La II 4526.12 50 .77 5.54 4.29 1.70 306 .53 185 4.43 1 29

La II 4559.28 53 .77 6.56 1.12 190 .34 71 4.76 5 29

La II 52 .77 1.28 218 .34 81 4.74 4 32

La II 6067.14 48 .77 .02 236 .10 21 5.35 1 2 La II 6129.56 47 .77 .80 330 .26 91 4.85 1 3 La II 4748.73 65 .93 6.18 5.04 1.52 286 .43 122 4.59 2 32

La II 6126.09 69 1.25 .75 306 .23 69 5.02 0 3 La II 5769.06 70 1.26 6.50 1.06 403 .43 183 4.74 0 21 La II 4619.87 76 1.75 6.46 1.60 287 .43 126 4.58 2 30

159
Table

B

Spect WavelengthMult EP -Log -Log

A';

Log -ex HW Rc

W

-Log

(Wj\)

Q

N

La II 5377.08 95 2.30 6.38 5.04 .95 270 .25 69 4.89 1 0

La II 5188.24 95 2.45 6.29 1.25 291 .27 87 4.81 1 25

La II 6399.05 104 2.64 .46 376 .11 38 5.30

L 6

Li

r 6707.84 1 .00 6.53 4.01 420 .07 29 5.36 1 8 Mg I 4571.10 1 .00 3.97 281 .64 199 4.36 4 30

Mg I 5172.68 2 2.71 1.37 -.32 .27 670 .88 693 3.87 5 25

Mg I 5183.60 2 2.72 1.03 -.50 .48 111 .95 903 3.76 4 25

Mg I 4702.98 11 4.34 2.43 1.02 -1.81 324 .69 288 4.21 4 32

Mg I 4730.03 10 4.34 4.90 3.39 -3.28 161 .43 122 4.59 2 0

Mg I 5528.39 9 4.34 2.68 1.03 -1.79 354 .72 292 4.28 2 14 Mg I 5711.07 8 4.34 4.51 3.22 -2.69 328 .46 162 4.55 3 21 Mg I 6318.72 23 5.11 5.69 304 .19 59 5.03 2 0

Mg I 6319.22 23 5.11 6.08 293 .14 41 5.19 2 0

Mn I 5394.67 1 .00 4.47 2.78 .46 329 .44 154 4.56 4 10

Mn I 5432.55 1 .00 4.92 3.39 .03 330 .34 112 4.70 2 11 Mn I 5420.36 4 2.14 4.62 2.58 .10 316 .40 137 4.61 5 10

Mn I 5457.47 4 2.16 5.94 4.84 -.75 178 .08 15 5.46 1 13 Mn I 5470.64 4 2.16 5.16 2.99 -.05 293 .33 114 4.71 2 13 Mn I 5516.77 4 2.18 5.25 3.14 -.16 354 .28 107 4.77 2 14 Mn I 4754.04 16 2.28 3.60 2.05 1.23 249 .64 181 4.42 5 32

Mn I 4783.42 16 2.30 3.18 1.95 1.19 292 .65 209 4.36 3 32

Mn I 4451.59 22 2.89 4.22 1.07 235 .68 187 4.38 5 28

Mn I 4709.72 21 2.89 4.81 3.37 .35 249 .47 129 4.55 3 32

Mn I 4762.38 21 2.89 4.11 2.64 1.01 296 .59 189 4.40 2 0

Mn I 4502.22 22 2.92 5.00 3.48 .54 250 .41 102 4.63 1 29

Mn I 4766.42 21 2.92 4.36 2.77 .83 311 .52 163 4.47 2 32

Mn I 4453.00 22 2.94 5.06 .39 244 .38 97 4.66 2 0

Mn I 4470.14 22 2.94 5.00 .48 242 .36 91 4.69 2 0

Mn I 4739.11 21 2.94 4.93 3.52 .24 249 .41 108 4.63 3 32

Mn I 4765.86 21 2.94 4.67 3.27 .61 239 .45 115 4.59 2 32

Mn I 4761.53 21 2.95 4.62 3.14 .38 295 .46 146 4.53 4 32

Mn I 4457.04 28 3.07 5.23 -.12 232 .30 72 4.79 2 0

Mn I 6013.50 27 3.07 4.72 3.19 .16 330 .40 157 4.61 4 2 Mn I 6016.64 27 3.07 4.66 3.19 .31 330 .42 151 4.60 3 2 Mn I 6021.80 27 3.07 4.60 3.19 .46 306 .43 132 4.62 4 2 Mn I 5377.63 42 3.84 5.33 3.81 -.14 274 .27 76 4.85 2 0

Mn I 5399.49 42 3.85 5.43 4.11 -.45 324 .20 64 4.96 1 10 Mo I 5506.49 4 1.33 6.16 2.19 281 .27 78 4.85 1 0

Mo I 5533.01 4 1.33 6.06 2.02 280 .26 75 4.87 1 0

Mo I 5570.46 4 1.33 6.09 1.68 348 .19 66 4.98 1 17 Mo I 6030.66 5 1.53 6.75 1.34 271 .10 27 5.35 2 0

Mo I 4411.57 2.08 6.22 1.95 220 .24 54 4.91 1 0

Na I 5889.95 1 .00 1.52 .04 3.89 685 .82 649 3.96 4 1 Na I 5895.92 1 .00 1.73 .38 3.59 590 .77 507 4.07 4 1 Na I 4668.56 12 2.10 5.15 3.38 -.00 251 .35 92 4.71 2 0

Na I 4751.82 11 2.10 5.73 4.50 -.79 193 .13 29 5.22 1 32

Na I 5682.63 6 2.10 4.31 2.80 .71 303 .49 167 4.52 1 21 Na I 5688.19 6 2.10 4.07 2.41 .96 346 .55 204 4.44 2 0

Na I 6154.23 5 2.10 5.56 4.02 -.14 330 .24 100 4.85 1 3 Na I 6160.75 5 2.10 5.27 3.89 .16 377 .30 117 4.76 1 3

160
Table

B

Wavelength

Mnlt FP

— Log -Log

Log

Kg)

A ;

HW J?

'Itw

— Log 0 / V

Nb I A T> AO 4573.08 .27 2.52 1 Al 203 AO .08 116

C AC 5.46 2 A0

Nb I 4606.77 .35

C AO 5.98 2.70 111 .16 35 5.12 2 0

Nd II 4451.99 6 .00 1.70 250 .53 141 4.67 0 28

XTH TT 4706 54 3 .00 2.02 249 .56 136 4.48 4 32

Nd II 4799.42 2 !oo LIO 273 .39 111 4^94 0 32

Nd II 4069.27 20 .06 5.71 2.54 251 .5o 1 CT 157

A yi 1 4.41 2 A Nd II 4475.57 AZT .06 1 A 1

1.01

CA 250 1 A

.30 li 4.79 2 A29

Nd II 4612.47 3

A^- .06 6.29 OA .89 312 .25

A 74A OA 4.84 2 TA30

Nd II 4811.34 3 .06 5.73 4.64 1.70 268 .50 140 4.52 5 32

Nd II 6549.54 .06 .31 258 .15 32 5.22 2 7

XT ^ TT Nd II 1 Q 1 on libCA .54 1^1 lolAA Z. 4.45 3 AU

XTJ Nd II 4059.97 63

A

.20 5.88 A*^ 2.42 242 .52 lie 135

A AO 4.48 2 0

Nd II 4446.39

AA4yTA

.20 5.71 2.14 282 /I 1 .61 1 A /4 iy4

A 1 4.3o 4 0 28

Nd II 4567.61 49 .20 6.39 1.28 219 .30 68 4.81 3 30

Nd II 4594.45 52 .20 1.28 256 .32 84 4.75 1 30

XT^ TT IN a II

C

O 1 T c DZlZ.ijAA 44 ^ A

.iU ^ 1 AD.IU 1. /I AC .40 152

AC /I 4.34 3 0 C 25

'KTA TT Nd II 5255.51A 1 43A

.20

C Al 5.93 1 no 1.78 Z A 354 .55A 230A Af\ 4.40 2 9

XT^ TT JNCl II

'>

A

.zu .61 3Z8 1 1.33 1 AO 1U8

A Al 4.y3A 1 Zl Nd II 6428.67 .20 7.14 .40 305 .20 69 4.99 2 6

Nd II 6591.43 .20 0.18 295 .09 27 5.39 2 0

JNQ II

A 1 AOAN 1 AlU .3z 4.8d Z.8d Ill "7/1 . /4 1/1

A

Z4d

A T) 4.ZZ z AU

XT /-I TT IN a IIA 1 11 1? 1 Qly .3Z

C HI 3.d3 oil Z.I3 ZjI .33 1 /1 0

148 AAA 4.44 z AU

vr,^ TT IN a IIA KQ 1 1 4338.1 / 1 AlU .3Z

A dA 4.y4 Z.3Z Zl<i .04 OAT zuz /111 4.33 3 AU Nd II 6550.19 .32 0.29 234 .20 54 5.04 1 7 Nd II 4485.95 .38 .97 250 .31 94 4.98 0 29

iNd II 4j41 .Z / ZQJO .38 1 Ql 1.8/ Lib .33 1 Ai 1d3 AAA 4.44 1 U

XT^ TT NCl II Duuy.3u 1 0

.38 1 A

.31) 001 Z83 AA .uy ZI J. 41) 1 z

XTrJ TT Nd II AO 1 o An

.4 / .66 Z4o 1 0.18 /1 048

C Al 3.1)3 z 1 /I 34

Nd II 5234.20 74 .55 5.90 4.78 1.84 392 .50 209 4.45 2 26

Nd II 5319.82 75 .55 5.76 1.87 374 .53 187 4.46 5 9

TT INd II

J j4o.4 / 1 3 c c.JJ

A A") 0.4Z CO .8y 1A ^ 343 .1 1 1 AT lUZA 7Q 4. /y 11 1 c 13

"KTA TT INd II 44Dz.yy CA cc. .JO j.bl z.zl 11

J

CA .04 ZUl /( 1 c 4.33 3 OAzy

XT^ TT INd II 4/y/.ioA60 .JOA 1 c o.3j 1 1 c 1.33 Zoj 1 A

.3y 1 AO 1U8 4.d3 Z AU Nd II 5361.17 46 .56 .83 260 .20 53 5.01 1 0

Nd II 5102.42 .68 1.45 311 .45 137 4.57 3 24

VTJ TT Nd II 5361.51 74 .60 5.80 11.62 1/11 341 .53 ly3A AC 4.4d 3 1 A

lU

Nd II 5442.27 76 .68 1.11 304 .32 1 AA 100

A '7C 4.75 3 12 Nd II 4817.20 .74 6.59 .82 244 .26 65 4.87 2 0

Nd II 5385 89 .74 6 64 1.19 298 .34 108 4.71 1 10

Nd II 5702.24 !74 1.24 315 !34 115 4J1 2 21 Nd II 5804.02 79 .74 1.34 330 .38 134 4.65 3 22

Nd II 6539.94 .74 0.20 294 .10 28 5.36 2 0

Nd II 5293.17 75 .82 5.83 1.99 399 .53 217 4.43 2 9

Nd II 5181.16 .86 6.17 1.27 342 1 1

.33 122

A CO 4.68 3 25

Nd II 5276.88 81 .86 6.64 1.32 265 .35 102 4.71 4 9

Nd II 5306.47 .86 6 81 1.19 265 .24 60 4.93 2 9

Nd II 5416.38 80 .86 6.81 1.00 266 .22 60 4.96 3 0

Nd II 5811.61 .86 1.02 278 .24 11 4.89 2 22

Nd II 6365.55 .93 .34 235 .14 29 5.19 2 6

Nd II 5474.76 .99 6.66 .78 227 .21 54 4.99 2 13

161
Table

B

Spect WavelengthMult EP

— Log -Log

^:

Log -ex HW Rc

W -Log

Q

N

Nd 11 5688.52 79 .99 1.44 318 .41 137 4.62 1 0

Nd II 5447.56 1.04 .69 290 .25 73 4.88 2 12 Nd II 5614.30 87 1.04 .68 353 .27 101 4.95 0 17 Nd II 5761.70 1.04 .61 323 .19 65 4.99 1 21 Nd II 5770.50 1.08 .75 302 .22 72 4.93 2 21 Nd II 5825.87 1.08 .95 302 .25 83 4.87 2 22

Nd II 5431.54 80 1.12 6.21 1.33 342 .27 98 4.79 4 11 Nd II 5740.90 1.16 .95 292 .27 81 4.85 2 0

Nd II 6385.20 85 1.16 .86 329 .18 61 5.04 1 6

Nd II 5356.98 80 1.26 6.56 1.38 316 .34 114 4.70 2 9

Nd II 5485.70 79 1.26 6.48 1.34 328 .36 119 4.68 4 13 Nd II 5842.38 86 1.28 6.72 .99 315 .21 73 4.94 2 22

Nd II 5744.77 1.35 .73 111 .21 62 4.97 1 21 Nd II 5769.87 1.35 .64 252 .14 35 5.19 1 21 Nd II 6382.07 1.44 .39 305 .13 41 5.22 2 6

Nd II 6034.24 1.54 6.93 .70 353 .25 85 5.00 0 2 Ni I 4331.64 52 1.68 4.71 .37 314 .56 179 4.41 3 27

Ni I 5102.97 49 1.68 5.11 3.69 -.53 328 .44 161 4.54 2 24

Ni I 5578.73 47 1.68 5.11 3.75 -.41 353 .45 168 4.54 3 17 Ni I 5748.34 45 1.68 5.50 4.29 -.88 291 .26 78 4.87 1 0

Ni I 5847.01 44 1.68 5.67 4.35 -1.10 297 .20 62 4.99 1 22

Ni I 6007.31 42 1.68 5.66 4.41 -1.05 306 .18 47 5.08 3 2 Ni I 6108.12 45 1.68 4.98 3.70 -.41 330 .38 132 4.66 1 3 Ni I 6128.98 42 1.68 5.65 4.34 -1.14 306 .19 58 5.03 1 3 Ni I 6327.60 44 1.68 5.36 4.07 -.90 318 .25 81 4.89 1 0

Ni I 6643.64 43 1.68 4.73 .06 328 .42 154 4.62 5 8 Ni I 5476.94 59 1.83 3.35 1.09 360 .69 285 4.28 2 0

Ni I 6177.26 58 1.83 6.00 4.47 -1.56 280 .11 31 5.30 1 0

Ni I 5754.68 68 1.93 4.76 3.62 -.06 302 .46 151 4.57 2 21 Ni I 6314.67 67 1.93 4.92 -.25 329 .41 140 4.64 5 5 Ni I 6482.81 66 1.93 5.37 4.04 -.49 258 .25 70 4.93 2 6

Ni I 5592.28 69 1.95 5.08 -.23 353 .44 176 4.54 3 17 Ni I 6586.33 64 1.95 5.43 4.12 -.63 281 .26 76 4.90 1 7 Ni I 5435.87 70 1.99 5.12 3.79 -.40 268 .34 101 4.73 3 11 Ni I 5892.88 68 1.99 4.88 -.27 401 .43 191 4.63 0 1 Ni I 4470.48 86 3.40 4.66 .40 282 .54 147 4.47 2 29

Ni I 4595.96 101 3.42 5.37 -.68 296 .49 151 4.85 0 30

Ni I 4648.66 98 3.42 4.75 2.87 .61 305 .52 161 4.47 2 30

Ni I 4604.99 98 3.48 4.84 .46 265 .49 132 4.53 3 30

Ni I 4756.52 98 3.48 4.64 3.26 .21 249 .47 139 4.54 2 32

Ni I 4686.22 98 3.60 4.97 3.40 -.08 234 .35 90 4.71 3 31 Ni I 4705.93 128 3.66 6.11 4.75 -1.24 206 .13 31 5.18 2 32

Ni I 4752.43 132 3.66 4.93 3.70 -.42 262 .39 107 4.65 2 0

Ni I 4812.00 130 3.66 5.62 4.27 -1.22 233 .22 58 4.94 3 32

Ni I 4807.00 163 3.68 4.78 3.79 -.29 279 .35 106 4.68 3 32

Ni I 4731.81 163 3.83 5.32 3.91 -.72 259 .38 103 4.66 3 0

Ni I 5462.49 192 3.85 5.43 4.15 -.86 329 .29 100 4.77 1 13 Ni I 5186.59 205 3.90 5.92 4.42 -1.42 190 .14 27 5.19 1 25

Ni I 5589.38 205 3.90 5.73 4.47 -1.13 240 .17 40 5.12 2 17 Ni I 5593.74 206 3.90 5.40 4.17 -.85 358 .30 98 4.77 2 17

162
Table B

Spect WavelengthMult EP — Log

At — Log

Log

-Ox

HW Rc W

— Log

/ IT/ / \ \ Q N

Ni I 5625.33 221 4.09 5.52 4.17 -.96 285 .26 76 4.87 2 0

Ni I 5694.99 220 4.09 5.45 -.82 278 .27 87 4.83 2 21 Ni I 6111.06 230 4.09 5.59 4.27 -1.32 288 .16 46 5.12 1 0

Ni I 6116.18 218 4.09 5.14 -.89 353 .29 104 4.79 2 3 Ni I 6175.42 217 4.09 5.59 4.07 -.90 353 .26 91 4.85 3 3 Ni I 6176.82 228 4.09 5.37 3.91 -.66 306 .30 97 4.80 4 3 Ni I 6204.64 226 4.09 6.02 -1.41 294 .12 41 5.26 3 4

Ni I 5494.89 231 4.10 5.91 4.58 -1.30 189 .08 14 5.46 1 13 Ni I 5641.88 234 4.10 5.78 4.45 -1.24 262 .17 48 5.08 2 19 Ni 1 5682.20 232 4.10 5.28 4.03 -.68 328 .26 93 4.83 1 21 Ni I 5760.85 231 4.10 5.70 4.20 -.91 282 .22 69 4.94 1 21 Ni I 6186.74 229 4.10 5.87 4.33 -1.28 259 .17 40 5.14 2 4 Ni I 6223.99 228 4.10 5.82 -1.34 306 .16 49 5.11 2 5 Ni I 5614.78 250 4.15 5.48 -.84 252 .23 68 4.93 1 17 Ni I 6322.17 249 4.15 5.95 4.55 -1.53 287 .11 31 5.30 2 0

Ni I 6378.26 247 4.15 5.78 4.33 -1.09 300 .16 48 5.12 1 0

Ni I 6414.60 244 4.15 6.07 4.68 -1.23 291 .11 32 5.30 1 0

Ni I 4551.24 236 4.17 5.69 3.97 -1.17 219 .52 128 4.98 0 29

Ni I 5805.23 234 4.17 5.52 4.15 -.96 290 .21 64 4.97 3 22

Ni I 6360.80 229 4.17 6.04 4.52 -1.49 297 .15 45 5.15 2 0

Ni I 6366.48 230 4.17 5.81 4.25 -1.28 423 .15 60 5.08 1 6

Ni I 5996.74 249 4.23 5.94 4.55 -1.54 274 .12 33 5.26 1 0

Ni I 6086.29 249 4.26 5.49 4.15 -1.13 353 .23 72 4.93 2 2 Ni I 6635.15 264 4.42 6.00 4.44 -1.36 351 .13 40 5.22 2 8 0 I 6300.31 1 .00 6.18 288 .12 34 5.26 1 0

0 I 6363.79 1 .02 6.63 282 .08 22 5.46 3 0

Pb I 4057.81 1 1.32 5.53 2.47 227 .41 98 4.62 1 0

Pr II 4408.84 4 .00 5.67 2.81 293 .71 233 4.28 2 0

Pr II 4612.07 .00 6.14 1.67 287 .23 69 4.88 2 30

Pr II 4413.76 26 .22 6.14 2.16 265 .53 151 4.47 2 0

Pr II 4570.61 .22 6.39 1.35 187 .14 27 5.19 1 30

Pr II 4510.16 20 .42 6.53 2.42 313 .55 180 4.42 3 29

Pr II 5322.78 35 .48 6.49 2.03 291 .37 113 4.67 5 9

Pr II 5352.41 .48 6.77 1.70 260 .20 53 5.01 2 0

Pr II 5259.74 35 .63 6.32 5.33 2.22 286 .37 111 4.68 3 0

Pr II 5219.03 37 .79 6.41 1.93 240 .28 71 4.85 3 26

Pr II 6165.95 39 .92 6.59 5.36 1.73 283 .17 54 5.07 1 3 Pr II 6025.72 1.44 1.42 259 .11 30 5.30 2 2 Ru I 4584.44 5 1.00 6.60 2.37 206 .10 20 5.35 1 0

Ru I 4709.48 14 1.13 6.26 2.19 204 .05 10 5.67 0

S I 4694.13 2 6.52 6.27 4.65 -5.46 226 .19 43 5.03 1 0

S I 4695.45 2 6.52 6.45 4.83 -5.60 218 .14 31 5.19 \ 0

S I 4696.25 2 6.52 6.45 4.93 -5.85 226 .19 43 5.03 \ 0

S I 5278.96 4 6.86 6.62 -6.13 241 .12 29 5.26 1 0

S I 5696.63 11 7.86 7.01 246 .05 12 5.67 0

S I 6046.04 10 7.87 6.39 4.27 276 .12 33 5.26 1 0

S I 6052.66 10 7.87 6.55 4.67 -6.18 287 .17 49 5.09 2 0

Sc I 6210.68 2 .00 6.50 5.18 2.22 273 .07 19 5.52 2 0

Sc I 6239.41 2 .00 6.04 5.40 1.37 285 .12 34 5.26 2 0

Sc I 6305.67 2 .02 6.28 2.29 286 .11 31 5.30 1 0

163
Table B

Spcct WavelengthMult EP -Log -Log

X'.

1 .Off -dyA HW I\. c -Log

(IVIK) nV L T

Sc I 57UU.23 12 1 A1 1.4 J J.I J Z.5Z 1 Al 303 .25 no78 A OO 4.88 3 21 Sc T 5686 84 12 1.44 5.85 2.38 260 .12 31 5.26 2 0

Sc T 4743.81 14 1.45 5.97 4.93 2.43 212 .09 19 5.40 1 0

Sc T 5671.81 12 1.45 5.78 4.67 2.47 261 .13 34 5.22 2 0

Sc I 5484.62 16 1.85 6.46 1.98 235 .04 9 5.78 1 0

Sc I 5355.73 ly 1V.yj CIA D.34 1 CO liy .09 21 c An 5.40 2 0

Sc II 4325.01 15 .60 3.48 2.63 302 .81 280 4.19 3 0

Sc II 4415.56 14 .60 4.06 2.17 282 .73 238 4.27 2 28

Sc II 4431.37 14 .61 5.15 .86 257 .47 126 4.54 2 28

Sc II 6604.60 19 1.36 5.36 4.39 .82 351 .36 133 4.69 4 7 oC II ZD 11. 4J

A QQ 4.07 1 TO i. /o 1 (^1 l.D/ ir\i 3U3 .j3 1 TQ 1 /y 4.4 / cJ Zo Sc II 5640.97 29 1.50 5.23 3.93 .97 312 .45 155 4.56 2 17 Sc II 5667.16 29 1.50 5.50 4.31 .79 297 .40 125 4.64 2 18 Sc II 6279.76 28 1.50 5.60 4.55 .69 335 .34 119 4.72 3 0

Sc II 6309.90 28 1.50 5.62 .45 310 .22 70 4.96 2 0

XT oc II Zo 1 Q A OA .Z3 3U4 1 Q .ly jy < r\i z U Sc II 5657.87 29 1.51 4.83 3.86 1.46 306 .55 193 4.46 4 17 Sc II 5684.19 29 1.51 5.27 4.28 1.05 327 .46 160 4.55 2 0

Sc II 6245.63 28 1.51 5.45 4.32 1.12 329 .39 130 4.66 3 5 Sc II 5526.81 31 1.77 4.64 3.64 1.88 328 .63 217 4.41 5 14

ol I A 1 n') Qyl 41UZ.y4 z

1 Q1 i. 1

1

— 1 /I <

1 .4J Zol .d3 1 QO lyo 4.3Z A n z AU

Si I 5665.55 10 4.92 5.55 4.05 -3.38 364 .24 89 4.85 3 20

Si I 5645.61 10 4.93 5.65 -3.47 280 .24 74 4.90 2 19

Si I 5690.42 10 4.93 5.34 4.03 -3.25 366 .26 92 4.83 4 21

Si I 5701.10 10 4.93 5.55 3.87 -3.41 303 .24 75 4.90 1 21

ol I C-7Q1 {\n J /yj.yj 1 Qy

A Ql j.ou A ^^\ 4.1U — 3.3 / 3Zj .Z / yz 4.oZ 3 T 1 Zi

Si I 5684.48 11 4.95 5.20 3.87 -3.06 310 .37 120 4.68 2 0

Si I 5772.14 17 5.08 5.47 -3.34 348 .31 106 4.75 2 21

Si I 5948.55 16 5.08 4.89 3.44 -2.86 354 .38 137 4.65 4 1 Si I 5666.68 5.61 5.98 245 .16 42 5.13 2 18

ol I J.Oi ^ AQ j.4o 3Zo .33 1 no iUo A 01 4.53 Au Zl

Si I 6125.02 30 5.61 5.74 4.38 259 .19 52 5.05 3 3 Si I 6131.57 30 5.61 5.93 4.49 292 .18 52 5.07 2 0

Si I 6145.02 29 5.61 5.71 4.32 302 .22 67 4.96 2 0

Si I 6237.32 28 5.61 5.39 3.84 353 .29 108 4.79 3 5

Ci T ol I 5243. ol 28 J.Ol J. 04 A 1 Q 4.1o 1 1 o 315 .Z / 00oo A QZ 4.5j z A

U

Si I 6244.47 27 5.61 5.60 4.27 316 .26 85 4.87 2 0

Si I 5675.73 5.62 6.26 253 .18 49 5.06 1 21

Si I 6142.49 30 5.62 5.79 4.34 296 .19 57 5.03 1 0

Si I 6155.13 29 5.62 5.20 3.51 330 .33 105 4.75 3 3

Si I 6407.27 5.87 5.98 3yy .ly /CO DO c f\r\ J.UU 1 cO

Si I 6414.97 5.87 5.65 309 .19 59 5.03 2 0

Si IT 6347.10 2 8.12 5.74 -4.66 322 .27 88 4.86 2 0

Si TT 6371.36 2 8.12 6.20 -4.96 307 .19 59 5.03 2 0

Olll Sm TT11 4704.40 1 .00 6.09 4.39 1.98 243 .37 88 4.70 4 32

Sm II 4604.18 .04 1.58 218 .29 74 4.80 1 30

Sm II 4676.91 3 .04 6.15 4.87 2.09 296 .37 109 4.65 3 31 Sm II 4458.52 7 .10 2.27 260 .48 133 4.53 3 0

Sm II 4475.18 .10 1.12 214 .18 39 5.06 1 0

Sm II 4791.58 7 .10 6.30 1.59 229 .18 42 5.06 3 0

164
Table B

Spect vv ave- length

Mult EP — Log

X'^ — Log

Log

HW Rc W

— Log

{W\K) Q

Sm II 4329.02 15 .18 5.60 2.54 282 .45 129 4.54 2 27

Sm II 4472.43 .18 6.15 1.93 240 .35 88 4.71 1 0

Sm II 4591.82 14 .18 6.51 1.70 242 .32 80 4.76 1 0

Sm II 4615.69 22 .19 5.78 1.89 263 .44 122 4.58 2 0

Sm II Zj y).iy 1 .oU Z4j yL A4.0y Z u Sm II 4505.05 .25 1.48 218 .20 44 5.01 1 0

Sm II 4577.69 23 .25 6.11 1.99 265 .40 109 4.63 1 30

Sm II 4318.94 27 .28 5.69 2.56 308 .53 172 4.43 1 27

Sm II 4452.73 26 .28 5.89 2.37 267 .53 152 4.47 3 0

omCm TTII tJDD.Zl .J J J.oH 4 84 11 .y\j QO Zj'+ 8^ 4 79 Z

"^0 Sm II 5312.23 .33 .68 232 .06 14 5.59 1 0

Sm II 4421.14 37 .38 5.71 2.22 263 .53 151 4.47 3 28

Sm II 4434.32 36 .38 5.52 2.48 271 .56 163 4.43 5 0

Sm II 4642.24 36 .38 5.86 4.68 2.14 299 .47 152 4.51 2 30

Cm TT 41't 1

A'i. J .Oo 4 "^Q 7 0"? LID A(y 11 99zz t. JO 1J 9QLy

Sm II 4362.04 45 .48 6.01 2.17 298 .52 167 4.45 2 27

Sm II 4424.34 45 .48 2.71 278 .61 189 4.37 4 0

Sm II 4537.96 45 .48 6.07 5.01 2.07 281 .51 142 4.50 3 29

Sm II 4655.13 .48 1.36 227 .21 49 • 4.98 2 0

Cm TT Jill 11 AQ f\ 04 4 70 z.;)D 1 41 4 SO 9QLy

Sm II 4467.34 53 .66 5.84 2.55 270 .54 156 4.46 2 0

Sm II 5836.37 1.00 .65 252 .05 12 5.67 1 0

Sm II 6307.06 1.06 .55 111, .05 13 5.67 1 0

Sm II 6267.28 1.17 .98 273 .06 16 5.59 1 0

Olll 11 1 Ifs . JZ 978 z / o 04 1

1

S 78 11 0

Sm II 6589.72 1.27 1.02 287 .06 17 5.59 1 0

Sm II 6472.34 1.38 .59 280 .05 14 5.67 1 0

Sm II 6291.82 1.41 .67 274 .06 16 5.59 1 0

Sm II 6542.76 1.46 .66 288 .07 20 5.52 1 0

olll Sm TT11 OD"J . J J . /D 904 Ly^ 07 90 JS . JZS9 1 Sm II 6426.63 1.75 .56 280 .06 16 5.59 1 0

Sr I 4607.35 2 .00 4.99 3.97 4.00 286 .59 183 4.40 2 0

Sr I 6504.00 8 2.26 6.86 1.52 300 .13 39 5.22 2 0

Sr I 6408.47 8 2.27 6.57 5.04 1.64 311 .20 63 5.01 2 0

olCr T

1 ^SSO uj JU.ZtOA 1 L, D. /U J.LJ ZJH .zu 70 S4 S 04 11 7

Ti I 4656.47 6 .00 AM 2.94 2.52 271 .47 135 4.54 3 30

Ti I 5192.97 4 .02 4.32 2.98 2.74 319 .57 196 4.42 3 0

Ti I 5219.70 4 .02 5.31 4.23 1.80 253 .27 70 4.86 1 26

Ti I 5426.26 3 .02 6.02 4.95 1.23 201 .09 16 5.40 2 11

11 I A/:Qt Q1 4do1 .yi D n< .Uj A Al 4.4 / 3.UO Z.DZ Zo4 c c

.J J loo A AA 4.44 11 AU

Ti I 5210.39 4 .05 4.23 2.82 2.76 304 .55 187 4.44 3 25

Ti I 5460.50 3 .05 5.84 4.66 1.31 251 .13 33 5.22 1 0

Ti I 4527.31 42 .81 4.46 2.94 2.46 306 .71 226 4.50 0 29

Ti I 4326.36 43 .83 5.35 1.80 226 .31 73 4.77 1 0

Ti I 4518.03 42 .83 4.55 2.97 2.57 263 .54 144 4.48 2 29

Ti I 4548.76 42 .83 4.55 3.15 2.54 250 .50 132 4.52 3 29

Ti I 4771.10 41 .83 5.46 224 .15 37 5.13 1 32

Ti I 5338.33 35 .83 5.72 4.77 316 13 38 5.22 1 9

Ti I 4512.75 42 .84 4.67 3.33 2.46 271 .53 154 4.47 3 0

Ti I 4534.79 42 .84 4.22 2.73 3.12 281 .62 189 4.38 4 29

165
Table B

opect Wavelengtli

Mult AlUlt -Log

-v: — Log

Log

"A n H' DAc TT' — Log

[WW)

Al l\

Ti I 4758.91 41 .84 6.19 4.88 174 .10 17 5.35 1 32

Ti T ^JJJ.L, 1 47 8'S 4 05 7 44 ^ ^4 z,o 7811 .D / 7z 1 s 1

J

44. jz^7 7 79Z7

Ti T HJ J J 85 AH. 77/ Z. J) . JUSO 7 41 77S . J4S4 11 60DU 4 .HD 46 z nu

Ti T 11 i ^7 8S J5 .\JJ 6i5 11 . JS7/ 707 1 7 "^8 Jo JS 1 1

. 1 1 2 76zo

Ti T 11 1 lA 1 05 S 4R 4 4^ 11 . 11 0VJ 778 z. / O . 11 4

1

J^97 JS . 11 9

7

2 Q7 Ti I 5300.01 74 1.05 5.51 4.71 253 .13 31 5.22 1 9

Ti11 T

1 6Q 1 OS f, 07 4 8^ 1 4"?

1 .Hj 771/

1

.U7 09 74 JS .HU 40 11 nu

Ti T 69 1 OS 5 71 11 .HO 48 J\J\J 7S 810

1

4 88 -iJ 2

Ti I 4675 1 7 77 1 07 5 23 A 07 1 36 718 77 66 4H.OJ8S 2 J) 1 Ti T 7X 74 1 .07 5.85 4 66 1 77 7S3 1 1 79^y S 30 1 Qy

Ti I 6126.22 69 1.07 5.61 4.42 1.47 306 .23 69 5.02 0 3 Ti T 44 S"^ ^1 1 1

1

1 4^ 4 66 7 .Hw 47 760 48 1 4^ .Js^J 1 u

Ti11 I1 6'>61 10 11 04WH 1 4^ S 77 11 . 87OZ, D^79Z.y 79 9870 A*T.O811

T. J J Ti11 T1 108 1 44 f, 7Q S Of^ . 97y 1 I/O 07 1 % 11

11

J

Ti11 Ti S471 '>0 106 1 44 U. 101 w 4 97 11 . 77z, / J J J . 1

7

11 0u

Ti I 6258.11 104 1.44 5.24 1.93 282 .29 93 4.82 1 5 Ti11 Ii 107 1 44 J5 . 84o*+ A S9 11 . 11 4*T ^S1 . 11 7/ JS80 _>S .u07/

11 7 Ti I 5145 47 109 1 46 S 19 4 1 6 1 87 764 78 76 4 83 11 VJ Ti I 5490.15 107 1 46 5 64 4 SI 1 S6 7141 H 1 4 30 S 1 9 11 1 3 Ti I 6'>58 71 1 04 1 4^> S

"'7

11 . 9^y D ^06 .HV 40 11 44HH A «\ 11 Ti I 4623.10 145 1.74 4.96 3.49 2.10 274 .38 98 4.67 3 30

Ti I 4617.27 145 1 75 4 90 3 . 84Ot^ 7 40 234 39 99 4 66 30

Ti I 4453.71 160 1.87 5.15 1.90 250 .32 77 4.76 3 28

Ti I 5978.54 154 1.87 5.68 4.41 1 .75 306 .18 55 5.05 1 2 Ti I 5965.83 154 1 88 5.60 4 16 1.61 377 .20 76 4.95 1 Ti I 5953.16 154 1.89 5.38 4.06 1.76 291 .21 62 4.98 1 0

Ti I 5201 10 1 83 7 09 S 91 4 6S 11 . 11 4

H

1i 90y\J 09 1

8

S 40 75

Ti11 Ti1 8^ 7 10 4 60 11 . z.77/ 778 . 11 7Z. 76 S 76 J 75 Ti I 4503 76 1 84 7 1 3 S 99 1 01 744 1 -K

. 1 32Z. S 22 2 29^y

Ti11 1i AllR If, 7^7 7 74 JS . 77/ Z. 11.1/17 110/87 1 3 79 S 27 2 ^32Z. Ti I 4759.27 233 2.25 5.13 4.02 1.86 264 .32 82 4.76 3 32

Ti I 5739 46 728 7 75 6 70 4H.J'97/ 1V . 19X y 252 07 17 5.52 0

Ti I 5689 47 249 2 30 ^5 . 97y 1 4.82 1 23 240 .13 31 5.22 1 21 Ti I 4796 21 760 7 33 5 51 4.47 .99 218 .15 32 5.16 32

Ti11 T1 ^488 70 76'S 7 40 5 74 4H . S4H 1L . 19I. y 747 1

7

. 1 / 45 5 1 5 0 13

Ti I 5648.57 269 2.49 6.03 4.88 1.11 204 .11 25 5.30 2 19

Ti T 11 1 J 1 DO. J J ^j.Ly7Q f\D. 11 97 4 99 .o4 84 7S7 ZJ / .U7 09 7"? ZJ JS .4U 40 11 u

Ti IT 11 11 11 Qy 11 .uo 08 ^ 4^ 11 .44SJ 11 . 79/ 7 .081

1

^71 4H. 141

1

A. 78Z.O Ti TT 11 11 11 8o 11 .Uo 08 J . jU J. 1 J — ^0 J^^8JO S6 110088 4 41 J 79^.y Ti TT 11 11 47Q8 ^A 11 7/

11 .Uo 08 4.00 A4.U404 78"? zoJ . JUSO 11 JSI

1

4H. JUSO 7 u

Ti II 4806.33 17 1.08 6.03 271 .21 59 4.94 2 32

Ti TI 11 II J

1

1 1 7 1 . 1 Z

? 77 J. /Z 1 "^8

1 .JO 1 .DO 469 4D7 .03 8^ 409 4U7 44.U404 /I 79Z7

Ti IT 11 II 4400. jU J 11 1 1 1 . 1 J J. J4 11 .447/

11 .OJ 8S JUSOIi .08SJ 444 44.UU00 J 79z.y Ti TT 11 II 4

1

1 . 1 o

4 ^7 4. JZ 1 ^ . 1 J 788 Zoo . 77/ z 7^7 Zj / 44. 76ZD 11 nu

Ti TT 11 II 44AA 1 7 77 1 / . /

Z

4U 1 1 1 . 1

D

J.1 Q474 7 71 Z.Z 1 1

1 .zo 76 J^^8JO 77 776 Z / D 4 70 IJ 78

Ti II 4470.86 40 1.16 4.73 2.70 .58 294 .68 202 4.35 2 29

Ti II 4583.44 39 1.16 5.34 3.92 250 .44 120 4.58 1 30

Ti II 4636.35 38 1.16 5.66 4.43 306 .41 124 4.59 2 30

Ti II 4609.26 39 1.18 5.76 4.62 275 .34 96 4.70 3 30

Ti II 4394.06 51 1.22 4.38 2.36 .86 307 .71 241 4.26 3 28

166
Table B

Spect vv d\ e- length

Mult EP Log Log

Log

fx

HW Rc W

— Log

{WW) 0 A'

Ti II 4563.76 50 1.22 3.59 1.40 1.49 387 .79 368 4.09 3 30

Ti II 4568.31 60 1.22 5.35 4.11 .42 250 .39 96 4.66 4 30

Ti II 4391.03 61 1.23 5.12 .29 445 .74 350 4.60 0 28

Ti II 4524.73 60 1.23 5.53 3.79 .27 264 .48 135 4.53 2 0

TT 11 II ATDl 1 .Zt 4 J1 . 11 8o 6S 7Q0 70 778 ZZO 4H.ZO78 z

Ti II 4399.77 51 1.24 3.60 1.63 1.23 301 .11 260 4.23 3 0

Ti II 4418.35 51 1.24 4.41 2.27 .65 301 .65 222 4.30 3 28

Ti II 4533.97 50 1.24 3.78 1.69 500 .85 438 4.02 4 29

Ti II 4544.01 60 1.24 5.12 3.56 .25 312 .63 214 4.53 0 29

Ti TT 11 11 SO 1 74 4 47 7 87 77 ^06 .UO 68 77Q 4 ^0 ^0

Ti II 4657.21 59 1.24 5.08 3.60 286 .57 176 4.42 1 0

Ti II 4708.66 49 1.24 4.93 3.82 278 .50 148 4.50 2 0

Ti II 4764.54 48 1.24 5.25 3.84 273 .45 130 4.56 2 0

Ti II 5336.81 69 1.58 4.67 3.66 .36 334 .60 216 4.39 2 0

Ti TT 11 11 JH 1 O.OU 11 .JoS8 4 00 — .uu 06 17Q j^y so 1v 7Qly 4 4Q z.1

0

1 u

Ti II 5185.91 86 1.89 4.87 349 .53 201 4.44 3 25

Ti II 4316.81 94 2.05 5.11 3.75 .38 267 .50 135 4.50 2 27

Ti II 4780.00 92 2.05 4.50 3.62 286 .58 174 4.43 3 32

Ti II 4805.10 92 2.06 4.14 .72 311 .64 223 4.33 3 32

Ti TT 6491 58 Ql 5 78 ^05 ^7 1 1

7

4 71 7

Ti II 5211.54 103 2.59 5.47 4.19 -.35 304 .39 135 4.62 3 25

V I 4330.02 5 .00 4.96 2.41 237 .38 95 4.66 2 0

V I 4577.17 4 .00 5.22 2.40 234 .30 74 4.79 3 30

V I 4580.39 4 .02 4.87 2.50 375 .46 183 4.76 0 30

V I 4586 36 4 04 4 95 7 60 317 40 145 4 85 0 30

V I 4416.47 22 .27 4.99 2.49 244 .39 100 4.65 1 0

V I 6274.67 19 .27 6.07 4.88 1.66 291 .14 41 5.19 2 0

V I 4389.97 22 .28 4.07 3.37 279 .63 198 4.35 1 0

V I 6216.37 19 .28 5.33 4.23 2.08 329 .20 66 4.99 2 5 V T 67S6 Ql 11 Qy 78 6 "^6 1 "^6 77"^ .\J\J 06 16 5 59 7 0

V I 6285.18 19 .28 6.00 4.84 1.72 276 .07 19 5.52 2 0

V I 4459.76 21 .29 4.76 2.68 211 .38 82 4.70 4 28

V I 6199.20 19 .29 5.95 2.09 281 .11 31 5.30 2 0

V I 6251.83 19 .29 5.81 1.88 288 .13 37 5.22 1 0

VV T

1 69Q? 86 11 Qy 7Q JS . QOyyj 4 68 11 . 77/ ^ 7QQ Lyy 1 7 J 1 S 09 0u V I 4379.24 22 .30 3.60 3.78 226 .63 157 4.45 3 27

V I 4406.65 22 .30 4.17 3.05 282 .56 171 4.42 4 28

V I 6213.87 20 .30 6.36 4.91 1.54 275 .08 22 5.46 1 0

V I 6243.11 19 .30 5.46 4.11 2.28 307 .22 69 4.96 1 0

V T V I ^111 AT Dill .OZ 1 (\A 1 .U4 A 71 11 . 78/o 771 Z / 1 .Uo na 71Zl J.S 4Ato 7Z V I 5703.56 35 1.05 5.43 4.24 2.32 279 .21 59 4.98 2 0

V I 6081.42 34 1.05 5.74 4.58 2.01 286 .16 46 5.12 2 0

V I 6135.36 34 1.05 5.84 4.76 1.78 280 .12 34 5.26 2 0

V I 5698.53 35 1.06 5.27 2.44 434 .31 133 4.70 2 21 V I 5737.07 35 1.06 5.85 4.68 1.71 256 .09 23 5.40 1 0

V I 6039.69 34 1.06 5.87 4.69 1.99 306 .11 35 5.30 1 2 V I 6119.51 34 1.06 5.61 4.40 2.11 306 .18 56 5.05 2 3 V I 5727.02 35 1.08 5.23 3.87 2.28 302 .32 100 4.76 2 0

V I 6090.18 34 1.08 5.41 4.29 2.43 330 .21 61 4.99 1 2 V I 6452.32 48 1.19 6.17 5.14 1.16 281 .06 17 5.59 1 0

167
Table

B

opect WavelengthMult tr

— Log

— Log K

Log

fx

li IV Ac

— Log

{W\\)

Q /V

V I 4758.74 51 1.22 5.79 4.81 196 .10 23 5.35 1 32 V I 44jZ.U1 Q7 1 Q7 1.0/ ? /lO /./4 7 CA /jU CI .j3 141 A OO 4.98 0 28 V I C CAT 55U7. /5 i/y /.3d ^ <Q D.jy C /17 J.4 / 1 Al 1 .U3 17 1 1/1 AC .Uj 6 c cn 5.01 1 1 /I 14 W I 4U /4.3 /

/rD 17 .3 / ? 10 7/.JD 77

C //j in .3y 07y/A4.0J 1 A

Y I A^AI nCi 4543. /U

A4 AA .UU /I ^7 4.D / 7 7^ /. /d 7 C /I /j4 1 8

.3o 1 A 1

lUl 4.00 1 A0 Y I 4760.98 4 .07 6.30 2.02 228 .18 41 5.06 1 0 Y I C A1^ A1 / A7 C CA D.04 C C7 7 1/1 /.14 1 AC 3Uj .lo C /I j4 C A*? J.U/ / 6

\/T I I 4jUj.b'j 1 A 14 1 17 1.3/ D. jU 7 A*; /.UD 7 1 7 /I / 1 ^ .ID 1/1 34 5 17 J.l/ 11 AU

"VT

Y I J jZ /.j4 1/ 1 A(\ 1 .41) 1 Q1 1 .yi 7^8 /JO 1 c

.1

J

IQ3y < 1 < J.l J / AU

"V TT Y II 44//.

J 1 (\ .lU 1 Q^ 1 .yj /I A7 4U / 77 . / / 111 333

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168
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170

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