@prefix vivo: . @prefix edm: . @prefix ns0: . @prefix dcterms: . @prefix skos: . vivo:departmentOrSchool "Science, Faculty of"@en, "Physics and Astronomy, Department of"@en ; edm:dataProvider "DSpace"@en ; ns0:degreeCampus "UBCV"@en ; dcterms:creator "Nodwell, Roy Andrew"@en ; dcterms:issued "2012-03-07T17:22:04Z"@en, "1954"@en ; vivo:relatedDegree "Master of Applied Science - MASc"@en ; ns0:degreeGrantor "University of British Columbia"@en ; dcterms:description """The spectra of Indium in the region 1200 A to 6900 A have been investigated. For this purpose a vacuum spectrograph, equipped with two slits at angle of incidence of 80° and 21° 34’, has been used. Details of the method of adjustment and calibration of the instrument are given. An electrodeless discharge has been used as a source, and methods of securing satisfactory output from this source are discussed. About 338 Indium lines have been measured, of which 62 have been previously reported. Term value predictions for Indium III are discussed and from these predictions some new lines have been classified. Several of the lines previously classified as Indium III have been found to be in error by as much as 0.5 A. In addition a few of the new lines have been classified in the Indium II spectra."""@en ; edm:aggregatedCHO "https://circle.library.ubc.ca/rest/handle/2429/41189?expand=metadata"@en ; skos:note "TEE SPECTRA OF INDIUM by RQY ANDREW: NODWELL A TRESIS SUBMITTED IN PARTIAL FULFILMENT OF TBE REQUIREMENTS FOR THE DEGREE OF MASTER OF APPLIED SCIENCE, i n the Department of PHYSICS We accept this thesis as conforming to the standard required from candidates for the degree of MASTER OF APPLIED SCIENCE. Members of the Department of Physics THE UNIVERSITY OF BRITISH COLUMBIA April , 195A ABSTRACT The spectra of Indium i n the region 1200, A to; 690GL A have been investigated,. For this purpose a vacuum spectrograph, equipped with two s l i t s at angle of incidence of 80? and 21? 3 4 S has been used. Details of the method of adjustment and calibration of the instrument are given. An electrodeless discharge has been: used as a source, and methods of securing satisfactory output from this source are discussed. About 333 Indium lines have been measured, of which 62 have been previously reported*. Term value predictions for Indium III are discussed and from these predictions some new: lines have been classified.. Several of the lines previously classified as Indium III: have been found to be i n error by as much as 0.5 A .. In addition a few- of the new: lines have been classified i n the Indium II spectra. ACKNOWLEDGMENTS The author wishes to express his gratitude to Dr. A.M. Crooker for suggesting this project and for his continued interest and assistance throughout the course of the research. The author i s also indebted to the British Columbia Telephone Company for financial assistance. CONTENTS Page INTRODUCTION; . . 1 PART I THEORY 2 PART II THE SPECTROGRAPH 12 PART III THE SOURCE . . . » .21 PART IV RESULTS . . . . . . . .24 BIBLIOGRAPHY .27 Following Page Figures 1, 2, 3, 4, 5, 6 28 Tables 1, 2, 3, 4, 5, 6, 7, 8, 9 28 THE SPECTRA. OF INDIUM INTRODUCTION; Although a great deal of work has been done on the analysis of Atomic Spectra and a completely adequate and convincing theory has been, developed to interpret these results, there are s t i l l a great many atoms, particularly i n the higher atomic numbers, which have not been completely analysed. Table I gives a summary of the status of the spectra analysis of a l l the atoms i n 1952. A study of this table indicates that the second spark spectrum of Indium i s inadequately known. An investigation! into the current literature reveals only nineteen wavelengths definitely assigned to this; spectrum and only eight term values estimated. In view of the fact that Indium I and Indium II have been very completely analysed by Faschen and Campbell (1,2) and since Shenstone (3,4) has done thorough analyses of the f i r s t two members of the iso-electronic sequence Agl and Cdll i t was felt that an analysis of Indium III at this time could be useful and fruitful. Further i t seemed likely that the large nuclear angular momentum of Indium would lead to some interesting fine structures, and that, in studying these hyper-fine structures high resolution techniques could be developed which would prove useful i n later research into hyper-fine structure i n Hydrogen and Helium i n the vacuum ultraviolet region. Most of the interesting lines of Indium III are likely to be in the vacuum ultraviolet region, and hence i t was decided that the major part of this work would be carried out on a vacuum spectrograph. 2 PART I THEORY The theory of optical spectra has been completely developed and discussed i n many text books (5,6). I t i s our purpose, i n this section, to summarize the more prominent features of the theory, and to indicate i n a general way the development of the formulae which we have used i n inter-preting the results of our experimental work. Early investigation of atomic spectra revealed many regularities. The most significant features about those regularities may be summarized as followst: 1. The wave number of each Une i s conveniently rep-resented as the difference between two numbers. These numbers are usually referred to as terms. 2. The terms can be divided into two classes, even and odd, so that transition from one class to the other are favoured while transitions between mem-bers of the same class are forbidden. 3. The terms group themselves into ordered sequences, the terms of each sequence converging to a limiting value.. A» Series of lines having similar characteristics result from combinations of a single term i n one sequence with successive terms i n another sequence. 3 5. These terms are very strong evidence: that atoms exist i n stationary states and that optical emission i s the result of a transition from one stationary state to another state of lover energy. The f i r s t attempt to meet with any success i n establishing a relationship between the structure of an atom and the knovni regularities i n i t s spectrum was made by Bohr (7). As i s well known he assumed that the atom consisted of a heavy nucleus around which electrons revolve. By assuming that the electron revolved about the nucleus i n certain discrete orbits, and that l i g h t was emitted when an electron dropped from an orbit of high energy to one of low energy, he vas able to calculate with sur-prising accuracy the spectrum of the hydrogen atom. However Bohr's theory led to serious discrepancies when applied to atoms with more than one electron and has been completely replaced by the much more complete and satisfying theory of quantum mechanics. De Broglie (8) had speculated that matter might have either a copscular or undulatory form i n the same way that l i g h t exhibits a dual nature, and was led to conclude that the mass and the wavelength of a particle are connected by the simple relationship ^ = trTv • Following this suggestion Schrodinger (9) attempted to find a wave equation to describe the motion of a particle which would lead to a system of standing waves corresponding to the Bohr orbit. The equation which he developed i s 87r'm v ¥ _____ 4 This equation has proved very successful and i s the basic equation i n quantum mechanics. In general the potential energy V i s not a function of the time and therefore Schrodinger's time dependent equation can be separated giving us the amplitude equation v 2 * 8irfyT (£~ *= ° and the time dependent equation. ,p . The wave function TjF has no direct physical interpretation, but the square of the absolute value of the vave function i s proportional to the probability of finding the particle at the position given by the coordinates. I f one applies the boundary conditions that the wave function must be everywhere f i n i t e and continuous i t i s found that the kinetic energy E may have only certain discrete values called the eigenvalues. Thus the Schrodinger approach leads directly to the concept of stationary energy levels or terms. By analogy with the electromagnetic theory of dipole radiation, Dirac has been able to calculate the transition probabilities between energy levels and has shown i t to be proportional to; Actually analogous e l e c t r i c quadrupole radiation and magnetic dipole radiation may occur, but they are usually very much weaker than the usual dipole radiation.. I t can be seen that a knowledge of the wave function i s necessary i n order to calculate the selection rules. Except i n the simplest cases the wave functions are not accurately known but the selection rules may s t i l l be determined by consideration of the symmetry of the wave function. THE HYDROGEN ATOM In the hydrogen atom the potential energy of the electron i e v ~ r . I f this i s substituted for V i n the Schrodinger equation and the equation solved i n spherical co-ordinates i t may be shown that for a well behaved solution E. may assumeall positive values but only those negative values for which c ~ j~z— • -^z or V = - yf* = R ^ 2 where n i s a positive integer, called the principal quantum number. These negative eigenvalues are usually degenerate, that i s for each eigenvalue there are several eigenfunctions which satisfy the original d i f f e r e n t i a l equation and whose form depends on two other quantum numbers, ^£ . and m . The angular momentum of the electron i s determined by the value of ^ as ]/MJrl) ? TT where may be 0, 1 n-1. The component of this angular momentum i n the direction of a reference axis i s given as rrt • The wave function for the hydrogen atom has the form where Rlr) i s the part of the wave function depending on the radius only and /-^\"'cf-s & i s the associated Legendre polynomial. I f the transition probability formula mentioned previously i s applied to this wave function, i t follows that the only cases i n which the transition probabilities are not zero are those i n which = - I A m = °,- * Other one electron ions such as Hell, Id.Ill, etc. have spectra very similar to that of hydrogenj the only changes being a large magnifica-tion In scale due to the -£ factor and a small change due to variations i n the Rydberg constant. The Rydberg constant varies s l i g h t l y because i t i s dependent on the reduced mass of the atom and hence on the mass of the nucleus. THE ALKALI METALS The a l k a l i metals (Id, Na, K, etc..) have spectra which are very similar to those of the one electron spectra mentioned above due to the fact that they have a single electron moving about a central core whose charge i s Ze - (Z-l)e. ( i . e . the charge of the nucleus minus the charge of the electrons i n the inner shells) However they are not exactly similar because the outer electron may penetrate the electron shell, thus reducing the screening effect and giving a change i n the potential. This makes the mathematics much more complicated but by assuming that the f i e l d i s non-coulomb and that the potential may be represented by the approximation v = z*(- ) i t may be shown that the energy eigenvalues have the form y = ^fZ /r? ** where r? * ±Q the effective quantum number and i s equal t©j 77- A where A i s the quantum defect. The chief difference between this result and that for the hydrogen atom i s that the term values are now dependent on the value of 1 as well as n, because the quantum defect i s a function of 1. The quantum defect decreases with increasing 1 because the likelihood of the electron: pene-trating the shell decreases with increasing 1. 7 In practice i t i s usually found that terms given by the above formula are s p l i t into doublets. Goudsmit and Uhlenbeck (10) assumed that this s p l i t t i n g was due to an additional angular momentum coming from the electron i t s e l f . According to this assumption each electron rotates about 1/ h~ i t s own axis with an angular momentum equal to Vs(s+l) % jfs where s i s quantized and may have only the value * ^ . I n one electron spectra the resultant angular momentum i s equal to the vector sum of the orbital and spin angular momentum and may therefore take on the values |/j(j+l) ~^jf where j = yf i s, and consequently we get a sp l i t t i n g of the term into two terms. SPECTRA OF ATOMS WITH MORE THAN ONE OUTER ELECTRON So far we have discussed only one electron spectra. One might expect that with more than one electron the interaction between the electrons would tend to cause a further s p l i t t i n g of the terms and this actually i s found to be the case. There i s no simple formula which w i l l account for the coupling between the electrons but two systems, called L-S and j - j coupling, have been idealized to represent the term s p l i t t i n g actually found. I t should be emphasized however that usually the coupling i s neither pure L-S coupling nor pure j - j coupling but some intermediate state between them. The Russel-Saunders (L-S) coupling predicts the spl i t t i n g quite accurately i n the majority of cases, particularly i n the lighter atomic weights (11). In this coupling the interaction between 1 and s for a 8 particular electron i s quite weak but the interaction between the l ' s and between the s's of different electrons i s relatively strong. Thus; the individual l ' s combine to give a total orbital angular equal to |/L(L+1) where L. i s the vector sum of ^ * , Similarly the individual s's combine to give a total spin angular momentum equal to ys(S+l) where S, i s equal to the vector sum of v~ $2 t — , The t o t a l angular momentum i s then computed as |/J(J+l) ~xir where J i s the vector sum of L and S* When we make the opposite assumption to that made for the L-S coupling, namely that the interaction between the 1 and s of the i n d i -vidual electron i s strong but that the interaction between the l ' s and between the s's i s relatively weak we get j - j coupling. I t should be pointed out that the number of terms i n either type of coupling i s the same. An example w i l l perhaps serve to i l l u s t r a t e the relationship between the two types. Consider the configuration sp, that i s a two electron system i n which 1__ = G, s__ = 1/2, I2 - 1, S2 8 8 1/2, How, i n L-S coupling this would give ua L = 1^ + I2 8 81, Si = s^ + S £ *= 1 or 0 , and adding L and Si vectorially we get the terms; said ^ / # , the f i r s t of these being the combination of L with S = 0 , the l a t t e r three terms resulting from the combinations of L with S = 1, In j - j coupling, on the other hand we find j _ = 1_ + s_ = 1/2 and J2 ~ *2 + s2 = 1/2 or 3/2, and taking the vector sum of J_ + j'2 w e Set four term values with J = 0, 1, 1 or 2, the f i r s t two being combinations with; .J_ = 1/2, the l a t t e r two with J£ = 3/2. Figure 1 shows the relative positions of these terms. THE PAULI PRINCIPLE The Paul! principle states that the t o t a l eigenfunction of an atom must be antisymmetric i n a l l i t s electrons. I t may be shown that this statement i s identical with the statement that no two electrons i n an atom can have the same set of values for the four quantum numbers. The Heisenberg theorem wnich i s a direct consequence of the Pauli principle, w i l l be made use of i n the prediction of the number and order of terms for certain electron configurations. This theorem states that x electrons, each with quantum number 1 ( i . e . an l x configuration) w i l l lead to the same states as (41 + 2) - x electrons with quantum number 1. Thus a 4d95s2 configura-tion, such as may be expected i n Indium III, w i l l lead to the same terms as ,2 - * a 4d5s^ configuration, namely s/z MOSELEY DIAGRAMS As was shown.previously the value of a term value i s given by the formula V- or rearranging \\j = . Thus i t follows that i f ^ i s plotted against for a series of atoms i n an isoelectronic sequence we should get a straight line whose slope i s n * . Hence i t i s possible, using known term values of some members of the isolectronic sequence, to predict graphically new term values for other atoms of the sequence. Conversely, having located a term i t i s possible to assign i t s principal quantum number by in s i s t i n g that i t f i t the Moseley diagram. 10 IRREGULAR DOUBLET LAW The irregular doublet lav may be stated i n terms of energy levels as follows: the difference between the square roots of the absolute term values of the levels having the same principal quantum number n i s independent of the atomic number Z. In other words, lines on the Moseley diagram with the same n run paral l e l to eaeh other* I t follows from this that for transitions i n which A rr = 0 the wave number increases linearly with increasing atomic number i n the isolectronic sequence* Although this rule does not hold rigorously i t s successful use i n a large number of cases has established i t as a very useful tool* REGULAR DOUBLET LAW This rule i s used to estimate the separation of doublets, that i s the s p l i t t i n g of terms i n Russel-Saunders coupling. This separation i s given; by the formula = R ^ where«tf= ^ r i s the fine structure constant equal approximately to 1/137, and -5 i s the screening constant which cannot be determined theoretically but must be estimated from knowledge of i t s value i n other atoms of the isoelectronic sequence*. 11 TERM VALUE PREDICTIONS It was mentioned in the introduction that the term values of Agl and Cdll had been established very accurately by Shenstone. Using these term values i t has been possible to estimate term values for Indium III by means of Moseley diagrams and the Irregular Doublet Lav. A summary of the calculations i s given i n Tables.1 and 2 which i s self-explanatory* Graphs of the Moseley curves are given i n Fig. 3. Some term values have also been predicted by extending the n* sequences. Details of this calculation are given i n Table 3. Rydberg conversion tables, have been used to convert from term value to n and * from n to term value* In both the above mentioned tables newly predicted terms; for Indium III are enclosed i n brackets* Finally, the doublet separation for the terms tW5sr D^ , - W5-r- ± has been estimated by means of the regular doublet law/as follows* Z_ Atom A y Z - s j _ 47 Agl 4471.9 23.31 23.69 48 Call 5363.7 24.69 23.31 49 I n l l l 6921.0 26.00 23.00 12 PART II THE SPECTROGRAPH The spectrograph used was the Vacuum spectrograph designed by Lubzinski and described i n his thesis* The main details of the optical arrangement are indicated i n F i g . 4. Since the arrangement i s s l i g h t l y unusual a detailed discussion of the method of calibration and adjustment would seem to be of interest. In order to make the procedure as clear as possible I shall describe the adjustments i n approximately chronological order. TBE GRATING The f i r s t step i n adjusting any grating spectrograph i s the accurate determination of the radius of curvature of the grating., This has been done by means of a Foucault knife edge bu i l t especially for the purpose. The radius has been measured as 199.50 i .05 cm. In the course of measuring the radius by the Foucault test one also has an opportunity to study the quality of the spherical surface.. The grating i s reasonably good although there i s a slight \" h i l l \" near the right hand side of the grating which appears to be about one fringe high. A sketch of the appearance of the surface at best focus i s given i n F i g . 2. 13 THE FIDUCIAL MARKS: The measurement of distances between the principal parts of a vacuum grating is usually difficult because the parts are not readily accessible. To overcome this difficulty ve established two accessible fiducial marks; namely a pointer which i s attached to the grating mount and i s 1.81 cm. from the grating face, and a mark on the near edge of the adjusting unit of the s l i t and which i s 6.17 cm. from the s l i t . These distances vere established by removing the parts: from the spectrograph and measuring them with a travelling microscope. PLACING THE SLIT ON. THE ROWLAND CIRCLE Zernicke (12) and others (13) have shown that the equation for focus i n a concave grating i n which aberrations due to orders of higher power than the f i r s t are neglected i s c os * \" c o s -y. cos & _ cos 0 _ n vhere A is the angle of incidence 0 i s the angle of diffraction! p i s the distance from object to grating Cf i s the distance from image to grating F{ is the radius of curvature of the grating An obvious solution to this equation i s the set of parametric: equations p - /Rcos-i, CJ= Rcos & which of course means that the object H and image both l i e on a circle of radius R (called tbe Rowland circle). Now for the direct reflected image = ~ & and hence i f the s l i t i s on the Rowland circle the distance from s l i t to grating must equal the distance from grating to image. This property has been used to set the s l i t on the Rowland circle i n the following manner: The grating and s l i t were located i n approximately the correct position and a pointer was accurately placed at the image of the s l i t by means of the parralax test with a low. power microscope. Owing to the vacuum tank and equipment i t was impossible to measure p and <7 directly so the measurement was made indirectly by triangulation with a precise theo-dolite kindly lent us by Mr. P. Demos of the Faculty of Engineering. The theodolite was used to measure the angles subtended by the s l i t fiducial mark, the grating fiducial mark, and the image at two arbitrary points A and B. From these angles and the accurately measured distance AB the distances IG and SG were calculated thus determining how much p differed from q . Based on this the s l i t was moved the correct amount and the measurements repeated until SG + SS = IG. At the final setting these r distances were measured as SG = 135.17 and IG = 185.15. ANGLE OF INCIDENCE AND SLIT DISTANCE From measurements previously described we have the distance » i SG = 185.16,cm. and the distance GG = 1.81 cm. Also from the triangulation we found that i = 20° Al' and therefore from simple geometry i t may be calculated that SG « p = 186.85 cm. and i = 20° 30'. (See Fig. 1.) 15 LOCATION OF THE CENTRE OF THE ROWLAND CIRCIE From the drawing i t can be seen that a = R/2 - 66' = 99.75 - 1*81 « 97.94 em. b = a s i n i = 97.94 sin 20° 4 I 1 = 34.60 cm. c = p - a cos i = 185.16 - 97.94 cos 20° 4I' = 93.53 cm. and hence by measuring the distances c and b from the image (establishing the lin e of sight with the theodolite) the position of the; centre of the Rowland circle may be located. FOCUSSING The plate holder was placed on the Rowland circ l e by making i t s ' distance from the centre equal to R/2. When this was completed a f i n a l check on the focussing was made by photographing the iron arc spectrum. In order to increase the sensitivity of this test a mask was placed i n front of the grating masking off the central part of the grating so that the image was formed by two converging beams coming from opposite ends of the grating. With this arrangement any small displacement of the plate from true focal plane w i l l cause the image to become very blurred or even doubled, and hence the method i s very sensitive. I t was found with this check that the plate holder had to be shifted s l i g h t l y to obtain the position of best focus. Although this i s not surprising i t i s worthwhile to estimate how much the plate would have to move to compensate for small errors i n the s l i t distance p and the angle of incidence i . 16 As stated previously the basic equation for focussing the grating ._ ccsx-< __ c o*s cosx 6 _ cos & _ ^ 19 -re ~^r~ ~*r - ° Taking the derivative with respect to p we get px <72 77p \"\" . or since we are close to the Rowland c i r c l e p^= R^co^e, ^ coj-'t? and therefore c/q = - cfp> . Furthermore, as may be seen from the sketch, the normal displacement of the plate i s given as oY-x =• c/) and for the comparison source If we are working at one point on the photographic plate so that 0 i s the same for both spectra we get n. 71. - /?„ AL ~~ (s\"> ~ = Thus i n determining 711 one measures i t as i f i t were a l i n e i n the iron spectrum and one calculates i t s equivalent iron wave length. Subtracting this value from the constant then gives . I t should be noted that a l l wave lengths above 2,000 A are given i n a i r and i t i s necessary to convert these values to vacuum wave lengths when using these formulae. As a preliminary check on this method iron arcs were photographed from both s l i t s , the lines identified and the constant f<, determined. The results of this measurement are as follows: 7939.50 7651.0A 6883.43 6486.92 6412.52 5399.18 3075.72 3366.87 4132.06 4529.89 4602.94 5615.65 11,018.40 11,018.50 11,018.61 11,018.60 11,018.52 11,018.40 21 PART III THE SOURCE The source used was an electrodeless discharge. This type of source was chosen because i t could be expected to give high excitation with very l i t t l e broadening of the lines due either to Doppler, c o l l i s i o n or Stark effects (16). Some d i f f i c u l t y has been encountered i n adapting this source to Indium and hence i t i s f e l t that a f a i r l y detailed discussion of our procedure w i l l be of interest. The source was arranged as shown i n Fig. 6. The spark gap was set at about 1 l/A\" and served to build up the voltage on the condensers before the gap breaks down. The sudden discharge then sets up a high voltage, high frequency o s c i l l a t i o n i n the c o i l wrapped around the quarts tube. Measurement of the Q factor of the c o i l indicates that the frequency of the oscillations i s approximately 20 megacycles. The condensers, which must be of high capacity and have high breakdown voltage, were Leyden jars. In order to get a reasonably bright and continual discharge i t i s necessary to have a vapour pressure of Indium of about IO\"-*- to 10\"^ mm. Reference to Table 5 indicates that this means that the temperature of the Indium must be about 10$0° C. In our f i r s t arrangement the heating was done e l e c t r i c a l l y but i t was d i f f i c u l t to maintain the temperature required because the elements burned out. The e l e c t r i c a l heat was abandoned and a gas and oxygen torch was used. This could maintain the temperature but i t was now found that the copper c o i l , which was necessarily heated to near the melting point of copper, corroded very rapidly. To overcome this d i f f i c u l t y the 22 copper c o i l was nickel plated. An attempt was made to protect the c o i l by placing i t outside the oven, which was made as small as was compatible with a proper f i r e chamber and adequate insulation, but i t was found that the increased diameter very seriously reduced the excitation. Pressure inside the tube was controlled by means of a variable pinch cock between the vacuum pump and the tube. I t i s necessary to adjust the pressure because the excitation obtained i s dependent on the pressure as the mean free path i s increased the average terminal velocity of the electrons i s increased and hence higher energies are attained. On the other hand, i f the pressure becomes too low there i s no discharge. A direct vision spectroscope was set up to look into the back end of the discharge tube and the relative intensities of known Indium I and Indium III lines were watched and the pressure was adjusted to bring the Indium III lin e up to maxiTrmni brightness. The tube was made as long as practical so the end windows were relat i v e l y far from the heat and the Indium vapor condensed on the walls before reaching the windows. This eliminated condensation on the window near the grating but the back window could not be as far from the furnace and this window gradually became coated. I t was necessary to play a flame on this window about every half hour to evaporate the condensed metal. Two indentations were made i n the bottom of the tube and at the centre of i t s length. The Indium was placed between these indentations and was thus prevented from flowing down the tube (which could not be precisely levelled) away from the heat. 23 With these precautions taken the source could be made to work very satisfactorily. However when the source was attached to the vacuum spectrograph with no window the spectrograph vacuum pump removed the vapour from the tube more rapidly than i t could be evaporated. I t was found that the oven had to be heated to 1500° G i n order to get a reasonably satis-factory discharge. Obviously the copper c o i l could not be used at this temperature so we substituted a nickel plated iron c o i l , but i t was s t i l l impossible to keep the source running for more than a few minutes before the iron c o i l melted. We f i n a l l y compromised by putting a thin fluor i t e window between the tube and the s l i t . The fluorit e transmits down to about 1200 A . Two other types of sources were considered; a vacuum arc i n a weak magnetic f i e l d and a high voltage spark operated under a low pressure of helium gas. The f i r s t of these was tried but the excitation did not appear to be high so i t was abandoned. We were not successful i n getting results from the l a t t e r source but I f e e l that i t s t i l l holds promise and should be investigated further. 24 PART I? RESULTS. Several plates taken on the vacuum spectrograph have been measured with a Hilger comparator and the wave lengths computed as outlined i n the section on the two s l i t method. In addition, plates taken on a Hilger E l prism spectrograph have been measured. The Hartman formula was used to calculate the wave lengths. These calculated wave lengths were then adjusted to f i t a correction curve which was obtained by comparing several of the wave lengths; with the wave length obtained from the grating. A typical correction curve i s shown i n Fig. 5. About 338 lines, have been measured. Of these 62 are lines which have been reported previously and which have been classified. The remainder are new unclassified lines. A l l the lines* either confirmed or nev are listed i n Table 6 which also gives the intensity of each line as measured by us under various conditions and as given i n the M.I.T. wave length tables. Our measured wave lengths for Indium I and Indium II agree very well with the published values with one exception i n Indium I which w i l l be mentioned later. However i n Indium III we find a large number are quite different from those published. INDIUM I The square array of Table 7 displays the term values and transitions for Indium I as measured by Sawyer and Lang (17). We have found a l l term 25 values to be accurate with the exception of the 5s5p 4Pi term, which should be 11,691 cm\"1 instead of 11,697 cm\"1 as given by them. A l l transitions which we have measured and confirmed are marked with an asterisk. The transitions involving 5s5p ^ P^ are given our value which differ from the published value by about 0.6 A . INDIUM II As previously mentioned, Indium II has been completely and accurately analysed by Paschen and Campbell (2) and by others (18,19,20,21), The square array of Table 8 displays the term values and wave lengths found by them. Those values which we have confirmed are marked with an asterisk. Several of our new lines may be classified as Indium II lines and may be fitted into the square array. A l l these newly classified lines are marked with a dagger ( T ) . Perhaps the most interesting of these new transi-tions i s the one 5s5p 3Po - 5p2 which has AJ =0 , J = 0, 4 5 = / and hence should be a strongly forbidden line. That this line i s actually observed i s due to the interaction with the nucleus. In addition to those lines marked on the square array we have discovered two interesting odd-odd transitions; namely 1228.2 A between 5s5p %o \" 5s4f ^3 and 1650.07 A between 5s5p ^ i - 5sAf ^ • these transitions have very low intensities. 26 INDIUM III The results of our measurements and classification of Indium III are given In Table 9. The energy of the ground state 4d^° 5s % ^ has been taken as 226,133 c-T-L i n accordance with Rao's estimate* As previously mentioned, we were unable to confirm some of the wave lengths found by Rao so this square array i s based on our own measurements. Although we found a very strong line for the transition 4d 1 0 5d 2D ? # i - 4a 1 0 Af 2 F 3 / / i , at 3008.23 A, we were unable to find any trace of a line for the transition 4_L0 5 d 2_)_//r_ m ^10 2p /^;_ 9 which Rao measured as 3009.96 A. Since this leaves only one line assigned to the ^zv^ term and only two lines assigned to the ^3//^ term, these term values should tbe regarded with skepticism. I have attempted to classify new terms based on the newly found wave lengths. The two terms 4d9 5s 2 , 4d? 5s 2 2D,^ have been l i s t e d with new lines i n each* Since these lines are a l l quite weak the term values given should be regarded as tentative, although they are reasonably close to the predicted values* 27 BIBLIOGRAPHY (1) Paschen, F.., Ann. der Efaysik, __, 152, (1938). (2) Paschen, F. and Campbell, J.S.., Arm. der Physik, 29, (1938). (3) Shenstone, A.G.., Phys. Rev., __> 894, (1940). (4) Shenstone, A.G., J.O.S.A., __, 219, (1949). (5) Herzberg, G., Atomic Spectra and Atomic Structure. Dover Publications, New York, 1940. (6) White, H.E., Introduction to Atomic Spectra. McGraw-Hill, New York, 1934. (7) Bohr, N., P h i l . Mag., 26, 476, (1913). (8) De Broglie, L., P h i l . Mag., _2, 446, (1924), Am. de Phys., _, 22, (1925). (9) Schrodinger, E., Ann. de Phy., __, 361, 489, 734, (1926), Phy. Rev., 28, 1049, (1926). (10 (11 (12 (13 (14 (15 (16 (17 (18 (19 (20 (21 Vhlonbeck and Goudsmidt, Nature, 117. 264, (1926). Russel, H.N. and Saunders, F.A., Astrophy. Jour., 6_, 38, (1925). Zerrdcke, F. von, Verhaudelihger, Op. 25 Mei, (1935), Aangobadon Aon Prof. Dr. P. Zeeman, (1935), 'S-Gravonhage, Martinus Nijhoff. Beulter, H.G.., J.O.S.A., _5, 311, (1945). Mack, Stohn and Edlen, J.O.S.A., __>, 245, (1932). Mack, Stohn and Edlen, J.O.S.A., 2_, 184, (1933). Boyce, J.G.., Rev. Mod. Phy.., __, 1, (1941). Sawyer, R.A. and Lang, R.J.., Phys. Rev., __, 718, (1929). Sawyer, R.A. and Lang, R.J., Z.S.f. Phy.,, _a,» 453, (1933). Rao, K.R., Proc. London, Phys. S oc, 161, (1927). Lang, R.J., Phy. Rev., _0, 762, (1927). Green, J.B, and Loring, R.A., Ehys* Rev., 574, (1927). (22) Lang, R.J., Proc. Hat. Acad. Sci., 12, 341, (1927). (23) Lang, R.J., Proc. Nat. Acad. Sci., 1£, 414. (1929). (24) Rao, K.R., Narayan A.L., Rao, A.S., Indian Journal Physics, g, 482, (1928). OTHER PAPERS ON INDIUM SPECTRAr NOT DIRECTLY REFERRED TO IN THE THESIS de Gramont, Compte Rondu. 171. 1106, (1920). Vhler and Tanch, Astrophy. Jour., j>5., 291, (1922). Frayne, Phys. Rev., J l , 152, (1928). Saunders, Astrophy. Jour., AJ, 24O, (1916). Weinberg, H., Proc. Roy. Soc., 122, 133, (1925). Green, J.B. and Lang, R.T., Proc. Nat. Acad. Sci., 14, 706, (1928). Lande, A., Zeits f. Physik, 80, 59, (1933). Sugiura, Jap. Journ. Ehys.,, J , 155, (1924). Hartree, D.R., Proc. Camb. Phil. Soc., £2, 304, (1926). Badami, E,., Proc. Phys. Soc., A2, 538, (1931). Jackson, D.A.., Zeits f. Physik, 80, 59, (1933). Schular and Schmidt, Zeits f. Physik, 104-5-6. 468, (1937). McLennan, All i n and Hall, Proc Roy. Soc., 122, 333, (1931). Bacher, R.F. and Tomboulian, P.H., Phys. Rev., j£, 836, (1938). Hamilton, D.R.., Phys. Rev., jj6, 30, (1939). 3P >?• / / / / • / / / / / / 3 I 2 * 2 0 . 0 \" 2 * 2 L-S COUPLING - COUPLING F I G U R E I - RELATIVE POSITIONS OF TERMS F I G U R E 2 - THE GRATING SURFACE UNDER FOUCAULT TEST F I G U R E 3 TYPICAL MOSELEY DIAGRAMS \\ G GRATING G GRATING FIDUCIAL MAR S* SLIT S SLIT FIDUCIAL MARK I DIRECT IMAGE PP PLATE HOLDER C CENTRE R ROWLAND CIRCLE / / / / / R / ERROR (ANGSTROMS) to CO o O o O TO PUMP 1 0-4 /^F l\" SPARK 5 0 , 0 0 0 V A PP. 110 V F I G U R E 6 — T H E S O U R C E P L A T E I M 111 • » raaaum i« w i» A i u m c to 1 IU X-tl WW kill T A B L E A G 1 CD II IN III T E R M vw T / R V T / R T ^ 2% 5s2 % 2 2 8 1 3 5 3 0 3 6 116 • 7 8 2 0 1 0 3 5 1 0 7 2 1 2 0 , 8 0 0 2 4 0 5 4 9 0 4 5 6 0 3 7 4 8 5 ( 0 2 0 1 0 4 0 114,1 0 0 5S5P 4P • 0 4 4 5 •2 110 2751 5 2 4 5 • 8 2 • 6 7 2 7 3 , 7 0 0 5P 2 P • 0 6 4 4 • 2 5 3 7 • 2 1 8 8 4 6 7 8 • € 8 • 4 6 2 5 $ , 7 0 0 8s 2 S • 0 5 0 4 2 2 4 4 •1671 • 4 0 8 7 • 6 0 • 3 6 0 3 9 , 5 0 0 7d 2 D • 0 4 0 5 2 0 0 4 • 1 5 3 2 • 3 9 1 4 •5 9 • 3 3 6 3 6 , 9 0 0 8P 2 P 0 4 0 9 2 0 2 2 1 4 3 6 3 7 9 0 • 5 5 5 • 3 0 8 3 3 , 8 0 0 9s 2 S « • 0 3 3 6 • 1 8 3 2 M 5 0 3 3 9 2 • 51 • 2 6 0 2 8 , 5 0 0 8d 2D • 0 2 7 9 • 1 6 6 9 • 1 0 7 2 • 3 2 7 4 • 4 9 2 4 0 2 6 , 3 0 0 T A B L E I — T E R M V A L U E P R E D I C T I O N S F R O M M O S E L E Y D I A G R A M S T E R M 5 s 2 * z 5P 5sl V A v A G I 3 1 , 5 5 4 3 0 , 8 6 4 6 9 0 3 1 , 5 5 4 2 6 , 3 9 2 5 ,16 2 2 4 . 4 3 3 25 . 5 9 5 CD II 9 2 , 2 3 8 67,1 I 5 2 5 , 1 2 3 9 2 , 2 3 8 6 1,4 81 3 0 , 7 5 7 2 3 ^ 0 0 0 2 4 . 1 0 0 IN III 1 6 8 , 9 4 8 1 2 0 , 8 2 5 4 8 , I 2 3 I 6 8 , 9 4 8 I I 4 . 0 9 I 5 4 , 8 5 7 53 5p P 6 1 , 1 0 6 4 ,8 8 3 5 6 , 2 2 3 4 9 , 9 9 6 1 3 6 , 3 7 4 3 0 , 1 8 5 1 0 6 , 1 8 9 4 8 , 0 0 0 2 2 6 , 1 3 3 7 1 , 9 3 3 1 5 4 , 2 0 0 T A B L E 2 — T E R M V A L U E PRED ICT IONS B Y T H E I R R E G U L A R D O U B L E T L A W i T a b l e 3 M - - « S B O D V B QUANTUM MJMBER SEQUENCES TERM VALUE PREDICTIONS FROM E t F E C T I V J i Q 8 31 9 5 6 1.3409 1.0913 2.4322 ° '/^ ? p , 1.8927 1.0578 2.9505 2.9818 1.0082 3.9900 4.9957 4.9966 1.2518 1.5784 z • „ a 1.0066 4 . 4 5 6 6 ^ 6 - « 9 7 1.0178 3 . 4 5 0 0 i > o o l 3 1 . 0 W 0 3 . S 6 3 5 4 - 9 6 8 1 m p 1.0012 6.9965 1.0019 5.9953 1.0034 4.9934 Cd II 1.0181 4.9478 5.9925 ^ *P 2, / 2 I - 9 9 1 7 •fi 1.0074 4 . 8 9 3 0 1 ' 0 0 5 9 S - 8 9 6 9 X 7 9 4 1 1 - ° 7 5 4 2 - 8 6 7 5 ^ 3 , 8 8 5 1.0067 5 . 2 9 3 7 <>.9890 ^ 2 l — — \" 4 ' 2 8 7 0 L 0 0 6 X 6 . 1 1 5 1 - 0 0 3 4 7 . H 8 5 '0714 ^ 4.0988 - 0 X 0 2 5 . 1 0 9 0 D;'/2 3.U/X* 6.9368 4 > 9 4 7 8 1.0013 5 . 9 « 0 0 IS rJC5.. ••• ,*> 4 S O tarn - • * ••\" *4 \"Xf si i H <0 H ?3 o * «0 ' CM. €9 © o O tB £*• • • *• to 0> 0> til - *, * i0't> ca 0 ; * *3 o 9. m o •ft I S3 05 am M H H 05 &4 N _ 5s 1° I*3 Table 4 R «• 1995 mnu b = 17,361 A d(nA) = b ]/1 - s i n 2 9 ds - R 5000 6000 0 6.268 25 6.257 50 6.245 75 6.233 100 6.638 6.221 125 6.629 6.209 150 6.620 6.197 175 6.611 6.185 200 6.602: 6.172 225 6.593 6.160 250 6.584 6.148 275 6.575 6.135 DISPERSION 1 = 2 0 ° 3 0 ' s i n i = . 3 5 0 2 s i n 9 • s i n i b 7000 8000 9000; 5.738 5.083 4*303 5.723 5.065 4.282 5-708 5 . 0 4 7 4.261 5.693 5.029 4.240 5.678 5.011 4.218 5.663 4.993 4.197 5.648 4.975 4.176 5.633 4.956 4.154 5.617 4.937 4.132 5.602 4.919 4.111 5.587 4.900 4.089 5.571 4.881 4.067 3 0 0 6.565 6.122 5.555 4.862 4 .045 325 6.556 6.110 5.539 4.343 4.023 350 6 .546 6.097 5.523 4.824 4,001 375 6.536 6.084 5,507 4.805 3.979 4 0 0 6.-526 6.071 5.491 4.786 3.956 4 2 5 6.516 6.058 5.475 4.767 3.934 450 6.506 6 .045 5.459 4.748 3.912 475 6.496 6.032 5.443 4.729 3.889 500 6 . 4 8 6 6.019 5.426; 4.709 3.866 525 6.476 6.006 5 .410 4.690 3.844 550 6 . 4 6 6 5.993 5.394 4.670 3.821 575 6.456 5.979 5.377 4.650 3.798 600 6.445 5.965 5 .360 4-630 3.775 625 6.435 5.952. 5.344 4.610 3.752 650 6.425 5.938 5.327 4.590^ 3.729 675 6 .414 5.924 5.310 4.570 3.706 Table 4 Continued 5000 6000 7000 8000 9000 700 6.403 5.910 5.293 4.550 3.683 725 6.392 5.896, 5.276 4.530 3.660 750: 6.331 5.882 5.259 4.510 3.637 775 6.370 5.868 5.242 4.49© 3.613 300 6.359 5.854 5.224 4.469 3.589 825 6.348 5.840 5.207 4.449 850 6.337 5.826 5.190 4.429 875 6.326. 5.812 5.172 4.408 900 6.214 5.797 5.154 4.387 925 6.303 5.783 5.137 4.366 950 6.292 5*768 5.119 4.345 975 6.280 5.753 5.101 4.324 Table 5 VAPOR PRESSURE OF INDIUM Vapor Pressure Temperature Melting Point 157°C 10\"5 mm 667°C IO\"\"4 mm 746°C 10-3 mm 84Q6C IO\"2 mm 952°C IO\"\"1 mm 1088°C 1 mm 1260°C Source - Tube Laboratory Manual M.I.T. Table 6 i [.I.T. P.F.. P.Q.. G.A. G.V. Ex. A V Class 20 7455.16 13409.9 12 7425.82 13462.7 12 7367.24 13570.3 5 7279.76 13720.2 5 7226.08 13768.8 30 7221.32 13844.1 5 7181.10 13922.0 12 7171.92 13939.4 5 7167.86 13947.4 5 6902.98 T/,/,82.4 50 I 6900.37 I4488.O I 150 200 II 6891.63 14506.4 II 30 6875.02 I454I.4 60 50. I 6847.73 14599.3 I 100 20 II 6783.72 U737.1 II 90 5 II 6751.78 I48O6.8 II 1 6748.30 14814.5 1 6746.89 14317.7 1 6745.66 14820.2 5 6679.44 14967.2 10 6664.12 15001.6 5 6582.82 15186.9 12 6578.16 15197.6 5 6517.22 15339.7 30 6512.18 15351.6 120 300 II 6305.14 15855.7 II 20 200: III 6197.19 16131.9 III 20 6160.60 16227.7 50 6147.88 16261.2 80 20 6142.77 16274.6 25 • 20 II 6141*04 16279.4 II 100 5W II 6128.11 16313.7 II 60 100 II 6115.51 16347.4 II 5 6097.02 16396.9 10 6018.00 16612.2 0 5935.60 16844.5 150 100 100 II 5918.70 16890.9 II 200 2 II 5915*67 16899.6 II 15 5905.04 16930.0 1000 150 100 II 5903.44 16934.6 II Table 6 Continued i i M.I.T.. P.F. P.Q. G.A.. G.V. Ex.. A Class 5 5854.58 17075.9 500 100 10 II 5853.03 17080.4 II 15 100 5 III 5819*48 17178.9 III 5 50 0 III 5722.95 17469,0 III 50 0 0 5709.50 17509.8 I 0 5695.40 17553.2 2 5679.08 17603.6 0 5666.22 17643.5 0 5662..50 17655.2 70 100 10 5644.88 17710.3 III 30 5609.13 17823.1 15 2. 0 II 5528.35 18083.5 II 500 0 II 5519.09 18113.9 II 400 100 2 II 5512.91 18134.2 II 0 5478.79 18247.1 0 5431.97 18404.4 0 5431.33 18406.6 2 . 1 . 5366.12 18630.4 3 0 5349.07 18689.6 1 0 5337.11 18731*5 0 5322.31 18783.6 0 5317.14 18801.9 250 40 50 1 II 5309.46 18829.1 II 5 200 100 20 III 5248.77 19048.1 III 1 5244.74 19061.4 200 0 5197,70 19233.9 300 400 2. 5184.25 19283.8 10 5128.83 19492.2 300 0 II 5117.37 19539.5 II 200 100 II 5116.25 19540.1 II 300W 5 II 5109.38 19566.4 II 0 5105.70 19580.5 0 5097.49 19612.0 5 5085.98 19656.4 2 5054.70 19778.1 1 5045.48 19814*0 0 5030.72 19872.4 00 5014*18 19937.9 5 5012.01 19946*5 00 5006.67 19967.8 Table 6 Continued 111 M.I.T. P.F* P.Q. G.A. G.V, Ex. A V Class 0 4972.35 20105.6 2 4957.12 20167.4 0 4949.08 20282.1 0 4919.73 20320.7 0 4874.44 20509.5 0 4819.87 20741.7 5 4800.01 20827.5 0 4778.49 20921.3 0 4764.66, 20982.1 0 4757.57 21013.3 35 OV 4701.58 21263.5 300 10W II 4684.65 21340.6 II 2500 4682.00 21352.4 200 100 II 4681.U 21356.5 II 30 4678.17 21369.9 5 ow II 4673.30 21392.2 II 0 4660.00 21453.2 250 500 100W II 4655.63 21473.4 II 200 100 10 II 4644.6I 21524.3 II 70 4638.86 21551.0 200 100 II 4638.ll 21554.5 II 5 4625.74 21612.1 150 4612.13 21675.9 20h 4593.70 21762.9 10 4579.32 21831,2 3h 4576.10 21846.6 5 4535.50 22042.1 10 4530.05 22068.6 10 4523.57 22100.3 10 4517.42 22130.4 5000R 20 100 I 4511.32 I 10 4505.42 22189.3 10 4487.36 22278.6 15h 4415.69 22640.2 5h 4389.48 22775.4 5h 4383.76 22805.0 2 0 5 III 4358.53 22937.1 II 10 III 4252.66 23508.1 III 5 4245.33 23548.7 5 4223.57 23670.2 Table 6 Continued i v M.I.T. P.F. ?..Q. G.A.. G.V. Ex. Class 5 4215.90 23713.1 100 20 II 4205.10 23774.0 II 10 4196.99 23825.6 15 4180.94 23911.4 8 4158.08 2/,0/,?.8 2W, 4156.73 2405O.I 15 4132.90 24189.3 200R 100 20 20d 200 I. 4101.77 24373.9 I 200Wh 10 • 1 20 4072.68 24547.0 8W 40 I l l 4071.57 24553.6 III 2 3 10 III 4062.23 246IO.I III 10 4057.86 24636.7 3 40 II 4056.99 24641.9 II 10 2 100 III 4032.33 24792.6 III Z 4031.95 24794.9 lOWh 3 2 20: III 4023.56 24846.6 III 100 1 5 II 3962.17 25232.6 II 15 3957.46 25261.6 o; 2 3953.29 25288.2 3 3941.33 25365.0 18 3936.79 30 l 1 II 3934.02 25412.1 II 1 3932.30 25423.2 18 3920.54 25499.5 1 3913.98 25542.C 50 5 50 3902.12. 25619.9 II 100 1 3890.26 25698.0 20bh 3883.20 25744.7 20bh 3871.30 25823.8 3bh 3861.48 . 25889.5 50 8 100 3853.00 25946;5 III lbh 3850.00 25966.7 100 10 150 3842.27 26018.9 II 15 3835.18 26067.0 200 20 500 3834.60 26071.0 II 80 1 II 3799.38 26312.6 II 80) 400 10 100 II 3795.22 26341.5 II 3 3739.95 26730.8 150 30 10 II 3718.49 26885.0 II 50 10 2 40 II 3716.13; 26902.1 II 5 3709.60 26949.4 Table 6 Continued J.T. P.F. P.Q. G.A.. G.V. Ex. A V Class 5 1 . - . . - . 3708.3 26958.* I 25 10 1 20 II 3693.97 27063.5 II 10 3689.5 27096.3 15 3683.52 27140.3 Obh 3664.3 27282.6 10 3649.95 27389.9 0, 3644.7 27436.8 0 3642.7 27444.4 0 3638.5 27476a 10 2 0 3628.9 15 3612.86 27671 18 3610.51 27689 3 3602.88 27747.6 10 0 III 3590.4 27844.7 12 10 0 3586.0 27878.3 12 10 3584.0 27893.9 a 3582.5 27905.5 0 3576.2 27954.7 6 3572.75 27981.7 0 0 2 3550.37 28158.0 3 3546.83 28186.2 3Wh 3542.82 28218.0 1 3542.08 28223.9 10d 3536.3 28270.1 .OWh 3535.71 28274.0 5d 3533.1 28295.7 lOd e II 3517.6 28420*4 II 2 3498.09 28579.6 1 3483.70 28696.9 2 hh 3438.3 29076.7 0 bh 3433.4 29177.3 0 bh 3421.4 29219.5 50 1 II 3404.12 29367.8 II 1 bh 3399.46 29408.0 25 1 0 II 3376.63 29606.9 II 50 1 2 3370.98 29656.3 3 3370.0 29665.1 1 3363.0 29726.8 I 6 200 1 10 3360.15 29752.0 6 3358.0 29771.1 I Table 6 Continued v i M.I.T.. P.Q. G.A.. G.V.. Ex. A V Class 1 3343.85 29897.1 40 50 20 50 II 3338.67 29943.5 II 3 3336.26 29965 0 b 3302.6 30270.5 00 3293.0 30358.7 4d 3281.8 30462.3 4d 3278.4 30493.9 4d 3272.9 30545.2 4d 3268.2 30589.1 2d 3267.1 30599.4 20 2 1 3264.12 30627.3 2d 3262.6 30641.6 2d 3260.6 30660.4 500R 80 10 2003 I 3258.52 30680.0 I 1000R loo; 20 500 I 3256.07 30703.0 I 10 3250.4 30757\" 15 3247.61 30783' 1 3245.9 30-799.2 5 80- 10. 50 II 3236.82 30885.6 II 2 1 3198.22 31258.4 50 5 1 II 3194.70 31292.8 II 12 100 20 40 III 3187.03 31368J. 30 2 II 3176.39 31473.2 II 10W. 5 III 3160.20 31634.4 100 80 20 10 II 3158.64 31650.0 II 200 10 5 0 II 3156.08 31675.7 II 75 80 20 20 II 3147.04 31766.7 II 35 0 II 3142.64 31811.2 II 80 20 10 3138.91 31849.0 3 3132.93 31910 3 3121.55 32026 1 3104.16 32205.5 3 3100.92 32239.2 80. 10 II 3100.05 32248.2 II 15 10 5 II 3083.84 32417.7 II 3 3081.05 32447 10 3078.27 32476 3 3067.73 32588 6 3066.55 32600.4 10 3056.58 32706.8 Table 6 Continued v i i M.I.T. P.F. P.Q,. G.A. G.V. Ex. A V Class 15 40 30, 40 I 3051.25 32764.0 I 3 30 20 IG III 3047.94 32799.5 oh 3047.0 32809.7 3 3043.40 32848.5 1000R 50 30 100 I 3039.42 32891.5 I 3 3038.67 32899.5 12 3037.11 32916.7 1 3034.12 32949.2 3 3023.39 33066.9 18 2 3 II 3022.86 33071.7 II 33 3017.78 33127.3 500W 200 40 100 III 3008.23 33232.5 III 50 10 5 0. - II 2999.60 33328.1 II 2 2989*59 33439*7 2 2986.92 33469*6 2 2983.99 33502.4 , 30 200 40 100 III 2982.88 33515*P III 10 2979,58 33551*9 4W 2976.24 33589*7 2W 2970.89 33650.1 25 5 4 II 2966.20 33703.4 II 4 hh 2962.00 33751*1 2 2959.72 33777.1 50 50 40 100 I 2957.08 33807.3 I 80 100 100 100 II 2941.03 33991.7 II 10, 2939.36 34011.1 3 2933,27 34081.7 500 50 50; 40 I 2932.57 34089.7 I 2 2928.04 34142.6 2 2927.08 34153.8 10 2 1 II 2916.47 34277.9 II 3 2911.45 34337.1 5 2910,52 34348.1 2 2907.93 34378.7 2 2907.08 34388.7 2 2905.16 34411.4 12 2900.56 34466.0 60 200 50 200 II 2890.20 34589.6 II 2 2884.08 34663.0 2 2881.61 34692.7 Table 6 Continued v i i i [.1..T. P.F., P.Q. G.A. G.7.. Ex. A V Class 2 2873.50 34791 20 0 2867.3 34865.8 20 0 2866.46 34876.0 6 0 5 20 II 2865.70 34885.3 II 3 2864.23 34903.2 5 2860.52 34948.4 3 0 100 50 30 I 2858.10 34978.0 I 2 2844.51 35145.1 2 2839.98 35201*2 2 2839.33 35209.2 6 2838.87 35215.0 80 2 50 40 100 I 2836.89 35239.5 I 3 2835.95 35251.2 1 2833.93 352763 3 2833.06 35287.2 3 2823.99 35400.85 50 2 II 2819.17 35460.9 II 2 2811.93 35552*3 2 2810.90 35565.3 2 3 1 0 II 2805.12 35638.6 II 2 2803.18 35663*3 0 2 2802.54 35671*4 3 2802.01 35678.2 30 0 o; II 2798.70 35720.4 II 1 3 2795.36 35763.0 2 2792.74 35796.6 8 2786.25 35880.0 0 2783.48 35915.6 I 80 80 40 40 I 2775.35 36020.9 I 3 2773.04 36050.9 m 2755.5 36280*4 300Wh 30 10W 20 I 2753.65 36304.7 I 20 5W 1 II 2752.78 36316.1 II 80 100 15 20 40 II 2749.70 36356.9 II 25Wh, 2748.72 36369.8 2 2747.9 36381 2¥ 2746.8 36395.3 1 0 2740.01 36485.6 0 2732.0 36592.4 2 2726.27 36669.3 Table 6 Continued ix M.I.T.. P.F. P.Q.. G.A. G.V. Ex. A V Class 30 8W 2725.95 36673.7 20 8W 2725.34 36681.8 2. 2715.72 36811.7 125 50 20 4 20 I 2713.93 36836.O I 200Rh 80 20 10 50 I 2710.26 36885.9 I 5 2709.2 36900.0 2 2705.2 36955 30 0 2 II 2704.41 36965.7 II 50 10 10 2 II 2683.0 37260.7 II 80. 6 10 II 2674*55 37378.3 II 25 0 1 II 2672.10 37412.6 II 80 4 10 II 2668.65> 37461.0 II 60 0 2 II 2662.70 37544.7 II 2 2634*70 37944 2 0 1 2631.0 37998 36 00 0 II 2623.35 38107.8 II 2 0 0 2614.31 38240 2 0 2612.01 38273 150 8 40 2W. I 2601.91 38421.8 I 30 5 10 II 2598.74 38468.6 11 10 2¥ III 2591.97 38567.2 II 2 2589.5 38606 2 2585.8 38661 2 1 0 III 2584.6 38679 2 2580.8 38736 3 2578.9 38765 2 2570.3 38894 AO 0 0 II 2565.13 38972.7 II 50Rh 80 40 10 I 2560.25 39047.0 I 1 2559.12 39064.2 140 50 40 10 II 2554.45 39135.8 II 2 2552.0 39173 20 2 2545.90 39367.1 2 2541.6 39333 10 5 2536.49 39412.7 5 2528.17 39542 50 15 0 LE 2527.50 39552.9 2 2524.20 39605 10 10 20 I- 2523.00 39623.4 I 30 20 30 2 2521.65 39649.8 I 2 2521.32 39644.6 Table 6 Continued x M.I.T. P.F. P.Q. G.A. G..V. Ex. A V Class 2 2519.41 39680 3 2516.40 39727 4 2510.41 39822.1 8 2508.37 39854.5 2 2505.04 39907.5 3 2497.20 40032.8 2 2495.97 40052.5 40 10 10. II 2486.17 40210.2 II 10. 2 2 0 HE 2478.55 40333.9 12 2475.56 40332.7 1 2470.64 40463.I I 2Wh 4 20 0 I 2468.08 40505.O I 2 2466.47 40531.5 5Wh 5 2 II 2460.15 40635.6 3 2455.68 40709.6 0 2455.35 40715.1 2 2449.14- 40883.3 3 2438.75 40992 2 2433.9 41074 10R 2: 2430.99 41122.8 I 20R 10 2429.86 /.Tl/,2.1 I 0 2429 41156.7 3 2428.4 41167 0. 1 2422.92 41260.0 I 2 242O.6O 41300 2 2417.66 41349.6 1 15 I 2399.18 41668.1 I 4 20.- I 2389.54 41836.2 I 5 1 1 II 2384.50 41924.7 II 60 10 20 2382.63 41957.6 II 5 I 2358.70 42383.3 I 3 2351.45 42514 15 50 20 20 20. II 2350.78 42525.9 II 0 2347.09 42592.7 I 0 2346.02 42612*3 I 3 2341.84 42688.3 I 8 0, I 2340.19 42718.4 I 1 2339.72 42727.1 4W. 2336.97 42777*2 5 00 I 2332.74 42854.9 I Table 6 Continued x l M.I.T. P.F.. P.Q, G.A. G.V, Ex.. 7\\ V Glass 2 2324.36 43009..3 2 2321..83 43057 2 I 2315.09 43181.5 I 43 1 II 2313.22 43216.4 II 1 I 2309.42 43287.6 I 100 10 100 200 BE 2306.10 43349.9 II 1 0 2301.28 43440.7 2 I 2298.37 43495,5 I 10 2297.09 43520 2 0 2292.8 43601 1 2290,27 43649,5 0 I 2283.75 4 3 7 7 4 a I 2 I 2273.23 43880.1 I 6 3 2265.06 44134 5 2 2261.26 44209.6 1 I 2260.25 44229a 1 I 2241,66 44595,9 I 1 I 2230.67 44815.6 I LE 2229.8 44833.1 2 2227.50 44879.4 2 2216.3 45106.2 2: 2211.40 45206.1 25 1 II 2205.35 45330a n 0 2203.57 45366.7 00 2198.40 45472.1 1 0 2197.41 45494.0 1 2177.7 45906 2171.0 46047 2 2158.4 463I6 2 2157.0 46346 2 1 2154.36 46402.7 0 2144.81 46609.4 27 4 200 2078.70 48092.2 11 12 2062.0 48481.0 12 2025.44 49355.9 20 100 II 1977.36 50572.4 11 10 50 II 1966.67 50847.3 11 1 1942.433 51481.9 10 50 II 1936.41 51641.9 11 8 50 II 1930.60 51797.3 11 Table 6 Continued x i i i M.I.T. FJ.. P.Q.. G*A. G.V.. Ex* Class 5 30 III 1530.18 65351.7 III 6 1521.7 65715.9 10. 10 III 1494*1 66929.0 III 5 1492.96 66981*0 5 uo III 1487.59 67222*8 III 50: 1469.36 68056.8 0 1442*8 69309.6 20 III 1434.85 69693*6 III 8 1406.2 71113*6 10 20 III 1403*1 71270.9 III 0 1381.35 72393.9 5 1344.6 74371*5 6 1330.9 75137.1 1 1322.55 75611 5 1320.2 75746.0 9 1296.0 77160*4 10 0 II 1280*59 78089 II 0 1265*66 79010.0 0 1228.2 81419.9 2 1158.0 86355.7 M.I.T. P*P* P.Q.. G.A. G.V.. Ex. Class Intensity from M.I.T. Tables. Intensity on Prism Spectrograph with Eastman F Plate. Intensity on Prism Spectrograph with Ilford Q Plate. Intensity on Grating Spectrograph in air.. Intensity on Grating Spectrograph in vacuum. Probable Excitation. Wavelength. Wave number. Classification. U(,.f,L7 •? 9*7, fSS- 3 19, 911 1*7, 8 6 960 3 *P ?P *7*900 3 297 3 9P . 3?bi>9 6f V C - T 30SO /Op 'f?/jt 2391 9 IOp> *7°I'/T. 237O F •ZZHO s *\\ 22, 29M 8 Viol 7Z U~ 3.1,373 1 VSt/-*7 * ZZ/bO S 69OO 3 7_. ii,*vt9. o *>i97 77_^ 11, S99.3 S 721 2-7 17, *6Z-S 3-709. 7& 11, So 9. 1 sz*,: >.0 Z7S3. gj * 3(J30/ 8 2932 bO 3*7, o 89.-1 Get 20_y_ * 39,oi%. 3 2-713-9 S * 36, f3S- f I bc< *oef3. 7S69. 6 27/0 Zg 3d 98S7 9s *s//x 6 03/ a Zlbo Ob * lO.b* 7 O ZbOI. 7S\" 3 e, izi. 2 T A B L E - 7 INDIUM 1 993/ e Z389 S f c ^ i/l, f3S 9 2SZ2 99 *-39 bZ3C 7cl *Ds/jt ¥806> 1 2S2.I 3 b 39, (.19 Z NOTE — ALL TERM AND TRANSITION VALUES ARE FROM SAWYER S LAN G ( ) EXCEPT THOSE INVOLING 5s5/o'% 'z * INDICATES A LINE CONFIRMED BY US 9s 39Y9 S 23*70ZZ HZ, 7/7? Z1b8ol *yo,sof> z. 33Z? 3 2306 7 t/3Z3i. k z*Yz9 t>8 fl, 127 9 33/0 I Z*Y3o 7 *7/, \"IS- o /Oz Z 7? 7 8 93, f 90 6 23 99 * 9c7 *D„t 2Y*73 6 Z2t>0 s *1*1, 3 • 9c( xOs-u 2 -Y 2379 66 t/2po99 lis zobf g 2Z*i1 s ^ 1*7,^9 9- 1 /oc( zDi/^ IS ss it/213 123 •* J '/-. it>oo 221 9 z */•?, 06 9 lief *Q zz// 1 *vs ziz SP 2P,/z ,6 8, 9VS 169, 6 Olf-6p 6 p *Pi '/g 80, 2 Of H f ZFz<^ 69, IS 9 1 f 'Fs'/* 6 y, if 8 2Z6, 133 loo n«8 (.s S7, '67 I6Z-3f (,,,SZf o II8.ZOZ 1 HI SI 3 to HC, lOZ 7 ZiSIO ' 37, 998 l Sff8/f So 67 II ' 3Z, 7 ZS3 xo If3° 66 9*1- 0 0,97,1 *\" lb, 13/ f 17,169-0 Z9&Z88 '00 33,StS. O * G 10 ?3so8 1 SS, S9S 38S3 OO 10 fOtZ Z3 SS, tit 100 H03Z 3 3 2f 6 39, S9S HOT, si 2*7,S53 6 T A B L E 9 - INDIUM III S Q U A R E A R R A Y "@en ; edm:hasType "Thesis/Dissertation"@en ; edm:isShownAt "10.14288/1.0085262"@en ; dcterms:language "eng"@en ; ns0:degreeDiscipline "Physics"@en ; edm:provider "Vancouver : University of British Columbia Library"@en ; dcterms:publisher "University of British Columbia"@en ; dcterms:rights "For non-commercial purposes only, such as research, private study and education. Additional conditions apply, see Terms of Use https://open.library.ubc.ca/terms_of_use."@en ; ns0:scholarLevel "Graduate"@en ; dcterms:title "The spectra of indium"@en ; dcterms:type "Text"@en ; ns0:identifierURI "http://hdl.handle.net/2429/41189"@en .