Energy Levels and Observed Spectral Lines of Xenon, Xe I through Xe LIV
`
`E. B. Saloman
`National Institute of Standards and Technology, Gaithersburg, Maryland 20899-8422
`
`~Received 14 May 2003; revised manuscript received 13 November 2003; accepted 15 December 2003; published online 25 August 2004!
`
`The energy levels and observed spectral lines of the xenon atom, in all stages of
`ionization for which experimental data are available, have been compiled. Sufficient data
`were found to generate level and line tables for Xe I–Xe XI, Xe XIX, Xe XXV–Xe XXIX,
`Xe XLIII–Xe XLV, and Xe LI–Xe LIV. For Xe LIII and Xe LIV theoretical values are com-
`piled for the energy levels. In 15 of the other stages a few lines are reported. Experimen-
`tal g factors are included for Xe I, Xe II, and Xe III. A value, either experimental, semi-
`empirical, or theoretical, is included for the ionization energy of each ion. © 2004 by the
`U.S. Secretary of Commerce on behalf of the United States. All rights reserved.
`@DOI: 10.1063/1.1649348#
`Key words: compilation; critically evaluated data; energy levels; observed spectral lines; spectra; Xe; xenon;
`xenon ions.
`
`Contents
`
`Introduction. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`1.
`2. Acknowledgments. . . . . . . . . . . . . . . . . . . . . . . . . .
`3. Explanation of Tables of Compiled Levels and
`Lines. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4. Tables of Energy Levels and Observed Lines. . . .
`4.1. Xe I. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.2. Xe II. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.3. Xe III. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.4. Xe IV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.5. Xe V. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.6. Xe VI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.7. Xe VII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.8. Xe VIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.9. Xe IX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.10. Xe X. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.11. Xe XI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.12. Xe XII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.13. Xe XIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.14. Xe XIV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.15. Xe XV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.16. Xe XVI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.17. Xe XVII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.18. Xe XVIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.19. Xe XIX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.20. Xe XX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.21. Xe XXI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.22. Xe XXII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.23. Xe XXIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.24. Xe XXIV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.25. Xe XXV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.26. Xe XXVI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`
`766
`766
`
`766
`767
`767
`797
`820
`847
`863
`869
`874
`879
`884
`889
`892
`898
`898
`899
`899
`899
`899
`899
`900
`900
`901
`901
`901
`901
`901
`903
`
`© 2004 by the U.S. Secretary of Commerce on behalf of the United States.
`All rights reserved.
`
`4.27. Xe XXVII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.28. Xe XXVIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.29. Xe XXIX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.30. Xe XXX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.31. Xe XXXI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.32. Xe XXXII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.33. Xe XXXIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.34. Xe XXXIV. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.35. Xe XXXV. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.36. Xe XXXVI. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.37. Xe XXXVII. . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.38. Xe XXXVIII. . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.39. Xe XXXIX. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.40. Xe XL. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.41. Xe XLI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.42. Xe XLII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.43. Xe XLIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.44. Xe XLIV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.45. Xe XLV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.46. Xe XLVI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.47. Xe XLVII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.48. Xe XLVIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.49. Xe XLIX. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.50. Xe L. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.51. Xe LI. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.52. Xe LII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.53. Xe LIII. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`4.54. Xe LIV. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
`
`List of Tables
`1. Sources of Xe I levels. . . . . . . . . . . . . . . . . . . . . . . .
`2. Parameter X for adjusting 70HUM levels. . . . . . . .
`3. Sources of Xe I lines. . . . . . . . . . . . . . . . . . . . . . . .
`4. Sources of Xe II lines. . . . . . . . . . . . . . . . . . . . . . . .
`5. Sources of Xe VI lines. . . . . . . . . . . . . . . . . . . . . . .
`6. Sources of Xe VII lines. . . . . . . . . . . . . . . . . . . . . . .
`7. Sources of Xe VIII lines. . . . . . . . . . . . . . . . . . . . . .
`
`905
`906
`907
`908
`908
`909
`909
`909
`910
`910
`910
`910
`910
`911
`911
`911
`911
`913
`914
`916
`916
`917
`917
`917
`917
`919
`920
`921
`
`767
`767
`768
`798
`870
`875
`885
`
`0047-2689(cid:213)2004(cid:213)33(cid:132)3(cid:133)(cid:213)765(cid:213)157(cid:213)$39.00
`
`765
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`ASML 1020
`
`

`
`766766
`
`E. B. SALOMAN
`
`1. Introduction
`
`In 1958 Moore @58MOO# published a compilation of the
`energy levels of xenon containing detailed analyses of Xe I–
`Xe III and a very partial analysis of Xe IV. In 1968 Striganov
`and Sventitskii @68STR# published a compilation of xenon
`lines containing a long list of observed lines for Xe I–Xe III,
`a limited calculated list for Xe IV, and a few lines for Xe V–
`Xe VIII. Since these compilations were completed, much
`work on Xe has been published. This work includes results
`obtained with new techniques such as laser spectroscopy,
`beam foil spectroscopy, electron beam ion trap ~EBIT!, laser
`excited plasmas, laser implosion, and fusion devices such as
`tokamaks. As a result we now have energy levels for 24
`stages of ionization of Xe and at least one line for 39 stages.
`This compilation takes into account published work
`through December 2002. There are occasional exceptions in
`which later work is considered, particularly for the ion Xe XI.
`Generally, only experimentally derived energy levels are
`used; these include semiempirical results obtained by inter-
`polation and extrapolation along isoelectronic sequences. An
`exception is made for Xe LIII and Xe LIV where good theo-
`retical values exist. The use of calculated values is indicated
`by enclosing the energy value in square brackets for these
`ions and for a very few levels in other ionization stages.
`We tabulate only those lines that have defined levels but
`include some additional lines in the text for highly ionized
`stages. For tabulated lines, the wavelengths are compared to
`the energy level differences and must be consistent to be
`included. For many of the stages, decisions are made about
`which of several possible classifications to include by calcu-
`lating the respective transition probabilities with the Cowan
`code @81COW#. As a result of this process, in a few cases the
`line classifications may differ from those given in the stated
`references.
`Occasionally two groups may differ in their published
`analyses of the spectra of a particular stage of ionization and
`in the identification of lines belonging to that stage. In such
`cases we select the analysis we believe to be better. How-
`ever, the choice is not always clear.
`Many laser spectroscopy papers provide data about Ryd-
`berg series with results up to very high values of the princi-
`pal quantum number n. In this compilation we limit the tabu-
`lated levels ~and thus also the corresponding lines! to include
`only n less than or equal to 20.
`For the first ionization energy we try to provide the best
`available values obtained experimentally. We do not average
`experimental values by different authors. Where experimen-
`tal values are not available, we prefer to use semiempirical
`results which adjust calculations along an isoelectronic se-
`quence to fit available information about some of the mem-
`bers. For one- and two-electron ions there are very good
`theoretical values. Where no information of these types is
`available, we use the calculations of Carlson et al. @70CAR#
`which are based on a simple spherical shell solution for neu-
`tral atoms. Their results seem to be within about 7% of val-
`ues obtained by experimental or semiempirical methods for
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`xenon. We note that another calculation was carried out by
`Magomedov and Omarova @90MAG# using the method of
`the quasiclassical self-consistent field. The available xenon
`experimental and semiempirical values tend to fall between
`the two calculations except for the highest ionization stages.
`All energy levels are given in units of cm21 and all wave-
`lengths in units of Å ~0.1 nm!. Ionization energies are pro-
`vided in both cm21 and eV. We use the conversion factor
`8 065.544 7760.000 32 cm21/eV as determined by Mohr and
`Taylor @99MOH#.
`Although it is often difficult to determine, uncertainties in
`the referenced publication of energy levels and lines are
`likely 1s values. In many cases only the number of decimal
`places indicates the uncertainty in the quoted values. We
`generally use a ‘‘rule of 20’’ whereby an uncertainty of
`greater than 20 in the least significant digit serves as the
`criterion for dropping that digit.
`The text for each ion does not attempt to provide a com-
`plete review of all work on that stage of ionization. Rather, it
`intends to credit the major contributions, especially those
`from which values are included in the line and level tables.
`
`References
`
`58MOO
`
`68STR
`
`70CAR
`
`81COW
`
`90MAG
`
`99MOH
`
`C. E. Moore, Atomic Energy Levels, Vol. III,
`National Bureau of Standards ~U.S.! Circ. No.
`467 ~U.S. Government Printing Office, Wash-
`ington, D.C., 1958!.
`A. R. Striganov and N. S. Sventitskii, Tables of
`Spectral Lines of Neutral and Ionized Atoms
`~IFI/Plenum, New York, 1968!.
`T. A. Carlson, C. W. Nestor, Jr., N. Wasserman,
`and J. D. McDowell, Atomic Data 2, 63 ~1970!.
`R. D. Cowan, The Theory of Atomic Structure
`and Spectra ~University of California Press,
`Berkeley, 1981!.
`K. M. Magomedov and P. M. Omarova, Opt.
`Spectrosc. ~USSR! 68, 10 ~1990!.
`P. J. Mohr and B. N. Taylor, J. Phys. Chem. Ref.
`Data 28, 1713 ~1999!.
`
`2. Acknowledgments
`
`I wish to thank J. Reader, C. J. Sansonetti, and W. C.
`Martin for many helpful discussions and advice on the selec-
`tion of data to include in this compilation. I thank J. Reader
`for providing prepublication access to the Xe XI data. This
`work was supported in part by the Office of Fusion Energy
`Sciences of the U.S. Department of Energy and by the Na-
`tional Aeronautics and Space Administration.
`
`3. Explanation of Tables of Compiled
`Levels and Lines
`
`In the Energy Level Tables the first column provides the
`energy level in units of cm21. The values have been rounded
`using the ‘‘rule of 20.’’ The absence of a decimal point in a
`whole number is used to indicate that the last digit is not
`significant. The second column provides the parity of the
`
`

`
`SPECTRAL LINES OF XENON
`
`767767
`
`TABLE 1. Sources of Xe I levels
`
`Source
`
`58MOO
`
`58THE
`
`67HUM
`
`Number
`of levels
`
`86
`
`20
`
`8
`
`Method
`
`Compilation of published and
`unpublished work to Dec. 1957
`Classical spectroscopy
`
`Classical spectroscopy
`
`70HUM
`
`101
`
`Interferometric spectroscopy on 136Xe
`
`72COD
`
`81GRA
`
`82LAB
`
`85YOS
`
`89HUI
`98AHM
`
`01BRA
`
`50
`
`18
`
`74
`
`28
`
`37
`16
`
`5
`
`Absorption spectroscopy using
`synchrotron radiation
`Optogalvanic spectroscopy
`
`Laser excitation with optogalvanic
`spectroscopy
`Absorption spectroscopy of discharge
`source
`Laser spectroscopy
`Optogalvanic spectroscopy
`
`Isotope resolved laser spectroscopy
`
`aL is the value of the level as published. X is given in Table 2.
`
`Adjustmenta
`~cm21!
`
`L20.508
`
`L20.508
`
`L20.508
`
`L2X
`
`None
`
`L20.508
`
`L20.501
`
`None
`
`None
`None
`
`To natural isotope
`mix
`
`Comment
`
`To match ground to excited state separation as determined from
`01BRA ~adjusted!
`To match ground to excited state separation as determined from
`01BRA ~adjusted!
`To match ground to excited state separation as determined from
`01BRA ~adjusted!
`X given in Table 2. Adjusted to natural isotope mix using several
`reported isotope measurements and ground to excited state
`separation as determined from 01BRA ~adjusted!
`
`To match ground to excited state separation as determined from
`01BRA ~adjusted!
`To match the value we use for the 6p@5/2#3 level
`
`Uses same value of reference level as we do to the precision of the
`results
`Isotope-specific results adjusted to natural isotope mix by using
`average weighted by abundance of isotopes in the natural mix
`
`energy level; ‘‘0’’ signifies even parity and ‘‘1’’ signifies odd
`parity. The next three columns specify the configuration,
`term, and J value of the level. In the cases of Xe I–Xe III
`there is an additional column next which provides the g fac-
`tor of the level ~when known!. Finally in the last column a
`reference is given to the source of the compiled level.
`In the Line Tables wavelengths between 2 000 and 20 000
`Å are in air. All others are vacuum wavelengths. The first
`column is the observed wavelength in angstroms ~Å!. The
`second column is the vacuum wave number corresponding to
`the observed wavelength. The wave numbers are provided in
`units of cm21 for ionization stages Xe I–Xe VI and in units of
`103 cm21 for the higher ionization stages. The absence of a
`decimal point indicates that the last zero is not a significant
`digit. The conversion between air wavelengths and vacuum
`wavelengths and wave numbers is made using the three-term
`formula given in Eq. ~3! of Peck and Reeder @72PEC#. The
`wave number values are rounded to the appropriate number
`of significant digits using the ‘‘rule of 20.’’ The third column
`is the relative intensity assigned to the line. Also included
`here are codes which are defined for each ion. The next six
`columns specify the classification of the transition respon-
`sible for the line by providing the configuration, term, and J
`value first for the lower level and then for the upper level.
`The next to last column is an estimate of the uncertainty in
`the wavelength of the observed line. The last column identi-
`fies the source of the observed line.
`
`Reference
`72PEC
`
`E. R. Peck and K. Reeder, J. Opt. Soc. Am. 62,
`958 ~1972!.
`
`4. Tables of Energy Levels and Observed
`Lines
`4.1. Xe I
`
`Z554
`Ground state
`1s 22s 22p 63s 23p 63d 104s 24p 64d 105s 25p 6 1S0
`Ionization energy 97 833.78760.012 cm21 ~12.129 842
`60.000 002 eV!
`The energy levels of Xe I have been compiled from 11
`different sources @58MOO#, @58THE#, @67HUM#, @70HUM#,
`@72COD#,
`@81GRA#,
`@82LAB#,
`@85YOS#,
`@89HUI#,
`@98AHM#, @01BRA# which are summarized in Table 1.
`Where necessary, the published energy levels ~denoted by L
`in Table 1! have been adjusted to put all sources on a com-
`mon basis. The adjustments used are specified in Tables 1
`and 2. The largest part of the adjustments has been to obtain
`a common value for the large separation between the ground
`state and the excited levels. The value we used was obtained
`
`TABLE 2. Parameter X for adjusting 70HUM levels
`
`Level
`
`4 f , 5 f – 9 f
`5d
`6s
`6p
`7p
`8p
`10f
`all others
`
`X (cm21)
`
`0.496
`0.497
`0.500
`0.495
`0.496
`0.497
`0.497
`0.498
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`

`
`768768
`
`Source
`
`30GRE
`33HUM
`
`34MEG
`
`35BEU
`35MEG
`
`49SIT
`52HUM
`55THE
`58THE
`60HUM
`61HEP
`63HUM
`64AGO
`64FAU
`64PET
`67HUM
`72COD
`72MOR
`73HUM
`85YOS
`
`98AHM
`00MIS
`01BRA
`
`E. B. SALOMAN
`
`TABLE 3. Sources of Xe I lines
`
`Number of
`classifications
`
`Light source
`
`Wavelength range
`~Å!
`
`Uncertainty
`~Å!
`
`2
`410
`
`132
`
`4
`25
`
`5
`11
`3
`39
`4
`4
`1
`2
`3
`1
`21
`50
`184
`103
`69
`
`34
`24
`3
`
`Geissler tube
`Geissler tube
`
`Geissler tube ~intensities taken from 33HUM!
`
`Absorption of carbon arc source
`Geissler tube
`
`Flash tube
`Geissler tube
`Xe discharges of varying pressures
`Strong Xe discharge at relatively high pressures
`Electrodeless discharge tubes
`Cooled Geissler tube
`Electrodeless discharge tube
`Wide band optical maser
`Maser
`Electrodeless discharge tube
`Electrodeless discharge tubes
`Absorption of synchrotron radiation
`Electrodeless discharge tube
`Electrodeless discharge tube
`Absorption of He discharge for l,1070 Å
`Absorption of Ar discharge for l.1070 Å
`Optogalvanic spectroscopy
`Electrodeless discharge tube
`Isotope-resolved laser spectroscopy from ground state
`
`5116–5523
`3340–10515
`
`3948–9923
`
`962–996
`10 550–12 623
`
`12 204 –19 467
`12 451–16 052
`5963–8559
`3738–10 324
`14 355–16 665
`23 198–26 518
`39 210
`32 752
`34 340–185 140
`1470
`38 679–40 769
`430–592
`36 518–54 447
`12 409–36 242
`926–1296
`
`6383–6753
`10 528–21 476
`1044 –1061
`
`0.03 ~estimate!
`0.01 for l<9000 Å
`0.02 for l.9000 Å
`0.0005 for 4 d.p. lines
`0.002 for 3 d.p. lines
`0.15
`0.03 for 2 d.p. lines
`0.1 for 1 d.p. lines
`0.5
`0.1
`0.2
`0.2
`Only Ritz wavelengths
`0.8
`2.
`3.
`10.
`0.003
`1.
`0.02–0.10
`1.–4.
`Only Ritz wavelengths
`0.002 for 3 d.p. lines
`0.01 for 2 d.p. lines
`0.13
`0.003–0.014
`0.000 03
`
`from the isotope-specific results of Brandi et al. @01BRA# for
`the 5p 6 – 5p 5nl energy difference by using an average of
`values for each isotope weighted according to its fraction in
`the natural isotope mix. This same method of averaging the
`isotope-specific values was used to obtain our quoted ioniza-
`tion energy from the isotope specific results of Brandi et al.
`@01BRA#.
`levels, by Moore
`The first major compilation of Xe I
`@58MOO#, was largely based on unpublished work of Edle´n.
`@58THE#,
`@67HUM#,
`@70HUM#,
`Several other
`sources
`@81GRA# use this work’s value for the ground–excited state
`separation and all are adjusted to the value based on Brandi
`et al. @01BRA#. Several other sources require no adjustment
`since they measure directly from the ground state @72COD#,
`@85YOS#, @89HUI# or, to the precision of their quoted results,
`use a reference level @98AHM# in agreement with the value
`used here. The most precise measurement of many excited
`levels was in the work of Humphreys and Paul @70HUM#.
`However, their work was for the single isotope 136Xe. In
`order to be able to use these results, their values were cor-
`rected to the natural isotope mix as specified in Tables 1 and
`2 by using isotope shift data @89PLI#, @74JAC#, @75JAC# and
`a weighted average over the isotopes. This results in a de-
`crease in precision from the four decimal places quoted in
`Humphreys and Paul @70HUM#. The uncertainty is estimated
`to be 0.0035 cm21 from the ground state and 0.001 cm21
`between excited levels.
`Note that in the level table the three energy levels in
`square brackets are predicted values furnished to Moore
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`@58MOO# by Edle´n. The energy of autoionizing levels can be
`specified in two different ways. One is to specify the reso-
`nance energy of the absorption profile. The other is to specify
`the energy at which the peak of the absorption profile occurs.
`We chose the latter in order to facilitate the use of these
`tables with observations of spectra. There is work reported
`using the former, e.g., @86WAN# and @00KOR#.
`The observed spectral lines of Xe I have been compiled
`from 23 distinct sources @30GRE#, @33HUM#, @34MEG#,
`@35BEU#,
`@35MEG#,
`@49SIT#,
`@52HUM#,
`@55THE#,
`@58THE#,
`@60HUM#,
`@61HEP#,
`@63HUM#,
`@64AGO#,
`@64FAU#,
`@64PET#,
`@67HUM#,
`@72COD#,
`@72MOR#,
`@73HUM#, @85YOS#, @98AHM#, @00MIS#, @01BRA# with
`seven additional sources @32RAS#,
`@36BOY#,
`@55PLY#,
`@56HEP#, @61HUM#, @67AND#, @74TAG# totally superseded
`by the others. The distinct sources are summarized in Table
`3. The priority in our choice of lines which appear in more
`than one reference is specified as follows by spectral region.
`~400–1500 Å!:
`@01BRA#,
`@85YOS#,
`Far ultraviolet
`@64PET#, @36BOY#, @72COD#, and finally @35BEU#.
`Near ultraviolet and visible ~3000–8000 Å!: @34MEG#,
`@33HUM#, @55THE# for lines between 5200 and 5710 Å,
`@30GRE#, @32RAS#, @58THE#, @55THE# outside range speci-
`fied above, @74TAG#, and finally @98AHM#.
`@00MIS#,
`infrared ~8000–20 000 Å!:
`@34MEG#,
`Near
`@30GRE#,
`@35MEG#,
`@33HUM#,
`@52HUM#,
`@55PLY#,
`@32RAS#, @58THE#, @55THE#, @49SIT#, @67AND#, @73HUM#,
`@61HUM#, and finally @60HUM#.
`Far infrared ~greater than 20 000 Å!: @49SIT#, @61HEP#,
`
`

`
`SPECTRAL LINES OF XENON
`
`769769
`
`@63HUM#,
`@73HUM#,
`
`@72MOR#,
`@67AND#,
`@61HUM#, and finally
`
`@56HEP#,
`@64FAU#,
`
`@67HUM#,
`@64AGO#,
`@60HUM#.
`As Table 3 indicates, two sources @60HUM#, @73HUM# do
`not provide observed wavelengths but
`instead give Ritz
`wavelengths, which are the wavelengths calculated from
`known energy levels. Since we do not know the actual wave-
`lengths observed, the Ritz wavelengths are quoted to only
`one decimal place. The corresponding vacuum wave num-
`bers are also given with only one decimal place. In addition
`for @73HUM#, the values quoted were for the isotope 136Xe.
`We recalculated these Ritz values to base them on our energy
`levels for the natural isotope xenon mix and also quoted
`these to one decimal place.
`There are some cases in which the authors’ choice of
`which transition to assign the observed line is questionable.
`For example, in @73HUM# ~using vacuum wavelengths! the
`33 536.1 Å line was classified as 5d8@5/2#2 – 9p@5/2#3 . But
`calculation using the Cowan codes @81COW# indicates that
`the 6p8@1/2#1 – 7d@1/2#0 transition should be about 20 times
`stronger. Its wavelength would be 33 543.3 Å. This may be
`the line actually observed but we report the classification of
`@73HUM# here.
`The classification of the three electric quadrupole lines is
`due to Edle´n @43EDL#. A few additional lines in the wave-
`length region 1027–1089 Å have been identified by Abbink
`@28ABB# as Xe I lines. We have been unable to classify these
`lines and so have not included them. Where possible we have
`corrected typographical errors in the references. For ex-
`ample, from the stated energy levels in @85YOS# it was clear
`that the line reported at 1030.453 Å was really at 1030.435
`Å.
`
`The wavelengths of lines between 5200 and 5710 Å given
`in the unpublished report @55THE# suggested higher preci-
`sion than those provided by @33HUM#. However, they did
`not agree as well as @33HUM# with the values predicted by
`the energy levels. Therefore the results of @33HUM# were
`given priority over @55THE# resulting in no @55THE# lines in
`this range being in the Xe I line table.
`The large uncertainties in the far infrared wavelengths of
`@72MOR# ~often 4 Å! made classification difficult and mul-
`tiple classification frequent. Lines and levels included in the
`tables were limited to n<20. A few additional lines were
`reported by @74TAG# but were not included because their
`ionization stage could not be determined. We also note that
`some far infrared stimulated emission lines reported by
`@65LIB# were also not included.
`All candidate lines were passed through a program to de-
`termine if they correspond to a transition between the known
`Xe I levels. Only classifiable lines are included in our com-
`pilation.
`Transition probability calculations using the Cowan codes
`@81COW# with empirically adjusted configuration average
`energies were used to help resolve choices between multiple
`possible classifications of lines. Convergence was not ob-
`tained for the 19s, 20s, 20d, and 20f levels and so we could
`not use the codes for guidance in transitions involving them.
`
`Intensities have been taken from the stated sources.
`The intensity codes given in the Xe I line table are taken
`from the specified sources. Their meaning is stated below:
`Symbol
`Definition
`
`a
`h
`hf
`l
`w
`E2
`f
`:
`
`¯
`*
`
`observed in absorption
`hazy
`line has hyperfine structure
`unsymmetrical-shaded to longer wavelength
`wide
`electric quadrupole line
`forbidden line
`Ritz line from levels in natural isotope mix of
`xenon. Given to only one decimal place since
`the observed wavelength was not reported.
`somewhat less intensity than the value given
`~two
`multiply
`classified
`line
`or more
`classifications of
`this line share the same
`intensity!
`
`The g J values included in the Xe I level table are compiled
`from eight sources @41GRE#, @71CHE#, @72PRI#, @79HUE#,
`@83ABU#, @83BIN#. Uncertainties
`@79HUSa#,
`@79HUSb#,
`have been included in parentheses for those g j values for
`which they were specified.
`
`References
`28ABB
`
`30GRE
`32RAS
`33HUM
`
`34MEG
`
`35BEU
`35MEG
`
`36BOY
`41GRE
`
`43EDL
`49SIT
`
`52HUM
`
`55THE
`
`55PLY
`
`56HEP
`58MOO
`
`J. H. Abbink and H. B. Dorgelo, Z. Phys. 47,
`221 ~1928!.
`W. Gremmer, Z. Phys. 59, 154 ~1930!.
`E. Rasmussen, Z. Phys. 73, 779 ~1932!.
`C. J. Humphreys and W. F. Meggers, J. Res.
`Natl. Bur. Stand. 10, 139 ~1933!.
`W. F. Meggers and C. J. Humphreys, J. Res.
`Natl. Bur. Stand. 13, 293 ~1934!.
`H. Beutler, Z. Phys. 93, 177 ~1935!.
`W. F. Meggers, J. Res. Natl. Bur. Stand. 14, 487
`~1935!.
`J. C. Boyce, Phys. Rev. 49, 730 ~1936!.
`J. B. Green, E. H. Hurlburt, and D. W.
`Bowman, Phys. Rev. 59, 72~1941!.
`B. Edle´n, Ark. Mat. Astron. Fys. 29A, 1~1943!.
`W. R. Sittner and E. R. Peck, J. Opt. Soc. Am.
`39, 474 ~1949!.
`C. J. Humphreys and H. J. Kostkowski, J. Res.
`Natl. Bur. Stand. 49, 73~1952!.
`M. Thekaekara, G. H. Dieke, and H. M.
`Crosswhite, ‘‘The Spectrum of Xenon I’’, Johns
`Hopkins
`Spectroscopic Report No.
`12,
`December, 1955 ~unpublished!.
`E. K. Plyler, L. R. Blaine, and E. D. Tidwell, J.
`Res. Natl. Bur. Stand. 55, 279 ~1955!.
`G. Hepner, C. R. Acad. Sci. 242, 1430 ~1956!.
`C. E. Moore, Atomic Energy Levels, Vol. III,
`National Bureau of Standard ~U.S.! Circ. No.
`~U.S. Government
`467
`Printing Office,
`Washington, D.C., 1958!.
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`

`
`770770
`
`58THE
`
`60HUM
`
`61HEP
`61HUM
`
`63HUM
`
`64AGO
`
`64FAU
`
`64PET
`65LIB
`67AND
`
`67HUM
`
`70HUM
`
`71CHE
`
`72COD
`
`72MOR
`
`72PRI
`
`73HUM
`
`E. B. SALOMAN
`
`M. Thekaekara and G. H. Dieke, Phys. Rev.
`109, 2029 ~1958!.
`C. J. Humphreys and E. Paul, Jr., ‘‘Infrared
`Atomic Spectra’’ in Naval Ordnance Laboratory
`Corona Quarterly
`Report:
`Foundational
`Research
`Projects,
`Jan.–March
`1960,
`NAVWEPS Report 5996, NOLC Report 503
`~unpublished!, pp. 23–40.
`G. Hepner, Ann. Phys. ~Paris! 6, 735 ~1961!.
`C. J. Humphreys, E. Paul, Jr., and K. B. Adams,
`‘‘Infrared Atomic Spectra’’ in Naval Ordnance
`Laboratory
`Corona
`Quarterly
`Report:
`Foundational Research Projects,
`July–Sept.
`1961, NAVWEPS Report 7205 ~unpublished!,
`pp. 25–52.
`C. J. Humphreys and E. Paul, Jr., ‘‘Infrared
`Atomic Spectra: The First Spectrum of Xenon
`in the 4-Micron Region and its Interpretation’’
`in Naval Ordnance Laboratory Corona
`Quarterly Report:
`Foundational Research
`Projects, Jan.–March 1963, NAVWEPS Report
`8150 ~unpublished!, pp. 33–39.
`R. der Agobian, J. L. Otto, R. Cagnard, and R.
`Echard, J. Phys. ~Paris! 25, 887 ~1964!.
`W. L. Faust, R. A. McFarlane, C. K. N. Patel,
`and C. G. B. Garrett, Phys. Rev. 133, A1476
`~1964!.
`B. Petersson, Ark. Fys. 27, 317 ~1964!.
`S. Liberman, C. R. Acad. Sci. 261, 2601 ~1965!.
`O. Andrade, M. Gallardo, and K. Bockasten,
`Appl. Phys. Lett. 11, 99~1967!.
`C. J. Humphreys, E. Paul, Jr., R. D. Cowan, and
`K. L. Andrew, J. Opt. Soc. Am. 57, 855 ~1967!.
`C. J. Humphreys and E. Paul, Jr., J. Opt. Soc.
`Am. 60, 1302 ~1970!.
`M. Chenevier and T. D. Nguyen, Phys. Lett.
`36A, 177 ~1971!.
`K. Codling and R. P. Madden, J. Res. Natl. Bur.
`Stand. Sect. A 76, 1~1972!.
`C. Morillon, Spectrochim. Acta, Part B 27, 527
`~1972!.
`M. H. Prior and C. E. Johnson, Phys. Rev. A 5,
`550 ~1972!.
`C. J. Humphreys, J. Phys. Chem. Ref. Data 2,
`519 ~1973!.
`
`74JAC
`
`74TAG
`
`75JAC
`
`79HUE
`
`79HUSa
`
`79HUSb
`
`81COW
`
`81GRA
`
`82LAB
`
`83ABU
`
`83BIN
`
`85YOS
`
`86WAN
`
`89HUI
`
`89PLI
`
`98AHM
`
`00KOR
`
`00MIS
`
`01BRA
`
`D. A. Jackson and M.-C. Coulombe, Proc. R.
`Soc. London, Sect. A 338, 277 ~1974!.
`A. A. Tagliaferri, E. Gallego Lluesma, M.
`Garavaglia, M. Gallardo, and C. A. Massone,
`Opt. Pura Apl. 7, 89~1974!.
`D. A. Jackson and M.-C. Coulombe, Proc. R.
`Soc. London, Sect. A 343, 453 ~1975!.
`M. Huet, H. Kucal, M. C. Bigeon, and X.
`Husson, J. Phys. ~Paris! 40, 541 ~1979!.
`X. Husson and J. P. Grandin, J. Phys. B 12 3649
`~1979!.
`X. Husson, J. P. Grandin, and H. Kucal, J. Phys.
`~Paris! 40, 551 ~1979!.
`R. D. Cowan, The Theory of Atomic Structure
`and Spectra ~University of California Press,
`Berkeley, 1981!.
`J.-P. Grandin and X. Husson, J. Phys. B 14, 433
`~1981!.
`P. Labastie, F. Biraben, and E. Giacobino, J.
`Phys. B 15, 2595 ~1982!.
`H. Abu-Safia and J. Margerie, J. Phys. B 16,
`927 ~1983!.
`G. Binet, X. Husson, and J. P. Grandin, J. Phys.
`Lett. ~Paris! 44, L151 ~1983!.
`K. Yoshino and D. E. Freeman, J. Opt. Soc. Am.
`B 2, 1268 ~1985!.
`L.-G. Wang and R. D. Knight, Phys. Rev. A 34,
`3902 ~1986!.
`A. L’Huillier, L. A. Lompre´, D. Normand, J.
`Morellec, M. Ferray, J. Lavancier, G. Mainfray,
`and C. Manus, J. Opt. Soc. Am. B 6, 1644
`~1989!.
`M. D. Plimmer, P. E. G. Baird, C. J. Foot, D. N.
`Stacey, J. B. Swan, and G. K. Woodgate, J.
`Phys. B 22, L241 ~1989!.
`M. Ahmed, M. A. Baig, and B. Suleman, J.
`Phys. B 31, 4017 ~1998!.
`A. Kortyna, M. R. Darrach, P.-T. Howe, and A.
`Chutjian, J. Opt. Soc. Am B 17, 1934 ~2000!.
`A. P. Mishra, R. J. Kshirsagar, V. P. Bellary, and
`T. K. Balasubramanian, J. Quant. Spectrosc.
`Radiat. Transfer 67, 1~2000!.
`F. Brandi, I. Velchev, W. Hogervorst, and W.
`Ubachs, Phys. Rev. A 64, 032505 ~2001!.
`
`Energy levels of Xe I
`
`Energy level
`~cm21!
`
`0.000
`
`67 067.547
`68 045.156
`76 196.767
`77 185.041
`
`77 269.145
`
`Parity
`
`Configuration
`
`0
`
`1
`1
`1
`1
`
`0
`
`5p 6
`
`+ )6s
`5p 5( 2P3/2
`+ )6s
`5p 5( 2P3/2
`+ )6s
`5p 5( 2P1/2
`+ )6s
`5p 5( 2P1/2
`+ )6p
`5p 5( 2P3/2
`
`Term
`
`1S
`
`2@3/2# +
`2@3/2# +
`2@1/2# +
`2@1/2# +
`
`2@1/2#
`
`J
`
`0
`
`2
`1
`0
`1
`
`1
`
`g J
`
`1.50095~11!
`1.2055~2!
`
`1.321
`
`1.852
`
`Source
`of level
`
`01BRA
`
`70HUM
`70HUM
`01BRA
`70HUM
`
`70HUM
`
`J. Phys. Chem. Ref. Data, Vol. 33, No. 3, 2004
`
`

`
`SPECTRAL LINES OF XENON
`
`771771
`
`Energy levels of Xe I–Continued
`
`Energy level
`~cm21!
`
`Parity
`
`Configuration
`
`78 119.798
`78 403.061
`78 956.031
`79 212.465
`80 118.962
`88 379.126
`89 162.356
`89 278.706
`89 860.015
`
`79 771.267
`79 986.618
`80 196.629
`80 970.438
`80 322.746
`83 889.971
`81 925.514
`82 430.204
`91 152.670
`91 746.564
`91 447.474
`93 618.24
`
`85 188.777
`85 440.017
`95 720.95
`95 800.584
`
`87 927.131
`88 351.681
`88 469.213
`88 744.559
`88 686.500
`88 842.256
`98 855.0
`99 052.8
`99 068.4
`
`88 491.020
`88 549.775
`88 708.466
`90 032.155
`88 911.692
`89 024.890
`89 243.258
`89 534.568
`100 418.
`
`90 804.538
`90 932.432
`101 426.
`
`90 839.777
`90 849.440
`90 860.655
`90 861.506
`90 907.090
`90 910.052
`90 944.050
`90 944.133
`101 424.8
`101 424.8
`101 424.8
`101 429.3
`
`0
`0
`0
`0
`0
`0
`0
`0
`0
`
`1
`1
`1
`1
`1
`1
`1
`1
`1
`1
`1
`1
`
`1
`1
`1
`1
`
`0
`0
`0
`0
`0
`0
`0
`0
`0
`
`1
`1
`1
`1
`1
`1
`1
`1
`1
`
`1
`1
`1
`
`0
`0
`0
`0
`0
`0
`0
`0
`0
`0
`0
`0
`
`+ )6p
`5p 5( 2P3/2
`+ )6p
`5p 5( 2P3/2
`+ )6p
`5p 5( 2P3/2
`+ )6p
`5p 5( 2P3/2
`+ )6p
`5p 5( 2P3/2
`+ )6p
`5p 5( 2P1/2
`+ )6p
`5p 5( 2P1/2
`+ )6p
`5p 5( 2P1/2
`+ )6p
`5p 5( 2P1/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P3/2
`+ )5d
`5p 5( 2P1/2
`+ )5d
`5p 5( 2P1/2
`+ )5d
`5p 5( 2P1/2
`+ )5d
`5p 5( 2P1/2
`+ )7s
`5p 5( 2P3/2
`+ )7s
`5p 5( 2P3/2
`+ )7s
`5p 5( 2P1/2
`+ )7s
`5p 5( 2P1/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P3/2
`+ )7p
`5p 5( 2P1/2
`+ )7p
`5p 5( 2P1/2
`+ )7p
`5p 5( 2P1/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P3/2
`+ )6d
`5p 5( 2P1/2
`+ )8s
`5p 5( 2P3/2
`+ )8s
`5p 5( 2P3/2
`+ )8s
`5p 5( 2P1/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P3/2
`+ )4 f
`5p 5( 2P1/2
`+ )4 f
`5p 5( 2P1/2
`+ )4 f
`5p 5( 2P1/2
`+ )4 f
`5p 5( 2P1/2
`
`Term
`
`2@5/2#
`2@5/2#
`2@3/2#
`2@3/2#
`2@1/2#
`2@3/2#
`2@3/2#
`2@1/2#
`2@1/2#
`
`2@1/2# +
`2@1/2# +
`2@7/2# +
`2@7/2# +
`2@3/2# +
`2@3/2# +
`2@5/2# +
`2@5/2# +
`2@5/2# +
`2@5/2# +
`2@3/2# +
`2@3/2# +
`
`2@3