VI/34 A Multiplet Table for MnI (Adelman+, 1989)
A Multiplet Table for MnI Adelman S.J., Svatek G.F., Van Winkler K., Warren Jr. W.H. <Astron. Astrophys. Suppl. Ser. 80, 285 (1989)> =1989A&AS...80..285A
ADC_Keywords: Multiplet; Spectroscopy; Atomic physics; Finding lists Abstract: The machine-readable version of "A Multiplet Table for MnI" contains data on excitation potentials, J values, multiplet terms, intensities of the transitions, and multiplet numbers. Files ordered by multiplet and by wavelength are included. Introduction: A Multiplet Table for Mn I was prepared by first calculating all possible transitions consistent with a change in J of 0, -1, and +1 from the atomic energy levels of Mn I (Corliss and Sugar 1977). The transitions selected for inclusion were observed lines from Cataln, Meggers, and Garcia-Riquelme (1964), Brown and Ginter (1978), and Baig, Connerade, and Newson (1979). Also included were predicted lines to complete multiplets in which one or more lines were seen by Cataln et al. (1964) and predicted multiplets contained in Kurucz and Peytremann (1975). These predicted transitions satisfy L-S coupling rules. Users should consult the source publication and the references to the original work that are cited in the bibliography at the end of this document for additional details. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file mult.dat 80 8724 Multiplet Order wavelen.dat 80 8724 Wavelength Order
Summary Description of Catalog Files: The record format of the multiplet table is identical in both files 1 and 2 except for the sorting order. The form is similar to that of A Multiplet Table of Astrophysical Interest and An Ultraviolet Multiplet Table. The older multiplet numbers were retained whenever possible. New multiplet numbers begin with 61, while multiplet 12 contains lines from old multiplets 9, 10, and 13; UV 25 from old multiplet UV 26; UV 24 from old multiplet UV 28; and UV 37 from old multiplet UV 38. For unclassified lines, the only information given is contained in the first 19 bytes of each record (bytes 20 through 80 are blank). Therefore, it is safest to buffer in records in an unformatted mode or read them with character (A) formats and test for blank data fields before processing with numerical formats for calculations and/or search purposes. Byte-by-byte Description of file: *.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [Mn] Element (Mn) 3- 4 I2 --- ---  Atomic species number (neutral atom) 7- 15 F9.3 0.1nm lambda *Wavelength 19 A1 --- Ref *Reference code 20 A1 --- --- [(] 21- 28 F8.2 --- Int *?Laboratory intensity 29- 33 A5 --- n_Int *Notes on the intensity 37- 40 F4.2 eV Elow *?Lower excitation potential 43- 47 F5.2 eV Ehigh *?Higher excitation potential 48- 50 F3.1 --- Jlow *?Lower J value 51- 53 F3.1 --- Jhigh *?Higher J value 55- 58 A4 --- Tlow *Lower term designation 59- 64 A6 --- Thigh *Higher term designation 66 A1 --- Rem *Remark on the line 67- 68 A2 --- UV *[UV] for UV lines 69- 75 F7.3 --- mult *?Multiplet number 76 A1 --- fl *[F] Forbidden transition code 77- 80 I4 --- Seq *Sequential number
Note on lambda: Wavelength of the transition. They are in air except shortward of 0.2 mu, where they are in vacuum. Note that the precision varies (the last two bytes can be blank). Note on Ref: The reference codes are as follows: A = Catalaen et al. (1964, J. Res. Nat. Bur. Stand. 68A, 9) B = Based on gf values of Kurucz and Peytremann (1975) using values of Catalaen et al. (1964) as a guide for lines of similar excitation potential C = Brown and Ginter (1978i, J. Opt. Soc. Am. 68, 1541), but divided by 10 D = Baig et al. (1979, Proc. R. Soc. London, Ser. A, 367, 381) P = Predicted line Users are advised to check the quality of each analysis from which the tables were assembled if uncertainties in identifications are encountered. Note on Int, n_Int: This data field is divided into several uniform parts, the wide spacing being required to isolate the various segments of the field. Thus, it is possible to read the numerical intensities by using the format specification (F6.1,A5) because character data are, in all cases, separate from the numerical intensities. Note, however, that a numerical intensity may be zero or blank. Also note that decimal points have been added to integer intensities so that the numerical field is always either a real number of blank. Parentheses in bytes 20 (left) and 32 (right) are used to indicate intensity scale changes and an asterisk (*) in byte 33 denotes that an intensity is affected by that of a neighboring, or impurity, line. Although numerical intensities may be read and tested upon or sorted, the overall data field must be considered for correct interpretation. Note on Elow, Ehigh: All limits and energy levels given in inverse centimeters have been multiplied by the factor 0.000123981 to obtain the respective values in electron volts (see Moore 1965). Note on Jlow: Value corresponding to the low level involved in the transition producing the line. Note on Jhigh: Value for high level. There is no specific secondary order of J values in the wavelength-ordered file when multiplet lines at an identical wavelength occur; i.e., no secondary sorts were attempted beyond that on wavelength, since there is no rational way to order the lines beyond wavelength. Note on Tlow, Thigh: Term designations from the source material, without the J values attached to them. The complete upper state designations from Brown and Ginter (1978) and Baig et al. (1979) are not given for lack of space, and some multiplets represent lines with unclassified upper states grouped together for convenience. These include many multiplets between UV 2.88 and UV 2.343. Note on Rem: The following codes are employed: A = Indicates a change from Catalaen et al. (1964), e.g., by the inclusion of additional lines of the same wavelength and differing J values, and where the upper limit term has been changed. B = Major component. Note on UV: The letters UV when a multiplet occurs shortward of 0.3 microns (stated in Moore 1965). However, multiplets having wavelength < 0.3 microns occur without the prefix and a few multiplets just longward of 0.3 microns contain the prefix. Note on mult: Older multiplet numbers, as used in RMT and UMT, are used wherever possible. New multiplet numbers begin with 61. Note that the dual numbering system described by Moore (1965) (see p. vii) is used in principle, but that decimal points have been added to the integers so that all numbers are uniform in format. Note on fl: The letter F indicates a forbidden transition. Note on Seq: The multiplet-ordered table was assigned a sequential numbering to provide an independent means of ordering the table. This was done because if the multiplet table is disordered, it is virtually impossible (at least we couldn't find a way) to reorder it by machine sorting. The sequential numbers are, of course, retained in the wavelength-ordered table to indicate where the lines are located in the multiplet table.
History: The data were compiled and computerized by S. J. Adelman, G. F. Svatek, and K. Van Winkler with financial support from The Citadel Development Foundation. A complex coding system was used in the original file to indicate upper and lower case letters in the intensity field, blended lines (* in intensity field), changes from Catalaen et al. (1964) in combination with other codes, and other combinations of individual codes. The format and coding system were extensively revised by W. H. Warren Jr. at the Astronomical Data Center in order to prepare a uniform file fully processable by machine, to replace all upper case characters by lower case where appropriate, to insert parentheses and asterisks, and to duplicate the format used in an earlier finding list for the NSRDS-NBS3 multiplet tables prepared by Adelman et al. (1985) to the extent possible. The complete table was sorted various ways to detect errors and was proofread in sections by S. J. Adelman. The final multiplet-ordered table was sorted by computer to produce the wavelength-ordered table. The original Script file was translated to ASCII and put into the current standard from by the undersigned. Acknowledgments: The partial support of The Citadel Development Foundation toward the computerization of the tabular data is gratefully acknowledged. References: Adelman, C. J., Adelman, S. J., Fischel, D., and Warren, W. H. Jr. 1985, A&A Suppl. 60, 339 (1985A&AS...60..339A) Baig, M. A., Connerade, J. P., and Newson, G. H. 1979, Proc. R. Soc. London, Ser. A, 367, 381. Brown, C. M. and Ginter, M. L. 1978, J. Opt. Soc. Am. 68, 1541. Catalaen, M. A., Meggers, W. F., and Garcia-Riquelme, O. 1964, J. Res. Nat. Bur. Stand. 68A, 9. Corliss, C. and Sugar, J. 1977, J. Phys. Chem. Ref. Data 6, 1253. Kurucz, R. L. and Peytremann, E. 1975, Smithson. Astrophys. Obs. Spec. Rep. No. 362. Moore, C. E. 1945, A Multiplet Table of Astrophsyical Interest, Contr. Princeton Univ. Obs. No. 20 (reprinted 1959, Nat. Bur. Stand. Technical Note 36). Moore, C. E. 1950, An Ultraviolet Multiplet Table, Nat. Bur. Stand. Circ. No. 488, Sect. 1-5 (Washington: U. S. Government Printing Office). Moore, C. E. 1965, Nat. Bur. Stand. Ref. Data System (NSRDS), Nat. Bur. Stand. (NBS) 3, Sect. 1.
(End) Nancy G. Roman [ADC/SSDOO] May-15-1995
|The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line|