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VI/34 A Multiplet Table for MnI (Adelman+, 1989)
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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
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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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
mult.dat 80 8427 Multiplet Order
wavelen.dat 80 8427 Wavelength Order
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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
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Bytes Format Units Label Explanations
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1- 2 A2 --- Mn Element (Mn)
3- 4 I2 --- spec Atomic species number ( 1)
7- 15 F9.3 0.1nm lam *Wavelength
19 A1 --- ref *Reference code
20- 33 A14 --- int *Laboratory intensity
37- 40 F4.2 eV low_ex *?Lower excitation potential
43- 47 F5.2 eV high_ex *?Higher excitation potential
48- 50 F3.1 --- low_J *?Lower J value
51- 53 F3.1 --- high_J *?Higher J value
55- 58 A4 --- low_term *Lower term designation
59- 64 A6 --- high_term *Higher term designation
66 A1 --- code *Code
67- 68 A2 --- code_UV *Code for UV
69- 75 F7.3 --- mult *?Multiplet number
76 A1 --- for_code *Forbidden transition code
77- 80 I4 --- no *Sequential number
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Note on lam:
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)
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 (1978), but divided by 10
D = Baig et al. (1979)
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:
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 (A3,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 low_ex and high_ex:
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 low_J:
Value corresponding to the low level involved in the transition
producing the line.
Note on high_J:
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 low_term and high_term:
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 code:
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 code_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 for_code:
The letter F indicates a forbidden transition.
Note on no:
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.
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.
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(End) Nancy G. Roman [ADC/SSDOO] May-15-1995