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VI/29A Finding list for multiplet tables of NSRDS-NBS 3 (Adelman+ 1985)
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A finding list for the multiplet tables of NSRDS-NBS 3, Section 1-10
Adelman C.J., Adelman S.J., Fischel D., Warren Jr. W.H.
<Astron. Astrophys. Suppl. Ser. 60, 339 (1985)>
=1985A&AS...60..339A
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ADC_Keywords: Atomic physics ; Multiplet ; Spectroscopy
Description:
The primary references for stellar line identifications in the optical
and ultraviolet spectral regions have been "A Multiplet Table of
Astrophysical Interest" (RMT, Moore 1945) and "An Ultraviolet Multiplet
Table" (UMT, Moore 1950, 1952, 1962). Dr. Charlotte Moore Sitterly has,
over the last two decades, undertaken a revision of certain multiplet
tables based on data derived from analyses of optical spectra. The
present finding list has been prepared from the data published in the
first ten sections of these revised tables:
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Section Year Elements
--------------------------------------------------
1 1965 Si II, Si III, Si IV
2 1967 Si I
3 1970 C I, C II, C III, C IV, C V, C VI
4 1970 N IV, N V, N VI, N VII
5 1975 N I, N II, N III
6 1972 H I, D I, T I
7 1976 O I
8 1979 O VI, O VII, O VIII
9 1980 O V
10 1983 O IV
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An earlier finding list containing Sections 1-7 only was published by
Adelman, Adelman and Fischel (1977) (Catalogue VI/11). We have
revised the format and added information to the earlier list, and have
appended Sections 8-10 to produce the present version. We intend to
incorporate future sections to produce new comprehensive lists as
the sections are published and can be computerized.
This document describes the machine version of the finding list as it
is currently being distributed from the Astronomical Data Center. It
is intended to enable users to read and process the data without
problems and guesswork, and to interpret the various codes used in the
list without recourse to the original publications. However, for
additional details concerning the multiplet tables and analyses of the
optical spectra, the source publications and their associated
references should be consulted.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog 70 9969 The finding list for multiplet tables
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Byte-by-byte Description of file: catalog
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element (D=Deuterium, T=Tritium).
3- 4 I2 --- Ion Ionisation stage (1=neutral)
5 A1 --- Left [[] a left bracket ([) for predicted
wavelength (1)
6- 16 F11.4 0.1nm lambda [14/4.e5]+= Wavelength of the transition
(in vacuum for lambda<2000A,
in air for lambda>2000A)
17 A1 --- Right []] a right bracket (]) (1)
18 A1 --- n_lambda [aDIm*?] See Note (2)
19 A1 --- Ref [A-KP] Reference for the original analysis (3)
20- 33 A14 --- Int Line intensity (4)
34- 40 F7.2 eV E1 ? Lower excitation potential (5)
41- 47 F7.2 eV E2 ? Higher excitation potential (5)
48- 50 F3.1 --- J1 ? Lower J quantum number
51- 53 F3.1 --- J2 ? H1gher J quantum number
54 A1 --- u_J2 [?] A query (?) if the J values are uncertain
(appears in source multiplet tables).
55- 56 A2 --- UV "UV" if an ultraviolet multiplet (6)
57- 62 F6.2 --- Mult ? Multiplet number (7)
63 A1 --- Fflag [F] denotes a forbidden transition.
64 A1 --- Blend [ACDEG-SUWXYZ12] See Note (8)
65- 66 I2 --- Sec Section number of HSRDS-NBS 3 publication
67- 70 I4 --- Seq Sequential number of the line in the
respective multiplet table. The original
tables can be reconstructed by sorting
the complete list by Sec,Seq
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Note (1): a wavelength is enclosed in brackets
(indicating that a theoretical value of either or both energy levels
of the transition has been used to derive the predicted wavelength;
[Moore 1967] in the multiplet table).
Note (2):
'a' Observed members of series shifted to longer waves by 0.309 A
to 0.052 A (n - 5 to 8) when autoionization is effective.
'D' Line deleted in a later publication.
'I' Denotes intersystem combinations of astrophysical interest (see
Moore 1965, p. VII for further remarks).
'm' Indicates that the line is masked. The spectrum of the masked line
then appears in the intensity column with element identified in
bytes 21-22 and atomic species number in byte 26.
'*' The line is blended throughout and has more than one classification
in the same spectrum (as opposed to appearance in intensity field,
byte 23; see explanation for bytes 20-33).
'?' for uncertain wavelength
Note (3): The references (letters A to K) are too extensive to be listed
in this document and the source publications will need to be consulted
if they are required. Users are advised to check the quality of each
analysis from which the tables are assembled if uncertainties in
identifications are encountered. The same letter codes denote
different references in different sections, so the correct section
must be consulted.
The code "P" indicates a predicted wavelength.
Note (4): various parts of this data field are uniform, e.g., it is
possible to read the numerical intensities if the field is read with
format (A3,F6.1,A5) since character data are in all cases separate
from numerical intensities. Note, however, that a numerical intensity
may be zero or blank, atomic species number may occur in a numerical
field if an element is specified in bytes 21-22, and parentheses and
asterisks are used to indicate intensity scale changes and that the
intensity is affected by that of a neighbouring line or an impurity
line. Thus, although numerical intensities may be read and tested
upon, the overall data field must be considered for correct
interpretation.
Note (5): All limits and energy levels given in cm-1 have been multiplied
by the factor 0.000123981 to obtain the respective values in eV
(see Moore 1965).
Note (6): The letters "UV" when a multiplet occurs shortward of 3000 A
and blank for multiplets longward of 3000 A (stated in Moore 1965);
however, multiplets having lambda < 3000 A occur throughout the
sections without the UV prefix.
Note (7): Due to the retention of earlier numbers from the RMT and UMT,
a dual numbering system consisting of real and integer numbers is used
(see Moore 1965, p. VII for a more detailed explanation); however, the
integer numbers are aligned so that the F format can be used to read
them as real numbers. Newly inserted numbers appear in decimal form,
while integer numbers only are used after the old multiplet numbers
are exhausted.
Note (8): A code to indicate blends of specific lines, ultimate lines,
italicized numerical intensities, as follows:
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A Blended with Ar I
C Expanded from single line in multiplet table (multiple J values)
D Blend of Si III and Si IV
E Blend of N III and N IV
G Blend of C I and C II
H Blend of C II and C III
I Blend of C III and C IV
J Blend of C IV and C V
K Blend of N IV and N V
L Blend of O IV and Si III
M Blend of O IV and O V
N Blend of O III and O V
O Blend of O II and O V
P Blend of O VI and O VII
Q Blend of O VI and Be III
R Blend of O III and O IV
S Blend of O II and O IV
U Ultimate line (raie ultime)
W Blend of N III and N VI
X Blend with N II
Y Blend with O III
Z Blend with Al II
1 Intensity given in italics (significance not found defined
in publications)
2 1 + C
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References:
Adelman, C.J., Adelman, S.J. and Fischel, D. 1977, NASA X-685-77-287.
(Catalogue: <VI/11>)
Moore, C.E. 1945, "A Multiptet Table of Astrophysical Interest",
Princeton Obs. Contr. No. 20 (reprinted 1959, Nat. Bur. Stand.
Technical Note 36).
Moore, C.E. 1950, 1952, 1962, "An Ultraviotet Multiptet Table",
Nat. Bur. Stand. Circular 488, Sec. 1-5.
Moore, C.E. 1965, 1967, 1970a, 1970b, 1972, 1975, 1976, 1979, 1980, 1983,
Nat. Bur. Stand. Ref. Data System (NSRDS), Nat. Bur. Stand. (NBS)
Vol. 3, Sec. 1-10.
Historical Notes:
* December 1984, at ADC/NSSDC, by Wayne H. Warren Jr.:
Sections 1-7 of the finding list (Adelman, Adelman and Fischel 1977)
were available on magnetic tape. The multiplet tables of sections 8-10
were transcribed to data sheets at The Citadel by CJA and SJA, and
transferred to disk storage at the ADC by WHW. A format was then
designed to accommodate the data of all sections and the differing
formats of both groups were changed to the new format. The individual
sections were then broken out of the groups for checking. Corrections
were made and detailed checks of the original publications performed,
the format being revised several times to allow for additional
information and to effect homogeneity in the data presentation. Groups
of lines which had been added in Sections 1-7 without resequencing
were moved to their correct locations and all sections were
resequenced to be certain that a sequence sort will recover the
original tables exactly. The individual sections were then combined
and the complete file sorted by wavelength with secondary sorting on
sequence number.
* 30-Aug-1995: the printed documentation was converted into an electronic
file at CDS. Problems which already occured in Catalogue VI/11
(Sections 1-7) have been corrected in records 4228, 5148, 6957, 7467,
and 9951.
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(End) Francois Ochsenbein [CDS] 30-Aug-1995