J/ApJS/216/2 MnI hyperfine lines in the 1.4-1.8um (H) band (Andersson+, 2015)
Hyperfine-dependent gf-values of Mn I lines in the 1.49-1.80µm H band.
Andersson M., Grumer J., Ryde N., Blackwell-Whitehead R., Hutton R.,
Zou Y., Jonsson P., Brage T.
<Astrophys. J. Suppl. Ser., 216, 2 (2015)>
=2015ApJS..216....2A 2015ApJS..216....2A
ADC_Keywords: Atomic physics ; Line Profiles ; Spectra, infrared
Keywords: atomic data; infrared: stars; line: identification;
methods: laboratory: atomic; methods: numerical; stars: abundances
Abstract:
The three Mn I lines at 17325, 17339, and 17349Å are among the 25
strongest lines (log(gf)>0.5) in the H band. They are all heavily
broadened due to hyperfine structure, and the profiles of these lines
have so far not been understood. Earlier studies of these lines even
suggested that they were blended. In this work, the profiles of these
three infrared (IR) lines have been studied theoretically and compared
to experimental spectra to assist in the complete understanding of the
solar spectrum in the IR. It is shown that the structure of these
lines cannot be described in the conventional way using the diagonal A
and B hyperfine interaction constants. The off-diagonal hyperfine
interaction not only has a large impact on the energies of the
hyperfine levels, but also introduces a large intensity redistribution
among the hyperfine lines, changing the line profiles dramatically. By
performing large-scale calculations of the diagonal and off-diagonal
hyperfine interaction and the gf-values between the upper and lower
hyperfine levels and using a semi-empirical fitting procedure, we
achieved agreement between our synthetic and experimental spectra.
Furthermore, we compare our results with observations of stellar
spectra. The spectra of the Sun and the K1.5 III red giant star
Arcturus were modeled in the relevant region, 1.73-1.74µm, using
our theoretically predicted gf-values and energies for each individual
hyperfine line. Satisfactory fits were obtained and clear improvements
were found using our new data compared with the old available Mn I
data.
Description:
We have combined theoretical synthetic and experimental spectra of the
3d54s(7S)4d e6D - 3d54s(7S)4f w6F 17325, 17339, 17349,
17357, and 17362Å lines in MnI to derive information about the
individual hyperfine lines that make up these five spectral features.
The emission spectrum of manganese, Figures 2-4, was recorded at the
NIST with the NIST 2m Fourier transform spectrometer using resolutions
of 0.008 to 0.03/cm.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 45 292 List of hyperfine lines in MnI
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See also:
VI/34 : A Multiplet Table for MnI (Adelman+, 1989)
J/ApJS/205/14 : Energy levels and spectral lines of MnII (Kramida+, 2013)
J/A+A/447/685 : Elemental abundance analyses. XXIX. (Adelman+, 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Trans Line transition
18- 22 I5 0.1nm lambda [17325/17362] Line wavelength λ (Å)
24 I1 --- F1 [0/8] Upper F (hyperfine) quantum number (1)
26 I1 --- F0 [0/7] Lower F (hyperfine) quantum number (1)
28- 36 F9.4 cm-1 E [5757.8/5770.6] Energy level
38- 45 E8.3 [-] log(gf) [0/11.1] Log oscillator strength time degeneracy
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Note (1): the nuclear spin is I=5/2
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 11-Feb-2015