J/MNRAS/441/3127 FeI oscillator strengths for Gaia-ESO (Ruffoni+, 2014)
Fe I oscillator strengths for the Gaia-ESO survey.
Ruffoni M.P., Den Hartog E.A., Lawler J.E., Brewer N.R., Lind K., Nave G.,
Pickering J.C.
<Mon. Not. R. Astron. Soc., 441, 3127-3136 (2014)>
=2014MNRAS.441.3127R 2014MNRAS.441.3127R
ADC_Keywords: Atomic physics ; Line Profiles ; Spectroscopy
Keywords: atomic data - line: profiles - methods: laboratory -
techniques: spectroscopic
Abstract:
The Gaia-ESO Public Spectroscopic Survey (GES) is conducting a
large-scale study of multi-element chemical abundances of some 100000
stars in the Milky Way with the ultimate aim of quantifying the
formation history and evolution of young, mature and ancient Galactic
populations. However, in preparing for the analysis of GES spectra, it
has been noted that atomic oscillator strengths of important FeI
lines required to correctly model stellar line intensities are missing
from the atomic data base. Here, we present new experimental
oscillator strengths derived from branching fractions and level
lifetimes, for 142 transitions of FeI between 3526 and 10864Å,
of which at least 38 are urgently needed by GES. We also assess the
impact of these new data on solar spectral synthesis and demonstrate
that for 36 lines that appear unblended in the Sun, Fe abundance
measurements yield a small line-by-line scatter (0.08dex) with a mean
abundance of 7.44dex in good agreement with recent publications.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 102 167 Experimental branching fractions, transition
probabilities, and log(gf)s for the FeI levels
listed in table 2 of the paper
table4.dat 116 32 Lines measured in previous studies, or predicted
to have a BF greater than 1%, that were omitted
from the BF measurements shown in table 3
table5.dat 62 36 Lines from table 3 selected for solar analysis
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Byte-by-byte Description of file (# headlines): table3.dat
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Bytes Format Units Label Explanations
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1 A1 --- State [A-L] State (G1)
3- 10 A8 --- Level Lower Level
12 A1 --- Note [*] Wavenumber from our spectra (G2)
14- 23 F10.4 0.1nm lam.Air [2722/13261] Transition air wavelength (Å)
25- 33 F9.3 cm-1 sigma [7539/36727] Transition wavenumber σ
35- 40 F6.4 --- BF [0/1]? Branching fraction (1)
42- 45 F4.1 % e_BF ? Precentage uncertainty in branching fraction
47- 52 F6.3 10-6s-1 Aul ? Transition probability
54- 58 F5.2 [-] loggf ? Oscillator strength measured in this work
60- 63 F4.2 [-] e_loggf ? Uncertainty in oscillator strength
65- 69 F5.2 [-] loggf0 ? Best previously published oscillator strength
71- 74 F4.2 [-] e_loggf0 ? Uncertainty in loggf0 (G3)
75- 76 A2 --- q_loggf0 [DE+ ] Uncertainty flag on loggf0 (G3)
78- 80 A3 --- r_loggf0 Reference to source of loggf0 (G4)
82- 84 A3 --- GES 'Yes' if the line is a GES target
(Gaia-ESO public Spectroscopic survey)
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Note (1): blank if no data is available for a given line or contain a floating
point value of the format given in the Explanations column. Process these
columns as character strings first when reading them in code, then convert
to a numeric value only if one is present.
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Byte-by-byte Description of file(#): table4.dat
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Bytes Format Units Label Explanations
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1 A1 --- State [A-L] State (G1)
3- 10 A8 --- Level Lower Level
12 A1 --- Note [*] Wavenumber from our spectra (G2)
14- 23 F10.4 0.1nm lam.Air [2722/13261] Transition air wavelength (Å)
25- 33 F9.3 cm-1 sigma [7539/36727] Transition wavenumber σ
35- 39 F5.2 [-] loggf0 Best previously published oscillator strength
41- 44 F4.2 [-] e_loggf0 ? Uncertainty in loggf0 (G3)
45 A1 --- q_loggf0 [DE] Uncertainty flag on loggf0 (G3)
47- 49 A3 --- r_loggf0 Reference to source of loggf0 (G4)
51 A1 --- l_BFp [<] Contains '<' if BFp is less than 0.001
52- 57 F6.4 --- BFp [0/1] Predicted branching fraction
59- 73 A15 --- Reason Reason for omission of the line
75-116 A42 --- Blend List of blended lines when Reason='Blended' (1)
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Note (1): The line at 31704.637cm-1 was observed to be significantly
stronger than expected. Its inclusion in the BF measurements resulted in
serious disagreement with published values for all lines belonging to the
51461.667cm-1 upper level.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 F10.4 0.1nm lam.Air [4423/10864] Transition air wavelength (Å)
12- 16 F5.3 eV chi Lower level transition energy χ
18- 25 F8.3 --- VdW Van der Waals damping parameter (1)
27- 31 F5.2 [-] loggf Oscillator strength measured in this work
33- 36 F4.2 [-] e_loggf Uncertainty in oscillator strength
38- 42 F5.2 [-] loggf0 Best previously published oscillator strength
44- 47 F4.2 [-] e_loggf0 ? Uncertainty in loggf0 (G3)
48 A1 --- q_loggf0 [DE] Uncertainty flag on loggf0 (G3)
50- 52 A3 --- r_loggf0 Reference to source of loggf0 (G4)
54- 57 F4.2 [-] eps Solar iron abundance, logε(Fe),
obtained for this line using loggf
59- 62 F4.2 [-] eps0 Solar iron abundance, logε(Fe),
obtained for this line using loggf0
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Note (1): Van der Waals broadening parameter. Values greater than zero were
obtained from Anstee, Barklem & O'Mara (ABO) theory (1991MNRAS.253..549A 1991MNRAS.253..549A,
1995MNRAS.276..859A 1995MNRAS.276..859A) and are expressed in the standard packed notation where
the integer component is the broadening cross section, σ, in atomic
units, and the decimal component is the dimensionless velocity parameter,
alpha. Values less than zero are the log of the VdW broadening parameter,
gamma6 (rad/s), per unit perturber number density, N (cm-3), at
10000K (i.e. log[gamma6/N] in units of (rad/s)*cm3). These were
used only when ABO data were unavailable. See Gray D. F., 2005, "The
Observation and Analysis of Stellar Photospheres" 3rd Ed., Chapter 11 for
more details.
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Global notes:
Note (G1): State as follows:
A = Level 43163.323 cm-1 3d64s(6D)5s e7D4
8.5ns ±5%; 100% complete; Residual 0.0012
B = Level 43633.530 cm-1 3d64s(6D)5s e7D2
8.4ns ±5%; 100% complete; Residual 0.0012
C = Level 44677.003 cm-1 3d6(5D)4s(6D)5s e5D4
15.4ns ±5%; 97% complete; Residual 0.0269; Sum(BFp) 0.0126
D = Level 47377.952 cm-1 3d7(4F)5s e5F4
19.9ns ±5%; 97% complete; Residual 0.027;
E = Level 47960.937 cm-1 3d7(4F)5s e3F4
22.1ns ±5%; 98% complete; Residual 0.0205; Sum(BFp) 0.0097
F = Level 48702.532 cm-1 3d6(3H)4s4p(3Po) y1Go4
21.0ns ±5%; 96% complete; Residual 0.0406; Sum(BFp) 0.0214
G = Level 51294.217 cm-1 3d6(5D)4s(4D)5s e3D3
9.9ns ±5%; 97% complete; Residual 0.0319; Sum(BFp) 0.0045
H = Level 51461.667 cm-1 3d64s(6D)4d f5F4
12.7ns ±5%; 88% complete; Residual 0.1256; Sum(BFp) 0.1108
I = Level 51770.554 cm-1 3d6(5D)4s(4D)5s g5D3
12.1ns ±5%; 92% complete; Residual 0.0798; Sum(BFp) 0.0350
J = Level 52039.889 cm-1 3d6(5D)4s(4D)5s e3D1
10.4ns ±5%; 87% complete; Residual 0.1345; Sum(BFp) 0.1056
K = Level 52067.446 cm-1 3d6(5D)4s(6D)4d e5P2
14.3ns ±5%; 77% complete; Residual 0.2284; Sum(BFp) 0.1864
L = Level 54683.318 cm-1 3d7(4F)4d f3F4
23.5ns ±5%; 92% complete; Residual 0.0810; Sum(BFp) 0.0849
Note (G2): Note as follows:
* = if the line is absent from Nave et al. (1994ApJS...94..221N 1994ApJS...94..221N). In these
cases, the quoted transition wavenumber and wavelength were obtained from
out FT spectra by calibrating the measured wavenumber scale to match the
calibrated scale used by Nave et al. (1994ApJS...94..221N 1994ApJS...94..221N).
Note (G3): Data from May et al. (1974A&AS...18..405M 1974A&AS...18..405M) are given the
uncertainty codes 'D' and 'E' to follow the notation used by Fuhr & Wiese,
(2006JPCRD..35.1669F 2006JPCRD..35.1669F). A letter 'D' indicates that the uncertainty is
likely to be up to 50%. A letter 'E' indicates a probable uncertainty
greater than 50% but within a factor of two in most cases. All numeric
uncertainties are quoted as they appear in the source publication.
Note (G4): References as follows:
B91 = Bard et al., 1991A&A...248..315B 1991A&A...248..315B
B82 = Blackwell et al., 1982MNRAS.199...43B 1982MNRAS.199...43B
M74 = May et al., 1974A&AS...18..405M 1974A&AS...18..405M
O91 = O'Brian et al., 1991, J. Opt. Soc. Am. B, 8, 1185
K07 = Kurucz, 2007, http://kurucz.harvard.edu/atoms/2700/
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Acknowledgements:
Matthew P. Ruffoni, m.ruffoni(at)imperial.ac.uk
(End) M. Ruffoni [Imperial College London], P. Vannier [CDS] 01-Oct-2014