J/A+A/584/A86 Abundance analysis of HD 140283 (Siqueira-Mello+, 2015)
High-resolution abundance analysis of HD 140283.
Siqueira-Mello C., Andrievsky S.M., Barbuy B., Spite M., Spite F.,
Korotin S.A.
<Astron. Astrophys. 584, A86 (2015)>
=2015A&A...584A..86S 2015A&A...584A..86S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, halo ; Stars, population II ; Abundances
Keywords: stars: abundances / stars: atmospheres / stars: Population II -
stars: individual: HD 140283 - stars: abundances - Galaxy: halo
Abstract:
HD 140283 is a reference subgiant that is metal poor and confirmed to
be a very old star. The abundances of this type of old star can
constrain the nature and nucleosynthesis processes that occurred in
its (even older) progenitors. The present study may shed light on
nucleosynthesis processes yielding heavy elements early in the Galaxy.
A detailed abundance analysis of a high-quality spectrum is carried
out, with the intent of providing a reference on stellar lines and
abundances of a very old, metal-poor subgiant.
Description:
The analysis is carried out using high-resolution (R=81000) and
high signal-to-noise ratio (800<S/N/pixel<3400) spectrum, in the
wavelength range 3700-10475, obtained with a seven-hour exposure
time, using the ESPaDOnS at the CFHT. The calculations in LTE were
performed with the OSMARCS 1D atmospheric model and the spectrum
synthesis code Turbospectrum, while the analysis in NLTE is based on
the MULTI code. We present LTE abundances for 26 elements, and NLTE
calculations for the species CI, OI, NaI, MgI, AlI, KI, CaI, SrII, and
BaII lines.
Objects:
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RA (2000) DE Designation(s)
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15 43 03.10 -10 56 00.6 HD 140283 = HIP 76976
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 63 301 Fe and Ti lines adopted. Atomic data and abundances
tablea2.dat 50 246 Line by line elemental abundances
tablea3.dat 74 44 Hyperfine coupling constants
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- El Element and degree of ionization
7- 14 F8.3 0.1nm lambda Wavelength of the line
17- 21 F5.3 eV chiex Excitation potential
24- 29 F6.3 [-] loggfVALD Oscillator strength of the transition
from VALD database
32- 37 F6.3 [-] loggfNIST ? Oscillator strength of the transition
from NIST database
40- 45 F6.2 0.1pm EW Equivalent widths
48- 51 F4.2 0.1pm e_EW Error on the equivalent widths (1)
54- 57 F4.2 [-] A(X) Elemental abundances (G1)
60- 63 F4.2 [-] e_A(X) Error on the elemental abundances
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Note (1): The uncertainties of the equivalent widths were computed based on
standard error propagation, using the errors given for the parameters of the
Gaussian profile obtained from the fitting procedure.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Species Element and degree of ionization
6- 14 F9.3 0.1nm lambda Wavelength of the line
17- 21 F5.3 eV chiex Excitation potential
24- 29 F6.3 [-] loggf Oscillator strength of the transition
31 A1 --- l_A(X) Limit flag on A(X)
32- 36 F5.2 [-] A(X) Elemental abundances (G1)
38 A1 --- l_[X/H] Limit flag on [X/H]
39- 43 F5.2 [-] [X/H] Abundance ratio (2)
45 A1 --- l_[X/Fe] Limit flag on [X/Fe]
46- 50 F5.2 [-] [X/Fe] Abundance ratio
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Note (2): [X/H]=A(X,star)-A(X,Sun), with solar abundances adopted from
Asplund et al. (2009ARA&A..47..481A 2009ARA&A..47..481A, The Chemical Composition of the Sun).
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- El Isotope and degree of ionization
9- 16 F8.3 0.1nm lambda Wavelength of the line
19- 21 F3.1 [-] JLower Total angular momentum of the lower level
24- 31 F8.3 MHz ALower ? HFS A coefficient of the lower level
36- 42 F7.3 MHz BLower ? HFS B coefficient of the lower level
46- 47 I2 --- r_JLower ? Reference for the HFS coefficients
of the lower level (1)
50- 52 F3.1 [-] JUpper Total angular momentum of the upper level
54- 61 F8.3 MHz AUpper ? HFS A coefficient of the upper level
64- 70 F7.3 MHz BUpper ? HFS B coefficient of the upper level
73- 74 I2 --- r_JUpper ? Reference for the HFS coefficients
of the upper level (1)
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Note (1): References as follows:
1 = Das & Natarajan (2008JPhB...41c5001D 2008JPhB...41c5001D)
2 = Safronova, Johnson & Derevianko (1999PhRvA..60.4476S 1999PhRvA..60.4476S)
3 = Brown & Evenson (1999PhRvA..60..956B 1999PhRvA..60..956B)
4 = Nakai et al. (2007JaJAP..46..815N 2007JaJAP..46..815N)
5 = Belin et al. (1975PhyS...12..287B 1975PhyS...12..287B)
6 = Falke et al. (2006PhRvA..74c2503F 2006PhRvA..74c2503F)
7 = Childs (1971PhRvA...4.1767C 1971PhRvA...4.1767C)
8 = Basar et al. (2004PhyS...69..189B 2004PhyS...69..189B)
9 = Villemoes et al. (1992PhRvA..45.6241V 1992PhRvA..45.6241V)
10 = Mansour et al. (1989PhRvA..39.5762M 1989PhRvA..39.5762M)
11 = Scott et al. (2015A&A...573A..26S 2015A&A...573A..26S)
12 = Unkel et al. (1989ZPhyD..11..259U 1989ZPhyD..11..259U)
13 = Gyzelcimen et al. (2014ApJS..214....9G 2014ApJS..214....9G)
14 = Palmeri et al. (1995JPhB...28.3741P 1995JPhB...28.3741P)
15 = Wood et al. (2014ApJS..214...18W 2014ApJS..214...18W)
16 = Armstrong et al. (2011PhyS...84e5301A 2011PhyS...84e5301A)
17 = Lawler et al. (2001ApJ...556..452L 2001ApJ...556..452L)
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Global notes:
Note (G1): We adopt the notation A(X)=log[n(X)/n(H)]+12, where n is the
number density of atoms.
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Acknowledgements:
Cesar Siqueira-Mello, cesar.mello(at)usp.br
(End) Cesar Siqueira-Mello [IAG-USP, Brazil], Patricia Vannier [CDS] 02-Sep-2015