J/A+A/575/A51 Line list for abundance determination in Sun siblings (Liu+, 2015)
Quest for the lost siblings of the Sun.
Liu C., Ruchti G., Feltzing S., Martinez-Barbosa A.C., Bensby T.,
Brown G.A.A., Portegies Zwart F.S.
<Astron. Astrophys. 575, A51 (2015)>
=2015A&A...575A..51L 2015A&A...575A..51L
ADC_Keywords: Clusters, open ; Stars, nearby ; Abundances ;
Spectroscopy ; Stars, ages
Keywords: stars: abundances - stars: fundamental parameters -
solar neighbourhood
Abstract:
The aim of this paper is to find lost siblings of the Sun by analyzing
high resolution spectra. Finding solar siblings will enable us to
constrain the parameters of the parental cluster and the birth place
of the Sun in the Galaxy. The solar siblings can be identified by
accurate measurements of metallicity, stellar age and elemental
abundances for solar neighbourhood stars. The solar siblings
candidates were kinematically selected based on their proper motions,
parallaxes and colours. Stellar parameters were determined through a
purely spectroscopic approach and partly physical method,
respectively. Comparing synthetic with observed spectra, elemental
abundances were computed based on the stellar parameters obtained
using a partly physical method. A chemical tagging technique was used
to identify the solar siblings. We present stellar parameters, stellar
ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Ti,
Cr, Fe, and Ni for 32 solar sibling candidates. Our abundances
analysis shows that four stars are chemically homogeneous together with
the Sun. Technique of chemical tagging gives us a high probability
that they might be from the same open cluster. Only one candidate,
HIP 40317, which has solar metallicity and age could be a solar
sibling. We performed simulations of the Sun's birth cluster in
analytical Galactic model and found that most of the radial velocities
of the solar siblings lie in the range -10≤Vr≤10km/s, which
is smaller than the radial velocity of HIP 40317 (Vr=34.2km/s),
under different Galactic parameters and different initial conditions
of the Sun's birth cluster. The sibling status for HIP 40317 is not
directly supported by our dynamical analysis.
Description:
On table 2 we list all spectral lines that have been used to determine
elemental abundances. Columns 1 gives the element with a degree of
ionization. The wavelength, excitation potential and adopted loggf
values are listed in the Columns 2, 3, and 4, respectively. References
to the adopted log gf values are given in Column 5.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 33 227 Atomic line data
refs.dat 42 20 References for loggf values
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See also:
J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ion Element and ionization stage (I=neutral)
7- 14 F8.3 0.1nm lambda [4508/8774] Line wavelength λ (Å)
17- 22 F6.4 eV LEP [0/6] Lower excitation potential χ
25- 30 F6.3 [-] loggf Oscillator strength
32- 33 I2 --- r_loggf Reference for loggf (see refs.dat)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference code
4- 22 A19 --- BibCode Bibcode
24- 42 A19 --- Aut Author's name
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Acknowledgements:
Cheng Liu, cheng(at)astro.lu.se
(End) Cheng Liu [Lund Obs., Sweden], Patricia Vannier [CDS] 05-Jan-2015