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J/ApJ/787/154  Elemental abundances of solar sibling candidates (Ramirez+, 2014)

Elemental abundances of solar sibling candidates. Ramirez I., Bajkova A.T., Bobylev V.V., Roederer I.U., Lambert D.L., Endl M., Cochran W.D., MacQueen P.J., Wittenmyer R.A. <Astrophys. J., 787, 154 (2014)> =2014ApJ...787..154R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Abundances ; Spectroscopy Keywords: stars: abundances - stars: fundamental parameters - stars: general - stars: individual: HD 162826 - stars: kinematics and dynamics Abstract: Dynamical information along with survey data on metallicity and in some cases age have been used recently by some authors to search for candidates of stars that were born in the cluster where the Sun formed. We have acquired high-resolution, high signal-to-noise ratio spectra for 30 of these objects to determine, using detailed elemental abundance analysis, if they could be true solar siblings. Only two of the candidates are found to have solar chemical composition. Updated modeling of the stars' past orbits in a realistic Galactic potential reveals that one of them, HD 162826, satisfies both chemical and dynamical conditions for being a sibling of the Sun. Measurements of rare-element abundances for this star further confirm its solar composition, with the only possible exception of Sm. Analysis of long-term high-precision radial velocity data rules out the presence of hot Jupiters and confirms that this star is not in a binary system. We find that chemical tagging does not necessarily benefit from studying as many elements as possible but instead from identifying and carefully measuring the abundances of those elements that show large star-to-star scatter at a given metallicity. Future searches employing data products from ongoing massive astrometric and spectroscopic surveys can be optimized by acknowledging this fact. Description: We used the Tull coude spectrograph on the 2.7 m Harlan J. Smith Telescope at McDonald Observatory (Tull et al. 1995PASP..107..251T) to observe most of our targets (23). All but three of them were observed in 2012 December; the others were observed in 2013 March. The rest of our targets (seven) have too-low declinations to be observed from McDonald Observatory. Instead, they were observed using the Magellan Inamori Kyocera Echelle (MIKE) spectrograph on the 6.5 m Telescope at Las Campanas Observatory (Bernstein et al. 2003SPIE.4841.1694B) in 2013 April. Slit sizes were chosen so that the spectral resolution of the data is about 60000 in the visible part of the spectrum. We targeted a S/N per pixel of at least 200 at 6000 Å. Only one of our targets (HD 46100) has a significantly lower S/N spectrum. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 30 127 Iron Line List table4.dat 30 539 Line List For Elements Other Than Iron
See also: J/A+A/420/183 : Spectroscopic survey in solar neighborhood (Allende Prieto+ 2004) J/A+A/575/A51 : Line list for abundance determination in Sun siblings (Liu+, 2015) Byte-by-byte Description of file: table2.dat table4.dat
Bytes Format Units Label Explanations
1- 10 F10.4 0.1nm Wave Wavelength; Angstroms (1) 12- 15 F4.1 --- ID Species identifier (2) 17- 22 F6.4 eV ExPot Excitation Potential 24- 30 F7.4 [-] log(gf) Log of the oscillator strength
Note (1): Lines where hyperfine structure was taken into account are listed as one positive wavelength followed by a set of negative wavelengths whose absolute values correspond to the HFS components. Note (2): The number to the left of the decimal point indicates the atomic number. The number to the right of the decimal point indicates the ionization state, where "0" is neutral and "1" is singly ionized.
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 30-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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