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J/A+A/440/321      Chemical abundances in 43 metal-poor stars   (Jonsell+, 2005)

Chemical abundances in 43 metal-poor stars. Jonsell K., Edvardsson B., Gustafsson B., Magain P., Nissen P.E., Asplund M. <Astron. Astrophys. 440, 321 (2005)> =2005A&A...440..321J
ADC_Keywords: Stars, population II ; Abundances, peculiar ; Space velocities ; Photometry, uvby ; Equivalent widths Keywords: stars: Population II - stars: fundamental parameters - stars: abundances - Galaxy: halo - Galaxy: abundances - Galaxy: evolution Abstract: We have derived abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Fe, Ni and Ba for 43 metal-poor field stars in the solar neighbourhood, most of them subgiants or turn-off-point stars, with iron abundances [Fe/H] ranging from -0.4 to -3.0. About half of this sample has not been analysed spectroscopically in detail before. Effective temperatures were estimated from uvby photometry, and surface gravities primarily from Hipparcos parallaxes. The analysis is differential relative to the Sun, and carried out with plane-parallel MARCS models. Various sources of error are discussed and found to contribute a total error of about 0.1-0.2dex for most elements, while relative abundances, such as [Ca/Fe], are most probably more accurate. For the oxygen abundances, determined in an NLTE analysis of the 7774Å triplet lines, the errors may be somewhat larger. Description: Data from an analysis of 43 metal-poor field stars with iron abundances [Fe/H] ranging from -0.4 to -3.0dex are presented here. Photometric data, stellar velocities, masses, fundamental parameters, spectral classifications and notations of possible binarity are given. Tables with line data for O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Fe, Ni and Ba, equivalent widths and resulting abundances are also given. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 31 1727 Equivalent widths table2.dat 101 43 Stellar data table3.dat 72 62 Atomic line data and solar abundances table4.dat 102 43 Chemical abundances
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD identification number 8- 9 A2 --- Elem Element abbreviation 11- 12 I2 --- Z Atomic number 14 I1 --- Stage [1/2] Ionization stage: 1: neutral, 2: singly ionized 16- 23 F8.3 0.1nm Lambda Air wavelength in Angstrom 26- 30 F5.1 0.1pm EW Equivalent width 31 A1 --- u_EW Uncertainty flag on EW
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD identification number 8- 12 F5.3 mag Vmag Visual apparent magnitude 14- 18 F5.3 mag (b-y) Stromgren colour index 20- 24 F5.3 mag c1 Stromgren Balmer discontinuity index 26- 30 A5 --- r_(b-y) References for Stromgren photometry (1) 32- 35 I4 km/s UVel Stellar U velocity relative to the LSR (2) 37- 40 I4 km/s VVel Stellar V velocity relative to the LSR 42- 45 I4 km/s WVel Stellar W velocity relative to the LSR 47- 50 F4.2 solMass Mass Stellar mass derived from evolutionary tracks 52 I1 --- Model [1/2] Reference for Evolutionary tracks (3) 53 I1 --- r_Mass [2/3]? Marker of uncertain stellar mass (4) 55- 58 I4 K Teff Effective temperature in K 60 I1 --- r_Teff [1]? 1: Teff from Zacs et al., 1998A&A...337..216Z 62- 66 F5.2 [Sun] [Fe/H] Iron abundance set equal to the overall model metal abundance (5) 68- 71 F4.2 [cm/s2] logg Log of surface gravity 73 I1 --- r_logg [1]? 1: logg from Zacs et al., 1998A&A...337..216Z 75- 77 F3.1 km/s vt Microturbulence parameter 79 I1 --- r_vt [1]? 1: vt from Zacs et al., 1998A&A...337..216Z 81- 90 A10 --- Class MK spectral classification of the stars according to the SIMBAD database 92-101 A10 --- Note Notes about the stars (6)
Note (1): References for Stromgren photometry are numbered as follows: 1 = Olsen, 1983A&AS...54...55O 2 = Schuster & Nissen, 1988A&AS...73..225S 3 = Lindgren H., ESO (unpublished) 4 = Olsen, 1993, Cat. J/A+AS/102/89 5 = Hauck & Mermilliod, 1998, Cat. II/215 6 = Gronbech &.Olsen, 1976-77, Cat. II/33 7 = SIMBAD database Note (2): The U velocity is positive in the direction of the galactic center Note (3): Reference for Evolutionary tracks as follows: 1 = Adopted mass 0.80M 2 = VandenBerg et al., 2000ApJ...532..430V Note (4): Marker of uncertain stellar mass as follows: 2 = The star is located on the lower side of the track 3 = The star is located where the tracks are very compact Note (5): Abundances are expressed as the logarithm of the number abundance of an element relative to hydrogen, and normalized to 0.0 for the Solar ratio Note (6): Notes about the stars have the following meaning: Ba = barium star b = binary sp. b = spectroscopic binary v = variable
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Elem Element abbreviation 4- 5 I2 --- Z Atomic number 7 I1 --- Stage Ionization stage: 1: neutral, 2: singly ionized 9- 16 F8.3 0.1nm Lambda Air wavelength in Angstrom 19- 22 F4.2 --- logeps Solar photospheric abundance (1) 25- 29 F5.1 0.1pm EWSun Solar equivalent width in mA 32- 36 F5.2 --- loggf The oscillator strength multiplied with the statistical weight, all in logarithm 39- 43 F5.3 eV Elow Lower transition level excitation energy 46 I1 --- Dflag [1/2] Pressure damping flag (2) 48- 51 F4.2 --- Dcorr Damping correction factor applied when Dflag set to 0 54- 61 E8.2 s-1 Gamma Radiation damping constant 64- 65 A2 --- LevelL Lower level identification of the transition 67- 68 A2 --- LevelU Upper level identification of the transition
Note (1): Abundances are expressed as the logarithm of the number abundance of an element relative to hydrogen, plus 12.0 Note (2): Pressure damping flags defined as follows: 1 = The hydrogen collision broadening was adopted from Barklem et al., 2000, Cat. J/A+AS/142/467, and references therein. 2 = Unsoeld (1955, Physik der Stematmospharen, 2nd ed., Berlin Springer Verlag) approximation, i.e. the hydrogen collision broadening was calculated following Mihalas D. 1978, "Stellar Atmospheres", (W.H. Freeman & Co., San Francisco), with the correction factor in column Dcorr multiplied to the resulting broadening FWHM, Gamma
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD identification number 8- 12 F5.2 [Sun] [FeI/H] Iron abundance from Fe I (1) 14- 18 F5.2 [Sun] [OI/H] ? Oxygen abundance from O I (1),(2) 20- 24 F5.2 [Sun] [NaI/H] ? Sodium abundance from Na I (1) 26- 30 F5.2 [Sun] [MgI/H] ? Magnesium abundance from Mg I (1) 32- 36 F5.2 [Sun] [AlI/H] ? Aluminium abundance from Al I (1) 38- 42 F5.2 [Sun] [SiI/H] ? Silicon abundance from Si I (1) 44- 48 F5.2 [Sun] [CaI/H] ? Calcium abundance from Ca I (1) 50- 54 F5.2 [Sun] [ScII/H] ? Scandium abundance from Sc II (1) 56- 60 F5.2 [Sun] [TiI/H] ? Titanium abundance from Ti I (1) 62- 66 F5.2 [Sun] [VI/H] ? Vanadium abundance from V I (1) 68- 72 F5.2 [Sun] [CrI/H] ? Chromium abundance from Cr I (1) 74- 78 F5.2 [Sun] [FeII/H] ? Iron abundance from Fe II (1) 80- 84 F5.2 [Sun] [NiI/H] ? Nickel abundance from Ni I (1) 86- 90 F5.2 [Sun] [BaII/H] ? Barium abundance from Ba II (1) 92- 96 F5.2 [Sun] [alpha/H] ? alpha element abundance (1)(3) 98-102 F5.2 [Sun] [alpha'/H] ? alpha' element abundance (1)(4)
Note (1): Abundances are expressed as the logarithm of the number abundance of an element relative to hydrogen, and normalized to 0.0 for the Solar ratio Note (2): For oxygen, NLTE corrections have been applied Note (3): The α element abundance is the straight mean value of the abundances derived from Mg I, Si I, Ca I and Ti I Note (4): The α' element abundance is the straight mean value of the abundances derived from Mg I, Si I and Ca
Acknowledgements: Karin Jonsell
(End) Karin Jonsell [Uppsala Astron. Obs.], Patricia Vannier [CDS] 02-May-2005
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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