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J/A+A/425/187     Chemical abundances of 23 subgiants & giants   (Thoren+, 2004)

Subgiants as probes of galactic chemical evolution. Thoren P., Edvardsson B., Gustafsson B. <Astron. Astrophys. 425, 187 (2004)> =2004A&A...425..187T (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, giant ; Abundances, peculiar ; Space velocities Keywords: stars: abundances - stars: evolution Description: Chemical abundances, stellar parameters, and atomic and molecular line data are given for a study of 23 subgiant and giant stars in the solar vicinity. With the exception of Li and possibly C we show that subgiant stars show no "chemical" traces of post-main-sequence evolution and that they are therefore and because of their simple age dating very useful targets for studies of galactic chemical evolution. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 46 149 Atomic line data table2.dat 30 185 Molecular line data table6.dat 264 23 Chemical abundances and stellar parameters
See also: J/A+A/275/101 : Chemical evolution of the galactic disk I. (Edvardsson+ 1993) J/A+AS/102/603 : Chemical evolution of the galactic disk II. (Edvardsson+ 1993) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Elem Element 4- 5 A2 --- Ion Ionization state (I: neutral, II: singly ionized) 7- 14 F8.3 0.1nm Lambda Air wavelength (Angstroem) 16- 21 F6.3 eV Exc Lower transition level excitation energy 23- 29 F7.3 --- loggf Logarithm of the oscillator strength value 31 I1 --- Dflag Pressure damping flag (1) 33- 36 F4.2 --- Dcorr ? Damping correction factor (1) 38- 46 E9.3 s-1 DRad Radiation damping
Note (1): - When Dflag = 1 (Quantum mechanics calculation), the hydrogen collision broadening was adopted from Barklem & O'Mara (1998MNRAS.300..863B), and references therein. - When Dflag = 0 (Unsoeld approximation), the hydrogen collision broadening was calculated following Mihalas D. 1978, "Stellar Atmospheres", (W.H. Freeman & Co., San Francisco), (1978stat.book.....M) with the correction factor in column Dcorr multiplied to the resulting broadening FWHM, Gamma
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm Lambda Air wavelength (Angstroem) 10- 14 F5.3 eV Exc Lower transition level excitation energy 16- 21 F6.3 --- loggf Logarithm of the oscillator strength value 23- 30 A8 --- Trans Identification
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 10 A3 --- Class SGB = subgiant star, RGB = giant star 12- 15 I4 K Teff Effective temperature in K 17- 20 F4.2 [cm/s2] logg Log of surface gravity 22- 26 F5.2 [Sun] [M/H] Overall model metal abundance (1) 28- 31 F4.2 km/s xi Microturbulence parameter 33- 36 F4.2 mag VMAG Absolute V magnitude 38- 41 F4.1 Gyr Age Stellar age in gigayears 43- 45 F3.1 solMass Mass Stellar mass in solar units 47- 50 I4 km/s Uvel Stellar U velocity relative to the LSR (2) 52- 55 I4 km/s Vvel Stellar V velocity relative to the LSR 57- 60 I4 km/s Wvel Stellar W velocity relative to the LSR 62- 64 I3 km/s VelTot Stellar total velocity relative to the LSR 66- 70 F5.2 [Sun] ALi ? Lithium abundance or upper limit (1) 72 I1 --- l_ALi [0,1]? Lithium abundance upper limit flag (0: determination, 1: upper limit) 74- 78 F5.2 [Sun] ACI ? Carbon abundance from [C I] (1) 80- 84 F5.2 [Sun] ACH ? Carbon abundance from CH (1) 86- 90 F5.2 [Sun] AC2 ? Carbon abundance from C2 (1) 92- 93 I2 --- C12/C13 ? Carbon isotope abundance ratio C12/C13 95- 96 I2 --- e_C12/C13 ? rms uncertainty in C12/C13 ratio 98-102 F5.2 [Sun] ANI ? Nitrogen abundance from N I (1) 104-108 F5.2 [Sun] ANCN ? Nitrogen abundance from CN (1) 110-114 F5.2 [Sun] AOI ? Oxygen abundance mainly f. [O I] (1) 116-120 F5.2 [Sun] ANaI ? Sodium abundance from Na I (1) 122-126 F5.2 [Sun] AMgI ? Magnesium abundance from Mg I (1) 128-132 F5.2 [Sun] AMgH ? Magnesium abundance from MgH (1) 134-138 F5.2 [Sun] AAlI ? Aluminium abundance from Al I (1) 140-144 F5.2 [Sun] ASiI ? Silicon abundance from Si I (1) 146-150 F5.2 [Sun] ASiII ? Silicon abundance from Si II (1) 152-156 F5.2 [Sun] ASI ? Sulphur abundance from S I (1) 158-162 F5.2 [Sun] AKI ? Potassium abundance from K I (1) 164-168 F5.2 [Sun] ACaI ? Calcium abundance from Ca I (1) 170-174 F5.2 [Sun] AScII ? Scandium abundance from Sc II (1) 176-180 F5.2 [Sun] ATiI ? Titanium abundance from Ti I (1) 182-186 F5.2 [Sun] ATiII ? Titanium abundance from Ti II (1) 188-192 F5.2 [Sun] AVI ? Vanadium abundance from V I (1) 194-198 F5.2 [Sun] ACrI ? Chromium abundance from Cr I (1) 200-204 F5.2 [Sun] ACrII ? Chromium abundance from Cr II (1) 206-210 F5.2 [Sun] AFeI Iron abundance from Fe I (1) 212-216 F5.2 [Sun] AFeII ? Iron abundance from Fe II (1) 218-222 F5.2 [Sun] ACoI ? Cobalt abundance from Co I (1) 224-228 F5.2 [Sun] ANiI Nickel abundance from Ni I (1) 230-234 F5.2 [Sun] ACuI ? Cupper abundance from Cu I (1) 236-240 F5.2 [Sun] AZnI ? Zinc abundance from Zn I (1) 242-246 F5.2 [Sun] AYII ? Yttrium abundance from Y II (1) 248-252 F5.2 [Sun] AZrI ? Zirconium abundance from Zr I (1) 254-258 F5.2 [Sun] ANdII ? Neodymium abundance from Nd II (1) 260-264 F5.2 [Sun] Aalpha ? alpha-element abundance (3)
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): The U velocity is positive in the direction of the galactic center Note (3): The alpha element abundance is the straight mean value of the abundances derived from Mg I, Si I, Ca I and Ti I
Acknowledgements: Bengt Edvardsson
(End) Bengt Edvardsson [Uppsala Astronomical Observatory] 19-May-2004
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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