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J/A+A/489/403       Line abundances for solar stars                (Pace+, 2008)

Abundances of four open clusters from solar stars. Pace G., Pasquini L., Francois P. <Astron. Astrophys. 489, 403 (2008)> =2008A&A...489..403P
ADC_Keywords: Clusters, open ; Stars, dwarfs ; Abundances Keywords: stars: abundances - Galaxy: open clusters and associations: individual: NGC 3680, IC4651, Praesepe, M67 Abstract: We present the abundance measurements of several elements (Fe, Ca, Na, Ni, Ti, Al, Cr, Si) for 20 solar-type stars belonging to four Galactic open clusters: NGC 3680, IC 4651, Praesepe, and M 67. Oxygen abundances were in addition measured for most stars in each cluster apart from IC 4651. For NGC 3680, accurate abundance determinations using high-resolution spectra covering a large spectral domain are computed for the first time. We used UVES high-resolution, high signal-to-noise (S/N) ratio spectra and performed a differential analysis with respect to the sun, by measuring equivalent widths and assuming LTE. Description: Line list used, from Randich et al. (2006A&A...450..557R), including EW measurements done therein, plus the resulting solar abundance values, computed for each line using the OSMARCS code (Edvardsson et al., 1993, Cat. J/A+A/275/101). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file linels.dat 32 142 Line list used (table1 of the paper)
See also: J/A+A/275/101 : Chemical evolution of the galactic disk I. (Edvardsson+ 1993) Byte-by-byte Description of file: linels.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm Lambda Wavelength 10- 11 A2 --- X Element 13 I1 --- i Ionization stage (1=neutral) 18- 22 F5.1 0.1pm EW Equivalent width (mÅ) 29- 32 F4.2 --- X/H Abundance (log scale, H=12)
Acknowledgements: Giancarlo Pace, gpace(at)
(End) Giancarlo Pace [CAUP], Patricia Vannier [CDS] 16-Jun-2008
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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