Access to Astronomical Catalogues

← Click to display the menu
J/A+A/508/L17         Abundances in solar analogs         (Ramirez+, 2009)

Accurate abundance patterns of solar twins and analogs. Does the anomalous solar chemical composition come from planet formation? Ramirez I., Melendez J., Asplund M. <Astron. Astrophys., 508, L17-L20 (2009)> =2009A&A...508L..17R
ADC_Keywords: Stars, G-type ; Stars, dwarfs ; Abundances Keywords: stars: abundances - Sun: abundances - planetary systems Abstract: We derive the abundance of 19 elements in a sample of 64 stars with fundamental parameters very similar to solar, which minimizes the impact of systematic errors in our spectroscopic 1D-LTE differential analysis, using high-resolution (R∼60000), high signal-to-noise ratio (S/N∼200) spectra. The estimated errors in the elemental abundances relative to solar are as small as ∼0.025dex. The abundance ratios [X/Fe] as a function of [Fe/H] agree closely with previously established patterns of Galactic thin-disk chemical evolution. Description: Our sample stars were selected from the Hipparcos catalog (I/239) by applying constraints on color, based on the color-Teff calibrations by Ramirez & Melendez (2005ApJ...626..465R), corrected by suspected zero point errors (Casagrande et al., 2009, submitted), trigonometric parallaxes, and literature values for [Fe/H] and chromospheric activity, if available. About 100 stars satisfied our selection criteria and, given our observational constraints, data for 64 of them were acquired. We also observed the asteroids Vesta and Ceres as solar reference. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 55 64 Derived stellar parameters, average abundance ratios [X/Fe] of volatile elements (<900K), and slope of the [X/Fe] vs. Tc relation for refractory elements (>900K) abund.dat 240 64 Abundance ratios [X/Fe] for C, O, Na, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Ni, Cu, Zn, Y, Zr, and Ba (tables 2-4 of the paper)
See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/A+A/468/663 : Li abundances in solar-analog stars (Takeda+, 2007) J/ApJS/181/62 : Survey of young solar analogs (Metchev+, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HIP HIP star number 8- 11 I4 K Teff Effective temperature 13- 16 F4.2 [cm/s2] logg Surface gravity 18- 23 F6.3 [Sun] [Fe/H] Metallicity 25- 29 F5.3 [Sun] e_[Fe/H] rms uncertainty on [Fe/H] (1) 31- 36 F6.3 [Sun] [X/Fe] Average [X/Fe] value for volatile elements (Tc<900K) 38- 42 F5.3 [Sun] e_[X/Fe] rms uncertainty on [X/Fe] 44- 49 F6.3 K-1 dA/dT Slope of the [X/Fe] vs. Tc relation for refractory elements (Tc>900K) 51- 55 F5.3 K-1 e_dA/dT rms uncertainty on slope
Note (1): Errors in [Fe/H] correspond to the 1-σ scatter of the line-by-line abundances.
Byte-by-byte Description of file: abund.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HIP HIP star number 8- 13 F6.3 [Sun] [C/Fe] Abundance ratio [C/Fe] 15- 19 F5.3 [Sun] e_[C/Fe] rms uncertainty on [C/Fe] (1) 21- 26 F6.3 [Sun] [O/Fe] Abundance ratio [O/Fe] 28- 32 F5.3 [Sun] e_[O/Fe] rms uncertainty on [O/Fe] (1) 34- 39 F6.3 [Sun] [Na/Fe] ? Abundance ratio [Na/Fe] 41- 45 F5.3 [Sun] e_[Na/Fe] ? rms uncertainty on [Na/Fe] (1) 47- 52 F6.3 [Sun] [Al/Fe] Abundance ratio [Al/Fe] 54- 58 F5.3 [Sun] e_[Al/Fe] rms uncertainty on [Al/Fe] (1) 60- 65 F6.3 [Sun] [Si/Fe] Abundance ratio [Si/Fe] 67- 71 F5.3 [Sun] e_[Si/Fe] rms uncertainty on [Si/Fe] (1) 73- 78 F6.3 [Sun] [S/Fe] ? Abundance ratio [S/Fe] 80- 84 F5.3 [Sun] e_[S/Fe] ? rms uncertainty on [S/Fe] (1) 86- 91 F6.3 [Sun] [Ca/Fe] Abundance ratio [Ca/Fe] 93- 97 F5.3 [Sun] e_[Ca/Fe] rms uncertainty on [Ca/Fe] (1) 99-104 F6.3 [Sun] [Sc/Fe] ? Abundance ratio [Sc/Fe] 106-110 F5.3 [Sun] e_[Sc/Fe] ? rms uncertainty on [Sc/Fe] (1) 112-117 F6.3 [Sun] [Ti/Fe] Abundance ratio [Ti/Fe] 119-123 F5.3 [Sun] e_[Ti/Fe] rms uncertainty on [Ti/Fe] (1) 125-130 F6.3 [Sun] [V/Fe] Abundance ratio [V/Fe] 132-136 F5.3 [Sun] e_[V/Fe] rms uncertainty on [V/Fe] (1) 138-143 F6.3 [Sun] [Cr/Fe] Abundance ratio [Cr/Fe] 145-149 F5.3 [Sun] e_[Cr/Fe] rms uncertainty on [Cr/Fe] (1) 151-156 F6.3 [Sun] [Mn/Fe] ? Abundance ratio [Mn/Fe] 158-162 F5.3 [Sun] e_[Mn/Fe] ? rms uncertainty on [Mn/Fe] (1) 164-169 F6.3 [Sun] [Ni/Fe] Abundance ratio [Ni/Fe] 171-175 F5.3 [Sun] e_[Ni/Fe] rms uncertainty on [Ni/Fe] (1) 177-182 F6.3 [Sun] [Cu/Fe] ? Abundance ratio [Cu/Fe] 184-188 F5.3 [Sun] e_[Cu/Fe] ? rms uncertainty on [Cu/Fe] (1) 190-195 F6.3 [Sun] [Zn/Fe] Abundance ratio [Zn/Fe] 197-201 F5.3 [Sun] e_[Zn/Fe] rms uncertainty on [Zn/Fe] (1) 203-208 F6.3 [Sun] [Y/Fe] ? Abundance ratio [Y/Fe] 210-214 F5.3 [Sun] e_[Y/Fe] ? rms uncertainty on [Y/Fe] (1) 216-221 F6.3 [Sun] [Zr/Fe] ? Abundance ratio [Zr/Fe] 223-227 F5.3 [Sun] e_[Zr/Fe] ? rms uncertainty on [Zr/Fe] (1) 229-234 F6.3 [Sun] [Ba/Fe] Abundance ratio [S/Bae] 236-240 F5.3 [Sun] e_[Ba/Fe] rms uncertainty on [Ba/Fe] (1)
Note (1): Errors correspond to the 1-σ scatter of the line-by-line abundances. A conservative value of 0.050 for the error was assumed when only one line was available.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Mar-2010
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

catalogue service