J/MNRAS/450/1900 Chemical abundances of 257 giant stars (Adibekyan+, 2015) ================================================================================ Chemical abundances and kinematics of 257 G-, K-type field giants. Setting a base for further analysis of giant-planet properties orbiting evolved stars. Adibekyan V.Zh., Sousa S.G., Santos N.C. , Delgado Mena E., Gonzalez Hernandez J. I., Israelian G., Mayor M., Khachatryan G., Adibekyan V., Benamati L., Santos N.C., Alves S., Lovis C., Udry S., Israelian G., Sousa S.G., Tsantaki M., Mortier A., Sozzetti A., De Medeiros J.R. =2015MNRAS.450.1900A ================================================================================ ADC_Keywords: Stars, nearby ; Planets ; Space velocities ; Abundances, peculiar Keywords: methods: observational - techniques: spectroscopic - stars: abundances - planetary systems Abstract: We performed a uniform and detailed abundance analysis of 12 refractory elements for a sample of 257 G- and K-type evolved stars from the CORALIE planet search program. This sample, being homogeneously analyzed, can be used as a comparison sample for other planet-related studies, as well as for different type of studies related to stellar and Galaxy astrophysics. The abundances of the chemical elements were determined using an LTE abundance analysis relative to the Sun, with the spectral synthesis code MOOG and a grid of Kurucz ATLAS9 atmospheres. To separate the Galactic stellar populations both a purely kinematical approach and a chemical method were applied. Description: The file ew.dat lists the equivalent widths (EW) of all the spectral lines. Columns 1, 2, and 3 list the name of the stars, wavelength and EWs of the lines. The file linelist.dat lists the lines that were used in this study. The last column shows the difference (in n*sigma) between chemical abundances of giant and dwarf stars with solar metallicity derived from each line. The file table2.dat lists the derived abundances of the elements, rms, and number of measured lines for each star. The file ab_best.dat lists the abundances of the elements derived by using the "best" linelist. The file vel.dat lists the parameters used to assign the Galactic population to which each star belongs. Galactic space velocity components and the probabilities to assign the stellar population to which each star belongs according to Bensby (2003A&A...410..527B) and Robin (2003A&A...409..523R) criteria. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 348 257 Abundances, rms, error, and number of lines for each star and element ab_best.dat 80 257 Abundances for each star and element derived by using only the "best" lines vel.dat 65 183 Parameters to assign the stars to a Galactic population ew.dat 22 30228 Equivalent widths of the spectral lines used to derive abundances linelist.dat 28 118 Atomic parameters for lines selected in the paper -------------------------------------------------------------------------------- See also: J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003) J/A+A/418/551 : Galactic disk stars abund. & velocities (Mishenina+, 2004) J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006) J/A+A/497/563 : Chemical abundances of 451 stars (Neves+, 2009) J/A+A/545/A32 : Chemical abundances of 1111 FGK stars (Adibekyan+, 2012) Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Star Star's identifier 10- 14 F5.2 [Sun] [Na/H] ? Abundance [Na/H] (Z=11) (G1) (1) 16- 19 F4.2 [Sun] e_[Na/H] rms uncertainty of [Na/H] 21- 24 F4.2 [Sun] s_[Na/H] Total error of [Na/H] 26- 30 F5.2 [Sun] [Na/H]c Abundance [Na/H] after correction for effective temperature trend (2) 32 I1 --- o_[Na/H] Number of Na lines used 34- 38 F5.2 [Sun] [Mg/H] Abundance [Mg/H] (Z=12) (G1) (1) 40- 43 F4.2 [Sun] e_[Mg/H] rms uncertainty of [Mg/H] 45- 48 F4.2 [Sun] s_[Mg/H] Total error of [Mg/H] 50- 54 F5.2 [Sun] [Mg/H]c Abundance [Mg/H] after correction for effective temperature trend (2) 56 I1 --- o_[Mg/H] Number of MgI lines used 58- 62 F5.2 [Sun] [Al/H] ? Abundance [Al/H] (Z=13) (G1) (1) 64- 67 F4.2 [Sun] e_[Al/H] ? rms uncertainty of [Al/H] 69- 72 F4.2 [Sun] s_[Al/H] Total error of [Al/H] 74- 78 F5.2 [Sun] [Al/H]c Abundance [Al/H] after correction for effective temperature trend (2) 80 I1 --- o_[Al/H] ? Number of AlI lines used 82- 86 F5.2 [Sun] [Si/H] Abundance [Si/H] (Z=14) (G1) 88- 91 F4.2 [Sun] e_[Si/H] rms uncertainty of [Si/H] 93- 96 F4.2 [Sun] s_[Si/H] Total error of [Si/H] 98-102 F5.2 [Sun] [Si/H]c Abundance [Si/H] after correction for effective temperature trend (2) 104-105 I2 --- o_[Si/H] Number of SiI lines used 107-111 F5.2 [Sun] [Ca/H] Abundance [Ca/H] (Z=20) (G1) 113-116 F4.2 [Sun] e_[Ca/H] rms uncertainty of [Ca/H] 118-121 F4.2 [Sun] s_[Ca/H] Total error of [Ca/H] 123-124 I2 --- o_[Ca/H] Number of CaI lines used 126-130 F5.2 [Sun] [ScI/H] Abundance [ScI/H] (Z=21.0) (G1) (1) 132-135 F4.2 [Sun] e_[ScI/H] rms uncertainty of [ScI/H] 137-140 F4.2 [Sun] s_[ScI/H] Total error of [ScI/H] 142-146 F5.2 [Sun] [ScI/H]c Abundance [ScI/H] after correction for effective temperature trend (2) 148 I1 --- o_[ScI/H] Number of ScI lines used 150-154 F5.2 [Sun] [ScII/H] Abundance [ScII/H] (Z=21.1) (G1) 156-159 F4.2 [Sun] e_[ScII/H] rms uncertainty of [ScII/H] 161-164 F4.2 [Sun] s_[ScII/H] Total error of [ScII/H] 166-170 F5.2 [Sun] [ScII/H]c Abundance [ScII/H] after correction for effective temperature trend (2) 172 I1 --- o_[ScII/H] Number of ScII lines used 174-178 F5.2 [Sun] [TiI/H] Abundance [TiI/H] (Z=22.0) (G1) 180-183 F4.2 [Sun] e_[TiI/H] rms uncertainty of [TiI/H] 185-188 F4.2 [Sun] s_[TiI/H] Total error of [TiI/H] 190-191 I2 --- o_[TiI/H] Number of TiI lines used 193-197 F5.2 [Sun] [TiII/H] Abundance [TiII/H] (Z=22.1) (G1) 199-202 F4.2 [Sun] e_[TiII/H] rms uncertainty of [TiII/H] 204-207 F4.2 [Sun] s_[TiII/H] Total error of [TiII/H] 209 I1 --- o_[TiII/H] Number of TiII lines used 211-215 F5.2 [Sun] [V/H] Abundance [V/H] (Z=23) (G1) 217-220 F4.2 [Sun] e_[V/H] rms uncertainty of [V/H] 222-225 F4.2 [Sun] s_[V/H] Total error of [V/H] 227-231 F5.2 [Sun] [V/H]c Abundance [V/H] after correction for effective temperature trend (2) 233 I1 --- o_[V/H] Number of VI lines used 235-239 F5.2 [Sun] [CrI/H] Abundance [CrI/H] (Z=24.0) (G1) 241-244 F4.2 [Sun] e_[CrI/H] rms uncertainty of [CrI/H] 246-249 F4.2 [Sun] s_[CrI/H] Total error of [CrI/H] 251-255 F5.2 [Sun] [CrI/H]c Abundance [CrI/H] after correction for effective temperature trend (2) 257 I1 --- o_[CrI/H] Number of CrI lines used 259-263 F5.2 [Sun] [CrII/H] ? Abundance [CrII/H] (Z=24.1) (G1) (1) 265-268 F4.2 [Sun] e_[CrII/H] ? rms uncertainty of [CrII/H] 270-273 F4.2 [Sun] s_[CrII/H] ? Total error of [CrII/H] 275-279 F5.2 [Sun] [CrII/H]c ? Abundance [CrII/H] after correction for effective temperature trend (2) 281 I1 --- o_[CrII/H] ? Number of CrII lines used 283-287 F5.2 [Sun] [Mn/H] Abundance [Mn/H] (Z=25) (G1) (1) 289-292 F4.2 [Sun] e_[Mn/H] rms uncertainty of [Mn/H] 294-297 F4.2 [Sun] s_[Mn/H] Total error of [Mn/H] 299 I1 --- o_[Mn/H] Number of MnI lines used 301-305 F5.2 [Sun] [Co/H] Abundance [Co/H] (Z=27) (G1) 307-310 F4.2 [Sun] e_[Co/H] rms uncertainty of [Co/H] 312-315 F4.2 [Sun] s_[Co/H] Total error of [Co/H] 317-321 F5.2 [Sun] [Co/H]c Abundance [Co/H] after correction for effective temperature trend (2) 323 I1 --- o_[Co/H] Number of CoI lines used 325-329 F5.2 [Sun] [Ni/H] Abundance [Ni/H] (Z=28) (G1) 331-334 F4.2 [Sun] e_[Ni/H] rms uncertainty of [Ni/H] 336-339 F4.2 [Sun] s_[Ni/H] Total error of [Ni/H] 341-345 F5.2 [Sun] [Ni/H]c Abundance [Ni/H] after correction for effective temperature trend (2) 347-348 I2 --- o_[Ni/H] Number of NiI lines used -------------------------------------------------------------------------------- Note (1): When only one line was used to derive the abundances, 0.1dex rms is considered. Note (2): Abundances for the elements after correction for the systematic trends with effective temperature. -------------------------------------------------------------------------------- Byte-by-byte Description of file: ab_best.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Star Star's identifier 10- 14 F5.2 [Sun] [Mg/H] Abundance [Mg/H] (Z=12) (G1) 16- 20 F5.2 [Sun] [Al/H] ? Abundance [Al/H] (Z=13) (G1) 22- 26 F5.2 [Sun] [Si/H] Abundance [Si/H] (Z=14) (G1) 28- 32 F5.2 [Sun] [Ca/H] Abundance [Ca/H] (Z=20) (G1) 34- 38 F5.2 [Sun] [ScI/H] Abundance [ScI/H] (Z=21.0) (G1) 40- 44 F5.2 [Sun] [ScII/H] Abundance [ScII/H] (Z=21.1) (G1) 46- 50 F5.2 [Sun] [TiI/H] Abundance [TiI/H] (Z=22.0) (G1) 52- 56 F5.2 [Sun] [TiII/H] Abundance [TiII/H] (Z=22.0) (G1) 58- 62 F5.2 [Sun] [V/H] Abundance [V/H] (Z=23) (G1) 64- 68 F5.2 [Sun] [CrI/H] Abundance [CrI/H] (Z=24.0) (G1) 70- 74 F5.2 [Sun] [Co/H] Abundance [Co/H] (Z=27) (G1) 76- 80 F5.2 [Sun] [Ni/H] Abundance [Ni/H] (Z=28) (G1) -------------------------------------------------------------------------------- Byte-by-byte Description of file: vel.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Star Star's identifier 10- 13 I4 km/s Ulsr U velocity of the star relative to the LSR (1) 15- 18 I4 km/s Vlsr V velocity of the star relative to the LSR (1) 20- 23 I4 km/s Wlsr W velocity of the star relative to the LSR (1) 25- 28 F4.2 --- pD1 [0/1] Probability of a star belonging to the thick disc according to B03 (2) 30- 33 F4.2 --- ptD1 [0/1] Probability of a star belonging to the thin disc according to B03 (2) 35- 38 F4.2 --- pH1 [0/1] Probability of a star belonging to the halo according to B03 (2) 40- 44 A5 --- pop1 probable population where the star belongs according to B03 (thin, thick or trans) 46- 49 F4.2 --- pD2 [0/1] Probability of a star belonging to the thick disc according to R03 (3) 51- 54 F4.2 --- ptD2 [0/1] Probability of a star belonging to the thin disc according to R03 (3) 56- 59 F4.2 --- pH2 [0/1] Probability of a star belonging to the halo according to R03 (3) 61- 65 A5 --- pop2 probable population where the star belongs according to R03 (thin, thick or trans) -------------------------------------------------------------------------------- Note (1): The Galactic space velocities were calculated using the procedure from Johnson & Soderblom (1987AJ.....93..864J) and corrected for the solar motion relative to the Local Standard of Rest (LSR) using (U',V',W')=(+11.1, +12.24, +7.25)km/s from Schonrich et al. (2010MNRAS.403.1829S). Note (2): The mean values (asymmetric drift) and dispersion in the Gaussian distribution (characteristic velocity dispersion), and the population fractions were taken from Bensby et al. (2003A&A...410..527B) Note (3): The mean values (asymmetric drift) and dispersion in the Gaussian distribution (characteristic velocity dispersion), and the population fractions were taken from Robin et al. (2003A&A...409..523R). -------------------------------------------------------------------------------- Byte-by-byte Description of file: ew.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 ----- Star Star's identifier 10- 16 F7.2 0.1nm lambda Central wavelength 18- 22 F5.1 0.1pm EW Equivalent width of the line -------------------------------------------------------------------------------- Byte-by-byte Description of file: linelist.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 A3 --- El Element and ionization state 5- 11 F7.2 0.1nm lambda [4792/6773] Central wavelength 13- 16 F4.2 eV EP Excitation potential 18- 23 F6.3 [-] loggf Oscilator strength 25- 28 F4.1 [-] Dab [-3.9/10.8] Difference in abundances between dwarfs and giants relative to {sigma} (1) -------------------------------------------------------------------------------- Note (1): Negative value means that the abundances for giant stars are lower than for dwarfs. Values are relative to the dispersion (N*{sigma}) -------------------------------------------------------------------------------- Global notes: Note (G1): Solar abundances for the selected elements: Na I : log({epsilon}_0_)=6.33 Mg I : log({epsilon}_0_)=7.58 Al I : log({epsilon}_0_)=6.47 Si I : log({epsilon}_0_)=7.55 Ca I : log({epsilon}_0_)=6.36 Sc I : log({epsilon}_0_)=3.10 Sc II : log({epsilon}_0_)=3.10 Ti I : log({epsilon}_0_)=4.99 Ti II : log({epsilon}_0_)=4.99 Mn I : log({epsilon}_0_)=5.39 Cr I : log({epsilon}_0_)=5.67 Cr II : log({epsilon}_0_)=5.67 V I : log({epsilon}_0_)=4.00 Co I : log({epsilon}_0_)=4.92 Ni I : log({epsilon}_0_)=6.25 -------------------------------------------------------------------------------- Acknowledgements: Vardan Adibekyan, Vardan.Adibekyan(at)astro.up.pt ================================================================================ (End) Vardan Adibekyan [CAUP], Patricia Vannier [CDS] 31-Mar-2015