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J/A+A/497/563       Chemical abundances of 451 stars         (Neves+, 2009)

Chemical abundances of 451 stars from the HARPS GTO planet search program. Thin disc, thick disc, and planets. Neves V., Santos N.C., Sousa S.G., Correia A.C.M., Israelian G. <Astron. Astrophys., 497, 563-581 (2009)> =2009A&A...497..563N
ADC_Keywords: Stars, nearby ; Planets ; Space velocities ; Abundances, peculiar Keywords: stars: abundances - stars: chemically peculiar - stars: fundamental parameters - stars: planetary systems - galaxy: disc - galaxy: kinematics and dynamics - galaxy: solar neighbourhood Abstract: We present a uniform study of the chemical abundances of 12 elements (Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Na, Mg, and Al) derived from the spectra of 451 stars observed as part of one of the HARPS GTO planet search programs. Sixty eight of these are planet-bearing stars. The main goals of our work are: i) the investigation of possible differences between the abundances of stars with and without planets; ii) the study of the possible differences in the abundances of stars in the thin and the thick disc. We confirm that there is a systematically higher metallicity in planet host stars, when compared to non planet-hosts, common to all studied species. We also found that there is no difference in the galactic chemical evolution trends of the stars with and without planets. Stars that harbour planetary companions simply appear to be in the high metallicity tail of the distribution. We also confirm that Neptunian and super-Earth class planets may be easier to find at lower metallicities. A statistically significative abundance difference between stars of the thin and the thick disc was found for [Fe/H]<0. However, the populations from the thick and the thin disc cannot be clearly separated. Description: The file table1.dat lists the parameters used to assign the Galactic population to which each star belongs. Columns 2, 3, and 4 list the U,V and W velocities relative to the local standard of rest (LSR). Columns 5, 6, and 7 list the Gaussian distributions of each population: thin disc, thick disc, and halo, respectively. In Cols. 8 and 9, we provide the relative probabilities of the thick disc relative to the thin disc and of the thick disc relative to the halo. The last column depicts the probable population where each star belongs. The file table3.dat lists the derived abundances of the elements, rms, and number of measured lines for each star. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 93 451 Parameters to assign the stars to a Galactic population table2.dat 32 180 Atomic parameters for lines selected in the paper table3.dat 225 451 Abundances, rms, and number of lines for each star and element
See also: J/A+A/275/101 : Chemical evolution of Galactic disk I. (Edvardsson+ 1993) J/A+AS/102/603 : Chemical evolution of Galactic disk II. (Edvardsson+ 1993) J/A+A/392/491 : Galactic abundance gradient. III. (Andrievsky+, 2002) J/A+A/410/527 : Abundances in the Galactic disk (Bensby+, 2003) J/A+A/413/159 : Galactic abundance gradient. V. (Andrievsky+, 2004) J/A+A/418/551 : Galactic disk stars abund. & velocities (Mishenina+, 2004) J/AJ/128/1177 : Galactic stellar abundances (Venn+, 2004) J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 10 A10 ----- Star HD or HIP name of the star 12- 19 F8.3 km/s Ulsr U velocity of the star relative to the LSR (1) 21- 28 F8.3 km/s Vlsr V velocity of the star relative to the LSR (1) 30- 37 F8.3 km/s Wlsr W velocity of the star relative to the LSR (1) 39- 46 E8.3 ----- fD Distribution of the thin disc population (2) 48- 55 E8.3 ----- fTD Distribution of the thick disc population (2) 57- 64 E8.3 ----- fH Distribution of the halo population (2) 66- 73 F8.3 ----- TDD Probability of a star belonging to the thick disc relative to the thin disk 75- 82 F8.3 ----- TDH Probability of a star belonging to the thick disc relative to the halo 84- 93 A10 ----- pop probable population where the star belongs
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')=(+10.00,+5.25,+7.17)km/s from Dehnen & Binney (1998MNRAS.298..387D). Note (2): The selection of the different populations was completed using the method proposed by Bensby (2003, Cat. J/A+A/410/527, 2005, Cat. J/A+A/433/185).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 5 A5 --- El Element (1) 8- 14 F7.2 0.1nm lambda Central wavelength 16- 19 F4.2 --- EP Excitation potential 21- 26 F6.3 --- loggf Oscilator strength 28- 32 F5.1 0.1pm EWsun Solar equivalent width
Note (1): Abundances for selected elements as follows: Na I : log(eps0)=6.33 Mg I : log(eps0)=7.58 Al I : log(eps0)=6.47 Si I : log(eps0)=7.55 Ca I : log(eps0)=6.36 Sc I : log(eps0)=3.10 Sc II : log(eps0)=3.10 Ti I : log(eps0)=4.99 Ti II : log(eps0)=4.99 Mn I : log(eps0)=5.39 Cr I : log(eps0)=5.67 Cr II : log(eps0)=5.67 V I : log(eps0)=4.00 Co I : log(eps0)=4.92 Ni I : log(eps0)=6.25
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Star HD or HIP name of the star 12- 17 F6.3 [Sun] [Si/H] Abundance [Si/H] (Z=14) 19- 22 F4.2 [Sun] e_[Si/H] rms uncertainty of [Si/H] 24- 25 I2 --- o_[Si/H] Number of SiI lines used 27- 32 F6.3 [Sun] [Ca/H] Abundance [Ca/H] (Z=20) 34- 37 F4.2 [Sun] e_[Ca/H] rms uncertainty of [Ca/H] 39- 40 I2 --- o_[Ca/H] Number of CaI lines used 42- 47 F6.3 [Sun] [ScI/H] Abundance [ScI/H] (Z=21.0) 49- 52 F4.2 [Sun] e_[ScI/H] rms uncertainty of [ScI/H] 54 I1 --- o_[ScI/H] Number of ScI lines used 56- 61 F6.3 [Sun] [ScII/H] Abundance [ScII/H] (Z=21.1) 63- 66 F4.2 [Sun] e_[ScII/H] rms uncertainty of [ScII/H] 68 I1 --- o_[ScII/H] Number of ScII lines used 70- 75 F6.3 [Sun] [TiI/H] Abundance [TiI/H] (Z=22.0) 77- 80 F4.2 [Sun] e_[TiI/H] rms uncertainty of [TiI/H] 82- 83 I2 --- o_[TiI/H] Number of TiI lines used 85- 90 F6.3 [Sun] [TiII/H] Abundance [TiII/H] (Z=22.1) 92- 95 F4.2 [Sun] e_[TiII/H] rms uncertainty of [TiII/H] 97 I1 --- o_[TiII/H] Number of TiII lines used 99-104 F6.3 [Sun] [V/H] Abundance [V/H] (Z=23) 106-109 F4.2 [Sun] e_[V/H] rms uncertainty of [V/H] 111 I1 --- o_[V/H] Number of VI lines used 113-118 F6.3 [Sun] [CrI/H] Abundance [CrI/H] (Z=24.0) 120-123 F4.2 [Sun] e_[CrI/H] rms uncertainty of [CrI/H] 125-126 I2 --- o_[CrI/H] Number of CrI lines used 128-133 F6.3 [Sun] [CrII/H] Abundance [CrII/H] (Z=24.1) 135-138 F4.2 [Sun] e_[CrII/H] rms uncertainty of [CrII/H] 140 I1 --- o_[CrII/H] Number of CrII lines used 142-147 F6.3 [Sun] [Mn/H] Abundance [Mn/H] (Z=25) 149-152 F4.2 [Sun] e_[Mn/H] rms uncertainty of [Mn/H] 154 I1 --- o_[Mn/H] Number of MnI lines used 156-161 F6.3 [Sun] [Co/H] Abundance [Co/H] (Z=27) 163-166 F4.2 [Sun] e_[Co/H] rms uncertainty of [Co/H] 168 I1 --- o_[Co/H] Number of CoI lines used 170-175 F6.3 [Sun] [Ni/H] Abundance [Ni/H] (Z=28) 177-180 F4.2 [Sun] e_[Ni/H] rms uncertainty of [Ni/H] 182-183 I2 --- o_[Ni/H] Number of NiI lines used 185-190 F6.3 [Sun] [Na/H] Abundance [Na/H] (Z=11) 192-195 F4.2 [Sun] e_[Na/H] rms uncertainty of [Na/H] 197 I1 --- o_[Na/H] Number of Na lines used 199-204 F6.3 [Sun] [Mg/H] Abundance [Mg/H] (Z=12) 206-209 F4.2 [Sun] e_[Mg/H] rms uncertainty of [Mg/H] 211 I1 --- o_[Mg/H] Number of MgI lines used 213-218 F6.3 [Sun] [Al/H] Abundance [Al/H] (Z=13) 220-223 F4.2 [Sun] e_[Al/H] rms uncertainty of [Al/H] 225 I1 --- o_[Al/H] Number of AlI lines used
Acknowledgements: Vasco Neves, vasco(at) History: 19-Jan-2010: table2 added
(End) Vasco Neves [CAUP/U. Aveiro, Portugal], Patricia Vannier [CDS] 29-May-2009
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