J/A+A/545/A32 Chemical abundances of 1111 FGK stars (Adibekyan+, 2012)
Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program.
Galactic stellar populations and planets.
Adibekyan V.Zh., Sousa S.G., Santos N.C., Delgado Mena E.,
Gonzalez Hernandez J.I., Israelian G., Mayor M., Khachatryan G.
<Astron. Astrophys. 545, A32 (2012)>
=2012A&A...545A..32A 2012A&A...545A..32A
ADC_Keywords: Stars, nearby ; Stars, double and multiple ; Space velocities ;
Abundances, peculiar
Keywords: stars: abundances - planetary systems -
stars: fundamental parameters - Galaxy: disk - solar neighborhood -
stars: kinematics and dynamics
Abstract:
We performed a uniform and detailed abundance analysis of 12
refractory elements (Na, Mg, Al, Si, Ca, Ti, Cr, Ni, Co, Sc, Mn and V)
for a sample of 1111 FGK dwarf stars from the HARPS GTO planet search
program. 109 of these stars are known to harbour giant planetary
companions and 26 stars are hosting exclusively Neptunians and
super-Earths. The main goals of this paper are i) to investigate
whether there are any differences between the elemental abundance
trends for stars of different stellar populations; ii) to characterise
the planet host and non-host samples in term of their [X/H]. The
extensive study of this sample, focused on the abundance differences
between stars with and without planets will be presented in a parallel
paper. The equivalent widths of spectral lines are automatically
measured from HARPS spectra with the ARES code. The abundances of the
chemical elements are determined using a LTE abundance analysis
relative to the Sun, with the 2010 revised version of the spectral
synthesis code MOOG and a grid of Kurucz ATLAS9 atmospheres. To
separate the Galactic stellar populations we applied both a purely
kinematical approach and a chemical method. We found that the
chemically separated (based on the Mg, Si, and Ti abundances) thin and
thick discs are also chemically disjunct for Al, Sc, Co and Ca. Some
bifurcation might also exist for Na, V, Ni, and Mn, but there is no
clear boundary of their [X/Fe] ratios. We confirm that an
overabundance in giant-planet host stars is clear for all the studied
elements. We also confirm that stars hosting only Neptunian-like
planets may be easier to detect around stars with similar
metallicities as non-planet hosts, although for some elements
(particulary alpha-elements) the lower limit of [X/H] are very abrupt.
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 table4.dat lists the derived abundances of the elements, rms,
and number of measured lines for each star.
The file table5.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 2003A&A...410..527B) and
Robin (2003A&A...409..523R 2003A&A...409..523R) criteria.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 310 1111 Abundances, rms, and number of lines for each
star and element
table5.dat 67 1111 Parameters to assign the stars to a Galactic
population
ew.dat 24 179638 Equivalent widths of the spectral lines used to
derive abundances
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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)
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Star Star's identifier
12- 15 I4 K Teff Effective Temperature (1)
17- 20 F4.2 [cm/s2] logg Surface gravity (1)
22- 26 F5.2 --- [Fe/H] Iron abundance [Fe/H] (1)
28- 31 F4.2 km/s Vtur Turbulence speed (1)
33- 38 F6.3 [Sun] [Na/H] ? Abundance [Na/H] (Z=11) (2)
40- 44 F5.3 [Sun] e_[Na/H] ? rms uncertainty of [Na/H]
46 I1 --- o_[Na/H] ? Number of Na lines used
48- 53 F6.3 [Sun] [Na/H]c ? Abundance [Na/H] after correction for
effective temperature trend (3)
55- 60 F6.3 [Sun] [Mg/H] Abundance [Mg/H] (Z=12) (2)
62- 66 F5.3 [Sun] e_[Mg/H] rms uncertainty of [Mg/H]
68 I1 --- o_[Mg/H] Number of MgI lines used
70- 75 F6.3 [Sun] [Al/H] ? Abundance [Al/H] (Z=13) (2)
77- 81 F5.3 [Sun] e_[Al/H] ? rms uncertainty of [Al/H]
83 I1 --- o_[Al/H] ? Number of AlI lines used
85- 90 F6.3 [Sun] [Al/H]c ? Abundance [Al/H] after correction for
effective temperature trend (3)
92- 97 F6.3 [Sun] [Si/H] Abundance [Si/H] (Z=14)(2)
99-103 F5.3 [Sun] e_[Si/H] rms uncertainty of [Si/H]
105-106 I2 --- o_[Si/H] Number of SiI lines used
108-113 F6.3 [Sun] [Ca/H] Abundance [Ca/H] (Z=20)(2)
115-119 F5.3 [Sun] e_[Ca/H] rms uncertainty of [Ca/H]
121-122 I2 --- o_[Ca/H] Number of CaI lines used
124-129 F6.3 [Sun] [ScI/H] ? Abundance [ScI/H] (Z=21.0) (2)
131-135 F5.3 [Sun] e_[ScI/H] ? rms uncertainty of [ScI/H]
137 I1 --- o_[ScI/H] ? Number of ScI lines used
139-144 F6.3 [Sun] [ScI/H]c ? Abundance [ScI/H] after correction for
effective temperature trend (3)
146-151 F6.3 [Sun] [ScII/H] Abundance [ScII/H] (Z=21.1)(2)
153-157 F5.3 [Sun] e_[ScII/H] rms uncertainty of [ScII/H]
159 I1 --- o_[ScII/H] Number of ScII lines used
161-166 F6.3 [Sun] [TiI/H] Abundance [TiI/H] (Z=22.0) (2)
168-172 F5.3 [Sun] e_[TiI/H] rms uncertainty of [TiI/H]
174-175 I2 --- o_[TiI/H] Number of TiI lines used
177-182 F6.3 [Sun] [TiI/H]c Abundance [TiI/H] after correction for
effective temperature trend (3)
184-189 F6.3 [Sun] [TiII/H] Abundance [TiII/H] (Z=22.1) (2)
191-195 F5.3 [Sun] e_[TiII/H] rms uncertainty of [TiII/H]
197 I1 --- o_[TiII/H] Number of TiII lines used
199-204 F6.3 [Sun] [V/H] ? Abundance [V/H] (Z=23) (2)
206-210 F5.3 [Sun] e_[V/H] ? rms uncertainty of [V/H]
212 I1 --- o_[V/H] ? Number of VI lines used
214-219 F6.3 [Sun] [V/H]c ? Abundance [V/H] after correction for
effective temperature trend (3)
221-226 F6.3 [Sun] [CrI/H] Abundance [CrI/H] (Z=24.0) (2)
228-232 F5.3 [Sun] e_[CrI/H] rms uncertainty of [CrI/H]
234-235 I2 --- o_[CrI/H] Number of CrI lines used
237-242 F6.3 [Sun] [CrII/H] Abundance [CrII/H] (Z=24.1) (2)
244-248 F5.3 [Sun] e_[CrII/H] rms uncertainty of [CrII/H]
250 I1 --- o_[CrII/H] Number of CrII lines used
252-257 F6.3 [Sun] [CrII/H]c Abundance [CrII/H] after correction for
effective temperature trend (3)
259-264 F6.3 [Sun] [Mn/H] Abundance [Mn/H] (Z=25)(2)
266-270 F5.3 [Sun] e_[Mn/H] rms uncertainty of [Mn/H]
272 I1 --- o_[Mn/H] Number of MnI lines used
274-279 F6.3 [Sun] [Co/H] ? Abundance [Co/H] (Z=27) (2)
281-285 F5.3 [Sun] e_[Co/H] ? rms uncertainty of [Co/H]
287 I1 --- o_[Co/H] ? Number of CoI lines used
289-294 F6.3 [Sun] [Co/H]c ? Abundance [Co/H] after correction for
effective temperature trend (3)
296-301 F6.3 [Sun] [Ni/H] Abundance [Ni/H] (Z=28) (2)
303-307 F5.3 [Sun] e_[Ni/H] rms uncertainty of [Ni/H]
309-310 I2 --- o_[Ni/H] Number of NiI lines used
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Note (1): The stellar parameters for the stars were taken from Sousa et al.
(2008A&A...487..373S 2008A&A...487..373S, 2011A&A...526A..99S 2011A&A...526A..99S, 2011A&A...533A.141S 2011A&A...533A.141S)
Note (2): Abundances for selected elements are:
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
Note (3): Abundances for the elements after correction for the systematic
trends with effective temperature.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 ----- Star Star's identifier
12- 15 I4 km/s Ulsr U velocity of the star relative to the LSR (4)
17- 20 I4 km/s Vlsr V velocity of the star relative to the LSR (4)
22- 25 I4 km/s Wlsr W velocity of the star relative to the LSR (4)
27- 30 F4.2 ----- pDB Probability of a star belonging to the thick
disc according to B03 (5)
32- 35 F4.2 ----- pTDB Probability of a star belonging to the thin
disc according to B03 (5)
37- 40 F4.2 ----- pHB Probability of a star belonging to the halo
according to B03 (5)
42- 46 A5 ----- popB probable population where the star belongs
according to B03 (halo, thin, thick, trans) (5)
48- 51 F4.2 ----- pDR Probability of a star belonging to the thick disc
according to R03 (6)
53- 56 F4.2 ----- pTDR Probability of a star belonging to the thin disc
according to R03 (6)
58- 61 F4.2 ----- pHR Probability of a star belonging to the halo
according to R03 (6)
63- 67 A5 ----- popR probable population where the star belongs
according to R03 (halo, thin, thick, trans) (6)
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Note (4): The Galactic space velocities were calculated using the procedure
from Johnson & Soderblom (1987AJ.....93..864J 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 2010MNRAS.403.1829S).
Note (5): 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 2003A&A...410..527B).
Note (6): 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 2003A&A...409..523R).
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Byte-by-byte Description of file: ew.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 ----- Star Star's identifier
12- 18 F7.2 0.1nm lambda Central wavelength (Å)
20- 24 F5.1 0.1pm EW Equivalent width of the line (mÅ)
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Acknowledgements:
Vardan Adibekyan, Vardan.Adibekyan(at)astro.up.pt
(End) Vardan Adibekyan [CAUP], Patricia Vannier [CDS] 13-Jul-2012