J/A+A/580/A24 Abundances in dwarfs, subgiants, and giants (da Silva+, 2015)
Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and
without giant planets.
da Silva R., Milone A.C., Rocha-Pinto H.J.
<Astron. Astrophys. 580, A24 (2015)>
=2015A&A...580A..24D 2015A&A...580A..24D
ADC_Keywords: Stars, fundamental ; Abundances ; Spectroscopy
Keywords: stars: fundamental parameters - stars: abundances -
planetary systems - methods: data analysis -
methods: statistical - techniques: spectroscopic
Abstract:
We have analyzed high-resolution and high signal-to-noise ratio
optical spectra of nearby FGK stars with and without detected giant
planets in order to homogeneously measure their photospheric
parameters, mass, age, and the abundances of volatile (C, N, and O)
and refractory (Na, Mg, Si, Ca, Ti, V, Mn, Fe, Ni, Cu, and Ba)
elements. Our sample contains 309 stars from the solar neighborhood
(up to the distance of 100pc), out of which 140 are dwarfs, 29 are
subgiants, and 140 are giants. The photospheric parameters are derived
from the equivalent widths (EWs) of FeI and FeII lines. Masses and
ages come from the interpolation in evolutionary tracks and isochrones
on the HR diagram. The abundance determination is based on the
equivalent widths of selected atomic lines of the refractory elements
and on the spectral synthesis of C2, CN, CI, OI, and NaI features.
We apply a set of statistical methods to analyze the abundances
derived for the three subsamples. Our results show that: i) giant
stars systematically exhibit underabundance in [C/Fe] and
overabundance in [N/Fe] and [Na/Fe] in comparison with dwarfs, a
result that is normally attributed to evolution-induced mixing
processes in the envelope of evolved stars; ii) for solar analogs
only, the abundance trends with the condensation temperature of the
elements are correlated with age and anticorrelated with the surface
gravity, which is in agreement with recent studies; iii) as in the
case of [Fe/H], dwarf stars with giant planets are systematically
enriched in [X/H] for all the analyzed elements, except for O and Ba
(the former due to limitations of statistics), confirming previous
findings in the literature that not only iron has an important
relation with the planetary formation; and iv) giant planet hosts are
also significantly overabundant for the same metallicity when the
elements from Mg to Cu are combined together.
Description:
Photospheric parameters mass, age, and the abundances of C, N, O, Na,
Mg, Si, Ca, Ti, V, Mn, Fe, Ni, Cu, and Ba for a sample of FGK dwarfs,
subgiants, and giants are derived. We used spectra of high-resolution
(R∼42,000) and high S/N (>150 on average) available in the ELODIE
online database (Moultaka et al., 2004PASP..116..693M 2004PASP..116..693M). These are
spectra collected with the ELODIE high-resolution spectrograph
(Baranne et al. 1996) of the Haute Provence Observatory (France). Only
spectra with individual S/N>20 and with an image type classified as
"object fibre only" (OBJO) were used.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 254 309 Photospheric parameters and [X/Fe] abundances
table7.dat 111 309 Photometric and evolutionary parameters together
with the population membership
table8.dat 112 120 Slopes of the linear regressions on [X/Fe] vs. Tc
table2.dat 35 178 Atomic line parameters and solar EWs
table3.dat 31 109 Atomic parameters for lines with important
hyperfine structure
table5.dat 43 9183 Atomic and molecular line parameters
table6.dat 34 57 Atomic parameters for strong atomic lines
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See also:
J/A+A/526/A71 : C abundances in G and K nearby stars (da Silva+, 2011)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name HD, BD, or HIP stellar number
13- 20 A8 --- SpType Spectral type
23- 27 F5.2 km/s Vbroad [0/15] Broadening velocity
30- 33 I4 K Teff [4169/6503] Star's effective temperature
36- 38 I3 K e_Teff [21/163] Error in star's effective temperature
41- 44 F4.2 --- logg [1/5] Star's surface gravity
47- 50 F4.2 --- e_logg [0.1/0.6] Error in the star's surface gravity
53- 56 F4.2 km/s xi [0.03/5.6] Star's microturbulent velocity ξ
59- 62 F4.2 km/s e_xi [[0.03/3] Error in microturbulent velocity
65- 69 F5.2 [Sun] [Fe/H] Abundance ratio [Fe/H]
72- 75 F4.2 [Sun] e_[Fe/H] Error in [Fe/H]
78- 82 F5.2 [Sun] [C/Fe] ? Abundance ratio [C/Fe]
85- 88 F4.2 [Sun] e_[C/Fe] ? Error in [C/Fe]
91- 95 F5.2 [Sun] [N/Fe] ? Abundance ratio [N/Fe]
98-101 F4.2 [Sun] e_[N/Fe] ? Error in [N/Fe]
104-108 F5.2 [Sun] [O/Fe] ? Abundance ratio [O/Fe]
111-114 F4.2 [Sun] e_[O/Fe] ? Error in [O/Fe]
117-121 F5.2 [Sun] [Na/Fe] ? Abundance ratio [Na/Fe]
124-127 F4.2 [Sun] e_[Na/Fe] ? Error in [Na/Fe]
130-134 F5.2 [Sun] [Mg/Fe] ? Abundance ratio [Mg/Fe]
137-140 F4.2 [Sun] e_[Mg/Fe] ? Error in [Mg/Fe]
143-147 F5.2 [Sun] [Si/Fe] ? Abundance ratio [Si/Fe]
150-153 F4.2 [Sun] e_[Si/Fe] ? Error in [Si/Fe]
156-160 F5.2 [Sun] [Ca/Fe] ? Abundance ratio [Ca/Fe]
163-166 F4.2 [Sun] e_[Ca/Fe] ? Error in [Ca/Fe]
169-173 F5.2 [Sun] [Ti/Fe] ? Abundance ratio [Ti/Fe]
176-179 F4.2 [Sun] e_[Ti/Fe] ? Error in [Ti/Fe]
182-186 F5.2 [Sun] [V/Fe] ? Abundance ratio [V/Fe]
189-192 F4.2 [Sun] e_[V/Fe] ? Error in [V/Fe]
195-199 F5.2 [Sun] [Mn/Fe] ? Abundance ratio [Mn/Fe]
202-205 F4.2 [Sun] e_[Mn/Fe] ? Error in [Mn/Fe]
208-212 F5.2 [Sun] [Ni/Fe] ? Abundance ratio [Ni/Fe]
215-218 F4.2 [Sun] e_[Ni/Fe] ? Error in [Ni/Fe]
221-225 F5.2 [Sun] [Cu/Fe] ? Abundance ratio [Cu/Fe]
228-231 F4.2 [Sun] e_[Cu/Fe] ? Error in [Cu/Fe]
J234-238 F5.2 [Sun] [Ba/Fe] ? Abundance ratio [Ba/Fe]
241-244 F4.2 [Sun] e_[Ba/Fe] ? Error in [Ba/Fe]
247-254 A8 [Sun] Class Spectral luinosity classification: dwarf,
giant or subgiant
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name HD, BD, or HIP stellar number
13- 17 F5.3 mag B-V [0.47/1.3] B-V color index
20- 24 F5.2 mag VMag [-0.71/7.7] Absolute magnitude at the V band
27- 31 F5.1 pc Dist [3/100] Heliocentric distance
34- 39 F6.3 --- BC [-0.9/0.02] Bolometric correction
42- 47 F6.3 [Lsun] logL [-1/2.3] Logarithmic luminosity
50- 54 F5.3 [Lsun] e_logL [0.005/0.09] Error in the logarithmic luminosity
57- 60 F4.2 Msun Mass [0.6/3.6]? Mass of the star
63- 66 F4.2 Msun e_Mass [0.01/9.99]? Error in the stellar mass
69- 72 F4.1 Gyr Age [0.1/32]? Age of the star
75- 78 F4.1 Gyr e_Age [0/12]? Lower error in the stellar age
81- 84 F4.1 Gyr E_Age [0/12]? Upper error in the stellar age
87- 96 A10 --- Popul Population membership (thin, thick or a
transition population thin/thick)
99-106 A8 --- Rem Remarks on some special cases (1)
109-111 A3 --- Ref References related to the special cases (2)
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Note (1): The special cases are:
a = errors in age are larger than 4Gyr (not used in the analysis)
b = star located outside the evolutionary tracks and isochrones used
c = star hosting at least one giant planet
d = member of a stellar moving group:
U: Ursa Major; P: Pleiades; H: Hyades; W: Wolf 630
e = subdwarf candidate
Note (2): The references for some of the special cases are as follows:
1 = http://exoplanet.eu, for case c
2 = Montes et al. (2001MNRAS.328...45M 2001MNRAS.328...45M), for cases d (U), d (P)
3 = Sandage & Fouts (1986AJ.....91.1140S 1986AJ.....91.1140S), for case e
4 = Eggen (1950ApJ...111...65E 1950ApJ...111...65E), for case d (H)
5 = Bubar & King (2010AJ....140..293B 2010AJ....140..293B), for case d (W)
6 = Madsen et al. (2002A&A...381..446M 2002A&A...381..446M), for case d (H)
7 = Jao et al. (2009AJ....137.3800J 2009AJ....137.3800J), for case e
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name HD, BD, or HIP stellar number
13- 21 F9.6 --- slope0 Slope of the regressions before CCE (1)
24- 31 F8.6 --- e_slope0 Error in the slopes
34- 38 F5.2 --- r0 [-1/1] Correlation coefficient
41- 44 F4.2 --- std0 [0.01/0.15] Standard deviation of regressions
47- 55 F9.6 --- slope1 Slope of the regression after CCE, age-based (1)
58- 65 F8.6 --- e_slope1 Error in the slopes
68- 72 F5.2 --- r1 [-1/1] Correlation coefficient
75- 78 F4.2 --- std1 [0.02/0.15] Standard deviation of regressions
81- 89 F9.6 --- slope2 Slope of the regression after CCE,
[Fe/H]-based (1)
92- 99 F8.6 --- e_slope2 Error in the slopes
102-106 F5.2 --- r2 [-1/1] Correlation coefficient
109-112 F4.2 --- std2 [0.01/0.13] Standard deviation of regressions
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Note (1): CCE = correction for the Galactic chemical evolution effects;
the chemical correction is based on age or on metallicity ([Fe/H]).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 F8.2 0.1nm lambda0 [4518/6753] Spectral line central wavelength
11- 14 A4 --- Line Atomic line identification
17- 20 F4.2 eV chi [0/5.7] Lower-level excitation potential χ
23- 28 F6.3 --- loggf ? Logarithmic statistical weight of the lower
level multiplied by the oscillator strength
31- 35 F5.1 0.1pm EW [5/122] Solar equivalent width (mÅ)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Line Atomic line identification
7- 13 F7.2 0.1nm lambda0 [4571/6286] Spectral line central wavelength
16- 23 F8.3 0.1nm lambda [4571/6286] Hyperfine component wavelength
26- 31 F6.3 --- loggf Logarithmic statistical weight of the lower
level multiplied by the oscillator strength
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 10 F10.4 0.1nm lambda0 [4200/6315] Spectral line central wavelength
13- 17 F5.1 --- Line Atomic and molecular line identification
20- 25 F6.3 eV chi [0/40] Excitation potential χ
28- 36 E9.3 [-] loggf Logarithmic statistical weight of the lower
level multiplied by the oscillator strength
39- 43 F5.3 eV D0 ? Dissociation energy for molecular features
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 10 F10.4 0.1nm lambda0 S[4200/6163] pectral line central wavelength
13- 16 F4.1 --- Line Atomic and molecular line identification
19- 23 F5.3 eV chi [0/4.5] Excitation potential χ
26- 34 E9.3 [-] loggf Logarithmic statistical weight of the lower
level multiplied by the oscillator strength
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Acknowledgements:
Ronaldo da Silva, ron.oliveirasilva(at)gmail.com
(End) Patricia Vannier [CDS] 28-May-2015