J/MNRAS/423/122 Abundances of 93 solar-type Kepler targets (Bruntt+, 2012)
Accurate fundamental parameters and detailed abundance patterns from
spectroscopy of 93 solar-type Kepler targets.
Bruntt H., Basu S., Smalley B., Chaplin W.J., Verner G.A., Bedding T.R.,
Catala C., Gazzano J.-C., Molenda-Zakowicz J., Thygesen A.O.,
Uytterhoeven K., Hekker S., Huber D., Karoff C., Mathur S., Mosser B.,
Appourchaux T., Campante T.L., Elsworth Y., Garcia R.A., Handberg R.,
Metcalfe T.S., Quirion P.-O., Regulo C., Roxburgh I.W., Stello D.,
Christensen-Dalsgaard J., Kawaler S.D., Kjeldsen H., Morris R.L.,
Quintana E.V., Sanderfer D.T.
<Mon. Not. R. Astron. Soc., 423, 122-131 (2012)>
=2012MNRAS.423..122B 2012MNRAS.423..122B
ADC_Keywords: Stars, dwarfs ; Stars, G-type ; Abundances
Keywords: stars: abundances - stars: atmospheres -
stars: fundamental parameters - stars: solar-type
Abstract:
We present a detailed spectroscopic study of 93 solar-type stars that
are targets of the NASA/Kepler mission and provide detailed chemical
composition of each target. We find that the overall metallicity is
well represented by Fe lines. Relative abundances of light elements
(CNO) and α elements are generally higher for low-metallicity
stars. Our spectroscopic analysis benefits from the accurately
measured surface gravity from the asteroseismic analysis of the Kepler
light curves. The accuracy on the log g parameter is better than
0.03dex and is held fixed in the analysis.
Description:
The spectra were obtained with the ESPaDOnS spectrograph at the 3.6-m
Canada-France-Hawaii Telescope (CFHT) in USA and with the NARVAL
spectrograph mounted on the 2-m Bernard Lyot Telescope at the Pic du
Midi Observatory in France. In both the facilities, the observations
were carried out as service observations from May to September in
2010.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 37 1042 Atomic data used in the spectral analysis
table3.dat 96 93 Observed targets and their properties
table4.dat 218 186 Abundances relative to the Sun and the number of
lines used for 13 elements
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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2- 5 A4 --- El Element with ionization state
8- 15 F8.3 0.1nm lambda wavelength λ (Å)
17- 22 F6.3 eV Ep excitation potential
24- 29 F6.3 [-] loggfV Oscillator strength from VALD
31- 37 F7.3 [-] loggf Adjusted oscillator strength value
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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- 8 I8 --- KIC KIC number (Cat. V/133)
10- 14 I5 --- HIP ? HIP number (Cat. I/311)
16- 21 I6 --- HD ? HD number (Cat. III/135)
23- 28 F6.3 mag VTmag Tycho V magnitude
30- 34 F5.3 mag VT-K VT-Ks colour index
36- 39 F4.2 mag E(B-V) ? B-V colour excess
41- 44 F4.2 mag e_E(B-V) ? rms uncertainty on E(B-V)
46- 49 I4 K Teff1 ? Effective temperature from KIC
51- 54 F4.2 [cm/s2] logg1 ? Gravity surface from KIC
56- 60 F5.2 [Sun] [Fe/H]1 ? Metallicity from KIC
62- 65 I4 K Teff2 Effective temperature from spectroscopy
(±70K)
67- 70 F4.2 [cm/s2] logg2 Gravity surface from spectroscopy (±0.08dex)
72- 75 I4 K Teff Final (asteroseismic) effective temperature
(±60K)
77- 80 F4.2 [cm/s2] logg Final (asteroseismic) gravity surface
(±0.03dex)
82- 86 F5.2 [-] [Fe/H] Final (asteroseismic) metallicity (±0.06dex)
88- 91 F4.2 km/s xi Final (asteroseismic) microturbulent velocity
ξ (±0.06km/s) (1)
93- 96 F4.1 km/s vsini Final (asteroseismic) rotational velocity (1)
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Note (1): We only list the `asteroseismic' values of vsini and xi, since
the `spectroscopic' values are almost identical.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC number (1)
10 I1 --- Ion [1/2] Ionisation state:
1 for neutral, 2 for singly-ionized
12- 16 F5.2 [Sun] Li ?=- Lithum abundance (2)
19- 22 F4.2 [Sun] e_Li ?=- rms uncertainty on Li
24- 26 I3 --- o_Li ?=- Number of lines used for Li
28- 32 F5.2 [Sun] C ?=- Carbon abundance (2)
35- 38 F4.2 [Sun] e_C ?=- rms uncertainty on C
40- 42 I3 --- o_C ?=- Number of lines used for C
44- 48 F5.2 [Sun] N ?=- Nitrogen abundance (2)
51- 54 F4.2 [Sun] e_N ?=- rms uncertainty on N
56- 58 I3 --- o_N ?=- Number of lines used for N
60- 64 F5.2 [Sun] O ?=- Oxygen abundance (2)
67- 70 F4.2 [Sun] e_O ?=- rms uncertainty on O
72- 74 I3 --- o_O ?=- Number of lines used for O
76- 80 F5.2 [Sun] Na ?=- Sodium abundance (2)
83- 86 F4.2 [Sun] e_Na ?=- rms uncertainty on Na
88- 90 I3 --- o_Na ?=- Number of lines used for Na
92- 96 F5.2 [Sun] Mg ?=- Magnesium abundance (2)
99-102 F4.2 [Sun] e_Mg ?=- rms uncertainty on Mg
104-106 I3 --- o_Mg ?=- Number of lines used for Mg
108-112 F5.2 [Sun] Si ?=- Silicium abundance (2)
115-118 F4.2 [Sun] e_Si ?=- rms uncertainty on Si
120-122 I3 --- o_Si ?=- Number of lines used for Si
124-128 F5.2 [Sun] Ca ?=- Calcium abundance (2)
131-134 F4.2 [Sun] e_Ca ?=- rms uncertainty on Ca
136-138 I3 --- o_Ca ?=- Number of lines used for Ca
140-144 F5.2 [Sun] Ti ?=- Titanium abundance (2)
147-150 F4.2 [Sun] e_Ti ?=- rms uncertainty on Ti
152-154 I3 --- o_Ti ?=- Number of lines used for Ti
156-160 F5.2 [Sun] V ?=- Vanadium abundance (2)
163-166 F4.2 [Sun] e_V ?=- rms uncertainty on V
168-170 I3 --- o_V ?=- Number of lines used for V
172-176 F5.2 [Sun] Cr ?=- Chromium abundance (2)
179-182 F4.2 [Sun] e_Cr ?=- rms uncertainty on Cr
184-186 I3 --- o_Cr ?=- Number of lines used for Cr
188-192 F5.2 [Sun] Fe ?=- Iron abundance (2)
195-198 F4.2 [Sun] e_Fe ?=- rms uncertainty on Fe
200-202 I3 --- o_Fe ?=- Number of lines used for Fe
204-208 F5.2 [Sun] Ni ?=- Nickel abundance (2)
211-214 F4.2 [Sun] e_Ni ?=- rms uncertainty on Ni
216-218 I3 --- o_Ni ?=- Number of lines used for Ni
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Note (1): For each star there are two rows: One for the neutral species and
one for the singly-ionized species (for example Fe 1 and Fe 2).
Note (2): All abundances are relative to the Solar values.
"---" means that no lines were available to determine the abundance.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 31-Mar-2013