J/A+A/564/A119 CoRoT red giants abundances (Morel+, 2014)
Atmospheric parameters and chemical properties of red giants in the CoRoT
asteroseismology fields.
Morel T., Miglio A., Lagarde N., Montalban J., Rainer M., Poretti E.,
Eggenberger P., Hekker S., Kallinger T., Mosser B., Valentini M.,
Carrier F., Hareter M., Mantegazza L.
<Astron. Astrophys. 564, A119 (2014)>
=2014A&A...564A.119M 2014A&A...564A.119M
ADC_Keywords: Stars, giant ; Equivalent widths ; Abundances
Keywords: asteroseismology - stars: fundamental parameters - stars: abundances -
stars: interiors
Abstract:
A precise characterisation of the red giants in the seismology fields
of the CoRoT satellite is a prerequisite for further in-depth seismic
modelling. High-resolution FEROS and HARPS spectra were obtained as
part of the ground-based follow-up campaigns for 19 targets holding
great asteroseismic potential. These data are used to accurately
estimate in a self-consistent manner their fundamental parameters and
the abundances of 16 chemical species. Some powerful probes of mixing
are investigated (the Li and CNO abundances, as well as the carbon
isotopic ratio in a few cases). The information provided by the
spectroscopic and seismic data is combined to provide more accurate
physical parameters and abundances. The stars in our sample follow the
general trends between various abundance ratios and the metallicity
observed in stars of the Galactic disk. After allowance is made for
the chemical evolution of the interstellar medium, the observational
signature of internal mixing phenomena is revealed through the
detection at the stellar surface of the products of the CN and, in the
case of the most massive stars, NeNa cycles. Together with the
asteroseismic constraints, these data will pave the way for a detailed
theoretical investigation of the physical processes responsible for
the transport of chemical elements in evolved, low- and
intermediate-mass stars.
Description:
The equivalent widths were measured manually assuming Gaussian
profiles or Voigt profiles for the few lines with extended damping
wings. Lines with an unsatisfactory fit or significantly affected by
telluric features were discarded. Only values eventually retained for
the analysis are provided.
For the chemical abundances, the usual notation is used:
[X/Y]=[log(ε(X))-log(ε(Y))]star -
[log(ε(X))-log(ε(Y))]☉
with logε(X)=12+log[N(X)/N(H)] (N is the number density of
the species). For lithium, the following notation is used:
[Li/H]=log(N(Li))star-log(N(Li))☉. The adopted solar
abundances are taken from Grevesse & Sauval (1998SSRv...85..161G 1998SSRv...85..161G),
except for Li for which we adopt our derived values:
log(ε(Li))☉=1.09 and 1.13 in LTE and NLTE, respectively
(see text).
All the abundances are computed under the assumption of LTE, except Li
for which values corrected for departures from LTE using the data of
Lind et al. (2009A&A...503..541L 2009A&A...503..541L) are also provided. All the quoted
error bars are 1-sigma uncertainties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 104 24 Observations and basic target parameters
tablea2.dat 32 2784 Equivalent width measurements
tablea3.dat 40 116 Line list and atomic data
tablea4.dat 123 41 Abundance data for Mg, Al, Si, Ca, Sc, Ti, Cr,
Co, Ni, and Ba
tablea5.dat 135 41 Abundance data for the mixing indicators
(Li, C, N, O, Na, and 12C/13C)
tablea6.dat 79 41 Logarithmic Abundance ratios of C, N, and O
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See also:
B/corot : CoRoT observation log Release 13 (CoRoT, 2009-2014)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD identification
9- 12 I4 --- HR ? HR (Bright Star) designation
14- 19 I6 --- HIP ? Hipparcos identification (I/311)
22- 32 A11 --- Name Star name (as in the other tables)
35- 42 A8 --- SpT MK spectral type (from Simbad)
44- 48 F5.2 mag Vmag Magnitude in theV band (from Simbad)
53- 57 F5.2 mas Plx ? Parallax
59- 62 F4.2 mas e_Plx ? Mean error on Plx
63 A1 --- n_Plx [a] Parallax of NGC 6633
(van Leeuwen 2009A&A...497..209V 2009A&A...497..209V)
66- 77 A12 --- Instr Instrument
79- 84 I6 --- R Resolving power (λ/Δλ)
87- 91 F5.3 0.1nm Broad Instrumental broadening (Å)
94- 96 I3 --- Nsp [1/181] Number of spectra
100-103 I4 --- S/N Signal/Noise at 5815Å (see associated flag)
104 A1 --- f_S/N Flag on S/N: b = mean S/N over 3600-9300Å,
c = S/N at 5500Å
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13- 17 A5 --- Ion Ion designation
19- 26 F8.3 0.1nm lambda Line wavelength λ
28- 32 F5.1 0.1pm EW ?=999.9 Equivalent width
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ion Ion designation
7- 14 F8.3 0.1nm lambda Line wavelength λ
16- 20 F5.3 eV LEP Lower excitation potential
22- 27 F6.3 [-] log(gf) Oscillator strength
29- 35 F7.3 [-] log(C6) ?=999.999 Interaction constant for
van der Waals interaction (1)
37- 40 F4.2 --- Egamma ?=9.99 Enhancement factor to the line
width parameter (to the power 5/2)
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Note (1): The interaction constants were derived from the line broadening
cross sections computed by Barklem et al. (2000A&AS..142..467B 2000A&AS..142..467B)
and Barklem & Aspelund-Johansson (2005A&A...435..373B 2005A&A...435..373B).
Value for SiI 5948.541 from Barbuy et al. (2006A&A...449..349B 2006A&A...449..349B).
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13 A1 --- Met [A/I] Method to derive logg (G1)
15- 19 F5.2 [Sun] [Mg/Fe] Abundance ratio [Mg/Fe]
21- 24 F4.2 [Sun] e_[Mg/Fe] Uncertainty on [Mg/Fe]
26- 30 F5.2 [Sun] [Al/Fe] Abundance ratio [Al/Fe]
32- 35 F4.2 [Sun] e_[Al/Fe] Uncertainty on [Al/Fe]
37- 41 F5.2 [Sun] [Si/Fe] Abundance ratio [Si/Fe]
43- 46 F4.2 [Sun] e_[Si/Fe] Uncertainty on [Si/Fe]
48- 52 F5.2 [Sun] [Ca/Fe] Abundance ratio [Ca/Fe]
54- 57 F4.2 [Sun] e_[Ca/Fe] Uncertainty on [Ca/Fe]
59- 63 F5.2 [Sun] [Sc/Fe] ?=99.99 Abundance ratio [Sc/Fe]
65- 68 F4.2 [Sun] e_[Sc/Fe] ?=9.99 Uncertainty on [Sc/Fe]
70- 74 F5.2 [Sun] [Ti/Fe] Abundance ratio [Ti/Fe]
76- 79 F4.2 [Sun] e_[Ti/Fe] Uncertainty on [Ti/Fe]
81- 85 F5.2 [Sun] [Cr/Fe] Abundance ratio [Cr/Fe]
87- 90 F4.2 [Sun] e_[Cr/Fe] Uncertainty on [Cr/Fe]
92- 96 F5.2 [Sun] [Co/Fe] Abundance ratio [Co/Fe]
98-101 F4.2 [Sun] e_[Co/Fe] Uncertainty on [Co/Fe]
103-107 F5.2 [Sun] [Ni/Fe] Abundance ratio [Ni/Fe]
109-112 F4.2 [Sun] e_[Ni/Fe] Uncertainty on [Ni/Fe]
114-118 F5.2 [Sun] [Ba/Fe] Abundance ratio [Ba/Fe]
120-123 F4.2 [Sun] e_[Ba/Fe] Uncertainty on [Ba/Fe]
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13 A1 --- Met [A/I] Method to derive logg (G1)
15- 19 F5.2 [Sun] [Li/H]E LTE Abundance ratio [Li/H]
21- 24 F4.2 [Sun] e_[Li/H]E ?=9.99 Uncertainty on [Li/H]E
26- 30 F5.2 [Sun] [Li/H]N NLTE Abundance ratio [Li/H] (2)
32- 35 F4.2 [Sun] e_[Li/H]N ?=9.99 Uncertainty on [Li/H]N (2)
37 A1 --- f_[Li/H] [L/D] Flag for upper limit (L)
or detection (D) of Lithium
39- 43 F5.2 [Sun] [C/Fe] Abundance ratio [C/Fe]
45- 48 F4.2 [Sun] e_[C/Fe] Uncertainty on [C/Fe]
50- 54 F5.2 [Sun] [C/Fe]c Corrected [C/Fe] abundance ratio (3)
56- 59 F4.2 [Sun] e_[C/Fe]c Uncertainty on [C/Fe]c (3)
61- 65 F5.2 [Sun] [N/Fe] Abundance ratio [N/Fe]
67- 70 F4.2 [Sun] e_[N/Fe] Uncertainty on [N/Fe]
72- 76 F5.2 [Sun] [OI/Fe] Abundance ratio [OI 6300/Fe]
78- 81 F4.2 [Sun] e_[OI/Fe] Uncertainty on [OI/Fe]
83- 87 F5.2 [Sun] [OI/Fe]c Corrected [OI 6300/Fe] abundance ratio (3)
89- 92 F4.2 [Sun] e_[OI/Fe]c Uncertainty on [OI/Fe]c (3)
94- 98 F5.2 [Sun] [Otr/Fe] ?=99.99 O triplet 7774Å abundance
100-103 F4.2 [Sun] e_[Otr/Fe] ?=9.99 Uncertainty on [Ott/Fe]
105-109 F5.2 [Sun] [Na/Fe] Abundance ratio [Na/Fe]
111-114 F4.2 [Sun] e_[Na/Fe] Uncertainty on [Na/Fe]
116-120 F5.2 [Sun] [Na/Fe]c Corrected [Na/Fe] abundance ratio (3)
122-125 F4.2 [Sun] e_[Na/Fe]c Uncertainty on [Na/Fe]c (3)
127-130 I4 --- 12C/13C ?=9999 12C/13C isotopic ratio
132-135 I4 --- e_12C/13C ?=9999 Uncertainty on 12C/13C
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Note (2): Lithium abundances Corrected for departures from LTE according to
Lind et al. (2009A&A...503..541L 2009A&A...503..541L).
Note (3): Corrected for the chemical evolution of the Galaxy (see text).
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Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13 A1 --- Met [A/I] Method to derive logg (G1)
15- 19 F5.2 [Sun] [N/C] Abundance ratio [N/C]
21- 24 F4.2 [Sun] e_[N/C] Uncertainty on [N/C]
26- 30 F5.2 [Sun] [N/C]c Corrected [N/C] abundance ratio (4)
32- 35 F4.2 [Sun] e_[N/C]c Uncertainty on [N/C]c (4)
37- 41 F5.2 [Sun] [N/O] Abundance ratio [N/O]
43- 46 F4.2 [Sun] e_[N/O] Uncertainty on [N/O]
48- 52 F5.2 [Sun] [N/O]c Corrected [N/O] abundance ratio (4)
54- 57 F4.2 [Sun] e_[N/O]c Uncertainty on [N/O]c (4)
59- 63 F5.2 [Sun] [C/O] Abundance ratio [C/O]
65- 68 F4.2 [Sun] e_[C/O] Uncertainty on [C/O]
70- 74 F5.2 [Sun] [C/O]c Corrected [C/O] abundance ratio (4)
76- 79 F4.2 [Sun] e_[C/O]c Uncertainty on [C/O]c (4)
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Note (4): Corrected for the chemical evolution of the Galaxy (see text).
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Global notes:
Note (G1): Method to derive logg as follows:
I = logg derived from ionisation equilibrium of Fe
A = logg derived from asteroseismology
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Acknowledgements:
Thierry Morel, morel (at) astro.ulg.ac.be
(End) Patricia Vannier [CDS] 25-Feb-2014