J/A+A/523/A91 CoRoT/Exoplanet fields with MATISSE (Gazzano+, 2010)
Stellar characterization of CoRoT/Exoplanet fields with MATISSE.
Gazzano J.-C., de Laverny P., Deleuil M., Recio-Blanco A., Bouchy F.,
Moutou C., Bijaoui A., Ordenovic C., Gandoli D., Loeillet B.
<Astron. Astrophys. 523, A91 (2010)>
=2010A&A...523A..91G 2010A&A...523A..91G
ADC_Keywords: Galaxies, photometry ; Photometry, CCD
Keywords: techniques: spectroscopic -
stars: fundamental parameters - planetary systems - general
Abstract:
The homogeneous spectroscopic determination of the stellar parameters
is a mandatory step for transit detections from space. Knowledge of
which population the planet hosting stars belong to places constraints
on the formation and evolution of exoplanetary systems. We used the
FLAMES/GIRAFFE multi-fiber instrument at ESO to spectroscopically
observe samples of stars in three CoRoT/Exoplanet fields, namely the
LRa01, LRc01, and SRc01 fields, and characterize their stellar
populations. We present accurate atmospheric parameters, Teff, logg,
[M/H], and [alpha/Fe] derived for 1227 stars in these fields using
the MATISSE algorithm. The latter is based on the spectral synthesis
methodology and automatically provides stellar parameters for large
samples of observed spectra. We trained and applied this algorithm to
FLAMES observations covering the MgIb spectral range. It was
calibrated on reference stars and tested on spectroscopic samples from
other studies in the literature. The barycentric radial velocities and
an estimate of the vsini values were measured using cross-correlation
techniques. We corrected our samples in the LRc01 and LRa01 CoRoT
fields for selection effects to characterize their FGK dwarf stars
population, and compiled the first unbiased reference sample for the
in-depth study of planet metallicity relationship in these CoRoT
fields. We conclude that the FGK dwarf population in these fields
mainly exhibit solar metallicity. We show that for transiting planet
finding missions, the probability of finding planets as a function of
metallicity could explain the number of planets found in the LRa01 and
LRc01 CoRoT fields. This study demonstrates the potential of
multi-fiber observations combined with an automated classifier such as
MATISSE for massive spectral classification.
Description:
Atomic data modifications from VALD initial request, atmospheric
parameters for 1227 CoRoT targets, radial velocity for 1534 CoRoT
targets, and Vsini for 1604 CoRoT targets in three CoRoT/Exoplanet
fields LRa01, LRc01, and SRc01. The reported uncertainties are only
internal errors.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 29 304 *List of the modified atomic data
table9.dat 121 1604 Atmospheric parameters, radial velocities, and
vsini for the CoRoT targets
table9.fits 2880 38 Fits version of table9
table10.dat 56 90 Derived parameters for the S4N sample from
Allende Prieto et al. (2004, Cat. J/A+A/420/183)
and the Sun
table11.dat 51 118 Derived parameters for the Elodie3.1 sample
from Prugniel et al. (2007, 0703658)
table13.dat 57 39 Derived parameters for the Santos et al.
(2009A&A...493..309S 2009A&A...493..309S) sample
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Note on table4.dat: The lines not reported here are the values from VALD.
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See also:
B/corot : CoRoT observation log Release 7 (CoRoT, 2010)
J/AJ/134/766 : BEST variable stars in LRc1 field (Karoff+, 2007)
J/AJ/134/1560 : BEST periodic variable stars in IR01 field (Kabath+, 2007)
J/AJ/136/654 : BEST periodic variable stars in LRa1 field (Kabath+, 2008)
J/AJ/137/3911 : BEST periodic variable stars in LRc2 field (Kabath+, 2009)
J/A+A/506/569 : BEST-II periodic variables in CoRoT LRa02 field (Kabath+, 2009)
J/A+A/506/501 : Eclipsing binaries in CoRoT-LRc01 field (Cabrera+, 2009)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element name
4- 5 A2 --- Ion State of ionisation (I=1, II=2)
7- 14 F8.3 0.1nm lambda Center wavelength of the line
16- 21 F6.3 eV EP Excitation potential (not modified VALD value)
23- 29 F7.3 [-] log(gf) Modified oscillator strength
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- CoRoT Star identification in CoRoT catalogue EXO-DAT
11 A1 --- l_vsini Limit flag on vsini (1)
12- 15 F4.1 km/s vsini vsini measure
17- 18 A2 --- q_vsini [123+ ] Quality flag on the vsini (2)
19- 23 A5 --- --- [eq(3)]
25- 35 E11.5 km/s BRV ?=- Barycentric radial velocity
37- 45 E9.4 km/s e_BRV ?=- Uncertainty on barycentric radial velocity
47- 55 E9.4 K Teff ?=- Effective temperature (3)
57- 63 E7.2 K e_Teff ?=- Uncertainty on effective temperature (4)
65- 72 E8.3 [cm/s2] logg ?=- Surface gravity (3)
74- 80 E7.2 [cm/s2] e_logg ?=- Uncertainty on the surface gravity (4)
82- 90 E9.3 [-] [M/H] ?=- Overall metallicity (3)
92- 96 E5.1 [-] e_[M/H] ?=- Uncertainty on the overall metallicity (4)
98-105 E8.3 [-] alpha ?=- α enhancement [alpha/Fe](3)
107-111 E5.1 [-] e_alpha ?=- Uncertainty on the α enhancement (4)
113-121 E9.4 --- SNR Signal to noise ratio of the observed spectrum
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Note (1): >40km/s if the CCF was too large for the measure to be precise.
Note (2): Quality flag as follows:
1 = vsini estimate is not affected by noise or a second component in the CCF
2 = the target is a SB2 and the vsini is related to the main component
of the CCF
3 = the contrast and shape of the CCF are insufficient to assure a
proper estimate of its parameters
If followed by '+', the fit for fast rotators was used (Eq.(3))
Note (3): Atmospheric parameters measured by MATISSE
Note (4): Internal error only
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Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP HIPPARCOS identification number (0 for the Sun)
8- 11 I4 K Teff2 Effective temperature measured by
Allende Prieto et al. (J/A+A/420/183)
13- 17 F5.3 [cm/s2] logg2 Surface gravity measured by
Allende Prieto et al. (J/A+A/420/183)
19- 24 F6.3 [-] [Fe/H]2 Metallicity measured by
Allende Prieto et al. (J/A+A/420/183)
26- 31 F6.3 [-] alpha2 α enhancement measured by
Allende Prieto et al. (J/A+A/420/183) (1)
33- 36 I4 K Teff Effective temperature measured by MATISSE
38- 42 F5.3 [cm/s2] logg Surface gravity measured by MATISSE
44- 49 F6.3 [-] [M/H] Overall metallicity measured by MATISSE
51- 56 F6.3 [-] alpha α enhancement measured by MATISSE
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Note (1): calculated from the combination of [Mg/H], [Si/H], [Ca/H], and [Fe/H].
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [HD]
3- 8 I6 --- HD HD identification number (0 for the Sun)
10- 13 I4 K Teff2 Effective temperature measured by
Prugniel et al. (2007, 0703658)
15- 19 F5.3 [cm/s2] logg2 Surface gravity measured by
Prugniel et al. (2007, 0703658)
21- 26 F6.3 [-] [Fe/H]2 Metallicity measured by
Prugniel et al. (2007, 0703658)
28- 31 I4 K Teff Effective temperature measured by MATISSE
33- 37 F5.3 [cm/s2] logg Surface gravity measured by MATISSE
39- 44 F6.3 [-] [M/H] Overall metallicity measured by MATISSE
46- 51 F6.3 --- alpha α enhancement measured by MATISSE
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Byte-by-byte Description of file: table13.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
8- 9 A2 --- --- [No]
10- 14 I5 --- Star Star number within the cluster (1)
16- 19 I4 K Teff2 Effective temperature measured by
Santos et al. (2009A&A...493..309S 2009A&A...493..309S)
21- 25 F5.3 [cm/s2] logg2 Surface gravity measured by
Santos et al. (2009A&A...493..309S 2009A&A...493..309S)
27- 32 F6.3 [-] [Fe/H]2 Metallicity measured by
Santos et al. (2009A&A...493..309S 2009A&A...493..309S)
34- 37 I4 K Teff Effective temperature measured by MATISSE
39- 43 F5.3 [cm/s2] logg Gravity measured by MATISSE
45- 50 F6.3 [-] [M/H] Metallicity measured by MATISSE
52- 57 F6.3 --- alpha α enhancement measured by MATISSE
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Note (1): given by Santos et al. (2009A&A...493..309S 2009A&A...493..309S), identified as
Cl* "Cluster" MMU "Star"
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Acknowledgements:
Jean-Christophe Gazzano, jean-christophe.gazzano(at)oamp.fr
(End) Patricia Vannier [CDS] 12-Nov-2010