J/A+A/586/A94 Exoplanetary parameters for 18 bright stars (Ligi+, 2016)
Radii, masses, and ages of 18 bright stars using interferometry and
new estimations of exoplanetary parameters.
Ligi R., Creevey O., Mourard D., Crida A., Lagrange A.-M., Nardetto N.,
Perraut K., Schultheis M., Tallon-bosc I., Ten Brummelaar T.
<Astron. Astrophys., 586, A94-94 (2016)>
=2016A&A...586A..94L 2016A&A...586A..94L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Effective temperatures ;
Extinction ; Stars, ages ; Interferometry ; Stars, diameters
Keywords: stars: fundamental parameters - planetary systems -
techniques: interferometric - methods: numerical
Abstract:
We present the interferometric angular diameters of 18 bright stars:
HD3651 , HD9826, HD19994, HD75732, HD167042, HD170693, HD173416,
HD185395, HD190360, HD217014, HD221345, HD1367, HD1671, HD154633,
HD161178, HD161151, HD209369, HD218560. The first 11 host exoplanets
(except HD185395). We combined these angular diameters θLD
with the stellar distances to estimate the stellar radii. We perform
SED fitting of the photometry to derive the stars bolometric flux Fbol
with and without stellar extinction Av. We then give the effective
temperature TeffSED and angular diameter θSED from this SED
fit, considering fixed Av, metallicity [Fe/H] and gravity log(g).
Then, taking into account the stellar extinction, we derived from the
bolometric flux and the measured angular diameters the effective
temperature and luminosity to place the stars on the H-R diagram. We
then used the PARSEC models to derive the best fit ages and masses of
the stars, with error bars derived from Monte Carlo calculations.
Typically, for main sequence stars, two distinct sets of solutions
appear (an old and a young age).
For stars that host known exoplanets, we also derive the exoplanets
parameters considering the two different solutions (old and young):
semi-major axis, planetary minimum mass and habitable zone of the host
stars. Finally, we give the true mass, radius and density of the
transiting exoplanet 55 Cnc e using the inteferometric radius and
photometry.
Description:
We performed interferometric measurements from 2010 to 2013 using the
VEGA/CHARA instrument. VEGA is a spectro-interferometer working at
visible wavelengths ([450-850]nm) at medium (6000) or high (30000)
spectral resolution. It takes advantage of the CHARA baselines, which
range from 34 to 331 m, to reach a maximum spatial resolution of
∼0.3 millisecond of arc. VEGA is able to recombine the light coming
from two to four of the six one-meter telescopes hosted by the CHARA
array. The telescopes are arranged in a Y shape, which allows a wide
range of orientations and thus a rich (u,v) coverage. Our observations
were performed using three telescopes at medium spectral resolution
and at observing wavelengths generally ranging between 650 and 730nm.
This allowed us to reach an average of 1.9% uncertainty on angular
diameters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 341 18 Parameters of stars
exoplan.dat 130 18 Parameters of exoplanets
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1 A1 --- Planet [*] * indicates planet data in exoplan file
3- 8 I6 --- HD HD number
10- 16 A7 -- Name Other name
18- 24 A7 --- SpType Stellar spectral type
26- 29 F4.2 mag Vmag Magnitude in the V band
(Johnson-Cousin system)
31- 34 F4.2 mag Kmag Magnitude in the K band
(Johnson-Cousin system)
36- 37 I2 h RAh Right ascension (J2000)
39- 40 I2 min RAm Right Ascension (J2000)
42- 49 F8.5 s RAs Right ascension (J2000)
51 A1 --- DE- Declination sign (J2000)
52- 53 I2 deg DEd Declination (J2000)
55- 56 I2 arcmin DEm Declination (J2000)
58- 64 F7.4 arcsec DEs Declination (J2000)
66- 71 F6.4 mag Av Stellar extinction
73- 76 F4.1 [-] [Fe/H] Stellar metallicity
78- 80 F3.1 [-] e_[Fe/H] Adopted error on stellar metallicity
82- 84 F3.1 [cm/s2] log(g) Logarithm of the stellar gravity
86- 89 F4.2 [cm/s2] e_log(g) Error on logarithm of the stellar gravity
91- 94 I4 K TeffSED Effective temperature from SED fitting
96- 97 I2 K e_TeffSED Error on TeffSED
99-103 F5.3 mas thetaSED Angular diameter from SED fitting
105-109 F5.3 mas e_thetaSED Error on thetaSED
111-116 F6.2 pW/m2 Fbol Stellar bolometric flux from SED fitting
with Av ≠ 0 (in 10-8erg/s/cm2) (1)
118-123 F6.3 pW/m2 e_Fbol Error on Fbol
125-131 F7.3 pW/m2 Fbol0 Stellar bolometric flux from SED fitting
with Av=0 (in 10-8erg/s/cm2)
133-137 F5.3 pW/m2 e_Fbol0 Error on Fbol0
139-143 F5.3 mas thetaUD Uniform disk angular diameter
from interferometric measurements
145-149 F5.3 mas e_thetaUD Error on thetaUD
151-155 F5.3 --- mu Limb-darkening coefficient (µ{lamnda})
157-161 F5.3 mas thetaLD Limb-darkened disk angular diameter
from interferometric measurements
163-167 F5.3 mas e_thetaLD Error on thetaLD
169-172 F4.2 % ethetaLD Error on thetaLD in percent
174-177 F4.2 --- chi2 Reduced chi2 on thetaLD fit on
visibilities
179-182 I4 K Teff Effective temperature from thetaLD and Fbol
184-186 I3 K e_Teff Error on Teff
188-194 F7.3 pc D Hipparcos distance
195-199 F5.2 pc e_D Error on D
200-204 F5.2 % eD Error on D in percent
206-212 F7.4 solRad Rad Stellar radius from thetaLD and D
214-219 F6.4 solRad e_Rad Error on Rad
221-225 F5.2 % eRad Error on Rad in percent
227-234 F8.4 Lsun Lum Stellar luminosity from Rad and Teff
235-241 F7.4 Lsun e_Lum Error on Lum
243-246 F4.2 Msun Massgrav Stellar gravitational mass from Rad and D
248-251 F4.2 Msun e_Massgrav Error on Massgrav
253-257 F5.3 Msun Massold Stellar mass, old solution
259-263 F5.3 Msun e_Massold Error on Massold
265-270 F6.3 % eMassold Error on Massold in percent
271-276 F6.3 Gyr Ageold Stellar age, old solution
278-281 F4.2 Gyr e_Ageold Error on Ageold
283-285 I3 % eAgeold Error on Ageold in percent
287-289 F3.1 [cm/s2] log(g)old Logarithm of the stellar gravity from
Massold
291 A1 --- l_chi2old [~] Limit flag on chi2old
292-297 F6.4 --- chi2old chi2 of the isochrone fitting
299-303 F5.3 Msun Massyoung ?=- Stellar mass, young solution
305-309 F5.3 Msun e_Massyoung ?=- Error on Massyoung
311-314 F4.2 % eMassyoung ?=- Error on Massyoung in percent
316-321 F6.3 Myr Ageyoung ?=- Stellar age, young solution
323-327 F5.3 Myr e_Ageyoung ?=- Error on Ageyoung
329-330 I2 % eAgeyoung ?=- Error on Ageyoung in percent
332-334 F3.1 [cm/s2] log(g)young ?=- Logarithm of the stellar gravity from
Massyoung
336-341 F6.4 --- chi2young ?=- χ2 of the isochrone fitting
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Note (1): the determination of the stellar parameters (luminosity, effective
temperature) is performed using Fbol with Av ≠ 0.
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Byte-by-byte Description of file: exoplan.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- PName Exoplanet name
11- 17 F7.5 AU aold Semi-major axis of the exoplanet,
old solution
19- 25 F7.5 AU e_aold Error on aold
26- 32 F7.4 MJup Mpsin(i)old Minimum mass of the exoplanet,
old solution (1)
34- 39 F6.4 MJup e_Mpsin(i)old Error on Mpsin(i)old
old solution (1)
41- 46 F6.4 AU ayoung ?=- Semi-major axis of the exoplanet,
young solution
48- 53 F6.4 AU e_ayoung ?=- Error on ayoung
55- 60 F6.3 MJup Mpsin(i)young ?=- Minimum mass of the exoplanet,
young solution (1)
62- 66 F5.3 MJup e_Mpsin(i)young ?=- Error on Mpsin(i)young (1)
68- 72 F5.2 AU HZl Lower value of habitable zone of the star
hosting the exoplanet
73 A1 --- --- [-]
74- 78 F5.2 AU HZu Upper value of habitable zone of the star
hosting the exoplanet
80- 84 F5.3 Earth Rp ? Exoplanetary radius (R⊕ unit)
86 A1 --- --- [+]
87- 91 F5.3 Earth E_Rp ? Error (upper value) on Rp
(R⊕ unit)
93 A1 --- --- [-]
94- 98 F5.3 Earth e_Rp ? Error (lower value) on Rp in
(R⊕ unit)
100-104 F5.3 Earth Mp ? Exoplanetary mass (M⊕ unit)
106-110 F5.3 Earth e_Mp ? Error on Mp (M⊕ unit)
112-116 F5.3 g/cm3 rhop ? Exoplanetary density
118 A1 --- --- [+]
119-123 F5.3 g/cm3 E_rhop ? Error on rhop (upper value)
125 A1 --- --- [-]
126-130 F5.3 g/cm3 e_rhop ? Error on rhop (lower value)
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Note (1): The minimum mass of the exoplanets HD190360c and HD75732e are
expressed in Earth mass.
The minimum masses of the exoplanets of the 55 Cnc system are estimated
according to a direct estimate of the stellar mass, contrary to the
others that are estimated according to stellar masses from stellar models
(see paper).
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Acknowledgements:
Roxanne Ligi, roxanne.ligi(at)lam.fr
(End) Patricia Vannier [CDS] 02-Nov-2016