2016A&A...586A..94L


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST05:12:20

2016A&A...586A..94L - Astronomy and Astrophysics, volume 586A, 94-94 (2016/2-1)

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. and TEN BRUMMELAAR T.

Abstract (from CDS):

Accurate stellar parameters are needed in numerous domains of astrophysics. The position of stars on the Hertzsprung-Russell diagram is an important indication of their structure and evolution, and it helps improve stellar models. Furthermore, the age and mass of stars hosting planets are required elements for studying exoplanetary systems. We aim at determining accurate parameters of a set of 18 bright exoplanet host and potential host stars from interferometric measurements, photometry, and stellar models. Using the VEGA/CHARA interferometer operating in the visible domain, we measured the angular diameters of 18 stars, ten of which host exoplanets. We combined them with their distances to estimate their radii. We used photometry to derive their bolometric flux and, then, their effective temperature and luminosity to place them on the H-R diagram. We then used the PARSEC models to derive their best fit ages and masses, with error bars derived from Monte Carlo calculations. Our interferometric measurements lead to an average of 1.9% uncertainty on angular diameters and 3% on stellar radii. There is good agreement between measured and indirect estimations of angular diameters (either from SED fitting or from surface brightness relations) for main sequence (MS) stars, but not as good for more evolved stars. For each star, we provide a likelihood map in the mass-age plane; typically, two distinct sets of solutions appear (an old and a young age). The errors on the ages and masses that we provide account for the metallicity uncertainties, which are often neglected by other works. From measurements of its radius and density, we also provide the mass of 55 Cnc independently of models. From the stellar masses, we provide new estimates of semi-major axes and minimum masses of exoplanets with reliable uncertainties. We also derive the radius, density, and mass of 55 Cnc e, a super-Earth that transits its stellar host. Our exoplanetary parameters reflect the known population of exoplanets. This work illustrates how precise interferometric measurements of angular diameters and detailled modeling allow fundamental parameters of exoplanet host stars to be constrained at a level permiting analysis of the planet's parameters.

Abstract Copyright:

Journal keyword(s): stars: fundamental parameters - planetary systems - techniques: interferometric - methods: numerical

VizieR on-line data: <Available at CDS (J/A+A/586/A94): stars.dat exoplan.dat>

Simbad objects: 57

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Number of rows : 57

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 * 34 Psc * 00 10 02.2026446215 +11 08 44.925917994   5.456 5.530   5.58 B9Vn 123 0
2 HD 1367 PM* 00 17 47.6987294262 +01 41 19.425461276   7.126 6.176     K0III 32 0
3 * rho And PM* 00 21 07.2689567019 +37 58 06.972655202   5.60 5.18     F5IV-V 117 0
4 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 513 1
5 * 54 Psc b Pl 00 39 21.80589 +21 15 01.7081           ~ 43 2
6 * f Psc PM* 01 17 47.9567070 +03 36 52.084814   5.210 5.137     A1V 92 0
7 * ups And d Pl 01 36 47.84216 +41 24 19.6443           ~ 146 1
8 * ups And c Pl 01 36 47.84216 +41 24 19.6443           ~ 143 1
9 * ups And e Pl 01 36 47.84216 +41 24 19.6443           ~ 23 1
10 * ups And b Pl 01 36 47.84216 +41 24 19.6443           ~ 242 1
11 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 881 1
12 HD 10390 PM* 01 42 03.4894262410 +35 14 44.541144419 5.37 5.57 5.64   5.67 B9IV-V 68 0
13 * 4 Ari PM* 01 48 10.9213748577 +16 57 19.848252353   5.809 5.841     B9.5V 72 0
14 * 60 Cet PM* 02 03 11.6500176714 +00 07 42.628215059   5.579 5.423     A3IV 51 0
15 * 7 Tri * 02 15 56.2880251756 +33 21 32.020541944   5.239 5.249     A0V 49 0
16 * tet Ari * 02 18 07.5302184092 +19 54 04.171722434   5.580 5.572     A1Vn 56 0
17 * 94 Cet b Pl 03 12 46.4369076602 -01 11 45.949836281           ~ 43 1
18 * 94 Cet PM* 03 12 46.4369076602 -01 11 45.949836281   5.631 5.070     F8.5V 397 1
19 * v Eri * 03 30 37.0582300 -05 04 30.523884   4.631 4.725     B9III 79 0
20 * 47 Gem * 07 11 23.0672072902 +26 51 23.725446956 5.990 5.860 5.750     A4IV 45 0
21 * rho01 Cnc e Pl 08 52 35.81093 +28 19 50.9511           ~ 354 1
22 * rho01 Cnc c Pl 08 52 35.81093 +28 19 50.9511           ~ 121 1
23 * rho01 Cnc d Pl 08 52 35.81093 +28 19 50.9511           ~ 134 1
24 * rho01 Cnc b Pl 08 52 35.81093 +28 19 50.9511     13.16     ~ 224 1
25 * rho01 Cnc f Pl 08 52 35.81093 +28 19 50.9511           ~ 41 1
26 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 944 1
27 * 23 LMi PM* 10 16 14.4299725284 +29 18 37.709186350   5.500 5.488     A0Vn 60 0
28 HD 145454 PM* 16 06 19.6782054767 +67 48 36.484541338   5.407 5.441     A0Vn 50 0
29 HD 149681 PM* 16 25 43.1864031698 +78 57 49.887080430 5.870 5.800   5.4   F0V 31 0
30 * 15 Dra * 16 27 59.0160285398 +68 46 05.305188356 4.84 4.906 4.949     B9.5IV 82 0
31 HD 154633 * 17 02 15.7478994012 +64 36 02.664550695   7.070 6.094     G5V 30 0
32 HD 161178 * 17 37 08.8839920022 +72 27 20.858635792   6.886 5.869     G9III 51 0
33 HD 167042b Pl 18 10 31.6406187667 +54 17 11.593233378           ~ 12 0
34 HD 167042 PM* 18 10 31.6406187667 +54 17 11.593233378   6.89   5.4   K1III 129 1
35 * 36 Dra PM* 18 13 53.8327884671 +64 23 50.225272101   5.41   4.8   F5V 177 0
36 HD 167014 * 18 14 19.4710 -23 40 09.937   9.89 9.62     B3III 5 0
37 * 42 Dra b Pl 18 25 59.1383795957 +65 33 48.503958394           ~ 12 1
38 * 42 Dra PM* 18 25 59.1383795957 +65 33 48.503958394   6.005 4.823     K1.5IIIFe-1 133 1
39 HD 173416 PM* 18 43 36.1094855832 +36 33 23.781469921   7.093 6.037     G8 33 1
40 HD 173416b Pl 18 43 36.1094855832 +36 33 23.781469921           ~ 7 1
41 V* LV Dra a2* 19 00 13.6785216947 +50 32 00.465048161 4.42 5.202 5.377     B2.5IV 94 0
42 * tet Cyg PM* 19 36 26.5343563 +50 13 15.964573 4.83 4.86 4.48 4.13 3.92 F3+V 320 1
43 HD 190360 PM* 20 03 37.4049065078 +29 53 48.495330996   6.44   5.2   G7IV-V 380 1
44 HD 190360b Pl 20 03 37.4053 +29 53 48.489           ~ 47 1
45 HD 190360c Pl 20 03 37.4053 +29 53 48.489           ~ 42 1
46 * 17 Vul * 20 06 53.4080963906 +23 36 51.927236665   4.891 5.056     B3V 101 0
47 * 28 Vul * 20 38 31.9139376202 +24 06 57.443309622 4.35 4.915 5.049     B5IV 84 0
48 * 35 Vul * 21 27 40.0571342311 +27 36 30.932065572   5.421 5.379     A1VmA3 56 0
49 * 7 Cep * 21 27 46.1414392791 +66 48 32.740577662   5.299 5.410     B7V 47 0
50 * 16 Cep PM* 21 59 14.9658017099 +73 10 47.614771175       4.8   F5V 77 0
51 * 10 Lac ** 22 39 15.6786372 +39 03 00.971152 3.650 4.670 4.880 4.98 5.19 O9V 715 0
52 * 51 Peg ** 22 57 27.9804167474 +20 46 07.782240714 6.39 6.16 5.46 4.97 4.61 G2IV 1058 1
53 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 483 1
54 HD 218560 * 23 07 57.2046283630 +64 13 21.082180050   7.297 6.212     K0 12 0
55 HD 219485 * 23 14 37.1041129704 +74 13 52.574678092 5.850 5.870 5.890     A0V 43 0
56 * 14 And PM* 23 31 17.4127253191 +39 14 10.310491330   6.24   4.6   G8III 156 1
57 * 14 And b Pl 23 31 17.4127253191 +39 14 10.310491330           ~ 12 1

    Equat.    Gal    SGal    Ecl

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2019.10.17-05:12:20

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