2004A&A...426..601D

Query : 2004A&A...426..601D

2004A&A...426..601D - Astronomy and Astrophysics, volume 426, 601-617 (2004/11-1)

VLTI near-IR interferometric observations of Vega-like stars. Radius and age of α PsA, β Leo, β Pic, ε Eri and τ Cet.

DI FOLCO E., THEVENIN F., KERVELLA P., DOMICIANO DE SOUZA A., COUDE DU FORESTO V., SEGRANSAN D. and MOREL P.

Abstract (from CDS):

We report in this paper the direct interferometric measurement of the angular diameter of five nearby Vega-like stars: α PsA, β Leo, β Pic, ε Eri and τ Cet. The near-infrared (K and H bands) observations were conducted at the VLTI during the commissioning period with the VINCI instrument and three different baselines ranging from 66m to 140m. The five stellar photospheres are resolved and we derive their angular diameters with a 1 to 2% accuracy, except for βPic (14%). We discuss the detectability and the influence of a possible small amount of warm circumstellar dust on our measurements. In addition, we have used the stellar evolution code CESAM (Morel, 1997A&AS..124..597M) to compare the computed fundamental parameters to the observed values (linear diameter, luminosity, temperature and chemical abundance). As a result of the simulation, the age of the stars is inferred and found to be in good agreement with previous estimates from various other methods.

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Journal keyword(s): techniques: interferometric - infrared: stars - stars: fundamental parameters - stars: circumstellar matter - stars: general

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 * del Psc PM* 00 48 40.9443145328 +07 35 06.294902124 7.83 5.95 4.44 3.27 2.40 K5-III 187 0
2 * tet Cet HB* 01 24 01.4032816333 -08 10 59.739230440 5.57 4.65 3.59 2.83 2.26 K0IIIb 196 0
3 * del Phe PM* 01 31 15.1040942588 -49 04 21.730128530   4.918 3.935     G8.5IIIb 127 0
4 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1255 1
5 * chi Phe PM* 02 01 42.3763488264 -44 42 48.626334576 8.45 6.63 5.14 3.92 3.03 K5IV 61 0
6 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1932 1
7 * del Eri PM* 03 43 14.9005379551 -09 45 48.210955899 5.13 4.46 3.54 2.82 2.32 K0+IV 598 0
8 * 39 Eri PM* 04 14 23.6878980552 -10 15 22.620462156 7.18 6.07 4.90 4.01 3.44 K2III 112 0
9 * eps Ori s*b 05 36 12.81335 -01 12 06.9089 0.48 1.51 1.69 1.76 1.93 B0Ia 896 0
10 HD 38060 * 05 45 11.9666681568 +44 44 05.193837132   9.66 9.37     B9V 5 0
11 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1903 1
12 * gam02 Vol PM* 07 08 44.8656955896 -70 29 56.149447560   4.774 3.746     K0III 74 0
13 * 6 Leo * 09 31 57.5770044456 +09 42 56.755133244 7.97 6.44 5.07     K2.5IIIFe-0.5 77 0
14 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 577 1
15 * c Vir RG* 12 20 20.9813922197 +03 18 45.255217001 7.27 6.12 4.96 4.07 3.46 K0.5IIIbFe-0.5 360 0
16 * w Cen PM* 12 42 35.4513079543 -48 48 47.197138463 6.77 5.76 4.66 3.91 3.34 K0III 70 0
17 * 70 Aql * 20 36 43.6331948352 -02 32 59.836714368   6.475 4.880     K4+IIIBa1 77 0
18 * 7 Aqr * 20 56 54.0265592448 -09 41 51.150476328   6.97 5.48     K4III 42 0
19 * lam Gru PM* 22 06 06.8848137372 -39 32 36.070820047   5.843 4.458     K3III 63 0
20 HD 216149 * 22 51 02.1589579824 -39 09 24.608634876   6.851 5.400     K3III 56 0
21 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1236 3
22 * psi01 Aqr PM* 23 15 53.4940495770 -09 05 15.844964053 6.37 5.36 4.25 3.46 2.90 K1-IIIFe-0.5 244 1

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