The young, tight, and low-mass binary TWA22AB: a new calibrator for evolutionary models? Orbit, spectral types, and temperature

被引:32
作者
Bonnefoy, M. [1 ]
Chauvin, G. [1 ]
Dumas, C. [2 ]
Lagrange, A. -M. [1 ]
Beust, H. [1 ]
Desort, M. [1 ]
Teixeira, R. [3 ]
Ducourant, C. [4 ]
Beuzit, J. -L. [1 ]
Song, I. [5 ]
机构
[1] Astrophys Lab, F-38041 Grenoble 9, France
[2] European So Observ, Santiago 19, Chile
[3] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil
[4] CNRS, Observ Aquitain Sci Univers, UMR 5804, F-33270 Floirac, France
[5] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA
关键词
stars: fundamental parameters; stars:; low-mass; brown dwarfs; binaries: close; stars: formation; instrumentation: adaptive optics; instrumentation: spectrographs; TW-HYDRAE ASSOCIATION; NEAR-INFRARED SPECTRA; AB-DORADUS-C; BROWN DWARFS; SEQUENCE STARS; ESO VLT; RESOLUTION; SPECTROSCOPY; PHOTOMETRY; COMPANION;
D O I
10.1051/0004-6361/200810921
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. Tight binaries discovered in young, nearby associations are ideal targets for providing dynamical mass measurements to test the physics of evolutionary models at young ages and very low masses. Aims. We report the binarity of TWA22 for the first time. We aim at monitoring the orbit of this young and tight system to determine its total dynamical mass using an accurate distance determination. We also intend to characterize the physical properties (luminosity, effective temperature, and surface gravity) of each component based on near-infrared photometric and spectroscopic observations. Methods. We used the adaptive-optics assisted imager NACO to resolve the components, to monitor the complete orbit and to obtain the relative near-infrared photometry of TWA22 AB. The adaptive-optics assisted integral field spectrometer SINFONI was also used to obtain medium-resolution (R(lambda) = 1500-2000) spectra in JHK bands. Comparison with empirical and synthetic librairies were necessary for deriving the spectral type, the effective temperature, and the surface gravity for each component of the system. Results. Based on an accurate trigonometric distance (17.5 +/- 0.2 pc) determination, we infer a total dynamical mass of 220 +/- 21 M(Jup) for the system. From the complete set of spectra, we find an effective temperature T(eff) = 2900(-200)(+200) K for TWA22A and T(eff) = 2900(-100)(+200) for TWA22 B and surface gravities between 4.0 and 5.5 dex. From our photometry and an M6 +/- 1 spectral type for both components, we find luminosities of log(L/L(circle dot)) = -2.11 +/- 0.13 dex and log(L/L(circle dot)) = -2.30 +/- 0.16 dex for TWA22 A and B, respectively. By comparing these parameters with evolutionary models, we question the age and the multiplicity of this system. We also discuss a possible underestimation of the mass predicted by evolutionary models for young stars close to the substellar boundary.
引用
收藏
页码:799 / 810
页数:12
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