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Table 5

Physical parameters derived for TWA stars with known distances.

Siess et al. (2000) Baraffe et al. (1998)

Star ST T eff A V H abs log (L/L) log (M/M) log t log (M/M) log t Ref.
(K) (mag) (mag) (t in Myr) (t in Myr)

TWA 1 K8 3940 0.00 3.91 ± 0.25 −0.58 ± 0.12 −0.16 ± 0.01 6.90 ± 0.19 −0.10 ± 0.03 7.09 ± 0.21 1,2,3,4
TWA 2A M0.5 3704 0.33 4.22 ± 0.44 −0.75 ± 0.20 −0.34 ± 0.01 6.81 ± 0.26 −0.23 ± 0.08 7.02 ± 0.29 1,3,6,10
TWA 2B M2 3490 0.00 5.01 ± 0.44 −1.09 ± 0.20 −0.50 ± 0.03 6.91 ± 0.24 −0.39 ± 0.06 7.13 ± 0.27 1,3,5,6
TWA 3A M4 3160 0.00 4.79 ± 0.13 −1.03 ± 0.07 −0.75 ± 0.02 6.60 ± 0.05 −0.74 ± 0.04 6.38 ± 0.07 3,5,6
TWA 3B M4 3160 0.00 5.41 ± 0.14 −1.28 ± 0.08 −0.81 ± 0.02 6.78 ± 0.06 −0.81 ± 0.03 6.61 ± 0.06 3,5,6
TWA 4A K5 4140 0.00 3.31 ± 0.24 −0.31 ± 0.12 −0.06 ± 0.01 6.73 ± 0.20 −0.04 ± 0.01 6.81 ± 0.22 5,7,8
TWA 4B K7,M1 3970 0.00 3.32 ± 0.24 −0.34 ± 0.12 −0.16 ± 0.01 6.56 ± 0.18 −0.10 ± 0.03 6.70 ± 0.20 5,7,8
TWA 5Aa M2 3490 0.00 4.25 ± 0.26 −0.79 ± 0.12 −0.46 ± 0.01 6.55 ± 0.10 −0.40 ± 0.06 6.70 ± 0.17 1,3,5,9
TWA 5Ab M2 3490 0.00 4.35 ± 0.26 −0.83 ± 0.12 −0.47 ± 0.01 6.60 ± 0.14 −0.39 ± 0.05 6.75 ± 0.18 1,3,5,9
TWA 6 M0 3770 0.00 4.05 ± 0.64 −0.67 ± 0.28 −0.29 ± 0.01 6.72 ± 0.39 −0.19 ± 0.06 7.00 ± 0.43 1,3,4
TWA 7 M3 3360 0.00 4.44 ± 0.16 −0.87 ± 0.07 −0.56 ± 0.01 6.61 ± 0.08 −0.54 ± 0.05 6.55 ± 0.09 1,3,4
TWA 8A M3 3360 0.00 4.57 ± 0.21 −0.93 ± 0.11 −0.56 ± 0.02 6.63 ± 0.12 −0.55 ± 0.05 6.62 ± 0.15 1,3,10
TWA 9A K7 3970 0.00 4.60 ± 0.27 −0.86 ± 0.14 −0.16 ± 0.03 7.38 ± 0.22 −0.15 ± 0.08 7.58 ± 0.21 1,2,3,10
TWA 9B M3.5 3255 0.00 5.83 ± 0.16 −1.44 ± 0.09 −0.74 ± 0.01 7.02 ± 0.09 −0.72 ± 0.03 6.97 ± 0.11 1,3,10
TWA 10 M2 3490 0.36 4.47 ± 0.14 −0.88 ± 0.07 −0.47 ± 0.01 6.66 ± 0.08 −0.39 ± 0.05 6.82 ± 0.11 1,3,4
TWA 11A A0 9700 0.00 1.48 ± 0.06 1.40 ± 0.03 + 0.35 ± 0.01 6.80 ± 0.06 ................ ................ 2,4,5
TWA 11B M2 3490 0.00 4.30 ± 0.14 −0.81 ± 0.08 −0.46 ± 0.01 6.58 ± 0.09 −0.40 ± 0.05 6.73 ± 0.10 5,10
TWA 11C M4.5 3001 0.00 5.03 ± 0.08 −1.13 ± 0.04 −0.95 ± 0.01 6.60 ± 0.02 −1.00 ± 0.02 6.18 ± 0.08 1,4
TWA 12 M2 3490 0.27 4.23 ± 0.24 −0.78 ± 0.11 −0.46 ± 0.01 6.55 ± 0.12 −0.40 ± 0.06 6.69 ± 0.15 1,3,4
TWA 13A M1 3630 0.00 4.00 ± 0.11 −0.67 ± 0.06 −0.38 ± 0.01 6.54 ± 0.08 −0.27 ± 0.05 6.80 ± 0.08 1,3,4
TWA 13B M1 3630 0.31 3.76 ± 0.11 −0.57 ± 0.06 −0.38 ± 0.01 6.42 ± 0.07 −0.28 ± 0.05 6.67 ± 0.09 1,3,4
TWA 14 M0 3770 0.00 4.57 ± 0.26 −0.88 ± 0.12 −0.30 ± 0.01 7.02 ± 0.19 −0.21 ± 0.05 7.33 ± 0.19 4,5,11
TWA 15A M1.5 3562 0.00 4.73 ± 0.41 −0.97 ± 0.18 −0.44 ± 0.01 6.84 ± 0.22 −0.32 ± 0.06 7.10 ± 0.25 4,5,12
TWA 15B M2 3490 0.00 4.49 ± 0.41 −0.88 ± 0.18 −0.48 ± 0.02 6.73 ± 0.20 −0.39 ± 0.05 6.83 ± 0.26 4,5,12
TWA 16 M2 3490 0.00 4.56 ± 0.10 −0.91 ± 0.06 −0.47 ± 0.01 6.70 ± 0.06 −0.39 ± 0.05 6.88 ± 0.09 1,4,13
TWA 20 M3 3360 0.00 5.01 ± 0.13 −1.10 ± 0.07 −0.59 ± 0.01 6.81 ± 0.07 −0.56 ± 0.05 6.86 ± 0.10 1,4
TWA 21 K3 4550 0.00 3.84 ± 0.16 −0.43 ± 0.08 −0.04 ± 0.03 7.41 ± 0.10 −0.05 ± 0.05 7.40 ± 0.12 1,4
TWA 23 M1 3630 0.00 5.35 ± 0.19 −1.21 ± 0.09 −0.41 ± 0.01 7.25 ± 0.13 −0.28 ± 0.06 7.59 ± 0.14 1,4
TWA 25 K9 3880 0.33 3.79 ± 0.15 −0.55 ± 0.08 −0.21 ± 0.01 6.72 ± 0.11 −0.12 ± 0.03 6.98 ± 0.12 1,3,4

Notes. We provide for each star the spectral type, temperature, visual extinction, absolute magnitude from H flux, luminosity, mass, and age derived from the Siess et al. (2000) and Baraffe et al. (1998) models, and the sources of photometric/spectroscopic information. The photometry of TWA 2, TWA 3, TWA 4, TWA 5, TWA 8, TWA 9, and TWA 16 are corrected for binarity with the information provided in the corresponding references (last column). TWA 14, TWA 20, and TWA 23 are corrected for binarity assuming that the components have equal brightness (as done by Weinberger et al. 2013). Note that our age and mass estimates for TWA 11C derived from the Baraffe et al. (1998) tracks and isochrones are only indicative because of the grid limits of this model and the star position in the HR diagram (see Fig. 6).

Reference. (1) Pecaut & Mamajek (2013); (2) Hipparcos (ESA 1997); (3) Torres et al. (2006); (4) 2MASS (Cutri et al. 2003); (5) Schneider et al. (2012a); (6) Brandeker et al. (2003); (7) Fernández et al. (2008); (8) Prato et al. (2001); (9) Konopacky et al. (2007); (10) Webb et al. (1999); (11) Messina et al. (2010); (12) Barrado Y Navascués (2006); (13) Zuckerman et al. (2001); (14) Teixeira et al. (2008); (15) Looper et al. (2010a).

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