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Table 2.

J-band photometry, individual distances, and stellar and accretion parameters derived for sources in Table 1, except TWA 3B (see Appendix A).

Name J err d err SpT AV log L⋆ Teff err log g err RV err v sin i err r M⋆ err R⋆
[mag] [pc] [mag] [L⊙] [L⊙] [K] [km s−1] [km s−1] (6200 Å) [M⊙] [R⊙] [M⊙ yr−1]
Bona fide accretors:
TWA 1 [10 s] 8.217 0.017 60.10 0.14 M0.5 0.0 −0.55 −1.52 −1.54 3880 30 4.4 0.2 13.5 1.4 7 3 0.8 0.58 0.09 1.22 −8.59 −8.62
TWA 1 [60 s] ” ” ” ” M0.5 0.0 −0.55 −1.57 −1.60 3870 40 4.46 0.13 13.1 1.4 7 2 0.8 " " ” −8.64 −8.68
TWA 27 [P084] 13.00 0.02 64.4 0.7 M9 0.0 −2.19 −5.10 −4.55 2640 20 3.75 0.14 10 4 30 10 0.0 0.019 0.006 0.35 −11.23 −10.68
TWA 27 [P089] ” ” ” ” M9 0.0 −2.47 −5.22 −4.92 2730 100 3.8 0.2 27 4 25 10 0.0 " " ” −11.35 −11.05
TWA 28 13.03 0.02 59.9 0.7 M9 0.0 −2.47 −6.00 −5.15 2660 70 4.1 0.3 18 3 25 10 0.0 0.020 0.005 0.29 −12.24 −11.38
TWA 31 13.048 0.018 81.1 0.6 M5 0.7 −1.96 −3.28 −3.13 2990 50 4.49 0.11 7 2 < 8 1.2 0.078 0.018 0.39 −9.97 −9.82
TWA 32 10.69 0.02 63.7 1.4 M5.5 0.0 −1.68 −3.85 −3.43 2800 70 3.98 0.11 7 2 < 8 0.3 0.070 0.015 0.57 −10.35 −9.93
Possible accretors:
TWA 30A [P087, ns] 9.64 0.02 48.0 0.3 M4.5 2.2 −0.89 −3.21 −3.75 3110 80 4.36 0.15 12.8 1.5 28.2 1.7 0.3 0.15 0.02 1.26 −9.70 −10.23
TWA 30A [P087, ls] ” ” ” ” M4.5 2.4 −0.89 −3.39 −3.92 3050 60 4.42 0.13 14 3 19 11 0.3 " ” " −9.88 −10.40
TWA 30A [P287] ” ” ” ” M4.5 −3.49 3070 80 4.34 0.13 11 3 25 9 0.3 " ” " −9.97
TWA 22 8.554 0.013 19.61 0.12 M5 0.1 −1.74 −4.86 −4.31 2830 100 4.09 0.11 16 2 < 8 0.1 0.082 0.018 0.51 −11.46 −10.92
TWA 8A 8.337 0.017 46.27 0.19 M3 0.2 −0.66 −3.06 −2.96 3370 90 4.6 0.2 7.1 1.2 9 6 0.3 0.29 0.04 1.35 −9.79 −9.72
TWA 8B 9.84 0.02 46.5 0.2 M5.5 0.0 −1.52 −4.36 −4.15 2830 80 4.04 0.10 10 2 < 8 0.1 0.074 0.018 0.68 −10.80 −10.58
Upper limits:
TWA 3A 7.651 0.009 36.62 0.16 M4.5 0.0 −0.86 −3.74 −3.42 3180 80 4.23 0.13 −1/+29 3/3 < 8/< 8 0.2 0.15 0.02 1.30 −10.21 −9.89
Underluminous:
TWA 30B [P087] 15.35 0.05 46.3 0.6 M4 −4.46 −7.43 3180 50 4.35 0.14 18 3 30 8 0.4
TWA 30B [P287] ” ” ” ” −5.39 3410 100 4.4 0.3 19 4 30 15 0.2
No slab model solution:
TWA 40 15.49 0.06 67 4 M9.5/L0 1.0 −2.16 2500 70 4.4 0.2 20 7 0.0 0.015 0.002 0.44 −13.34†
J1247-3816 14.79 0.03 85 4 M8 0.35 −3.00 −5.84 2660 30 4.50 0.15 14 6 < 8 0.0 0.060 0.010 0.15 −12.85

Notes. The groupings into bona fide accretors, possible accretors, and upper limits are referred to the measured Balmer continuum emission from the multi-component fit (see Sect. 3.1.1). Objects in the possible accretors group are listed in decreasing order of strength of the measured Balmer continuum flux excess above the photospheric level. Objects for which no solution could be derived from the multi-component fitting procedure are listed under “no slab model solution”. A blank space is reported for a given parameter when no accurate estimate could be derived from the corresponding spectrum. “Name” = Target identifier, as reported in Table 1. The Pxxx notation following some of the target names identifies the program during which the corresponding observation was conducted for sources with multiple spectra in our sample. The ns and ls notations associated with TWA 30A indicate the observations obtained with narrower slit and larger slit, respectively, during program 087.C-0244. “J, err” = J-band apparent magnitudes from 2MASS, and associated uncertainties. “d” = Individual distances derived from Gaia DR2 parallaxes. “SpT, AV, log L⋆, ” = parameters corresponding to the best solution of the spectrum fitting procedure (see Sect. 3.1.1). “” = median estimate determined from the luminosity of emission lines (see Sect. 3.2.1). Typical uncertainties amount to 0.2 dex on log L⋆, 0.25 dex on , and 0.17 dex on . “Teff, err, log g, err, RV, err, v sin i, err, r” = parameters corresponding to the best fit to the spectra obtained with ROTFIT (see Sect. 3.1.2), and associated uncertainties. The two values of RV and v sin i reported for TWA 3A correspond to the measurements extracted separately for the two components of the spectroscopic binary by deblending the two peaks observed in the absorption lines. “M⋆, err, R⋆, ” = parameters computed as in Sect. 3.1.3. Typical uncertainties amount to 20% on R⋆, and 0.3 dex on . “” = accretion rate estimate derived from . Typical uncertainties amount to 0.2 dex. Notes on individual sources: TWA 30B is an edge-on disk source (Looper et al. 2010), therefore the derived L⋆ is a severe underestimate, and no stellar parameters could be estimated from it. † = upper limit.

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