Table 2
Properties of the CTT sample derived in this work.
| Name | Teff (±err) | SpT | AV (a) | AV (b) | L⋆ | R⋆ | M⋆ |
|---|---|---|---|---|---|---|---|
| (K) | (mag) | (mag) | (L⊙) | (R⊙) | (M⊙) | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| RY Tau | 5856 (151) | G1 | 2.25 | 2.32 | 8.87 | 2.89 | 1.80 |
| DG Tau | 4004 (153) | K7 | 1.50 | 1.79 | 0.44 | 1.38 | 0.70 |
| DL Tau | 4188 (100) | K5 | 1.50 | 1.45 | 0.40 | 1.20 | 0.90 |
| HN Tau A (†) | 4617 (97) | K4 | 1.25 | 1.53 | 0.15 | 0.60 | 0.80 (⋆) |
| DO Tau | 3694 (104) | M1 | 1.40 | 1.69 | 0.42 | 1.58 | 0.50 |
| RW Aur A | 4870 | K0 | 1.00 | 0.57 | 1.64 | 1.80 | 1.50 |
| CQ Tau (‡) | 6823 (136) | F4 | 0.50 | 0.60 | 2.71 | 1.18 | 1.50 (⋆) |
Notes. (a) Extinction derived using spectral templates only. (b) Extinction derived using spectral templates and veiling. (†)Subluminous YSO (Sect. 3.4). The L⋆, R⋆, and M⋆ values are underestimated. (‡)UX Ori type variable (Sect. 3.4). Parameters affected by variable circumstellar extinction. (⋆) Corrected values of L⋆, R⋆, and M⋆ for the two subluminousobjects are estimated in Sect. 4.4. The mass reported here is that of the closest PMS track on the HR diagram, with the uncorrected values of L⋆.
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