Table 1.
Sample of stars and number of observations per observational period.
| Star | SpT | v sin i | Av | i(*)(a) | 2018 | 2019a | 2019b | 2020a | 2020b | 2021a | 2021b | 2022a | References (b) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (km s−1) | (mag) | (°) | |||||||||||
| Accreting systems | |||||||||||||
| CI Tau | K4 | 9.5±0.5 | 0.65 | 55 |
2 | 6 | 26 | 5 | 39 | – | – | – | (1), (2), (2), (2) |
| DoAr 44 | K2-K3 | 17.0±1.1 | 2.0±0.2 | 30±5 | – | 8 | – | – | – | – | – | – | (3), (3), (3), (3) |
| GQ Lup | K7 | 5±1 | 0.7 | ∼30 | – | 8 | – | 18 | 6 | – | – | – | (4), (5), (4), (5) |
| TW Hya | K6 | 6.0±1.2 | 0.0 | 18±10 | – | 12 | – | 14 | – | 27 | – | – | (1), (1), (6), (7) |
| V2129 Oph | K5 | 14.5±0.3 | 0.6 | 60 | 9 | – | – | 17 | 8 | – | – | – | (1), (1), (8), (9) |
| BP Tau | K5 | 9.0±0.5 | 0.45 | ∼45 | – | – | 21 | – | – | – | 34 | – | (10), (11), (6), (11) |
| V347 Aur | M2-M3 | 11.7 |
3.4 | 40 | – | – | 18 | – | 13 | 12 | 22 | – | (12), (13), (12), (14) |
| DG Tau | K6 | 24.7±0.7 | 1.60±0.15 | 38±2 | – | – | – | 2 | 29 | – | – | – | (10), (10), (6), (15) |
| RU Lup | K7 | 8.5±4.8 | 0.0 | 24 | – | – | – | 9 | – | 17 | 13 | 1 | (16), (17), (14), (18) |
| V2247 Oph | M0 | 20.5±0.5 | 0.98±0.02 | 45±10 | – | – | – | 9 | 7 | – | – | – | (19), (20), (19), (20) |
| DO Tau | M0 | 14.3±0.5 | 0.75 | 37.0±3.7 | – | – | – | 3 | 8 | – | – | – | (6), (21), (6), (15) |
| J1604 (*) | K3 | 17.3±0.4 | 1.0 | > 61 | – | – | – | 12 | – | – | – | – | (22), (22), (24), (23) |
| PDS 70 | K7 | 16.0±0.5 | 0.01±0.07 | 50±8 | – | – | – | 4 | – | – | – | 6 | (19), (25), (19), (25) |
| GM Aur | K4-K5 | 14.9±0.3 | 0.3±0.3 | ≥63 | – | – | – | – | 2 | – | 34 | – | (26), (26), (26), (26) |
| Non-accreting systems | |||||||||||||
| V819 Tau | K4 | 9.5 | – | – | – | 1 | – | – | – | – | (27), (27) | ||
| TWA 25 | M0.5 | 12.9±1.2 | – | – | 25 | 14 | – | – | – | – | (6), (1) | ||
| TWA 9A | K6 | 7±3 | – | – | – | 1 | – | – | – | – | (6), (1) | ||
Notes.
The inclination (see references) between the stellar rotation axis and our line of sight obtained from v sin i, period, and radius of each target, except for the inclinations of DO Tau and DG Tau that were obtained from the outer disk parameters.
References. (1) Torres et al. (2006); (2) Donati et al. (2020b); (3) Bouvier et al. (2020); (4) Alcalá et al. (2017); (5) Donati et al. (2012); (6) Herczeg & Hillenbrand (2014); (7) Alencar & Batalha (2002); (8) Donati et al. (2007); (9) Alencar et al. (2012); (10) Nguyen et al. (2012); (11) Donati et al. (2008); (12) Connelley & Greene (2010); (13) Flores et al. (2019); (14) Alecian et al. (in prep.); (15) Simon et al. (2016); (16) Alcalá et al. (2014); (17) Frasca et al. (2017); (18) Stempels et al. (2007); (19) Pecaut & Mamajek (2016); (20) Donati et al. (2010); (21) Kounkel et al. (2019); (22) Dahm et al. (2012); (23) Davies (2019); (24) Preibisch & Zinnecker (1999); (25) Thanathibodee et al. (2020); (26) Bouvier et al. (in prep.); (27) Donati et al. (2015).
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