Table B.1
Stellar properties of sample sorted by right ascension. Columns are target name, Taurus group following Luhman (2023), distance, multiplicity, effective temperature, stellar luminosity, mass, and age.
| Target | Group | d (pc) | System | Teff (K) | L* (L⊙) | M* (M⊙) | t (Myr) |
|---|---|---|---|---|---|---|---|
| CQ Tau | HD35187* | 149.4 | (*) | 6900 | 6.30±0.27 | 1.4 | 12–14 |
| MWC758 | HD35187* | 155.9 | (*) | 8200 | 10.29±0.34 | 1.7 | 13–14 |
| RW Aur | L1517 | 183.3* | (*)(*) | 5100+4400 | (1.4+0.7)±0.3 | 1.3+0.9 | 7.2–9.7 |
| V836 Tau | L1544 | 167.0 | (*) | 3600 | 0.57±0.06 | 0.4 | 0.3–0.9 |
| MWC480 | L1517 | 156.2 | (*) | 8800 | 19.90±0.65 | 2.1 | 6.3–6.6 |
| SU Aur | L1517 | 157.0 | (*) | 5800 | 15.80±2.30 | 2.5 | 2 0–2 5 |
| AB Aur | L1517 | 155.9 | (*) | 9800 | 40.58±0.80 | 2.4 | 3.9–4.4 |
| GM Aur | L1517 | 158.1 | (*) | 4350 | 1.40±0.18 | 0.9 | 1.0–1.6 |
| UY Aur | L1517 | 152.3 | (*)(*) | 3800+3600 | (0.65+0.33)±0.04 | 0.5+0.4 | 0.9–2.1 |
| DS Tau | L1517 | 158.4 | (*) | 3900 | 0.93±0.10 | 0.5 | 0.7–1.0 |
| DR Tau | L1558 | 193.0 | (*) | 4200 | 2.53±0.21 | 0.4 | 0.3–0.5 |
| DQ Tau | L1558 | 195.4 | (**) | 3600 | (0.50+0.50)±0.04 | 0.4 | 0.7–1.2 |
| EM* LkCa15 | L1536 | 157.2 | (*) | 4600 | 1.11±0.11 | 1.2 | 3.2–4.5 |
| DO Tau | L1527 | 138.5 | (*) | 3800 | 0.56±0.06 | 0.5 | 1.0–1.4 |
| V* V1025 Tau | L1536 | 167.3 | (*) | 5800 | 8.54±1.91 | 2.0 | 3.6–5.0 |
| V* HP Tau | L1536 | 171.2 | (*) | 5000 | 1.87±0.61 | 1.5 | 3.5–4.1 |
| HQ Tau | L1536 | 161.4* | (*) | 4900 | 3.24±0.72 | 1.3 | 1.5–1.9 |
| DN Tau | L1524+ | 128.6 | (*) | 3850 | 0.59±0.06 | 0.5 | 1.0–1.3 |
| CI Tau | L1536 | 160.3 | (*) | 4600 | 1.35±0.26 | 1.0 | 1.3–2.1 |
| DM Tau | L1551 | 144.0 | (*) | 3700 | 0.21 ±0.03 | 0.4 | 2.9–6.0 |
| HN Tau | L1551 | 134.4* | (*)* | 4300 | – | (1.6) | – |
| DL Tau | L1521+ | 159.9 | (*) | 4000 | 0.89±0.11 | 0.6 | 0.9–1.2 |
| GK Tau | L1524 | 129.1 | (*) | 4400 | 0.84±0.06 | 0.5 | 0.6–1.0 |
| GI Tau | L1524 | 129.4 | (*) | 4100 | 0.80±0.11 | 0.7 | 1.5–1.7 |
| V807 Tau | L1524 | 184.1* | (*)** | 4400+2*3600 | (2.2+2*0.9)±0.3 | 0.5+2*0.4 | 0.4–0.6 |
| UZ Tau | L1524 | 123.1* | (**)** | 3700+3400 | (0.5+0.3)±0.09 | 0.4+0.3 | 0.9–1.4 |
| GG Tau | L1551 | 145.5 | ((**)(*)) | 3800+2*3500 | (0.7+2*0.3)±0.05 | 0.5+2*0.4 | 0.8–2.0 |
| V710 Tau | L1551 | 146.0 | (*)* | 3600 | 0.62±0.05 | 0.4 | 0.4–0.8 |
| XZ Tau | L1551 | (144) | (*)(*) | 2*3600 | 2*(0.29±0.04) | 2*0.4 | 1.7–2.8 |
| DK Tau | L1524 | 132.0 | (*)(*) | 3900+3600 | (1.2+0.5)±0.05 | 0.6+0.4 | 0.4–0.6 |
| UX Tau | L1551 | 142.2 | (*)** | 5200+3700 | (1.8+0.4)±0.2 | 1.4+0.5 | 6.1–10.0 |
| IQ Tau | L1524 | 131.5 | (*) | 3800 | 0.73±0.13 | 0.5 | 0.7–1.0 |
| DH Tau | L1524 | 133.4 | (*)(*) | 3600 | 0.58±0.12 | 0.4 | 0.4–0.9 |
| DG Tau | L1524 | 125.3* | (*) | 4000 | 1.53±0.29 | 0.6 | 0.3–0.6 |
| IP Tau | HD28354 | 129.4 | (*) | 3800 | 0.41±0.03 | 0.6 | 1.8–2.8 |
| T Tau | T Tau | 145.1 | (*)(**) | 5200 | 10.40±0.90 | 2+2+0.5 | 0.7–1.0 |
| RY Tau | L1495 | 138.2* | (*) | 5700 | 11.80±2.90 | 2.3 | 2.4–2.6 |
| DE Tau | L1495 | 128.0 | (*) | 3700 | 0.62±0.07 | 0.4 | 0.7–1.0 |
| BP Tau | L1495 | 127.4 | (*) | 3700 | 0.69±0.04 | 0.4 | 0.5–1.0 |
| V409 Tau | L1524 | 129.7 | (*) | 3600 | 0.22±0.03 | 0.4 | 2.7–5.6 |
| CY Tau | L1495 | 126.3 | (*) | 3700 | 0.38±0.04 | 0.5 | 1.8–2.2 |
| CX Tau | L1495 | 126.7 | (*) | 3500 | 0.26±0.02 | 0.4 | 1.3–2.8 |
| CW Tau | L1495 | 131.5 | (*) | 4800 | 1.59±0.34 | 1.3 | 3.1–5.1 |
Notes. The HD35187 group is formally an association near Taurus. The extended name of the group L1524 is L1524/L1529/B215 (Luhman 2023), comprising the three individual clouds. The same applies to L1521 (L1521/B213) and L1495 (L1495/B209). In sources with a poor Gaia solution (see Sect. 2.1), the distance is accompanied by an asterisk. In all other cases, the tabulated distance has an error of less than 1.5 pc. XZ Tau has no parallax available from Gaίa, and we assume the average distance to its group. Parentheses and asterisks indicate the geometry of disk and star(s), respectively. The effective temperature is relative to the primary and of any companion within 3" that is bright enough to account for a significant percentage of optical/NIR photometry (10% of the primary). The masses of T Tau are obtained astrometrically (Köhler et al. 2016) as most of the observed optical luminosity is from N (Sa and Sb are heavily extincted). The mass of HN Tau is obtained by Gangi et al. (2022) considering obscuration effects.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.