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Table 1

Overview of the objects in our sample.

Object RA (J2000) Dec (J2000) SpT d (pc) Teff (K) L* (L) Reference
CX Tau 04:14:47.862 26:48:11.014 M1.5 126.7 3487 0.34 (1)
CY Tau 04:17:33.728 28:20:46.812 M1.5 124.3 3516 0.37 (1)
BP Tau 04:19:15.834 29:06:26.926 K5/7 128.2 3777 0.83 (1)
FT Tau 04:23:39.189 24:56:14.250 M2.8 129.9 3415 0.44 (1)
DF Tau 04:27:02.793 25:42:22.453 M3 176.4 3900 3.89 (1)
DL Tau 04:33:39.077 25:20:38.101 K7 159.5 4276 1.47 (1)
DM Tau 04:33:48.734 18:10:09.973 M2 144.8 3715 0.16 (2,3)
AA Tau 04:34:55.420 24:28:53.033 K5 137.7 3762 0.72 (1)
DN Tau 04:35:27.378 24:14:58.910 M1: 127.2 3806 0.69 (1)
LkCa 15 04:39:17.791 22:21:03.390 K5 154.8 4276 1.12 (1)
DR Tau 04:47:06.215 16:58:42.813 K5 186.9 4202 3.71 (1)
RW Aur A 05:07:49.565 30:24:05.131 K0 a 150.0 4870 0.83 (1,4)
RW Aur B 05:07:49.456 30:24:04.775 K6.5a 150.0 4160 0.50 (1,4)
SY Cha 10:56:30.388 −77:11:39.401 K5 180.7 4060 0.43 (1)
TW Hya 11:01:51.905 −34:42:17.033 K6 59.9 4000 0.34 (1)
VW Cha A 11:08:01.482 −77:42:28.567 K7 188.1 4060 2.21 (1,5)
WX Cha A 11:09:58.853 −77:37:08.631 M1 189.3 3710 1.13 (1,5)
XX Cha 11:11:39.673 −76:20:15.032 M3 194.6 3340 0.29 (1)
Sz 50 13:00:55.382 −77:10:22.247 M3 148.9 3400 0.41 (6)
PDS 70 14:08:10.155 −41:23:52.573 K7 112.3 4138 0.38
GW Lup 15:46:44.729 −34:30:35.677 M1.5 155.2 3632 0.33 (1)
IM Lup 15:56:09.207 −37:56:06.126 M0 153.8 4350 2.57 (1)
Sz 98 16:08:22.494 −39:04:46.427 M0.4 156.2 4060 1.51 (1)
V1094 Sco 16:08:36.177 −39:23:02.464 K6/K5 152.4 4205 1.15 (1)
RNO 90 16:34:09.170 −15:48:16.776 G5 114.9 5662 5.7 (7)
WA Oph 6 16:48:45.633 −14:16:35.849 K6 122.5 4169 2.88 (8)

Notes. This compilation of stellar parameters is based on Henning et al. (2024). Coordinates (ICRS) and spectral types (SpT) are taken from SIMBAD, unless otherwise noted. Distances (d), effective temperatures (Teff), and stellar luminosities (L*) are collected from Gaia DR3 (not noted), (1) Testi et al. (2022), (2) Kenyon & Hartmann (1995), (3) Bertout et al. (2007), (4) Herczeg & Hillenbrand (2014), (5) Daemgen et al. (2013), (6) Sartori et al. (2003), (7) Ghez et al. (1993), and (8) Andrews et al. (2009). (a)Herczeg & Hillenbrand (2014).

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