Table 1
Stellar parameters.
| Source | RA (h.m.s.) | Dec (deg.m.s.) | Cloud | SpT (a) | Class (a) | d (pc) | M⋆ (M⊙) (e) |
|---|---|---|---|---|---|---|---|
| J13022287-7734494 | 13 02 22.8 | −77 34 49.6 | Member | M5 | II | 200.3 ± 2.1 (b) | 0.19 (0.13, 0.26) |
| J13071806-7740529 | 13 07 18.0 | −77 40 53.0 (a) | Member | M4.5 | II | 197.9 ± 3.1 (b) | 0.23 (0.17, 0.31) |
| J13082714-7743232 | 13 08 27.2 | −77 43 23.4 (a) | Member | M4.5 | II | 199.5 ± 2.6 (b) | 0.22 (0.16, 0.31) |
| CM Cha | 13 02 13.4 | −76 37 57.9 | Member | K7 | II | 194.1 ±1.5 (b) | 0.81 (0.63, 0.98) |
| Hn 22 | 13 04 22.8 | −76 50 05.6 | Member | M2 | II | 197.1 ± 1.9 (b) | 0.44 (0.34, 0.56) |
| Hn 23 | 13 04 24.0 | −76 50 01.3 | Member | K5 | II | 198.0 ± 1.8 (b) | 1.06 (0.88, 1.21) |
| Hn 24 A | 13 04 55.6 | −77 39 49.3 | Member | M0 | II | 196.7 ± 1.9 (b) | 0.57 (0.48, 0.72) |
| Hn 24 B | 13 04 55.6 | −77 39 51.0 | Uncertain | … | … | … | … |
| Hn 25 | 13 05 08.4 | −77 33 42.8 | Member | M2.5 | II | 198.0 ± 2.6 (b) | 0.37 (0.27, 0.49) |
| Hn 26 | 13 07 48.5 | −77 41 21.7 (a) | Member | M2 | II | 197.5± 2.5 (b) | 0.44 (0.33, 0.56) |
| IRAS12496-7650 | 12 53 17.1 | −77 07 10.9 | Background | F0 | II | 243.7 ± 22.0 (c) | >1.4 |
| IRAS12500-7658 | 12 53 42.7 | −77 15 11.8 | Uncertain | K5 | I | … | 0.08 (0.06, 0.11) |
| IRAS12535-7623 | 12 57 11.6 | −76 40 11.7 | Likely | M0 | II | 180.0 ± 9.5 (d) | 0.58 (0.49, 0.72) |
| ISO-CHAII 13 | 12 58 06.7 | −77 09 09.2 (a) | Uncertain | M7 | II | … | 0.08 (0.06, 0.11) |
| J130059.3-771403 | 13 00 59.2 | −77 14 03.0 | Likely | K3 | II | 200.2 ± 6.0 (d) | … |
| J130521.7-773810 | 13 05 21.7 | −77 38 10.1 (a) | Likely | … | F | 192.2 ± 3.6 (d) | … |
| J130529.0-774140 | 13 05 27.1 | −77 41 21.5 (a) | Uncertain | … | II | … | … |
| Sz 46 | 12 56 33.5 | −76 45 45.6 | Member | M1 | II | 195.6 ± 2.3 (b) | 0.54 (0.42, 0.66) |
| Sz 49 | 13 00 53.1 | −76 54 15.3 | Member | M0.5 | II | 194.3 ± 1.8 (b) | 0.57 (0.46, 0.70) |
| Sz 50 | 13 00 55.2 | −77 10 22.4 | Foreground | M3 | II | 147.4 ± 13.0 (c) | 0.33 (0.29, 0.40) |
| Sz 51 | 13 01 58.8 | −77 51 21.9 | Member | K8.5 | II | 195.9 ± 1.7 (b) | 0.71 (0.58, 0.86) |
| Sz 52 | 13 04 24.8 | −77 52 30.4 | Member | M2.5 | II | 199.4 ± 2.4 (b) | 0.40 (0.31, 0.51) |
| Sz 53 | 13 05 12.6 | −77 30 52.7 | Member | M1 | II | 198.3 ± 2.4 (b) | 0.54 (0.42, 0.66) |
| Sz 54 | 13 05 20.6 | −77 39 01.6 | Member | K5 | II | 196.7 ± 1.7 (b) | 1.03 (0.84, 1.24) |
| Sz 56 | 13 06 38.7 | −77 30 35.4 | Member | M4 | II | 194.1 ± 2.1 (b) | 0.25 (0.21, 0.32) |
| Sz 58 | 13 06 57.3 | −77 23 41.7 | Member | K5 | II | 193.5 ± 1.7 (b) | 1.01 (0.87, 1.14) |
| Sz 59 A | 13 07 09.2 | −77 30 30.9 | Likely | K7 | II | 193.3 ± 4.3 (d) | 0.78 (0.61, 0.99) |
| Sz 59 B | 13 07 09.1 | −77 30 30.2 | Uncertain | … | … | … | … |
| Sz 61 | 13 08 06.2 | −77 55 05.4 | Member | K5 | II | 199.0 ± 2.1 (b) | 1.07 (0.86, 1.26) |
| Sz 62 | 13 09 50.4 | −77 57 23.9 (a) | Likely | M2.5 | II | 212.7 ± 5.8 (d) | 0.36 (0.27, 0.48) |
| Sz 63 | 13 10 04.1 | −77 10 45.0 | Member | M3 | II | 200.0 ± 1.8 (b) | 0.33 (0.24, 0.45) |
| Sz 48 NE | 13 00 53.2 | −77 09 09.2 (a) | Unobserved | M0.5 | II | 198.6 ± 2.6 (b) | 0.59 (0.46, 0.71) |
| Sz 48 SW | 13 00 53.6 | −77 09 08.3 (a) | Unobserved | M1 | II | 197.8± 2.6 (b) | 0.54 (0.43, 0.66) |
| Sz 55 | 13 06 30.5 | −77 34 00.1 (a) | Unobserved | M2 | II | 198.2 ± 2.5 (b) | 0.44 (0.34, 0.57) |
| Sz 57 | 13 06 56.6 | −77 23 09.5 (a) | Unobserved | M5 | II | 195.6 ± 3.1 (b) | 0.23 (0.20, 0.27) |
| Sz 60 E | 13 07 23.3 | −77 37 23.2 (a) | Unobserved | M4 | II | 197.1± 2.6 (b) | 0.24 (0.19, 0.33) |
| IRASF 13052-1653N | 13 09 11.0 | −77 09 44.1 (a) | Unobserved | M1.5 | II | 201.5 ± 1.5 (b) | 0.48 (0.37, 0.61) |
| IRASF 13052-7653NW | 13 09 09.8 | −77 09 43.5 (a) | Unobserved | M0.5 | II | 196.9 ±1.8 (b) | 0.57 (0.46, 0.71) |
| Sz 64 | 13 14 03.8 | −77 53 07.8 (a) | Unobserved | M5 | II | 196.5± 2.6 (b) | 0.20 (0.13, 0.27) |
Notes. Coordinates are either from Spezzi et al. (2013, marked with (a)) or, for the sources detected with ALMA (see Table 2), from our continuum fit presented in Sect. 3.1. The column “Cloud” refers to the cluster membership discussed in Sect. 2.1. Stellar masses and confidence intervals are calculated with the pre-main sequence tracks by Baraffe et al. (2015), using luminosities and temperatures from Spezzi et al. (2008) rescaled using individual distances (Sect. 4.2.2).
References. (a)Spezzi et al. (2013), (b)Galli et al. (2021), (c)Gaia Collaboration (2021), (d)Gaia Collaboration (2018), (e)This work.
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