Table 5
Stellar properties and most probable disk parameters for the known YSOs in Cha II detected by the HGBS.
| Main | T eff † | A V † | R ⋆ † | M ⋆ † | Rin♣ | RC♣ | Mdisk♣ | Flaring angle♣ | Inclination | ε 0 |
| designation | [K] | [mag] | [R⊙] | [M⊙] | [AU] | [AU] | [M⊙] | [1 + φ] | angle♣ [deg] | |
|
|
||||||||||
| IRAS 12416-7703 | 3487 | 3.36 | 3♠ | 2♠ | 0.02–0.1 (32%) | >5 (27%) | >0.001 (40%) | 1.1 (26%) | 40 (33%) | 1.17 |
| IRAS 12496-7650 | 7200 | 10.55 | 2.77 | 2 | 0.05–0.1 (33%) | >50 (20%) | >0.1 (50%) | 1.3–1.4 (25%) | 10 (35%) | 0.39 |
| IRAS 12500-7658* | 4350 | 6.85 | 1.00 | 0.60 | 0.1 (33%) | >10 (19%) | >0.01 (36%) | 1.3–1.4 (26%) | 40 (27%) | 0.61 |
| IRAS 12535-7623 | 3850 | 3.36 | 2.71 | 0.67 | 0.02 (34%) | >50 (23%) | >0.0001 (99%) | 1.1–1.4 (25%) | 70 (28%) | 0.18 |
| WFI J12585611-7630105 | 3025 | 1.66 | 1.13 | 0.12 | 0.02–0.1 (33%) | >150 (20%) | >0.0001 (59%) | 1.3 (25%) | 70 (26%) | 0.07 |
| ISO-CHAII 28 | 4500 | 38.9 | 2.5♠ | 1.5♠ | 0.02 (34%) | >10 (37%) | >0.01 (36%) | 1.1 (27%) | 10 (34%) | 1.32 |
| C 41 | 3057 | 2.17 | 0.37 | 0.10 | 0.05–0.1 (30%) | >5 (25%) | >0.0001 (50%) | 1.1 (30%) | 90 (36%) | 0.28 |
| Sz 49 | 3777 | 2.28 | 1.03 | 0.62 | 0.05–0.1 (34%) | >100–200 (17%) | >0.001 (28%) | 1.3–1.4 (25%) | 10–70 (29%) | 0.07 |
| Sz 50 | 3415 | 3.78 | 3.10 | 0.35 | 0.02–0.05 (33%) | >100 (27%) | >0.0001 (99%) | 1.1–1.4 (25%) | 90 (27%) | 0.61 |
| RX J1301.0-7654a | 4350 | 1.93 | 2.67 | 0.7 | 0.02 (29%) | >100 (24%) | >0.0001 (86%) | 1.1 (26%) | 40 (35%) | 0.40 |
| IRASF 12571-7657 | 4730 | 9.03 | 2♠ | 1♠ | 0.02 (34%) | >10 (18%) | >0.0001 (92%) | 1.1 (30%) | 70 (28%) | 0.44 |
| Sz 51 | 3955 | 1.54 | 1.37 | 0.7 | 0.02–0.1 (33%) | >50 (25%) | >0.0001 (99%) | 1.1 (26%) | 10–90 (25%) | 0.35 |
| CM Cha | 4060 | 1.52 | 1.78 | 0.85 | 0.1 (34%) | >10–50 (17%) | >0.01 (28%) | 1.4 (26%) | 10–70 (29%) | 0.18 |
| IRAS 12589-7646 | 3300 | 3.98 | 2.8♠ | 2♠ | 0.02 (31%) | >100 (21%) | >0.0001 (88%) | 1.1 (27%) | 40 (33%) | 0.67 |
| Hn 22 | 3560 | 0.61 | 1.24 | 0.42 | 0.05–0.1 (34%) | > 5 (23%) | >0.001 (36%) | 1.2 (26%) | 70 (30%) | 0.23 |
| Hn 23 | 4350 | 1.24 | 1.60 | 1 | 0.02–0.1 (31%) | > 5 (19%) | >0.001 (45%) | 1.1 (26%) | 40 (31%) | 0.07 |
| Sz 52 | 3487 | 4.14 | 1.15 | 0.35 | 0.02–0.1 (31%) | >100 (21%) | >0.0001 (54%) | 1.2? (25%) | 40 (30%) | 0.25 |
| Hn 24 | 3850 | 2.76 | 2.37 | 0.65 | 0.02–0.1 (33%) | >50 (26%) | >0.0001 (99%) | 1.4 (26%) | 90 (26%) | 0.52 |
| Hn 25 | 3487 | 4.10 | 1.56 | 0.3 | 0.02 (34%) | >150 (26%) | >0.0001 (100%) | 1.2 (28%) | 10–90 (25%) | 0.26 |
| Sz 53 | 3705 | 3.68 | 1.39 | 0.55 | 0.02-0.1 (33%) | >50 (19%) | >0.0001 (97%) | 1.1 (27%) | 70 (28%) | 0.10 |
| Sz 54 | 4350 | 1.57 | 2.42 | 0.97 | 0.02 (33%) | >150 (39%) | >0.0001 (99%) | 1.1–1.2 (30%) | 10–70 (25%) | 0.63 |
| Sz 56 | 3270 | 3.18 | 1.78 | 0.23 | 0.02 (39%) | >200 (44%) | >0.0001 (89%) | 1.1 (30%) | 90 (28%) | 0.37 |
| Sz 58 | 4350 | 3.87 | 1.43 | 1 | 0.1 (33%) | >10 (17%) | >0.01 (29%) | 1.3–1.4 (25%) | 10–40 (31%) | 0.04 |
| Sz 59 | 4060 | 2.67 | 1.96 | 0.82 | 0.02–0.05 (34%) | >10–200 (18%) | >0.0001 (91%) | 1.1 (29%) | 10–70 (27%) | 0.28 |
| Sz 61 | 4350 | 3.13 | 1.87 | 1 | 0.02–0.1 (33%) | >10 (21%) | >0.01 (34%) | 1.3 (26%) | 10–70 (30%) | 0.15 |
| Sz 63 | 3415 | 1.61 | 1.38 | 0.32 | 0.05–0.1 (33%) | >200 (17%) | >0.001 (27%) | 1.4 (27%) | 10–70 (28%) | 0.04 |
Notes. For the disk parameters, we indicate the relative Bayesian probability in percentage between brackets. When several values of a given disk parameter are equally probable (i.e., partly flat Bayesian probability distribution, Figs. 7, 8), we report the compatible range. Disk mass (Mdisk) and size (RC) should be regarded as lower limits (Sect. 5.1). In the last column, we report the value of the intrinsic scatter (ε0) between the observed SED and the best-fitting SED model.
From Spezzi et al. (2008).
The values sample by the grid are as follows: Rin = [0.02, 0.05, 0.1, 0.5, 1, 5, 10] AU, RC = [5, 10, 50, 100, 150, 200] AU, Mdisk = [0.0001, 0.001,0.01, 0.1] M⊙, 1 + φ = [1.1, 1.2 ,1.3 ,1.4] and Inclination=[10, 40, 70, 90] deg.
Stellar mass and radius not provided in Spezzi et al. (2008). The values reported here are estimated from the best-fitting SED model, considering only models with the same Teff as the object.
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