Table 4.
Accretion properties of the Chameleon I PENELLOPE targets obtained with FRAPPE.
| Name | Dist | SpT | Teff | AV | L⋆ | log(Lacc/L⊙) | M⋆_B15 | Macc_B15 | M⋆_S00 | Macc_S00 |
|---|---|---|---|---|---|---|---|---|---|---|
| [pc] | [K] | [mag] | [L⊙] | [M⊙] | [M⊙/yr] | [M⊙] | [M⊙/yr] | |||
| CHX18N | 192.0 | K5.5 | 4164 | 0.70 | 1.40 | −1.42 | 0.77 | 4.48 × 10−9 | 0.85 | 4.06 × 10−9 |
| CHX18N_ep2 | 192.0 | K5.5 | 4164 | 0.70 | 1.41 | −1.22 | 0.77 | 7.11 × 10−9 | 0.86 | 6.40 × 10−9 |
| CSCha | 190.0 | K5.5 | 4164 | 0.40 | 1.79 | −1.13 | 0.76 | 9.81 × 10−9 | 0.85 | 8.75 × 10−9 |
| CVCha | 192.0 | K3.0 | 4540 | 1.10 | 4.03 | 0.14 | 1.19 | 1.52 × 10−7 | 1.47 | 1.23 × 10−7 |
| Hn5 | 195.0 | M5.0 | 2980 | 0.80 | 1.79 × 10−1 | −2.30 | ... | ... | 0.15 | 2.14 × 10−9 |
| INCha | 193.0 | M5.0 | 2980 | 0.00 | 2.18 × 10−1 | −2.75 | ... | ... | 0.16 | 7.91 × 1010 |
| IPTau | 129.4 | M0.0 | 3900 | 1.10 | 3.96 × 10−1 | −1.21 | 0.63 | 5.43 × 10−9 | 0.64 | 5.31 × 10−9 |
| SYCha | 181.0 | K7.5 | 3960 | 0.70 | 5.63 × 10−1 | −0.80 | 0.63 | 1.58 × 10−8 | 0.67 | 1.52 × 10−8 |
| Sz10 | 184.0 | M4.5 | 3084 | 0.70 | 1.46 × 10−1 | −2.04 | 0.15 | 3.17 × 10−9 | 0.17 | 2.87 × 10−9 |
| Sz19 | 189.0 | G8.5 | 5104 | 1.50 | 7.17 | −1.083 | ... | ... | 2.36 | 4.79 × 10−9 |
| Sz45 | 192.0 | M0.0 | 3900 | 0.50 | 4.57 × 10−1 | −1.56 | 0.61 | 2.64 × 10−9 | 0.61 | 2.62 × 10−9 |
| VWCha | 190.0 | K7.0 | 4020 | 2.10 | 2.32 | −0.194 | ... | ... | 0.71 | 1.13 × 10−7 |
| VZCha | 191.0 | K7.5 | 3960 | 1.20 | 6.83 × 10−1 | −0.29 | 0.63 | 5.79 × 10−8 | 0.67 | 5.40 × 10−8 |
| WZCha | 193.0 | M5.0 | 2980 | 0.60 | 1.97 × 10−1 | −1.83 | ... | ... | 0.15 | 6.37 × 10−9 |
| XXCha | 192.0 | M2.5 | 3484 | 0.50 | 2.38 × 10−1 | −2.14 | 0.33 | 1.16 × 10−9 | 0.35 | 1.11 × 10−9 |
Notes. The stellar mass and mass accretion rates are computed with both the isochrones of Baraffe et al. (2015b) (marked as B15) and Siess et al. (2000) (marked as S00). CV Cha and CS Cha are binaries (Reipurth et al. 2002; Guenther et al. 2007, respectively). We do not report values that are outside of the ranges of the Baraffe et al. (2015b) isochrones.
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