Table 2
Polarimetric properties of the sample.
| Source | r(′′) | PA (°) | δpol (10−3) | DoLP (%) | AoLP (°) | Remarks |
|---|---|---|---|---|---|---|
| CI Tau | 1.3 ± 0.3 | 0.56 ± 0.06 | 77.9 ± 2.8 | |||
| HD 287823 | 0.5 ± 0.4 | 0.16 ± 0.12 | 87.6 ± 42.5 | |||
| HD 287823 B | 2.32 | 329 | – | <0.6 | – | Upper limit on DoLP is not very constraining. |
| HD 245185 | 1.0 ± 0.2 | 1.14 ± 0.13 | 169.6 ± 3.5 | |||
| HD 290770 | <0.2 | 1.00 ± 0.04 | 88.4 ± 1.1 | Possible circumstellar unresolved polarization. | ||
| TW Cha | 0.5 ± 0.3 | 0.43 ± 0.01 | 148.3 ± 0.4 | |||
| DI Cha | <0.3 | 1.42 ± 0.03 | 143.7 ± 1.1 | Large AV. DoLP may be due to interstellar material. | ||
| DI Cha BC | 4.58 | 201 | – | 1.3 ± 0.6 | 141 ± 2 | Large AV. DoLP may be due to interstellar material. |
| DI Cha D | 0.22 | 245 | – | 1.3 ± 0.1 | 137 ± 2 | Large AV. DoLP may be due to interstellar material. |
| HD 98922 | 0.2 ± 0.1 | 0.42 ± 0.13 | 17.6 ± 4.2 | |||
| HD 98922 B | 4.61 | 1 | – | 0.4 ± 0.1 | 157 ± 9 | Foreground object (Gaia EDR3). |
| GW Lup | 0.4 ± 0.2 | 0.18 ± 0.11 | 161.6 ± 42.0 | |||
| HD 142666 | 1.4 ± 0.7 | 1.11 ± 0.23 | 68.8 ± 9.7 | |||
| HD 144432 | 0.5 ± 0.3 | 0.43 ± 0.17 | 12.2 ± 40.6 | |||
| HD 144432 B | 1.43 | 6 | – | >0.7 | 153 ± 3 | The stellar flux is saturated. |
| HD 144432 C | 0.08 | 336 | – | >0.7 | 145 ± 4 | The stellar flux is saturated. r and PA from B. |
| V1003 Oph | 0.2 ± 0.1 | 0.48 ± 0.05 | 163.3 ± 1.9 | |||
| WSB82 | 0.4 ± 0.2 | 3.55 ± 0.05 | 56.4 ± 0.5 | Large AV. DoLP may be due to interstellar material. | ||
| HD 150193 | <0.3 | 2.36 ± 0.81 | 58.4 ± 8.4 | Large AV. DoLP may be due to interstellar material. | ||
| HD 150193 B | 1.12 | 228 | – | 2.0 ± 0.3 | 58 ± 3 | Large AV. DoLP may be due to interstellar material. |
| AK Sco | 1.5 ± 0.8 | 1.25 ± 0.05 | 135.3 ± 3.0 | |||
| HD 179218 | 2.3 ± 0.6 | 0.98 ± 0.17 | 101.8 ± 6.0 | |||
| HD 179218 B | 2.35 | 139 | – | 0.8 ± 0.1 | 70 ± 1 | Possible circumstellar unresolved polarization. |
| HD 179218 C | 3.75 | 338 | – | <0.5 | – |
Notes. Columns: source name, separation and position angle from the primary star (for companions only), resolved polarized-to-stellar light contrast (see Sect. 3.3), degree and angle of linear unresolved polarization (see Sect. 3.4), remarks. The PA of a disk inducing the unresolved polarization is expected to be perpendicular to the AoLP. DI Cha B and C are not resolvedin our image.
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