Table 4
Perturbers close to detection based on the mass estimates of Sect. 4.1.
| ID | Gap | Location | Planet mass | AMES-DUSTY | BEX-HOT |
|---|---|---|---|---|---|
| (au) | (MJup) | (MJup) | (MJup) | ||
| HD 34282 | In-cavity | 44 | 11.7 | 10.0 | 11.8 |
| SZ Cha | In-cavity | 19 | 9.3 | 4.1 | 6.2 |
| HD 135344B | In-cavity | 12 | 8.8 | 5.8 | 7.0 |
| HD 135344B | Spiral | 100 | 5–10 | 3.8 | 4.9 |
| RX J1604 | In-cavity | 33 | 6.2 | 5.1 | 6.4 |
| HD 36112 | Spiral | 140 | 5.0 | 4.6 | 5.8 |
| PDS 70 | In-cavity | 27 | 4.9 | 4.1 | 5.3 |
| RX J1615 | In-cavity | 22 | 4.5 | 2.5 | 4.3 |
| HD 169142 | In-cavity | 10 | 3.5 | 8.1 | 9.5 |
| HD 97048 | In-rings | 127 | 1.3 | 3.9 | 5.5 |
| PDS 66 | In-rings | 55 | 1.2 | 2.5 | 3.5 |
Notes. Perturbers that, according to the estimations of Fig. 7, are the most promising to be found. PDS 70 treated as planet-less here. Planet masses in gaps and creating the spiral patterns are taken as described in Fig. 6. The columns AMES-DUSTY and BEX-HOT are our derived SPHERE detection limits (best of ANDROMEDA/IRDIS and ASDI/IFS) using the AMES-DUSTY and BEX-HOT models (see Sect. 3). References for the locations of the perturbers can be found in Appendix A. See also Fig. A.1 for a sketch of these morphologies.
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