Table 1
Full list of stellar and substellar companions detected in the NaCo-ISPY PPD sample.
| Target | Sep (″) | Proj. sep. (au) | PA (°) | ΔL′ | Method | Other reference |
|---|---|---|---|---|---|---|
| HD 35187 B | 1.366 ± 0.013 | 222.4 ± 2.8 | 193.8 ± 0.2 | 2.3 ± 0.1 | Gaussian fit | Dunkin & Crawford (1998) |
| HD 37411 B | 0.456 ± 0.013 | 161.0 ± 5.3 | 356.7 ± 0.2 | 1.7 ± 0.1 | Gaussian fit | Thomas et al. (2007) |
| HD 37411 C | 0.579 ± 0.013 | 204.4 ± 5.7 | 349.8 ± 0.2 | 2.0 ± 0.1 | Gaussian fit | Thomas et al. (2007) |
| HD 38120 B | 1.265 ± 0.013 | 490.1 ± 8.1 | 128.6 ± 0.2 | 0.4 ± 0.1 | Gaussian fit | – |
| V* NX Pup B | 0.182 ± 0.017 | 75.2 ± 16.6 | 86.1 ± 1 .7 | 6.3 ± 0.4 | MCMC | Schoeller et al. (1996) |
| HD 72106 B | 0.761 ± 0.013 | 293.3 ± 10.0 | 29.4 ± 0.2 | −0.1 ± 0.1 | Gaussian fit | Vieira et al. (2003) |
| HD 100453 B | 1.076 ± 0.013 | 112.5 ± 1.4 | 129.6 ± 0.2 | 6.1 ± 0.2 | Gaussian fit | Collins et al. (2009) |
| HD 101412B | 0.533 ± 0.005 | 221.2 ± 2.0 | 147.9 ± 0.3 | 8.0 ± 0.1 | MCMC | Ruh et al. (in prep.) |
| HD 101412C | 0.170 ± 0.009 | 70.7 ± 3.7 | 181.0 ± 1.3 | 7.4 ± 0.2 | MCMC | Ruh et al. (in prep.) |
| HD 104237 B | 1.373 ± 0.013 | 147.5 ± 0.7 | 254.0 ± 0.2 | 6.2 ± 0.1 | Gaussian fit | Grady et al. (2004) |
| PDS70b | 0.207 ± 0.015 | 23.4 ± 1.6 | 149.8 ± 1.7 | 6.8 ± 0.2 | – | Stolker et al. (2020a) |
| PDS70c | 0.254 ± 0.010 | 28.8 ± 1 .1 | 283.3 ± 2.0 | 6.6 ± 0.2 | – | Haffert et al. (2019) |
| HD 144432 BC | 1.490 ± 0.013 | 232.4 ± 2.2 | 5.9 ± 0.2 | 1.6 ± 0.1 | Gaussian fit | Müller et al. (2011) |
| V* KKOph B | 1.602 ± 0.013 | 269.6 ± 6.4 | 244.1 ± 0.2 | 2.5 ± 0.1 | Gaussian fit | Leinert et al. (1997) |
| V* R CrAB | 0.187 ± 0.006 | 23.4 ± 1.6 | 132 ± 0.7 | 6.7 ± 0.2 | – | Cugno et al. (2019b) |
Notes. If a method is reported, separation, position angle, and contrast were calculated as detailed in Sect. 4.3. If a method is not reported, the values of the astrometric and photometric parameters were taken from the reference reported in the last column, as the same dataset was already presented in those papers.
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