Table 8.
Mean parallaxes and distances to Orion star-forming regions derived from VLBA (this work) and Gaia DR3 data.
| VLBA | KHL17 | Gaia DR3 | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|
| Region | # |  |
 |
 |
RA | Dec | θ | # |  |
 |
| Name | (mas) | (pc) | (pc) | (h m) | (° ′) | (′) | (mas) | (pc) | ||
| NGC 2068 | 3 | 2.47 ± 0.10 | 405 ± 16 | 388 ± 10 | 5 46.8 | +0 4.0 | 3 | 19 | 2.454 ± 0.009 | 407.5 ± 1.5 |
| NGC 2024 | 8 | 2.48 ± 0.03 | 403 ± 5 | 423 ± 15 | 5 41.7 | –1 51.4 | 15 | 160 | 2.551 ± 0.005 | 392.0 ± 0.7 |
| σ Orionis | 1 | 2.48 ± 0.07 | 407 ± 12 | 302 ± 32 a | 5 38.7 | –2 36.0 | 10 | 140 | 2.463 ± 0.004 | 406.0 ± 0.6 |
| ONC | 21 | 2.57 ± 0.01 | 388.5 ± 1.7 | 388 ± 5 | 5 36.3 | –5 23.4 | 15 | 497 | 2.539 ± 0.002 | 393.9 ± 0.4 |
| L1641 | 2 | 2.29 ± 0.06 | 438 ± 12 | 428 ± 10 | 5 42.6 | –8 12.0 | 10 | 96 | 2.369 ± 0.004 | 422.2 ± 0.8 |
Notes.
KHL17 do not list this distance for the region. We added it here as it is related to the same source we analyzed. However, as noticed by those authors, the value is affected by the fact that the source was detected in three epochs and classified as a binary candidate.
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