Table 1
Stellar parameters, G0, measured flux, and derived dust mass of the Orion sample used in this work.
| Nr. | Name | RA (h:m:s) | Dec (deg:m:s) | Dist. (pc) | M⋆ (M⊙) | L⋆ (L⊙) | Sp.Tp. | Log10(G0) | Flux (mJy) | Mdust (M⊕) |
|---|---|---|---|---|---|---|---|---|---|---|
| 1. | BF Ori* | 05:37:13.3 | −06:35:01.0 | 378 | 1.9 | 13 | A2 | 1.87 | 0.8 | 1.1 ± 0.1 |
| 2. | CO Ori | 05:27:38.3 | +11:25:39.0 | 395 | 2.3 | 23 | F3 | 0.09 | 1.5 | 2.4 ± 0.5 |
| 3. | HBC 442 | 05:34:14.2 | −05:36:54.0 | 383 | 2.0 | 10 | F8 | 2.66 | 4.0 | 7.8 ± 1.6 |
| 4. | HD 244314 | 05:30:19.0 | +11:20:20.0 | 398 | 2.1 | 19 | A2 | 0.18 | 5.9 | 10.2 ± 2.0 |
| 5. | HD 244604 | 05:31:57.3 | +11:17:41.0 | 398 | 2.2 | 34 | A2 | 0.27 | 4.4 | 6.5 ± 1.3 |
| 6. | HD 245185* | 05:35:09.6 | +10:01:51.0 | 410 | 2.2 | 30 | B9 | 3.19 | 34.6 | 37.5 ± 3.8 |
| 7. | HD 287823 | 05:24:08.0 | +02:27:47.0 | 343 | 1.8 | 12 | A4 | 1.31 | 8.0 | 11.7 ± 2.3 |
| 8. | HD 288012 | 05:33:04.8 | +02:28:10.0 | 341 | <1.9 | 14 | A2 | 1.75 | <1.4 | <5.8 |
| 9. | HD 290380 | 05:23:31.0 | −01:04:24.0 | 343 | 1.6 | 6 | F5 | 1.09 | 10.6 | 18.6 ± 3.7 |
| 10. | HD 290409 | 05:27:05.5 | +00:25:08.0 | 404 | 2.2 | 25 | B9 | 0.90 | 10.1 | 16.8 ± 3.4 |
| 11. | HD 290500 | 05:29:48.1 | −00:23:43.0 | 402 | 1.9 | 13 | A2 | 1.45 | 11.9 | 23.7 ± 4.7 |
| 12. | HD 290764* | 05:38:05.3 | −01:15:22.0 | 397 | 2.0 | 22 | A5 | 1.71 | 210.1 | 91.2 ± 9.1 |
| 13. | HD 290770 | 05:37:02.4 | −01:37:21.0 | 393 | 2.6 | 55 | B8 | 1.70 | 3.5 | 4.4 ± 0.9 |
| 14. | HD 34282* | 05:16:00.5 | −09:48:35.0 | 306 | <1.9 | 14 | A0 | 0.05 | 99.0 | 86.7 ± 8.7 |
| 15. | HD 34700 | 05:19:41.4 | +05:38:43.0 | 347 | 2.6 | 23 | F8 | 0.02 | 8.1 | 10.2 ± 2.0 |
| 16. | HD 35929 | 05:27:42.8 | −08:19:39.0 | 377 | 3.5 | 93 | A9 | 0.73 | <0.7 | <2.0 |
| 17. | HD 36917 | 05:34:47.0 | −05:34:15.0 | 445 | 4.4 | 407 | B8 | 2.86 | <0.8 | <2.3 |
| 18. | HD 36982 | 05:35:09.8 | −05:27:53.0 | 404 | <6.4 | 1349 | B2 | 3.76 | <0.8 | <1.3 |
| 19. | HD 37258* | 05:36:59.3 | −06:09:16.0 | 377 | 2.3 | 26 | A0 | 2.30 | 1.8 | 2.1 ± 0.2 |
| 20. | HD 37357* | 05:37:47.1 | −06:42:30.0 | 465 | 2.8 | 87 | B9 | 2.01 | 2.9 | 3.8 ± 0.4 |
| 21. | HD 37371 | 05:38:09.9 | −00:11:01.0 | 405 | 3.1 | 100 | B8 | 2.36 | <0.6 | <2.0 |
| 22. | HD 37806 | 05:41:02.3 | −02:43:01.0 | 397 | 3.5 | 200 | B8 | 1.90 | 3.4 | 3.1 ± 0.6 |
| 23. | HD 38087 | 05:43:00.6 | −02:18:45.0 | 373 | 4.2 | 347 | B5 | 1.79 | <0.6 | <1.2 |
| 24. | HD 38120 | 05:43:11.9 | −04:59:50.0 | 381 | 2.8 | 71 | B8 | 0.13 | 31.9 | 35.6 ± 7.1 |
| 25. | NV Ori | 05:35:31.4 | −05:33:09.0 | 384 | 2.1 | 59 | F0 | 3.22 | 4.0 | 4.8 ± 1.0 |
| 26. | RY Ori | 05:32:09.9 | −02:49:47.0 | 347 | 1.6 | 6 | F4 | 0.64 | 10.6 | 19.1 ± 3.8 |
| 27. | T Ori | 05:35:50.5 | −05:28:35.0 | 399 | 2.5 | 59 | A0 | 3.25 | 1.5 | 1.9 ± 0.4 |
| 28. | UX Ori | 05:04:30.0 | −03:47:14.0 | 320 | 1.9 | 13 | A3 | 0.29 | 20.2 | 25.2 ± 5.0 |
| 29. | V1012 Ori* | 05:11:36.5 | −02:22:48.5 | 386 | 1.3 | 6 | A3 | 0.08 | 26.4 | 47.8 ± 4.8 |
| 30. | V1787 Ori* | 05:38:09.3 | −06:49:17.0 | 394 | 2.1 | 28 | A3 | 1.47 | 14.8 | 18.2 ± 1.8 |
| 31. | V346 Ori | 05:24:42.8 | +01:43:48.0 | 336 | 1.6 | 7 | A7 | 2.32 | 15.3 | 24.8 ± 5.0 |
| 32. | V350 Ori | 05:40:11.8 | −09:42:11.0 | 391 | <1.9 | 9 | A1 | 0.27 | 4.4 | 9.1 ± 1.8 |
| 33. | V351 Ori | 05:44:18.8 | +00:08:40.0 | 323 | 2.0 | 21 | A7 | 0.18 | 69.4 | 77.4 ± 15.5 |
| 34. | V380 Ori* | 05:36:25.4 | −06:42:58.0 | 374 | 2.8 | 95 | B9 | 1.84 | 6.2 | 5.1 ± 0.5 |
| 35. | V599 Ori* | 05:38:58.6 | −07:16:46.0 | 401 | 2.1 | 31 | A4 | 0.60 | 55.9 | 69.0 ± 6.9 |
Notes. For the disks with an asterisk the fluxes have been taken from Stapper et al. (2022); Stapper et al. (2024) and van Terwisga et al. (2022). In addition to the fluxes there is an absolute calibration error, which is 10% for ALMA, and 20% for NOEMA. Except for the UV irradiance G0, continuum flux, and inferred dust mass which we derive in this work, all parameters are taken from Guzmán-Díaz et al. (2021), see this paper for their corresponding uncertainties. For V1012 Ori, the parameters are taken from Vioque et al. (2018), and the continuum flux is determined from the ALMA pipeline product data. HD 290764 is ALMA Band 7 data.
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