Table E.1.
Identified emission lines in the V2376 Ori b spectrum and their associated Gaussian-integrated fluxes.
| Species | Wavelength (Å) | Fline (10−20 W/m2) |
|---|---|---|
| H↠| 4862 | 7.4 |
| [O I] | 6300 | 9.4 |
| [O I] | 6363 | 3.2 |
| [N II] | 6548 | 11* |
| Hα | 6565 | 93 |
| [N II] | 6584 | 18 |
| HeI | 6678 | 1.4* |
| HeI | 7065 | 1.9 |
| [O II] | 7320 | 4.6* |
| [O II] | 7330 | 2.0 |
| HeI | 8235 | 4.8* |
| OI | 8446 | 4.5 |
| HeI | 8499 | 7.1 |
| HI | 8543 | 6.1 |
| HI | 8599 | 1.1* |
| CaII | 8662 | 5.9 |
| [C I] | 8727 | 0.8 |
| HI | 8751 | 4.2* |
| HI | 8864 | 2.5* |
| HI | 9016 | 2.6 |
| HI | 9230 | 8.4 |
Notes. Unless otherwise indicated, fluxes are measured on the convolved spectrum. † this emission may be residual emission from the nebula, as there is significant noise in the spectrum at this wavelength. * non detection in the convolved spectrum: the flux is measured before convolution.
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