Table 3
Circumstellar spectrum overview in B243, B268, B275, and B337.
| Circumstellar lines | B243 | B268 | B275 | B337 | Fig. |
|---|---|---|---|---|---|
| Higher order H I lines | DV | DV | 5–7 | ||
| Lower order H I lines | DV | UV | UV | U | 5 |
| Na I doublet | AV | 11 | |||
| [O I] 630.0 nm | S | S | S | 7 | |
| Fe I & Fe II lines | A | D | 7 | ||
| O I 777.3nm | CV | AV | AV | A | 7 |
| O I 844.6 & 1128.7 nm | DV | DV | (D) | 5–7 | |
| C I lines | D | D | D | 7 | |
| Ca II triplet | (U) | DV | DV | DV | 5 |
| Mg I | D | D | D | 5 | |
| O I 926.2–926.6 nm | AV | A | A | A | 10 |
| Fe I 999.8 nm | S | S | S | 7 | |
| CO bandheads | (C) | C | C | C | 8 |
Notes. The presence and characteristic of the emission lines is indicated with ‘D’ if the line is double-peaked, ‘S’ for a single-peak line, ‘C’ when the emission is too complex to recognize a single or double peak, ‘U’ when it is unclear whether the line is double-peaked or has a single peak due to nebular subtraction residuals, and ‘A’ if the line is observed in absorption. Brackets mean that the line detection is weak, andV is added for a variable line, which is explored in Sect. 7. Not all stars show the same lines in their spectrum. The strongest differences in occurrence are between B243 and B268. Most emission lines are present and pronounced in B275. The last column indicates in which figure(s) the lines can be inspected.
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