Table 2
Improved spectral classification and key lines in medium resolution spectra of WELS CSPNs.
| PN G | Name | S.T. | 4542 | 4686 | 5412 | Hβ | N v | C iv | O v | N.S. |
|
|
||||||||||
| 000.3+12.2 | IC 4634 | O3 I f* | A | AE | A | A | A | E | A | y |
| 009.6+14.8 | NGC 6309 | O(He) | A | A | A? | A | E | E? | – | y |
| 015.4−04.5 | M 1-53 | O3 I f | A | E | A | A | A | E | A | y |
| 025.8−17.9 | NGC 6818 | not classif | A? | E | A? | A? | - | E | – | y |
| 034.6+11.8 | NGC 6572 | Of-WR(H) | A | E | E | E | E | E | A | y |
| 038.2+12.0 | Cn 3-1 | O7 Ib (f) | A | – | A | A | – | A | – | n |
| 051.9−03.8 | M 1-73 | O3.5 I f | A | E | A | AE | A | E | – | y |
| 054.1−12.1 | NGC 6891 | O3 Ib (f*) | A | AE | A | A | A | E | A | y |
| 057.2−08.9 | NGC 6879 | O3f(He) | A | E | A | A? | A | E? | A | n |
| 058.3−10.9 | IC 4997 | not classif | A | E | – | – | A? | E | – | n |
| 096.4+29.9 | NGC 6543 | Of-WR(H) | A? | E | E | E | E | E | A | y |
| 159.0−15.1 | IC 351 | Of(H) | A | E? | A | A | E | N/D | A? | n |
| 190.3−17.7 | J 320 | O3 V ((f)) | A | A | A | A | A | N/D | A | y |
| 307.2−09.0 | He 2-97 | Of-WR(H) | AE | E | – | E | E | E | – | n |
| 312.3+10.5 | NGC 5307 | O3.5 V | A | A | A | A | A | E | A | y |
| 345.0−04.9 | Cn 1-3 | not classif | A | E? | A | E? | – | E | – | n |
| 348.0−13.8 | IC 4699 | O3 V ((f)) | A | A | A | A | A | E | A | y |
| 349.3−01.1 | NGC 6337 | not classif | E | E | E | E | E | E | – | y |
| 355.7−03.5 | H 1-35 | not classif | A | E? | A? | E | E? | E? | E? | n |
Notes. The N.S. column indicates whether or not it was possible to subtract the nebular component. The letters A and E mean that the ion was in absorption and emission, respectively. An undetected ion was denoted (–), and N/D means no data available in the corresponding spectral range. The columns labeled “N v”, “C iv” and “O v” indicate the doublet at 4603–19 Å, the doublet at 5801–11 Å and 5114 Å respectively. References for the C iv doublet at 5806 Å are Weidmann & Gamen (2011a), Tylenda et al. (1993), and the spectra shown in Figs. 6.
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