Table 3
Spectral types from our observations.
| Name | PN G | AR(2000) | Dec(2000) | Sp. Type | E.T.[s] (grating) |
|
|
|||||
| H 1-62 | 000.0–06.8 | 18 13 17.9 | –32 19 43.0 | emission-line | 3600 (300) |
| PC 12 | 000.1+17.2 | 16 43 49.3 | –18 56 33.0 | OB | 2 × 1200 (300) |
| IC 4634 | 000.3+12.2 | 17 01 33.5 | –21 49 33.1 | emission-line | 3 × 1000 (300) |
| H 1-63 | 002.2–06.3 | 18 16 18.5 | –30 07 35.8 | OB? | 3600 (300) |
| M 1-38 | 002.4–03.7 | 18 06 05.8 | –28 40 34.3 | cont. | 3600 (300) |
| M 1-53 | 015.4–04.5 | 18 35 48.2 | –17 36 08.4 | emission-line? | 3600 (300) |
| Sa 1-8 | 020.7–05.9 | 18 50 44.2 | –13 31 02.4 | OB | 3600 (300) |
| IRAS 19021+0209 | 036.4-01.9 | 19 04 38.5 | 02 14 23.0 | cont. | 3600 (300) |
| M 1-6 | 211.2–03.5 | 06 35 44.6 | –00 05 41.1 | emission-line | 3600 (300) |
| SaSt 2-3 | 232.0+05.7 | 07 48 03.5 | –14 07 42.6 | OB | 3600 (300) |
| M 1-11 | 232.8–04.7 | 07 11 16.6 | –19 51 03.0 | emission-line | 3600 (300) |
| M 1-14 | 234.9–01.4 | 07 27 56.5 | –20 13 23.4 | OB | 2 × 3600 (300) |
| M 1-12 | 235.3–03.9 | 07 19 21.4 | –21 43 55.3 | emission-line | 3600 (300) |
| Y-C 2-5 | 240.3+07.0 | 08 10 41.7 | –20 31 32.9 | emission-line | 3600 (300) |
| KLSS 1-9 | 240.8–19.6 | 06 24 36.4 | –33 04 49.0 | OB | 3600 (300) |
| M 3-4 | 241.0+02.3 | 07 55 11.2 | –23 37 45.6 | cont. | 3600 (300) |
| M 3-1 | 242.6–11.6 | 07 02 49.6 | –31 35 41.3 | cont. | 3600 (300) |
| M 4-2 | 248.8–08.5 | 07 28 55.2 | –35 45 15.4 | emission-line | 3600 (300) |
| Ns 238 | 254.6+00.2 | 08 20 56.7 | –36 13 46.7 | OB | 2 × 3600 (300) |
| PB 2 | 263.0–05.5 | 08 20 39.8 | –46 20 13.2 | emission-line? | 2 × 1200 (300) |
| PB 4 | 275.0–04.1 | 09 15 07.6 | –54 52 38.5 | emission-line? | 3600 (300) |
| IC 2501 | 281.0–05.6 | 09 38 47.5 | –60 05 27.9 | emission-line | 2 × 3600 (300) |
| IC 2553 | 285.4–05.3 | 10 09 21.7 | –62 36 40.9 | emission-line | 4 × 300 (300) |
| He 2-47 | 285.6–02.7 | 10 23 09.0 | –60 32 34.3 | emission-line | 2 × 2700 (300) |
| IC 2621 | 291.6–04.8 | 11 00 19.5 | –65 14 54.2 | emission-line | 2 × 3600 (300) |
| Lo 6 | 294.1+14.4 | 12 00 43.5 | –47 33 12.0 | cont. | 3600 (300) |
| Th 2-A | 306.4–00.6 | 13 22 34.8 | –63 20 55.2 | emission-line | 3600 (300a |
| He 2-97 | 307.2–09.0 | 13 45 24.0 | –71 28 48.8 | emission-line | 3600 (300) |
| He 2-105 | 308.6–12.2 | 14 15 25.7 | –74 12 49.8 | OB | 3600 (300) |
| NGC 5307 | 312.3+10.5 | 13 51 03.3 | –51 12 15.9 | emission-line | 3600 (300) |
| He 2-107 | 312.6–01.8 | 14 18 42.5 | –63 07 10.7 | emission-line | 2 × 3600 (300) |
| He 2-434 | 320.3–28.8 | 19 33 50.7 | –74 32 58.7 | OB | 3600 (300) |
| NGC 5979 | 322.5–05.2 | 15 47 40.6 | –61 13 02.7 | emission-line | 2 × 1500 (300) |
| He 2-128 | 325.8+04.5 | 15 25 07.9 | –51 19 40.9 | emission-line? | 3600 (600) |
| WRAY 17-75 | 329.5–02.2 | 16 12 34.4 | –54 23 35.3 | OB | 3600 (300) |
| He 2-187 | 337.5–05.1 | 17 01 37.4 | –50 22 56.6 | OB | 3600 (300) |
| NGC 6026 | 341.6+13.7 | 16 01 20.8 | –34 32 38.0 | OB | 3600 (300) |
| PC 17 | 343.5–07.8 | 17 35 41.1 | –46 59 51.3 | emission-line | 3600 (600) |
| Cn 1-3 | 345.0–04.9 | 17 26 11.8 | –44 11 29.1 | emission-line? | 4 × 700 (300) |
| IC 4663 | 346.2–08.2 | 17 45 28.5 | –44 54 11.5 | emission-line? | 4 × 700 (600) |
| IC 4699 | 348.0–13.8 | 18 18 31.2 | –45 59 03.2 | emission-line | 3600 (600) |
| NGC 6337 | 349.3–01.1 | 17 22 16.0 | –38 28 57.6 | emission line | 3600 (300) |
| Fg 3 | 352.9–07.5 | 18 00 11.9 | –38 49 51.7 | cont. | 3600 (300) |
| H 1-35 | 355.7–03.5 | 17 49 13.9 | –34 22 53.3 | emission-line? | 2 × 1700 (300) |
| Te 2022 | 358.8–00.0 | 17 42 42.4 | –29 51 35.4 | OB | 3600 (300) |
Notes. The PNe are denoted by their common name and by their PN G designation. Fifth column lists the preliminary spectral type that we have adopted for each CSPN. The last column indicates the exposure time and grating used (300 or 600 line mm-1).
GEMINI observation, see Weidmann et al. (2008).
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