Table 1
Our sample of 11 PNe with known expansion distances and existing Gaia DR2 trigonometric distances.
| Object | DR2 Parallax | DDR2 | Dexp |  |
Vpost | Fshell |  |
Vrim | Frim |
|---|---|---|---|---|---|---|---|---|---|
| (mas) | (kpc) | (kpc) | (kpc) | (km s−1) | (kpc) | (km s−1) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| IC 418 | 0.6453 ± 0.0541 |  |
1.15 ± 0.20 | 0.88 ± 0.12 | 22 ± 2 |  |
– | – | – |
| IC 2448 | 0.2883 ± 0.0454 |  |
2.00 ± 0.30 | 1.20 ± 0.45 | 35 ± 2 |  |
1.43 ± 0.14 | 18 ± 1 |  |
| IC 4593 | 0.3803 ± 0.0794 |  |
3.00 ± 1.20 | 2.40 ± 0.95 | 24 ± 2 |  |
– | – | – |
| NGC 3132 | 1.1566 ± 0.0504 |  |
1.25 ± 0.30 | – | – | – | 0.89 ± 0.16 | 21 ± 2 |  |
| NGC 3242 | 0.6819 ± 0.0884 |  |
1.15 ± 0.15 | – | – | – | 0.73 ± 0.09 | 17 ± 1 |  |
| NGC 5882 | 0.5071 ± 0.0666 |  |
1.70 ± 0.30 | – | – | – | 1.21 ± 0.19 | 22 ± 1 |  |
| NGC 6543 | 0.6152 ± 0.0709 |  |
1.86 ± 0.15 | – | – | – | 1.24 ± 0.09 | 19 ± 2 |  |
| NGC 6826 | 0.6348 ± 0.0475 |  |
1.55 ± 0.20 | 1.20 ± 0.22 | 33 ± 2 |  |
0.85 ± 0.10 | 8.5 ± 1 |  |
| NGC 6891 | 0.4073 ± 0.0512 |  |
1.45 ± 0.45 | – | – | – | 0.66 ± 0.16 | 7 ± 1 |  |
| NGC 7009 | 0.8665 ± 0.1161 |  |
1.50 ± 0.35 | – | – | – | 1.00 ± 0.26 | 18 ± 1 |  |
| NGC 7662 | 0.5054 ± 0.0747 |  |
1.90 ± 0.30 | 1.32 ± 0.30 | 35 ± 3 |  |
1.55 ± 0.13 | 26 ± 1 |  |
Notes. The table contains the list of objects (Col. 1), the Gaia DR2 parallaxes (Col. 2), the corresponding distances (Col. 3), the expansion distances finally adopted by SBJ (see Table 7 therein) (Col. 4), the uncorrected expansion distances of the shells (Col. 5), the shell post-shock velocities (Col. 6), the empirical shell correction factors (Col. 7), the uncorrected expansion velocities of the rims (Col. 8), the rim (bulk) expansion velocities (Col. 9), and the empirical rim correction factors (Col. 10). The uncorrected expansion distances for shell and rim in Cols. 5 and 8 follow from the data in Tables 4 and 5 of SBJ. The velocities in Cols. 6 and 9 are in general mean values derived from the [N II] 6548/6583 Å and [O III] 4959/5007 Å lines as listed in Schönberner et al. (2014). For optically thin nebulae, velocities derived from both ions are very similar (cf. Fig. 8 in Schönberner et al. 2014).
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