Table 3.
Results of the kinematic analysis.
| Galaxy NCG | Classa | Point symm.b | Features in PAkin(R)c | Multiple kin. comp.d | Triaxiale | RTf | NOTESg |
|---|---|---|---|---|---|---|---|
| 0584 | F | y | n | n | n | – | Small number of tracers |
| 0821 | F | y | y | n | y | 60 ± 30 | (A,C) |
| 1023 | F | y | n | n | n | 160 ± 20 | (A) |
| 1316 | F | n | y | y | n | 75 ± 25 | (A) – merger remnant |
| 1344 | F | y | y | n | y | 30 ± 15 | (C) – prolate rotation |
| 1399 | S | y | y | y | y | 30 ± 15 | (B) – kinematically decoupled halo |
| 2768 | F | n | n | n | n | 145 ± 45 | (A) – fast rotating halo |
| 2974 | F | y | n | n | n | – | Small number of tracers |
| 3115 | F | y | y | n | n | 135 ± 45 | (A) – photometry reveals a perturbed disk at the interface with the spheroid component |
| 3377 | F | y | y | y | y | 55 ± 15 | (A) |
| 3379 | F | y | y | y | y | 60 ± 20 | (A,C) – hints for growing rotation in the outskirts |
| 3384 | F | y | n | n | n | – | Extended disk |
| 3489 | F | y | n | n | n | – | Small number of tracers |
| 3608 | S | y | y | n | y | 55 ± 35 | (B) |
| 3923 | S | y | y | n | y | 70 ± 30 | (B) |
| 4278 | F | y | n | n | n | 25 ± 15 | (A) |
| 4339 | F | y | n | n | n | – | Small number of tracers |
| 4365 | S | y | y | y | y | 125 ± 25 | (C) – kinematically decoupled halo |
| 4374 | S | y | y | n | y | 83 ± 33 | (B) |
| 4472 | S | n | y | y | y | 25 ± 10 | (B) – recent merger; kinematics dominated by in-falling satellite |
| 4473 | F | y | y | n | y | 25 ± 13 | (A) – minor axis rotation observed by Foster et al. (2013) |
| 4494 | F | y | y | y | y | 93 ± 43 | (A) |
| 4552 | S | y | y | y | y | 73 ± 58 | (B,C) |
| 4564 | F | y | n | n | n | 85 ± 45 | (A) – fast rotating halo |
| 4594 | F | y | n | n | n | 180 ± 90 | (A) – no detections in the plane of the disk (dust absorption) |
| 4636 | S | y | y | y | y | 140 ± 40 | (C) |
| 4649 | F | y | y | y | y | 115 ± 15 | (A) – no detections on the west side of the galaxy |
| 4697 | F | y | y | n | n | 85 ± 65 | (A) – hints for growing rotation in the outskirts; this PN sample contains a secondary PN population out of dynamical equilibrium (Sambhus et al. 2006) |
| 4742 | F | y | y | n | y | 43 ± 32 | (C) |
| 5128 | F | n | y | y | y | 95 ± 55 | (C) – recent merger |
| 5846 | S | y | y | n | y | 100 ± 50 | (B) |
| 5866 | F | y | y | n | y | 75 ± 25 | (A) – fast rotating halo |
| 7457 | F | y | n | n | n | – | Extended disk |
Notes.
The sample is divided into slow (S) and FRs (F), according to the definition of Emsellem et al. (2011).
Point symmetry properties of the PN smoothed velocity fields: “y” marks point symmetric galaxies while “n” marks galaxies showing asymmetries, see Sect. 5.
Significant kinematic twist or misalignment of PAkin with respect to PAphot: “y” marks galaxies showing at least one of these, see Sect. 6.4.
For the galaxies marked with “y”, the PN smoothed velocity fields reveal rotation along two perpendicular axes or a halo which is kinematically decoupled with respect to the innermost regions, see Sects. 7 and 6.4.2.
Galaxies marked with “y” have been classified as triaxial in Sect. 6.4.
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