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Table 2.

Measured parameters and typical errors for the smoothed velocity and velocity dispersion fields.

Galaxy NGC Aa (arcsec−1) Ba δvb (km s−1) 〈ΔṼ〉c (km s−1) 〈Δσ̃〉d (km s−1) Vsyse (km s−1) Rhalflight f (arcsec) g h Ref. phot.
0584 0.37 63.2 21. 21. 15. 1901.±27. 30 11.07 11.04 (4)
0821 0.50 9.7 21. 22. 16. 1697.±16. 38 10.97 10.87 (1);(2)
1023 0.26 15.3 14. 19. 13. 618.± 9. 39 10.93 11.06 (6)
1316 0.46 21.3 30. 24. 21. 1749.±30. 115 11.84 11.64 (4)
1344 0.40 10.8 10. 21. 13. 1190.±13. 44 11.06 11.01 (7)
1399 0.84 5.2 37. 27. 18. 1401.±19. 122 11.53 11.51 (4)
2768 0.33 17.5 20. 26. 22. 1378.±14. 70 11.30 10.90 (15);(19)
2974 0.57 33.6 21. 25. 21. 1803.±42. 43 10.87 11.06 (4)
3115 0.28 19.6 20. 30. 21. 624.±16. 73 10.98 10.96 (4)
3377 0.32 19.0 20. 12. 8. 708.± 9. 51 10.45 10.37 (1);(2);(3);(19)
3379 0.34 16.2 20. 21. 14. 934.±17. 58 10.89 10.89 (8);(9)
3384 0.25 18.9 20. 14. 10. 722.± 9. 42 10.77 10.88 (16);(20)
3489 0.32 14.7 20. 14. 11. 707.±12. 22 10.56 10.61 (16)
3608 0.37 24.6 21. 15. 11. 1235.±16. 108 10.84 11.18 (2);(3)
3923 0.60 24.3 30. 36. 26. 1677.±26. 164 11.54 11.66 (4)
4278 0.88 2.4 18. 18. 14. 605.±17. 59 10.89 10.87 (12);(19)
4339 0.43 20.3 21. 8. 6. 1300.± 7. 27 10.38 10.18 (13);(19)
4365 0.91 0.2 21. 20. 14. 1273.±11. 111 11.48 11.51 (14)
4374 0.86 1.6 23. 27. 19. 1050.±18. 122 11.45 11.56 (14)
4472 0.74 11.3 20. 38. 33. 959.±22. 193 11.71 11.76 (14)
4473 0.91 0.2 21. 18. 12. 2236.±13. 38 10.87 10.78 (17)
4494 0.41 12.8 21. 17. 12. 1348.±10. 49 11.05 10.87 (10)
4552 0.90 0.6 21. 23. 16. 361.±15. 101 11.11 11.18 (14)
4564 0.24 16.5 21. 19. 12. 1169.±17. 24 10.59 10.94 (1)
4594 0.54 19.3 30. 32. 28. 1060.±16. 102 11.37 11.10 (4);(21)
4636 0.68 9.5 21. 24. 16. 903.±19. 172 11.12 11.27 (14)
4649 0.86 1.5 20. 25. 18. 1059.±18. 132 11.55 11.55 (14)
4697 0.45 6.0 35. 23. 16. 1274.±11. 123 11.03 11.05 (2);(11)
4742 0.20 16.9 21. 13. 10. 1305.± 9. 13 10.38 10.37 (4);(22)
5128 0.29 25.6 4. 25. 21. 536.±17. 414 11.04 11.20 (4)
5846 0.90 0.1 21. 25. 17. 1716.±19. 193 11.42 11.49 (5);(18)
5866 0.34 18.7 21. 15. 10. 782.±10. 48 10.97 11.01 (16);(19)
7457 0.28 10.5 20. 7. 6. 843.± 5. 62 10.28 10.63 (16); (19)

Notes.

(a)

Kernel parameters, A and B, used in the smoothing procedure, see Sect. 3.

(b)

Mean error on the measured radial velocities.

(c)

Mean error on the smoothed velocity field.

(d)

Mean error on the velocity dispersion field.

(e)

Subtracted systemic velocity.

(f)

Half-light radius, see text.

(g)

Logarithm of the stellar mass M*1 in solar units. M*1 are derived from the K-band luminosities MK listed in Table 1, corrected for missing flux as in Scott et al. (2013): MKcorr = 1.07 × MK + 1.53, and applying a mass-to-light ratio of 1 (appropriate for old stellar population with a Kroupa IMF, Forbes et al. 2016).

(h)

Logarithm of the stellar mass M*2 in solar units.

M*2 are derived using total luminosities obtained by fitting the surface brightness profiles with a Sérsic law and integrating till very large radii. The apparent magnitudes obtained are converted to absolute magnitudes using the distances listed in Table 1, corrected for foreground galactic extinction, and homogenized to B magnitude using color indexes from the HyperLeda (Makarov et al. 2014, http://leda.univ-lyon1.fr/) database and from Sandage & Visvanathan (1978). We then applied a stellar mass to light ratio given by the relation from Bell et al. (2003): , where the (B − V) color index is from HyperLeda.

References. (1) Goudfrooij et al. (1994), (2) Lauer et al. (2005), (3) Jedrzejewski (1987), (4) Li et al. (2011), (5) Kronawitter et al. (2000), (6) Noordermeer et al. (2008), (7) Sikkema et al. (2007), (8) Capaccioli et al. (1990), (9) Gebhardt et al. (2000), (10) Napolitano et al. (2009), (11) de Lorenzi et al. (2008), (12) Peletier et al. (1990), (13) Caon et al. (1994), (14) Kormendy et al. (2009), (15) Hopkins et al. (2009), (16) Krajnović et al. (2013), (17) Caon et al. (1990), (18) Spavone et al. (2017), (19) Michard & Marchal (1993), (20) Meusinger & Ismail (2007), (21) Gadotti & Sánchez-Janssen (2012), (22) Lauer et al. (1995).

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