The procedure to estimate the kinematics at intermediate radii, between the radial coverage of the IFS and of the ePN.S data. In galaxies with “no gap” the velocity field is the juxtaposition of the IFS and PN velocity and velocity dispersion fields. “Interp” indicates galaxies where the velocities at intermediate radii are estimated from Eq. (1), with parameters given by a linear interpolation of the parameter fitted on the IFS field in the center and on the ePN.S field at large radii. In galaxies with SLUGGS dats available, we use V_rot(a) and PA_kin(a) profiles from the kinemetry analysis of Foster et al. (2016), while V_s3(a), V_c3(a) are the linear interpolation between the values fitted on the IFS and the PN data. In the three SRs with “no interp.”, the comparison with long slit velocities or kinemetric V_rot from IFS data (Simien & Prugniel 1997; Veale et al. 2017; Pu & Han 2011) assures the smooth continuity between the kinematic profiles from Atlas3D and ePN.S: the central regions of these galaxies are nonrotating as well as the most central PNe, and any contribution to the AM comes from the outskirts of these galaxies. In these cases we simply consider the combination of the Atlas3D and ePN.S velocity fields without adding any interpolation.

For NGC3923 and NGC5128, we only use PN data, as discussed in Sect. 2.2.

For NGC4742, only major axis slit data from are available from Davies et al. (1983). We build a two-dimensional velocity field in the center using Eq. (1), where V_rot(a) is given by the measured major axis velocities from the slit, the three parameters V_s3(a), V_c3(a), and PA_kin(a) are given between a linear interpolation between 0 at a = 0 and the measured values for the PN velocity field. The two-dimensional velocity dispersion field is instead build using the major-axis slit data and assuming azimuthally constant σ.

References for the blue-light photometric data: (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) Ragusa et al. (2022), (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), (23) Iodice et al. (2016), (24) Rejkuba et al. (2022).

Galaxies with available 3.6 μm Spitzer data are marked with 1, 0 otherwise.