M_K is the total absolute luminosity in the K band. These values are obtained from the total apparent total magnitudes K_T of the 2MASS atlas (Skrutskie et al. 2006) using the distance D, and correcting for foreground galactic extinction A_B (Schlegel et al. 1998): M_K = K_T − 5 log₁₀ D − 25 − A_B/11.8. We assume A_B/A_K = 11.8, consistently with Cappellari et al. (2011). The K_T magnitudes are from integrating the surface brightness profiles (∝ exp(−r/r_α)^(1/β)), extrapolated from the 20 mag arcsec⁻² isophote to ∼5r_α (Jarrett et al. 2003).

Distances of galaxies derived from the surface brightness fluctuation method. Whenever possible we adopt the distance moduli measured by Blakeslee et al. (2009, B09), otherwise we used the values from Jensen et al. (2003, J03) or from Tonry et al. (2001, T01). The distance moduli from J03 were rescaled to the zero-point calibration of B09 by applying a shift of +0.1 mag, while the distance moduli from T01 were zero-point- and bias-corrected using the formula from Blakeslee et al. (2010) and the data quality factor Q given by T01.

The sample is divided into SRs (S) and FRs (F), according to the definition of Emsellem et al. (2011), from the kinematics within 1R_e.

Adopted effective radius. The index in parenthesis corresponds to the references: (1) Ho et al. (2012), (2) Cappellari et al. (2011), (3) Caon et al. (1994), (4) Blakeslee et al. (2001), (5) Kormendy & Westpfahl (1989), (6) Capaccioli et al. (1987).

Mean radius of the last radial bin in units of effective radii.

Average value of the photometric position angle.

Ellipticity (ϵ), from Krajnović et al. (2011; within 2.5−3 R_e) and Ho et al. (2011; in the outer regions, where they converge to a constant value). For NGC 3384 and NGC 4564 we used the PA_phot from Meusinger & Ismail (2007) and Goudfrooij et al. (1994), respectively.

Objects for which we used circular radial bins (ϵ = 0), see Sect. 3.2.

Number of detected PNe.

References for the PNe datasets: (7) new PN.S catalogs presented in Arnaboldi et al. (in prep.), (8) Coccato et al. (2009), (9) Cortesi et al. (2013a), (10) McNeil-Moylan et al. (2012), (11) McNeil et al. (2010), (12) Teodorescu et al. (2005), (13) Teodorescu et al. (2011), (14) Méndez et al. (2009), (15) unpublished data from counter dispersed imaging (Arnaboldi et al. in prep.), (16) unpublished data from narrow band imaging and spectroscopic follow up (Arnaboldi et al. in prep.), (17) Peng et al. (2004) and Walsh et al. (2015).

References for absorption line data: kinemetry from (18) Foster et al. (2016) on SLUGGS + ATLAS^3D data, from (19) Krajnović et al. (2008) and from (20) Krajnović et al. (2011), major axis long slit spectroscopy from (21) Davies & Illingworth (1983), (22) Bedregal et al. (2006), (23) Teodorescu et al. (2005), (24) Saglia et al. (2000) and Scott et al. (2014), (25) Norris et al. (2006), (26) Carter et al. (1998), (27) Kormendy & Illingworth (1982), (28) Davies et al. (1983), (29) Marcelin (1983), (30) Simien & Prugniel (1997c), (31) Simien & Prugniel (1997a), (32) Statler & Smecker-Hane (1999), (33) Coccato et al. (2009), (34) De Bruyne et al. (2001), (35) de Lorenzi et al. (2008), (36) Napolitano et al. (2009), (37) Veale et al. (2017), (38) Simien & Prugniel (1997b), (39) Pu & Han (2011), (40) Weijmans et al. (2009), (41) Forestell & Gebhardt (2010).