Table 2
SAURON survey kinematic and stellar population parameters.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
|
|
|||||||
| Galaxy | a 4 | λ R | Rotator | GRP | Age(Gyr) | Metallicity | [α/Fe] |
| (Fast/Slow) | Re/8 & Re | Re/8 & Re | Re/8 & Re | ||||
|
|
|||||||
| NGC 3377 | 0.94 | 0.475 | F | SC | 
&  |
0.01 ± 0.04 & −0.21 ± 0.04 | 0.24 ± 0.04 & 0.20 ± 0.04 |
| NGC 4278 | −0.15 | 0.149 | F | MC | 
&  |
0.01 ± 0.02 & −0.07 ± 0.04 | 0.46 ± 0.05 & 0.38 ± 0.06 |
| NGC 4365 | – | 0.090 | S | KDC | – | – | – |
| NGC 4374 | −0.40 | 0.023 | S | SC | 
&  |
0.01 ± 0.04 & −0.15 ± 0.04 | 0.30 ± 0.04 & 0.31 ± 0.06 |
| NGC 4382 | 0.59 | 0.155 | F | CLV | 
&  |
0.051 ± 0.04 & −0.09 ± 0.04 | 0.16 ± 0.04 & 0.20 ± 0.04 |
| NGC 4406 | – | 0.060 | S | KDC | – | – | – |
| NGC 4473 | 1.03 | 0.195 | F | MC | 
&  |
0.09 ± 0.02 & −0.09 ± 0.04 | 0.24 ± 0.04 & 0.27 ± 0.04 |
| NGC 4486 | −0.07 | 0.019 | S | SC | 
& |
0.13 ± 0.02 & −0.03 ± 0.02 | 0.41 ± 0.05 & 0.44 ± 0.05 |
| NGC 4526 | −1.92 | 0.476 | F | MC | 
&  |
0.19 ± 0.02 & −0.01 ± 0.02 | 0.22 ± 0.04 & 0.28 ± 0.05 |
| NGC 4552 | 0.00 | 0.049 | S | KDC | 
&  |
0.21 ± 0.04 & 0.03 ± 0.04 | 0.25 ± 0.03 & 0.26 ± 0.05 |
| NGC 4570 | 1.90 | 0.561 | F | MC | 
&  |
0.17 ± 0.02 & −0.13 ± 0.04 | 0.17 ± 0.03 & 0.27 ± 0.04 |
| NGC 4621 | 1.66 | 0.268 | F | KDC | 
& |
0.09 ± 0.04 & −0.11 ± 0.04 | 0.28 ± 0.05 & 0.32 ± 0.06 |
| NGC 4649 | – | 0.130 | F | – | – | – | – |
| NGC 4660 | 0.66 | 0.472 | F | MC | 
&  |
0.15 ± 0.02 & −0.11 ± 0.02 | 0.24 ± 0.04 & 0.29 ± 0.05 |
Notes. (1) galaxy; (2) “diskyness” parameter (a4); (3) rotation parameter (λR); and (4) Slow or Fast rotator (Emsellem et al. 2007; Cappellari et al. 2007) according to (3); (5) kinematic group (GRP) (Emsellem et al. 2007: SC = single component, MC = Multiple Component, KDC = Kinematically Decoulpled Core, CLV = Central low-level velocity); (6) age estimates in Gyr within a circular aperture of Re/8 and Re respectively; (7) metallicity estimates within a circular aperture of Re/8 and Re respectively; and (8) [α/Fe] ratios. The last three columns are taken from Kuntschner et al. (2010) and are SSP-equivalent estimates.
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