Table 1
The Virgo sample in Kormendy et al. (2009) with Spitzer-IRS MIR class.
| Galaxy | RSA | n tot | % | M K s | MIR | Kinematical | Kinematical and morphological | Dust |
| type | light | class | class | peculiarities | ||||
|
|
||||||||
| Core | Missing light | |||||||
|
|
||||||||
| NGC 4472 | E1/S01(1) | 5.99 |
–0.50±0.05 | –25.73 | 1 | SR | CR s-s (1) | Y |
| NGC 4486 | E0 | 11.84 |
–4.20±1.00 | –25.31 | 4 | SR | SC(2), jet | Y |
| NGC 4649 | S01(2) | 5.36 |
–1.05±0.07 | –25.35 | 1 | FR | asym. rot. curve (6) | N |
| NGC 4365 | E3 | 7.11 |
–0.63±0.07 | –25.19 | 0 | SR | Faint SW fan (4) | N |
| NGC 4374 | E1 | 7.98 |
–1.52±0.05 | –25.13 | 2 | SR | V ≈ 0 (3); SC (2) | Y |
| NGC 4261 | E3 | 7.49 |
–1.84±0.05 | –25.24 | 4 | SR | NW tidal arm, faint SE fan (4) | Y |
| NGC 4382 | S01(3) pec | 6.12 |
–0.18±0.06 | –25.13 | 1 | FR | MC(2), shells (7) | Y |
| NGC 4636 | E0/S01(6) | 5.65 |
–0.22±0.04 | –24.42 | 2 | SR | gas irr. motion (a) | Y |
| NGC 4552 | S01(0) | 9.22 |
–1.23±0.09 | –24.31 | 2 | SR | KDC (2) shells (4) | Y |
|
|
||||||||
| Cuspy | Extra light | |||||||
|
|
||||||||
| NGC 4621 | E5 | 5.36 |
0.27±0.06 | –24.13 | 0 | FR | KDC (2) | N |
| NGC 4473 | E5 | 4.00 |
8.80±1.00 | –23.77 | 0 | FR | MC (2) | N |
| NGC 4478 | E2 | 2.07 |
1.12±0.15 | –23.15 | 0 | FR | ... | N |
| NGC 4570 | S01(7)/E7 | 3.69±0.50 | ... | –23.49 | 0 | FR | MC (2) | N |
| NGC 4660 | E5 | 4.43±0.38 | ... | –22.69 | 0 | FR | MC (2) | N |
| NGC 4564 | E6 | 4.69±0.20 | ... | –23.09 | 0 | FR | SC (2) | N |
Notes. Core and cuspy galaxies correspond to cuspy-core and core-less, respectively, in Kormendy et al. (2009). The Sersic’s index, ntot, and the percentage of extra light are taken from Kormendy et al. (2009). The MKs absolute magnitude and the MIR class is obtained from Brown et al. (2011) and Rampazzo et al. (2013). Kinematical classes are from Emsellem et al. (2011). Kinematical and morphological peculiarities are coded as follows: CR s-s: counter rotation stars vs. stars (1) Corsini et al. (1998); KDC indicates a kinematically decoupled component, not necessarily counter-rotation; MC multiple components; SC single component Krajnović et al. (2008); (2) A description of the kinematic and morphological peculiarities of the galaxies and full references are reported in: (3) Emsellem et al. (2004); (4) Tal et al. (2009); (5) Malin & Carter (1983); (6) Pinkney et al. (2003); (7) Kormendy et al. (2009). Dust properties (Y if present) are taken from Côté et al. (2006) and Table B3 in Rampazzo et al. (2013).
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