Table 1
Sample of dEs in the Virgo cluster.
| Galaxy | RA(J2000) | Dec(J2000) | Type | (vmax/σ)∗ | σ e | Age |
| (h:m:s) | (°:′:′′) | (km s-1) | (Gyr) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
|
|
||||||
| VCC 21 | 12:10:23.14 | +10:11:18.9 | dE(di, bc) | 0.94 ± 0.34 | 23.7 ± 4.9 |
|
| VCC 308 | 12:18:50.77 | +07:51:41.3 | dE(di, bc) | 0.96 ± 0.27 | 33.3 ± 1.2 |
|
| VCC 397 | 12:20:12.25 | +06:37:23.6 | dE(di) | 2.48 ± 0.57 | 39.4 ± 1.4 |
|
| VCC 523 | 12:22:04.13 | +12:47:15.1 | dE(di) | 1.50 ± 0.22 | 46.8 ± 0.9 |
|
| VCC 856 | 12:25:57.93 | +10:03:13.8 | dE(di) | 1.04 ± 0.23 | 34.0 ± 3.2 |
|
| VCC 917 | 12:26:32.40 | +13:34:43.8 | dE | 0.83 ± 0.29 | 36.9 ± 0.9 |
|
| VCC 990 | 12:27:16.91 | +16:01:28.4 | dE(di) | 0.90 ± 0.06 | 44.0 ± 1.4 |
|
| VCC 1087 | 12:28:17.88 | +11:47:23.7 | dE | 0.23 ± 0.21 | 49.7 ± 1.1 |
|
| VCC 1122 | 12:28:41.74 | +12:54:57.3 | dE | 0.47 ± 0.21 | 38.6 ± 0.9 |
|
| VCC 1183 | 12:29:22.49 | +11:26:01.8 | dE(di) | 0.46 ± 0.13 | 42.4 ± 2.2 |
|
| VCC 1261 | 12:30:10.35 | +10:46:46.3 | dE | 0.35 ± 0.13 | 50.5 ± 1.3 |
|
| VCC 1431 | 12:32:23.39 | +11:15:47.4 | dE | 0.13 ± 0.07 | 54.1 ± 1.6 |
|
| VCC 1549 | 12:34:14.85 | +11:04:18.1 | dE | 0.31 ± 0.13 | 41.1 ± 2.5 |
|
| VCC 1695 | 12:36:54.79 | +12:31:12.3 | dE(di) | 0.94 ± 0.21 | 35.1 ± 1.5 |
|
| VCC 1861 | 12:40:58.60 | +11:11:04.1 | dE | 0.15 ± 0.11 | 42.2 ± 1.0 |
|
| VCC 1910 | 12:42:08.68 | +11:45:15.9 | dE(di) | 0.38 ± 0.15 | 36.1 ± 1.5 |
|
| VCC 1912 | 12:42:09.12 | +12:35:48.8 | dE(bc) | 0.52 ± 0.14 | 38.6 ± 1.6 |
|
| VCC 1947 | 12:42:56.36 | +03:40:35.6 | dE(di) | 1.14 ± 0.09 | 49.4 ± 1.3 |
|
Notes. Column 4: morphological type classification according to Lisker et al. (2006a) and Lisker et al. (2006b): dE(di) indicates dwarf ellipticals with a certain, probable or possible underlying disk (i.e. showing spiral arms, edge-on disks, and/or a bar) or other structures (such as irregular central features (VCC21)); dE(bc) refers to galaxies with a blue centre; dE to galaxies with no evident underlying structure. VCC1947 was not in Lisker et al. sample, therefore we classified it attending to its boxyness/diskyness, as described in Paper I. Column 5: anisotropy parameter corrected for inclination from Paper I. Column 6: velocity dispersion measured collapsing the spectra up to the RSMA. Column 7: luminosity weighted ages of the stellar population from Michielsen et al. (2008).
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