Table 1.
Basic information of the 15 massive compact ETGs.
| Galaxy name | log(M*) | Re [kpc] | d [Mpc] | Rmax [kpc] | f∗,disk | f∗,halo | f∗,bulge | log(M∗,Sph) | RSph [kpc] | Environment | Merger-free? |
|---|---|---|---|---|---|---|---|---|---|---|---|
| MRK1216 | 11.34 | 3.0 | 94 | 6.8 | 0.19 | 0.21 | 0.60 | 11.22 | 1.9 | Isolated | Maybe |
| NGC 0384 | 10.96 | 1.8 | 59 | 7.2 | 0.17 | 0.14 | 0.69 | 10.69 | 0.9 | Group | Maybe |
| NGC 0472 | 11.07 | 2.4 | 74 | 7.2 | 0.11 | 0.21 | 0.68 | 10.98 | 1.5 | Group/isolated | Maybe |
| NGC 1270 | 11.31 | 2.2 | 69 | 8.4 | 0.12 | 0.31 | 0.57 | 11.17 | 1.5 | Group | No |
| NGC 1271 | 11.06 | 2.0 | 80 | 7.8 | 0.21 | 0.19 | 0.60 | 10.64 | 1.3 | Group | Maybe |
| NGC 1277 | 11.13 | 1.3 | 71 | 5.2 | 0.25 | 0.05 | 0.70 | 10.77 | 0.54 | Group | Yes |
| NGC 1281 | 11.00 | 1.6 | 60 | 5.8 | 0.16 | 0.22 | 0.62 | 10.76 | 1.2 | Group | Maybe |
| NGC 1282 | 10.77 | 1.3 | 31 | 3.8 | 0.11 | 0.07 | 0.82 | 10.58 | 0.64 | Group | Not sure |
| NGC 2767 | 11.12 | 2.4 | 74 | 7.2 | 0.31 | 0.14 | 0.55 | 10.85 | 0.76 | Group | Yes |
| PGC11179 | 11.16 | 2.1 | 94 | 6.8 | 0.35 | 0.05 | 0.60 | 10.75 | 0.71 | Group | Yes |
| PGC12562 | 10.74 | 0.7 | 67 | 4.9 | 0.17 | 0.05 | 0.78 | 10.46 | 0.51 | Group | Yes |
| PGC32873 | 11.28 | 2.3 | 112 | 10.9 | 0.26 | 0.09 | 0.65 | 10.90 | 1.2 | Isolated | Yes |
| PGC70520 | 10.95 | 1.6 | 72 | 8.7 | 0.23 | 0.11 | 0.66 | 10.67 | 0.74 | Isolated | Yes |
| UGC2698 | 11.58 | 3.7 | 89 | 8.6 | 0.11 | 0.38 | 0.51 | 11.41 | 2.38 | Group | No |
| UGC3816 | 10.96 | 2.1 | 51 | 7.4 | 0.33 | 0.10 | 0.56 | 10.60 | 0.77 | Group/isolated | Yes |
Notes. The columns from left to right show the galaxy name, stellar mass log(M*/M⊙), half-light radius Re in kpc, distance d in Mpc, the spatial coverage of the IFU data Rmax in kpc, the luminosity fraction of disk f∗,disk, hot inner stellar halo f∗,halo, and bulge f∗,bulge, stellar mass of the hot spheroid log(M∗,Sph/M⊙), half-light radius of the hot spheroid RSph in kpc, environments, and merger histories of these galaxies according to our analysis of their internal orbit distribution (Section 3).
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