| Observed property | Best hypothesis | Comments |
| much redder disk than the bulge | merger remnant | rapid disk rebuilt is predicted (Governato et al. 2007): renewed disks are thus star forming and dusty (Lotz et al. 2008b) |
| bar & two arms system | both | expected for both (see text) |
| misaligned dynamical axis | merger remnant | in absence of significant outflow, it reveals a system not at equilibrium, difficult to explain except by a merger |
| average disk velocity dispersion (74 km s-1) | merger remnant | unclear which perturbation other than merging can provide such a hot disk ( km s-1) |
| velocity dispersion peak locations | merger remnant | only two minor mergers near the two locations may explain such features in a perturbed disk |
| very high disk star formation density | merger remnant | regulation of star formation between gravitational instabilities and porosity is expected in rotating disks (e.g. Silk 1997) |
| discrepancy from the Tully Fisher | merger remnant | expected in a merger (e.g. Puech et al. 2007) and quite unexpected in a perturbed disk (see above) |
| half of the stars with ages lower than 800 Myr | merger remnant | correspond to the merger time-scale during which these stars are formed |
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