The Nucleus of the Sagittarius Dsph Galaxy and M54: a Window on the Process of Galaxy Nucleation

Using both velocity and metallicity information we selected two samples of 425 and 321 very likely members of M54 and of Sgr,N, respectively. The two considered systems display significantly different velocity dispersion profiles. M54 has a steeply decreasing profile from r = 0′, where σ ≃ 14.2 km s -1, to r ≃ 35 where it reaches σ ≃ 5.3 km s -1, then it appears to rise again to σ ≃ 10 km s -1 at r 7′. In contrast Sgr,N has a uniformly flat profile at σ ≃ 9.6 km s -1 over the whole 0′ ≤ r ≤ 9′ range. Using data from the literature we show that the velocity dispersion of Sgr remains constant at least out to r 100′ and there is no sign of the transition between the outer flat-luminosity-profile core and the inner nucleus in the velocity profile. These results, together with a re-analysis of the surface brightness profile of Sgr,N and a suite of dedicated N-body simulations, provide very strong support for the hypothesis that the nucleus of Sgr formed independently of M54, which probably plunged to its present position, coincident with Sgr,N, because of significant decay of the original orbit due to dynamical friction.