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The Andromeda galaxy is observed to have a system of two large dwarfellipticals and ~13 smaller satellite galaxies that are currently co-rotatingin a thin plane, in addition to 2 counter-rotating satellite galaxies. Weexplored the consistency of those observations with a scenario where themajority of the co-rotating satellite galaxies originated from a subhalo group,where NGC 205 was the host and the satellite galaxies occupied dark mattersub-subhalos. We ran N-body simulations of a close encounter between NGC 205and M31. In the simulations, NGC 205 was surrounded by massless particles tostatistically sample the distribution of the sub-subhalos expected in a subhalothat has a mass similar to NGC 205. We made Monte Carlo samplings and foundthat, using a set of reference parameters, the probability of producing athinner distribution of sub-subhalos than the observed NGC 205 + 15 smallersatellites (thus including the 2 counter-rotators, but excluding M32) increasedfrom <1e-8 for the initial distribution to ~0.01 at pericentre. The probabilityof the simulated sub-subhalos occupying the locations of the observedco-rotating satellites in the line of sight velocity versus projected on-skydistance plane is at most 0.002 for 11 out of 13 satellites. Increasing themass of M31 and the extent of the initial distribution of sub-subhalos gives amaximum probability of 0.004 for all 13 co-rotating satellites, but theprobability of producing the thinness would drop to ~ 0.001.

The potential role of NGC 205 in generating Andromeda's vast thin co-rotating plane of satellite galaxies