The mass of the Andromeda galaxy

This paper argues that the Milky Way galaxy is probably the largest member of the Local Group. The evidence comes from estimates of the total mass of the Andromeda galaxy (M31) derived from the three-dimensional positions and radial velocities of its satellite galaxies, as well as the projected posi tions and radial velocities of its distant globular clusters and planetary nebulae. The available data set comprises 10 satellite galaxies, 17 distant globular clusters and nine halo planetary nebulae with radial velocities. We find that the halo of Andromeda has a mass of similar to 12.3(-6)(+18) x 10(11) M., together with a scalelength of similar to 90 kpc and a predomin antly isotropic velocity distribution. For comparison, our earlier estimate for the Milky Way halo is similar to 19(-17)(+36) x 10(11) M.. Although th e error bars are admittedly large, this suggests that the total mass of M31 is probably less than that of the Milky Way. We verify the robustness of o ur results to changes in the modelling assumptions and to errors caused by the small size and incompleteness of the data set. Our surprising claim can be checked in several ways in the near future. The numbers of satellite galaxies, planetary nebulae and globular clusters wit h radial velocities can be increased by ground-based spectroscopy, while th e proper motions of the companion galaxies and the unresolved cores of the globular clusters can be measured using the astrometric satellites Space In terferometry Mission (SIM) and Global Astrometric Interferometer for Astrop hysics (GAIA). Using 100 globular clusters at projected radii 20 less than or similar to R less than or similar to 50 kpc with both radial velocities and proper motions, it will be possible to estimate the mass within 50 kpc to an accuracy of similar to 20 per cent. Measuring the proper motions of t he companion galaxies with SIM and GAIA will reduce the uncertainty in the total mass caused by the small size of the data set to similar to 22 per ce nt.