The Tucana dwarf spheroidal: a distant backsplash galaxy of M31?

Abstract

ABSTRACT We use the APOSTLE Local Group (LG) cosmological hydrosimulations to examine the properties of ‘backsplash’ galaxies, i.e. dwarfs that were within the virial boundaries of the Milky Way (MW) or M31 in the past, but are today outside their virial radius (r200). More than half of all dwarfs between $1\text{ and }2\, r_{200}$ of each primary are backsplash. More distant backsplash systems, i.e. those reaching distances well beyond $2\, r_{200}$, are typically close to apocentre of nearly radial orbits, and, therefore, essentially at rest relative to their primary. We use this result to investigate which LG dwarfs beyond ∼500 kpc of either primary could be a distant backsplash satellite of MW or M31. Tucana dSph, one of the few known quiescent LG field dwarfs, at dM31 ≈ 1350 kpc and dMW ≈ 880 kpc, is a promising candidate. Tucana’s radial velocity is consistent with being at rest relative to M31. Further, Tucana is located close to M33’s orbital plane around M31, and simple orbit integrations indicate that Tucana may have been ejected during an early pericentric passage of M33 ∼11 Gyr ago, a timing that approximately coincides with Tucana’s last episode of star formation. We suggest that Tucana may have been an early-infalling satellite of M31 or M33, providing a compelling explanation for its puzzling lack of gas and ongoing star formation despite its isolated nature. In this scenario, M33 should have completed some orbits around M31, a result that may help to explain the relative dearth of M33 satellite candidates identified so far.