  We present a series of monitoring observations of the ultrasoft broad-line
AGN RE J2248-511 with XMM-Newton. Previous X-ray observations showed a
transition from a very soft state to a harder state five years later. We find
that the ultrasoft X-ray excess has re-emerged, yet there is no change in the
hard power-law. Reflection models with a reflection fraction of >15, and
Comptonisation models with two components of different temperatures and optical
depths can be fit to the spectrum, but cannot be constrained. The best
representation of the spectrum is a model consisting of two blackbodies
(kT~90,200 eV) plus a power-law (Gamma=1.8). We also present simultaneous
optical and infrared data showing that the optical spectral slope also changes
on timescales of years. If the optical to X-ray flux comes primarily from a
Comptonised accretion disk we obtain estimates for the black hole mass of ~1e8
solar, accretion rate ~0.8xEddington and disk inclination cosi>0.8.
