Abstract

The discovery of the first confirmed QPO in an AGN (REJ1034+396) is the missing link in the timing properties of X-ray Binaries (XRBs) and AGN and provides a slow-motion look at the much shorter timescale variability seen in XRBs. By testing the shape of the rapid variability against potential spectral models we can deduce that the QPO has it’s orgins in the low-temperature comptonisation of the seed disc photons. This model fits the energy spectrum extremely well and naturally reproduces the large soft-excess seen in the source. The optical-X-ray SED of REJ1034 +396 together with a low mass estimate suggests that the source is accreting at super-Eddington rates, from which we speculate that the QPO is the analogy of the 67Hz QPO of GRS1915 +105, seen in a super-Eddington mass accretion rate state.