  We observed SN2002bu in the near-IR with the Hubble Space Telescope, the
mid-IR with the Spitzer Space Telescope and in X-rays with Swift 10 years after
the explosion. If the faint L_H\sim100 Lsun HST near-IR source at the transient
position is the near-IR counterpart of SN2002bu, then the source has
dramatically faded between 2004 and 2012, from L\sim10^6.0 Lsun to L\sim10^4.5
Lsun. It is still heavily obscured, tau_V\sim5 in graphitic dust models, with
almost all the energy radiated in the mid-IR. The radius of the dust emission
is increasing as R\simt^(0.7+/-0.4) and the optical depth is dropping as
tau_V\simt^(-1.3+/-0.4). The evolution expected for an expanding shell of
material, tau_V\sim1/t^2, is ruled out at approximately 2 sigma while the
tau_V\simt^(-0.8) to t^(-1) optical depth scaling for a shock passing through a
pre-existing wind is consistent with the data. If the near-IR source is a
chance superposition, the present day source can be moderately more luminous,
significantly more obscured and evolving more slowly. While we failed to detect
X-ray emission, the X-ray flux limits are consistent with the present day
emissions being powered by an expanding shock wave. SN2002bu is clearly a
member of the SN2008S class of transients, but continued monitoring of the
evolution of the spectral energy distribution is needed to conclusively
determine the nature of the transient.
