  We present results on the X-ray and optical/UV emission from the type IIP SN
2006bp and the interaction of the SN shock with its environment, obtained with
the X-Ray Telescope (XRT) and UV/Optical Telescope (UVOT) on-board the Swift
observatory. SN 2006bp is detected in X-rays at a 4.5 sigma level of
significance in the merged XRT data from days 1 to 12 after the explosion. If
the X-ray luminosity of (1.8+/-0.4)E39 ergs/s is caused by interaction of the
SN shock with circumstellar material (CSM), deposited by a stellar wind from
the progenitor's companion star, a mass-loss rate of ~E-05 M_sun/yr is
inferred. The mass-loss rate is consistent with the non-detection in the radio
with the VLA on days 2, 9, and 11 after the explosion and characteristic of a
red supergiant progenitor with a mass around 12-15 M_sun prior to the
explosion. In combination with a follow-up XMM-Newton observation obtained on
day 21 after the explosion, an X-ray rate of decline with index 1.2+/-0.6 is
inferred. Since no other SN has been detected in X-rays prior to the optical
peak and since type IIP SNe have an extended 'plateau' phase in the optical, we
discuss the scenario that the X-rays might be due to inverse Compton scattering
of photospheric optical photons off relativistic electrons produced in
circumstellar shocks. However, due to the high required value of the Lorentz
factor (~10-100) we conclude that Inverse Compton scattering is an unlikely
explanation for the observed X-ray emission. The fast evolution of the
optical/ultraviolet spectral energy distribution and the spectral changes
observed with Swift reveal the onset of metal line-blanketing and cooling of
the expanding photosphere during the first few weeks after the outburst.
