  We report two epochs of Chandra-ACIS X-ray imaging spectroscopy of the nearby
bright Type IIn supernova SN 2010jl, taken around 2 months and then a year
after the explosion. The majority of the X-ray emission in both the spectra is
characterized by a high temperature ($\ga 10$ keV) and is likely to be from the
forward shocked region resulting from circumstellar interaction. The absorption
column density in the first spectrum is high, ~ 10^{24} cm^{-2}, more than 3
orders of magnitude higher than the Galactic absorption column, and we
attribute it to absorption by circumstellar matter. In the second epoch
observation, the column density has decreased by a factor of 3, as expected for
shock propagation in the circumstellar medium. The unabsorbed 0.2-10 keV
luminosity at both epochs is ~7 x 10^{41} erg/s. The 6.4 keV Fe line clearly
present in the first spectrum is not detected in the second spectrum. The
strength of the fluorescent line is roughly that expected for the column
density of circumstellar gas, provided the Fe is not highly ionized. There is
also evidence for an absorbed power law component in both the spectra, which we
attribute to a background ultraluminous X-ray source.
