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HST and ground based observations of the Type IIn SN 2010jl are analyzed,including photometry, spectroscopy in the ultraviolet, optical and NIR bands,26-1128 days after first detection. At maximum the bolometric luminosity was$\sim 3\times10^{43}$ erg/s and even at 850 days exceeds $10^{42}$ erg/s. A NIRexcess, dominating after 400 days, probably originates in dust in thecircumstellar medium (CSM). The total radiated energy is $> 6.5\times10^{50}$ergs, excluding the dust component. The spectral lines can be separated intoone broad component due to electron scattering, and one narrow with expansionvelocity $\sim 100$ km/s from the CSM. The broad component is initiallysymmetric around zero velocity but becomes blueshifted after $\sim 50$ days,while remaining symmetric about a shifted centroid velocity. Dust absorption inthe ejecta is unlikely to explain the line shifts, and we attribute the shiftinstead to acceleration by the SN radiation. From the optical lines and theX-ray and dust properties, there is strong evidence for large scale asymmetriesin the CSM. The ultraviolet lines indicate CNO processing in the progenitor,while the optical shows a number of narrow coronal lines excited by the X-rays.The bolometric light curve is consistent with a radiative shock in an $r^{-2}$CSM with a mass loss rate of $\sim 0.1$ M_sun/yr. The total mass lost is $> 3$M_sun. These properties are consistent with the SN expanding into a CSMcharacteristic of an LBV progenitor with a bipolar geometry. The apparentabsence of nuclear processing is attributed to a CSM still opaque to electronscattering.

High Density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The first 1100 days