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We present results from deep (70 ks) Chandra ACIS observations and HubbleSpace Telescope ACS F475W observations of two highly optically polarizedquasars belonging to the MOJAVE blazar sample, viz., PKS B0106+013 and 1641+399(3C345). These observations reveal X-ray and optical emission from the jets inboth sources. X-ray emission is detected from the entire length of the 0106+013radio jet, which shows clear bends or wiggles - the X-ray emission is brightestat the first prominent kpc jet bend. A picture of a helical kpc jet with thefirst kpc-scale bend representing a jet segment moving close(r) to our line ofsight, and getting Doppler boosted at both radio and X-ray frequencies, isconsistent with these observations. The X-ray emission from the jet end howeverpeaks at about 0.4" (~3.4 kpc) upstream of the radio hot spot. Optical emissionis detected both at the X-ray jet termination peak and at the radio hot spot.The X-ray jet termination peak is found upstream of the radio hot spot byaround 0.2" (~1.3 kpc) in the short projected jet of 3C345. HST opticalemission is seen in an arc-like structure coincident with the bright radio hotspot, which we propose is a sharp (apparent) jet bend instead of a terminalpoint, that crosses our line of sight and consequently has a higher Dopplerbeaming factor. A weak radio hot spot is indeed observed less than 1"downstream of the bright radio hot spot, but has no optical or X-raycounterpart. By making use of the pc-scale radio and the kpc-scale radio/X-raydata, we derive constraints on the jet Lorentz factors (Gamma_jet) andinclination angles (theta): for a constant jet speed from pc- to kpc-scales, weobtain a Gamma_jet of ~70 for 0106+013, and ~40 for 3C345. On relaxing thisassumption, we derive a Gamma_jet of ~2.5 for both the sources. Upper limits ontheta of ~13 degrees are obtained for the two quasars. (ABRIDGED)

Chandra & HST Imaging of the Quasars PKS B0106+013 & 3C345: Inverse Compton X-rays and Magnetized Jets