  We present a detailed analysis of the best-quality multi-wavelength data
gathered for the large-scale jet in the core-dominated quasar 3C 273. We
analyze all the archival observations of the target with the Chandra X-ray
Observatory, the far-ultraviolet observations with the Hubble Space Telescope,
and the 8.4 GHz map obtained with the Very Large Array. In our study we focus
on investigating the morphology of the outflow at different frequencies, and
therefore we apply various techniques for the image deconvolution, paying
particular attention to a precise modeling of the Chandra and Hubble point
spread functions. We find that the prominent brightness enhancements in the
X-ray and far-ultraviolet jet of 3C 273 - the "knots" - are not point-like, and
can be resolved transversely as extended features with sizes of about $\simeq
0.5$ kpc. Also, the radio outflow is wider than the deconvolved
X-ray/ultraviolet jet. We have also found circumstantial evidence that the
intensity peaks of the X-ray knots are located systematically upstream of the
corresponding radio intensity peaks, with the projected spatial offsets along
the jet ranging from $\lesssim 0.2$ kpc up to $\simeq 1$ kpc. We discuss our
findings in the wider context of multi-component models for the emission and
structure of large-scale quasar jets, and speculate on the physical processes
enabling an efficient acceleration of the emitting ultra-relativistic electrons
along the entire jet length that exceeds 100 kpc.
