  Observations of positional offsets between the location of X-ray and radio
features in many resolved, extragalactic jets indicates that the emitting
regions are not co-spatial, an important piece of evidence in the debate over
the origin of the X-ray emission on kpc scales. The existing literature is
nearly exclusively focused on jets with sufficiently deep Chandra observations
to yield accurate positions for X-ray features, but most of the known X-ray
jets are detected with tens of counts or fewer, making detailed morphological
comparisons difficult. Here we report the detection of X-ray-to-radio
positional offsets in 15 extragalactic jets from an analysis of 22 sources with
low-count Chandra observations, where we utilized the Low-count Image
Reconstruction Algorithm (LIRA). This algorithm has allowed us to account for
effects such as Poisson background fluctuations and nearby point sources which
have previously made the detection of offsets difficult in shallow
observations. Using this method, we find that in 55 % of knots with detectable
offsets, the X-rays peak upstream of the radio, questioning the applicability
of one-zone models, including the IC/CMB model for explaining the X-ray
emission. We also report the non-detection of two previously claimed X-ray
jets. Many, but not all, of our sources, follow a loose trend of increasing
offset between the X-ray and radio emission, as well as a decreasing X-ray to
radio flux ratio along the jet.
