  We present an analysis of a Chandra observation of the field surrounding the
low-mass X-ray binary 4U 1755-33, which has been in quiescence since 1996. In
2003, Angelini and White reported the appearance of a narrow 7 arcmin long
jetlike feature centered on the position of 4U 1755-33 using the XMM-Newton
telescope. Though the source and jet are not visibly apparent in our
Chandra/ACIS-S image, there is a significant excess (4-6 sigma) of counts in a
region that encloses the jet when compared to adjacent regions. We examined a
knot of emission in the jet that was detected by XMM-Newton but not by Chandra
and calculated that if the knot flux observed by XMM-Newton was concentrated in
a point source, Chandra would have easily detected it; we therefore conclude
that this knot of emission is diffuse. In summary, we suggest that the jetlike
feature found previously in the XMM-Newton data is quite diffuse and likely a
true jet, and is not due to a chance alignment of discrete point sources or
point-like regions of emission associated with internal shocks.
