  We report on the results of XMM-Newton observations of the z=0.18 galaxy
group WARPJ0943.7+1644 and the nearby poor cluster WARPJ0943.5+1640 at z=0.256.
Tracing the X-ray gas out to ~425h^(-1) and ~500h^(-1) kpc in the two systems,
corresponding to roughly 70 per cent of the estimated virial radii, we find the
surface brightness profile of both groups to be well described by standard
beta-models across the entire radial range, but with a significantly lower
value of beta in the cooler WARPJ0943.7+1644. A Navarro-Frenk-White (NFW) model
for the gas density can also provide a good fit to the surface brightness data,
but a large scale radius is required, and gas-traces-mass is strongly ruled
out. Both systems fall close to the observed L_X-T relation for clusters. Gas
mass fractions increase with radius out to the radii probed, reaching
extrapolated values at the virial radius of 0.08 and 0.09h^(-3/2),
respectively. The latter is concordant with results obtained for more massive
systems. Gas entropy profiles show evidence for excess entropy out to at least
r_500, and are inconsistent with predictions of simple preheating models. This
study emphasizes the need for observing galaxy groups out to large radii, to
securely establish their global properties.
