  We explore the dependence of the radial alignment of subhalos on the mass of
the host halo they orbit in. As the effect is seen on a broad range of scales
including massive clusters as well as galactic systems it only appears natural
to explore this phenomenon by means of cosmological simulations covering the
same range in masses. We have 25 well resolved host dark matter halos at our
disposal ranging from 10^15 Msun/h down to 10^12 Msun/h each consisting of
order of a couple of million particles within the virial radius. We observe
that subhalos tend to be more spherical than isolated objects. Both the
distributions of sphericity and triaxiality of subhalos are Gaussian
distributed with peak values of s approx. 0.80 and T approx. 0.56, irrespective
of host mass. Interestingly we note that the radial alignment is independent of
host halo mass and the distribution of \cos\theta (i.e. the angle between the
major axis E_a of each subhalo and the radius vector of the subhalo in the
reference frame of the host) is well fitted by a simple power law P(\cos\theta)
proportional to \cos^4\theta with the same fitting parameters for all host
halos.
