We present simulations of dry-merger encounters between pairs of elliptical galaxies with dark matter halos .
The aim of these simulations is to study the intergalactic stellar populations produced in both parabolic and hyperbolic encounters .
We model progenitor galaxies with total-to-luminous mass ratios { M _ { T } / M _ { L } = } 3 and 11 .
The initial mass of the colliding galaxies are chosen so that { M _ { 1 } / M _ { 2 } = 1 } and 10 .
The model galaxies are populated by particles representing stars , as in Stanghellini et al .
( 2006 ) , and dark matter .
Merger remnants resulting from these encounters display a population of unbounded particles , both dark and luminous .
The number of particles becoming unbounded depends on orbital configuration , with hyperbolic encounters producing a larger luminous intracluster population than parabolic encounters .
Furthermore , in simulations with identical orbital parameters , a lower { M _ { T } / M _ { L } } of the colliding galaxies produces a larger fraction of unbounded luminous particles .
For each modeled collision , the fraction of unbounded to initial stellar mass is the same in all mass-bins considered , similarly to what we found previously by modeling encounters of galaxies without dark halos .
The fraction of intergalactic to total luminosity resulting from our simulations is \sim 4 \% and \sim 6 \% for dark-to-bright mass rations of 10 and 2 respectively .
These unbounded-to-total luminous fractions are down from 17 \% that we had previously found in the case of no dark halos .
Our results are in broad agreement with intergalactic light observed in groups of galaxies , while the results of our previous models without dark halos better encompass observed intracluster populations .
We suggest a possible formation scenario of intergalactic stars .