– 30 – the disk and large bodies within it. Photoevaporation and dynamical interactions are not mutually exclusive processes, as photoevaporation can also operate on a dynamically truncated disk as long as the disk mass and accretion rates are low enough. Coku Tau/4 is perhaps the most extreme example of this scenario. It is a 8 AU separation, equal-mass, binary system (Ireland & Kraus, 2008) resulting on a α$_{excess}$ value of ∼ 2. Just like targets #5, 12, and 19, Coku Tau/4 lacks accretion and has a very low disk mass (Najita et al. 2007), and is consequently also susceptible to photoevaporation. Our VLT-AO observations reveal no stellar companion within ∼ 8 AU of targets #5, 12, or 19. However, target #12 is already known to be very tight binary (r ≲ 1 AU), and the presence of stellar (or planetary mass) companions remains completely unconstrained for targets #5 and 19. Photoevaporation provides a natural mechanism for objects to transition from the primordial to the debris disk stage. Once accretion stops, photoevaporation is capable of removing the remaining gas in a very short ( << 1 Myr) timescale (Alexander et al. 2006). As the gas in the disk photoevaporates, it is likely to carry with it the smallest grains present in the disk. What is left represents the initial conditions of a debris disk: a gas poor disk with large grains, planetesmals and/or planets. The very short photoevaporation timescale implies that some of the systems shown in Figure 9 could already be in a debris disk stage. In fact, the 4 non-accreting objects with L$_{D}$/L$_{∗}$ < 10 − 3 have properties that are indistinguishable from those of young debris disks like AU Mic and GJ 182 (Liu et al. 2004). These 4 objects are # 12, 20, 23, and 25. These objects might have already formed planets or might be in a multiple system (like target #12 is). Either way, most of the circumstellar gas and dust has already been depleted, and what we are currently observing could be the initial architectures of different debris systems, now subjected to processes photodissociation region powered by DoAr 21 itself and not necessarily from a circumstellar disk (Jensen et al. 2009).