Naoz, Perets & Ragozzine 8 ally interacting satellites, creates a unique brand of tidal evolution. Multiple resonance crossings can excite ec- centricities and inclinations, perhaps leading to instabil- ity (e.g., Canup et al. 1999). In hierarchical systems with significant mutual inclination, the Kozai-Lidov ef- fect may destabilize the system (Perets & Naoz 2009). For all multiple systems, survival to the present epoch can be difficult, and multiples must have been more com- mon in the primordial population. Additional study of these multiple minor planet sys- tems will provide unique insights into the formation and evolution of these systems. See Benecchi et al. (2009b) for an additional review of multiple minor planet sys- tems, including a table of properties. counters formed/perturbed the binaries and strongly af- fected their orbital evolution. We suggest that these en- counters together with secular Kozai evolution and tidal effects, could have erased much of the direct signatures of the initial formation of BMPs, as possibly reflected by their observed orbits (see also Perets & Naoz 2009). More theoretical work, however, is required to under- stand the different parts played by the initial formation and configurations of BMPs vs. their later dynamical evolution. Especially important are better theoretical predictions for the observational signatures of different BMP formation scenarios, which could be compared with the data presented in this paper and additional future data. In this paper we compiled a catalog of BMPS, both binary TNOs and binary asteroids, with full orbital so- lutions. We presented a first analysis of the eccentricity and inclinations distribution of BMPs as well as their semi-major axis-eccentricity distribution. This data and its analysis can be used to study and constrain forma- tion and evolutionary scenario of BMPs. Specifically we find high relative inclinations for the BMPs as well as typically large (but not extremely high) eccentricities for BMPs not affected by tidal evolution. By themselves these results already suggest BMPs evolved in dense en- vironment in which collisions and close gravitational en- We thank Eran Ofek for useful discussion regarding the transformation from the ecliptic plane to the equato- rial frame of reference. SN acknowledge the partial sup- port by Israel Science Foundation grant 629/05 and U.S.- Israel Binational Science Foundation grant 2004386. SN and HBP acknowledge the generous support of the Dan David Fellowship. HBP is a CfA, Rothschild, FIRST and Fullbright fellow. HBP also acknowledges the Israeli commercial and industrial club for their support through the Ilan-Ramon-Fullbright fellowship. DR is grateful for the support by NASA Headquarters under the Earth and Space Sciences Fellowship. The mutual inclination i$_{m}$ represent the angle between the inner and the outer orbit. All of the heliocentric parameters are given with respect to the ecliptic plane, while the inner orbital parameters are given with respect to the equatorial frame of reference. Thus, we first transform the heliocentric inclination and the longitude of ascending node from the ecliptic plane ( i$_{c}$, Ω$_{c}$ ) to the equatorial frame of reference ( i$_{q}$, Ω$_{q}$ ). Let us define the pole vector with respect to the ecliptic (equatorial) frame, P$_{c}$ ( P$_{q}$ ): 4. SUMMARY APPENDIX CALCULATION OF THE MUTUAL INCLINATION ACKNOWLEDGMENTS The rotation matrix from the ecliptic to the equatorial is rotation with respect to the x axis of the invariable plane, i.e., where ϵ is the ecliptic angle. Thus, the resulting equations of the transformation from the ecliptic to the equatorial are: $_{P$_{c,q}$}$  x y z   =   sin Ω$_{c,q}$ sin i$_{c,q}$ − cos Ω$_{c,q}$ sin i$_{c,q}$ cos i$_{c,q}$   . (A1) R ( x )$_{c}$ $^{→}$q =   1 0 0 0 cos ϵ − sin ϵ 0 sin ϵ cos ϵ   . (A2) cos( i$_{q}$ ) = cos( i$_{c}$ ) cos( ϵ ) − sin( i$_{c}$ ) sin( ϵ ) cos(Ω$_{c}$) , (A3) cos(Ω$_{q}$) sin( i$_{q}$ ) = cos( i$_{c}$ ) sin( ϵ ) + sin( i$_{c}$ ) cos( ϵ ) cos(Ω$_{c}$) , sin(Ω$_{q}$) sin( i$_{q}$ ) = sin(Ω$_{c}$) sin( i$_{c}$ ) , P $^{out}$,s =   sin Ω $^{out}$,in sin i $^{out}$,in − cos Ω $^{out}$,in sin i $^{out}$,in cos i $^{out}$,in   , (A4) where from the last two equations we can find Ω$_{q}$ using the atan 2( x, y ) function. Now we turn to calculate the mutual inclination. We take the longitude of ascending node and inclinations with respect to equatorial frame (resulting from the above transformation) of the inner and outer orbit, i.e., i out , Ω out , and i$_{s}$, Ω$_{s}$ , and calculate the mutual inclinations. Again let us define the binary outer orbit and inner pole vectors as: