Context :

Aims : It is widely accepted that the past dynamical history of the solar system included a scattering of planetesimals from a primordial disk by the major planets .
The primordial scattered population is likely the origin of the current scaterring disk and possibly the detached objects .
In particular , an important argument has been presented for the case of 2004 XR _ { 190 } as having an origin in the primordial scattered disk through a mechanism including the 3:8 mean motion resonance ( MMR ) with Neptune ( Gomes 2011 ) .
Here we aim at developing a similar study for the cases of the 1:3 and 2:5 resonances that are stronger than the 3:8 resonance .

Methods : Through a semi-analytic approach of the Kozai resonance inside a MMR , we show phase diagrams ( e, \omega ) that suggest the possibility of a scattered particle , after being captured in a mean motion resonance with Neptune , to become a detached object .
We ran several numerical integrations with thousands of particles perturbed by the four major planets , and there are cases with and without Neptune ’ s residual migration .
These were developed to check the semi-analytic approach and to better understand the dynamical mechanisms that produce the detached objects close to a MMR .

Results : The numerical simulations with and without a residual migration for Neptune stress the importance of a particular resonance mode , which we name the hibernating mode , on the formation of fossilized detached objects close to MMRs .
When considering Neptune ’ s residual migration we are able to show the formation of detached orbits .
These objects are fossilized and can not be trapped in the MMRs again .
We find a ratio of the number of fossilized objects with moderate perihelion distance ( 35 < q < 40 au ) to the number of objects with high perihelion distance ( q > 40 au ) as 3.0/1 for objects close to the 2:5 , and 1.7/1 for objects close to the 1:3 resonance .
We estimate that the two fossilized population have a total mass between 0.1 and 0.3 Pluto ’ s mass .

Conclusions :