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Multiplicity is common in field stars and among protostellar systems. Modelssuggest two paths of formation: turbulent fragmentation and protostellar diskfragmentation. We attempt to find whether or not the coevality frequency ofmultiple protostellar systems can help to better understand their formationmechanism. The coevality frequency is determined by constraining the relativeevolutionary stages of the components in a multiple system. SEDs for knownmultiple protostars in Perseus were constructed from literature data. HerschelPACS photometric maps were used to sample the peak of the SED for systems withseparations >7", a crucial aspect in determining the evolutionary stage of aprotostellar system. Inclination effects and the surrounding envelope andoutflows were considered to decouple source geometry from evolution. Thistogether with the shape and derived properties from the SED was used todetermine each system's coevality as accurately as possible. SED models wereused to examine the frequency of non-coevality that is due to geometry. We finda non-coevality frequency of 33+/-10% from the comparison of SED shapes ofresolved multiple systems. Other source parameters suggest a somewhat lowerfrequency of non-coevality. The frequency of apparent non-coevality that is dueto random inclination angle pairings of model SEDs is 17+/-0.5%. Observationsof the outflow of resolved multiple systems do not suggest significantmisalignments within multiple systems. Effects of unresolved multiples on theSED shape are also investigated. We find that 1/3 of the multiple protostellarsystems sampled here are non-coeval, which is more than expected from randomgeometric orientations. The other 2/3 are found to be coeval. Higher ordermultiples show a tendency to be non-coeval. The frequency of non-coevalityfound here is most likely due to formation and enhanced by dynamical evolution.

Do siblings always form and evolve simultaneously? Testing the coevality of multiple protostellar systems through SEDs