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Statistics of low-mass pre-main sequence binaries in the Orion OB1association with separations ranging from 0.6" to 20" (220 to 7400 au at 370pc) are studied using images from the VISTA Orion mini-survey and astrometryfrom Gaia. The input sample based on the CVSO catalog contains 1137 stars of Kand M spectral types (masses between 0.3 and 0.9 Msun), 1021 of which areconsidered to be association members. There are 135 physical binary companionsto these stars with mass ratios above ~0.13. The average companion fraction is0.09+-0.01 over 1.2 decades in separation, slightly less than, but stillconsistent with, the field. We found a difference between the Ori OB1a and OB1bgroups, the latter being richer in binaries by a factor 1.6+-0.3. No overalldependence of the wide-binary frequency on the observed underlying stellardensity is found, although in the Ori OB1a off-cloud population these binariesseem to avoid dense clusters. The multiplicity rates in Ori OB1 and in sparseregions like Taurus differ significantly, hinting that binaries in the fieldmay originate from a mixture of diverse populations.

Statistics of wide pre-main sequence binaries in the Orion OB1 association