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The formation process of binary stars and multiple systems is poorlyunderstood. Here, we seek to determine the typical outcome of protostellarcollapse and to constrain models of binary formation by core fragmentationduring collapse, using high-resolution millimeter continuum imaging of veryyoung (Class 0) protostars observed at the beginning of the main accretionphase. We carried out a pilot high-resolution study of 5 Class 0 objects, usingthe most extended (A) configuration of the IRAM PdBI at 1.3 mm, which allow usto probe the multiplicity of Class 0 protostars down to separations a ~50 AUand circumstellar mass ratios q ~0.07. We show that our PdBI observationsrevealed only wide (>1500 AU) protobinary systems and/or outflow-generatedfeatures. When combined with previous millimeter interferometric observationsof Class 0 protostars, our pilot PdBI study tentatively suggests that thebinary fraction in the ~ 75-1000 AU range increases from the Class 0 to theClass I stage. It also seems to argue against purely hydrodynamic models ofbinary star formation. We briefly discuss possible alternative scenarios toreconcile the low multiplicity rate of Class 0 protostars on small scales withthe higher binary fraction observed at later evolutionary stages.

Toward understanding the formation of multiple systems - A pilot IRAM-PdBI survey of Class 0 objects