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We present centimeter and millimeter observations of the NGC 2071star-forming region performed with the VLA and CARMA. We detected counterpartsat 3.6 cm and 3 mm for the previously known sources IRS 1, IRS 2, IRS 3, andVLA 1. All these sources show SEDs dominated by free-free thermal emission atcm wavelengths, and thermal dust emission at mm wavelengths, suggesting thatall of them are associated with YSOs. IRS 1 shows a complex morphology at 3.6cm, with changes in the direction of its elongation. We discuss two possibleexplanations to this morphology: the result of changes in the direction of ajet due to interactions with a dense ambient medium, or that we are actuallyobserving the superposition of two jets arising from two components of a binarysystem. Higher angular resolution observations at 1.3 cm support the secondpossibility, since a double source is inferred at this wavelength. IRS 3 showsa clear jet-like morphology at 3.6 cm. Over a time-span of four years, weobserved changes in the morphology of this source that we interpret as due toejection of ionized material in a jet. The emission at 3 mm of IRS 3 isangularly resolved, with a deconvolved size (FWHM) of ~120 AU, and seems to betracing a dusty circumstellar disk perpendicular to the radio jet. Anirradiated accretion disk model around an intermediate-mass YSO can account forthe observed SED and spatial intensity profile at 3 mm, supporting thisinterpretation.

Multiplicity, Disks and Jets in the NGC 2071 Star-Forming Region