Disks and Outflows in the Intermediate-mass Star-forming Region NGC 2071 IR

We present Atacama Large Millimeter Array band 6/7 (1.3 mm/0.87 mm) and Very Large Array Ka-band (9 mm) observations toward NGC 2071 IR, an intermediate-mass star-forming region. We characterize the continuum and associated molecular line emission toward the most luminous protostars, i.e., IRS1 and IRS3, on ~100 au (0.″2) scales. IRS1 is partly resolved in the millimeter and centimeter continuum, which shows a potential disk. IRS3 has a well-resolved disk appearance in the millimeter continuum and is further resolved into a close binary system separated by ~40 au at 9 mm. Both sources exhibit clear velocity gradients across their disk major axes in multiple spectral lines including C<SUP>18</SUP>O, H<SUB>2</SUB>CO, SO, SO<SUB>2</SUB>, and complex organic molecules like CH<SUB>3</SUB>OH, <SUP>13</SUP>CH<SUB>3</SUB>OH, and CH<SUB>3</SUB>OCHO. We use an analytic method to fit the Keplerian rotation of the disks and give constraints on physical parameters with a Markov Chain Monte Carlo routine. The IRS3 binary system is estimated to have a total mass of 1.4-1.5 M <SUB>⊙</SUB>. IRS1 has a central mass of 3-5 M <SUB>⊙</SUB> based on both kinematic modeling and its spectral energy distribution, assuming that it is dominated by a single protostar. For both IRS1 and IRS3, the inferred ejection directions from different tracers, including radio jet, water maser, molecular outflow, and H<SUB>2</SUB> emission, are not always consistent, and for IRS1 these can be misaligned by ~50°. IRS3 is better explained by a single precessing jet. A similar mechanism may be present in IRS1 as well but an unresolved multiple system in IRS1 is also possible.