An Analysis of the Complex and Compact Outflow Cavity Carved by HOPS 361-A in NGC 2071 IR

Abstract

We present a combined Stratospheric Observatory for Infrared Astronomy (SOFIA) and two-epoch Hubble Space Telescope (HST) study of the region NGC 2071 IR containing the outflow from the protostar HOPS 361-A (NGC 2071 IRS 1). New [O I] 63 μm spectra, taken with the German REciever for Astronomy at Terahertz frequencies (GREAT) instrument aboard SOFIA, trace the outflow, spectrally resolve line profiles, and give radial velocities of the far-IR emission to yield 3D kinematics, shock properties, and feedback properties. Proper motions and extinction values from HST give a more complete quasi-3D picture that we use to model shock speeds and densities. We identify 14 distinct features that show proper motions. Combined with the GREAT data, we estimate that HOPS 361-A has a mass outflow rate of 3.16 × 10^‑6 M _⊙ yr^‑1 with shock speeds up to 51 km s^‑1. The outflow force summed over all knots per area is measured to be 1.45 × 10^‑4 M _⊙ km^‑1 s^‑1 yr^‑1 and a power summed over all knotsper area of 2.37 × 10^‑2 M _⊙ s^‑3 dissipated assuming constant Ṁ , with large uncertainties on the feedback values. The total [O I] luminosity using all SOFIA apertures encompassing the HOPS 361 clump is 0.7 L _⊙, corresponding to a mass outflow rate of 7 × 10^‑5 M _⊙ yr^‑1. This is the second 3D kinematic study of an outflow in NGC 2071 IR in the near- and far-IR regimes following Rubinstein et al. (2023). The SOFIA [O I] spectra add unique focus to the entrained gas connecting the recent episode of outflows from HOPS 361-A to the outflow cavity and the surrounding NGC 2071 IR star-forming environment.