HOPS 361-C’s Jet Decelerating and Precessing through NGC 2071 IR

E., Rubinstein, Adam; Karnath, Nicole; Quillen, Alice C.; Federman, Samuel; Green, Joel D.; Chambers, E. T.; Watson, D. M.; Megeath, S. Thomas

doi:10.3847/1538-4357/acc401

Cited by 4 publications

(2 citation statements)

References 118 publications

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“…(1) on the smallest scales and shocks in outflows at larger distances from protostars (e.g., Komarova & Fischer 2020;Rubinstein et al 2023b), while the [Fe II] and H 2 lines trace shocks in outflows (e.g., Stapelfeldt et al 1991;Zinnecker et al 1998;Reipurth et al 2000). The CO emission is known to arise from both inner disks and outflows (e.g., Herczeg et al 2011;Salyk et al 2011).…”

Section: Resultsmentioning

confidence: 99%

“…along jets are few. Although atomic hydrogen has been observed in jets in the form of HH objects (e.g., Lizano et al 1988;Garcia Lopez et al 2008Smith et al 2010;Reiter et al 2015;Rubinstein et al 2023b), in only a few instances has Brγ emission been found along a jet (Beck et al 2010) or in a jet knot (Davis et al 2011). To our knowledge, our data show the first collimated protostellar jets detected in the Brα line.…”

Section: Collimated Bipolar Jetsmentioning

confidence: 99%

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Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3–5 μm Spectral Mapping of Five Young Protostars

Federman,

Megeath,

Rubinstein

et al. 2024

ApJ

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Investigating Protostellar Accretion is a Cycle 1 JWST program using the NIRSpec+MIRI integral field units to obtain 2.9–28 μm spectral cubes of five young protostars with luminosities of 0.2–10,000 L ⊙ in their primary accretion phase. This paper introduces the NIRSpec 2.9–5.3 μm data of the inner 840–9000 au with spatial resolutions from 28 to 300 au. The spectra show rising continuum emission; deep ice absorption; emission from H2, H i, and [Fe ii]; and the CO fundamental series in emission and absorption. Maps of the continuum emission show scattered light cavities for all five protostars. In the cavities, collimated jets are detected in [Fe ii] for the four <320 L ⊙ protostars, two of which are additionally traced in Brα. Knots of [Fe ii] emission are detected toward the most luminous protostar, and knots of [Fe ii] emission with dynamical times of <30 yr are found in the jets of the others. While only one jet is traced in H2, knots of H2 and CO are detected in the jets of four protostars. H2 is seen extending through the cavities, showing that they are filled by warm molecular gas. Bright H2 emission is seen along the walls of a single cavity, while in three cavities narrow shells of H2 emission are found, one of which has an [Fe ii] knot at its apex. These data show cavities containing collimated jets traced in atomic/ionic gas surrounded by warm molecular gas in a wide-angle wind and/or gas accelerated by bow shocks in the jets.

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Section: Resultsmentioning

confidence: 99%

Section: Collimated Bipolar Jetsmentioning

confidence: 99%

Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3–5 μm Spectral Mapping of Five Young Protostars

Federman,

Megeath,

Rubinstein

et al. 2024

ApJ

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

Karnath,

Rubinstein,

Federman

et al. 2024

ApJ

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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 M ̇ , 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.

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IPA: Class 0 Protostars Viewed in CO Emission Using JWST

Rubinstein,

Evans,

Tyagi

et al. 2024

ApJ

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We investigate the bright CO fundamental emission in the central regions of five protostars in their primary mass assembly phase using new observations from JWST’s Near-Infrared Spectrograph and Mid-Infrared Instrument. CO line emission images and fluxes are extracted for a forest of ∼150 rovibrational transitions from two vibrational bands, v = 1−0 and v = 2−1. However, 13CO is undetected, indicating that 12CO emission is optically thin. We use H2 emission lines to correct fluxes for extinction and then construct rotation diagrams for the CO lines with the highest spectral resolution and sensitivity to estimate rotational temperatures and numbers of CO molecules. Two distinct rotational temperature components are required for v = 1 (∼600 to 1000 K and 2000 to ∼104 K), while one hotter component is required for v = 2 (≳3500 K). 13CO is depleted compared to the abundances found in the interstellar medium, indicating selective UV photodissociation of 13CO; therefore, UV radiative pumping may explain the higher rotational temperatures in v = 2. The average vibrational temperature is ∼1000 K for our sources and is similar to the lowest rotational temperature components. Using the measured rotational and vibrational temperatures to infer a total number of CO molecules, we find that the total gas masses range from lower limits of ∼1022 g for the lowest mass protostars to ∼1026 g for the highest mass protostars. Our gas mass lower limits are compatible with those in more evolved systems, which suggest the lowest rotational temperature component comes from the inner disk, scattered into our line of sight, but we also cannot exclude the contribution to the CO emission from disk winds for higher mass targets.

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HOPS 361-C’s Jet Decelerating and Precessing through NGC 2071 IR

Cited by 4 publications

References 118 publications

Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3–5 μm Spectral Mapping of Five Young Protostars

Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3–5 μm Spectral Mapping of Five Young Protostars

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

IPA: Class 0 Protostars Viewed in CO Emission Using JWST

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