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

Federman, Samuel A.; Megeath, S. Thomas; Rubinstein, Adam E.; Gutermuth, Robert; Narang, Mayank; Tyagi, Himanshu; Manoj, P.; Anglada, Guillem; Atnagulov, Prabhani; Beuther, Henrik; Bourke, Tyler L.; Brunken, Nashanty; Caratti o Garatti, Alessio; Evans, Neal J.; Fischer, William J.; Furlan, Elise; Green, Joel D.; Habel, Nolan; Hartmann, Lee; Karnath, Nicole; Klaassen, Pamela; Linz, Hendrik; Looney, Leslie W.; Osorio, Mayra; Muzerolle Page, James; Nazari, Pooneh; Pokhrel, Riwaj; Rahatgaonkar, Rohan; Rocha, Will R. M.; Sheehan, Patrick; Slavicinska, Katerina; Stanke, Thomas; Stutz, Amelia M.; Tobin, John J.; Tychoniec, Lukasz; Van Dishoeck, Ewine F.; Watson, Dan M.; Wolk, Scott; Yang, Yao-Lun

doi:10.3847/1538-4357/ad2fa0

Cited by 10 publications

(2 citation statements)

References 112 publications

(140 reference statements)

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“…A peculiarity of this spectrum is the detection of many gas features seen in absorption instead of emission, at variance with the JWST spectra of other low-mass protostars (e.g., Yang et al 2022;Federman et al 2024). This can be seen for example in the upper inset of Figure 11, which highlights the spectral region around 4.5 μm, where absorption lines from the CO rovibrational transitions of the v = 1−0 fundamental band are detected, and in the bottom inset covering the range 5.5-8 μm where many additional absorption lines, mostly from H 2 O are present (e.g., Gasman et al 2023).…”

Section: The Spectrum Of the Hh46 Irs Protostarmentioning

confidence: 87%

“…JWST observations of Class 0 sources are indeed now giving unprecedented details on the morphology and composition of their jets, wide-angle molecular flows, and cavities (e.g., Federman et al 2024), although in the youngest of these protostars, their highly embedded innermost region can be hardly traced even at mid-IR wavelengths (Ray et al 2023). On the other hand, JWST is best suited for the study of the intermediate age Class I objects (age ∼10 5 yr), which are still actively accreting from a massive disk, but their parental envelope, within which they are still embedded, can be easily penetrated at mid-IR wavelengths.…”

Section: Introductionmentioning

confidence: 99%

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PROJECT-J: JWST Observations of HH46 IRS and Its Outflow. Overview and First Results

Nisini,

Navarro,

Giannini

et al. 2024

ApJ

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We present the first results of the JWST program PROJECT-J (PROtostellar JEts Cradle Tested with JWST), designed to study the Class I source HH46 IRS and its outflow through NIRSpec and MIRI spectroscopy (1.66–28 μm). The data provide line images (∼6.″6 in length with NIRSpec, and up to ∼20″ with MIRI) revealing unprecedented details within the jet, the molecular outflow, and the cavity. We detect, for the first time, the redshifted jet within ∼90 au from the source. Dozens of shock-excited forbidden lines are observed, including highly ionized species such as [Ne iii] 15.5 μm, suggesting that the gas is excited by high velocity (>80 km s−1) shocks in a relatively high-density medium. Images of H2 lines at different excitations outline a complex molecular flow, where a bright cavity, molecular shells, and a jet-driven bow shock interact with and are shaped by the ambient conditions. Additional NIRCam 2 μm images resolve the HH46 IRS ∼110 au binary system and suggest that the large asymmetries observed between the jet and the H2 wide-angle emission could be due to two separate outflows being driven by the two sources. The spectra of the unresolved binary show deep ice bands and plenty of gaseous lines in absorption, likely originating in a cold envelope or disk. In conclusion, JWST has unraveled for the first time the origin of the HH46 IRS complex outflow demonstrating its capability to investigate embedded regions around young stars, which remain elusive even at near-IR wavelengths.

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Section: The Spectrum Of the Hh46 Irs Protostarmentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

PROJECT-J: JWST Observations of HH46 IRS and Its Outflow. Overview and First Results

Nisini,

Navarro,

Giannini

et al. 2024

ApJ

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Hunting for complex cyanides in protostellar ices with the JWST

Nazari,

Rocha,

Rubinstein

et al. 2024

A&A

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Nitrogen-bearing complex organic molecules have been commonly detected in the gas phase but not yet in interstellar ices. This has led to the long-standing question of whether these molecules form in the gas phase or in ices. The James Webb Space Telescope ( JWST ) offers the sensitivity, spectral resolution, and wavelength coverage needed to detect them in ices and investigate whether their abundance ratios are similar in gas and ice. We report the first tentative detection of CH$_3$CN, C$_2$H$_5$CN and the simple molecule, N$_2$O, based on the CN-stretch band in interstellar ices toward three (HOPS 153, HOPS 370, and IRAS 20126+4104) out of the five protostellar systems observed as part of the Investigating Protostellar Accretion (IPA) GO program with JWST -NIRSpec. We also provide upper limits for the two other sources with smaller luminosities in the sample. We detect OCN$^-$ in the ices of all sources with typical CH$_3$CN/OCN$^-$ ratios of around 1. Ice and gas column density ratios of the nitrogen-bearing species with respect to each other are better matched than those with respect to methanol, which are a factor of $ sim 5$ larger in the ices than the gas. We attribute the elevated ice column densities with respect to methanol to the difference in snowline locations of nitrogen-bearing molecules and of methanol, biasing the gas-phase observations toward fewer nitrogen-bearing molecules. Moreover, we find tentative evidence of the enhancement of OCN$^-$, CH$_3$CN, and C$_2$H$_5$CN in warmer ices; although, the formation of these molecules likely starts along with methanol in the cold prestellar phase. Future surveys combining NIRSpec and MIRI, and additional laboratory spectroscopic measurements of C$_2$H$_5$CN ice, are necessary for robust detection and conclusions on the formation history of complex cyanides.

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JWST Observations of Young protoStars (JOYS)

Tychoniec,

van Gelder,

van Dishoeck

et al. 2024

A&A

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Accretion and ejection dictate the outcomes of star and planet formation processes. The mid-infrared (MIR) wavelength range offers key tracers of processes that have been difficult to detect and spatially resolve in protostars until now. We aim to characterize the interplay between accretion and ejection in the low-mass Class I protobinary system TMC1, comprising two young stellar objects: TMC1-W and TMC1-E at a 85 au separation. Using the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) observations in 5 -- 28 mu m range, we measured the intensities of emission lines of H$_2$, atoms, and ions, for instance, the\ Fe II and Ne II and HI recombination lines. We analyzed the spatial distribution of the different species using the MIRI Medium Resolution Spectrometer (MRS) capabilities to spatially resolve emission at 0 scales. We compared these results are with the corresponding Atacama Large Millimeter/submillimeter Array (ALMA) maps tracing cold gas and dust. We detected H$_2$ outflow coming from TMC1-E, with no significant H$_2$ emission from TMC1-W. The H$_2$ emission from TMC1-E outflow appears narrow and extends to wider opening angles with decreasing from S(8) to S(1) rotational transitions, indicating the disk wind as its origin. The outflow from TMC1-E protostar shows spatially extended emission lines of Ne II Ne III Ar II and Ar III with their line ratios consistent with UV radiation as a source of ionization. With ALMA, we detected an accretion streamer infalling from $>$ 1000 au scaling onto the TMC1-E component. The TMC1-W protostar powers a collimated jet, detected with Fe II and Ni II making it consistent with energetic flow. A much weaker ionized jet is observed from TMC1-E, and both jets appear strikingly parallel to each other, indicating that the disks are co-planar. TMC1-W is associated with strong emission from hydrogen recombination lines, tracing the accretion onto the young star. MIRI-MRS observations provide an unprecedented view of protostellar accretion and ejection processes on 20 au scales. Observations of a binary Class I protostellar system show that the two processes are clearly intertwined, with accretion from the envelope onto the disk influencing a wide-angle wind ejected on disk scales. Finally, the accretion from the protostellar disk onto the protostar is associated with the source launching a collimated high-velocity jet within the innermost regions of the disk.

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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

Cited by 10 publications

References 112 publications

PROJECT-J: JWST Observations of HH46 IRS and Its Outflow. Overview and First Results

PROJECT-J: JWST Observations of HH46 IRS and Its Outflow. Overview and First Results

Hunting for complex cyanides in protostellar ices with the JWST

JWST Observations of Young protoStars (JOYS)

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