Feedback of atomic jets from embedded protostars in NGC 1333

Dionatos, O.; Güdel, M.

doi:10.1051/0004-6361/201629179

Cited by 28 publications

(29 citation statements)

References 49 publications

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“…Towards the south, there is a narrow 'u' shaped filament connecting the IRAS 2 and the IRAS 4 regions. At the bottom of the 'u' is a known Class 0 YSO source -SK 1 (Dionatos & Güdel 2017). There is another narrow short filament in this area extending towards the south-west from the IRAS 2 region.…”

Section: Ammonia (11) Resultsmentioning

confidence: 99%

Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333

Dhabal

Mundy

Chen

et al. 2019

ApJ

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We use NH 3 inversion transitions to trace the dense gas in the NGC 1333 region of the Perseus molecular cloud. NH 3 (1,1) and NH 3 (2,2) maps covering an area of 102 square arcminutes at an angular resolution of ∼3.7 are produced by combining VLA interferometric observations with GBT single dish maps. The combined maps have a spectral resolution of 0.14 km/s and a sensitivity of 4 mJy/beam. We produce integrated intensity maps, peak intensity maps and dispersion maps of NH 3 (1,1) and NH 3 (2,2) and a line-of-sight velocity map of NH 3 (1,1). These are used to derive the optical depth for the NH 3 (1,1) main component, the excitation temperature of NH 3 (1,1), and the rotational temperature, kinetic temperature and column density of NH 3 over the mapped area. We compare these observations with the CARMA J=1-0 observations of N 2 H + and H 13 CO + and conclude that they all trace the same material in these dense star forming regions. From the NH 3 (1,1) velocity map, we find that a velocity gradient ridge extends in an arc across the entire southern part of NGC 1333. We propose that a large scale turbulent cell is colliding with the cloud, which could result in the formation of a layer of compressed gas. This region along the velocity gradient ridge is dotted with Class 0/I YSOs, which could have formed from local overdensities in the compressed gas leading to gravitational instabilities. The NH 3 (1,1) velocity dispersion map also has relatively high values along this region, thereby substantiating the shock layer argument.

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Section: Ammonia (11) Resultsmentioning

confidence: 99%

Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333

Dhabal

Mundy

Chen

et al. 2019

ApJ

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“…The 2015) and Dionatos & Güdel (2017). In comparison to HIFI line profiles, only BHR71 and HH46 show the high-velocity wings in both [O I] and H 2 O 1 10 − 1 01 Green et al 2013;Mottram et al 2017…”

Section: High-velocity Emission In [O I]mentioning

confidence: 96%

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

Karska

Kaufman

Kristensen

et al. 2018

ApJS

118

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Recent observations from Herschel allow the identification of important mechanisms responsible for the heating of gas surrounding low-mass protostars and its subsequent cooling in the far-infrared (FIR). Shocks are routinely invoked to reproduce some properties of the far-IR spectra, but standard models fail to reproduce the emission from key molecules, e.g. H 2 O. Here, we present the Herschel-PACS far-IR spectroscopy of 90 embedded low-mass protostars (Class 0/I). The Herschel-PACS spectral maps covering ∼ 55 − 210 µm with a field-of-view of ∼50" are used to quantify the gas excitation conditions and spatial extent using rotational transitions of H 2 O, high-J CO, and OH, as well as [O I] and [C II]. We confirm that a warm (∼300 K) CO reservoir is ubiquitous and that a hotter component (760 ± 170 K) is frequently detected around protostars. The line emission is extended beyond ∼1000 AU spatial scales in 40/90 objects, typically in molecular tracers in Class 0 and atomic tracers in Class I objects. High-velocity emission ( 90 km s −1 ) is detected in only 10 sources in the [O I] line, suggesting that the bulk of [O I] arises from gas that is moving slower than typical jets. Line flux ratios show an excellent agreement with models of C-shocks illuminated by UV photons for pre-shock densities of ∼10 5 cm −3 and UV fields 0.1-10 times the interstellar value. The far-IR molecular and atomic lines are a unique diagnostic of feedback from UV emission and shocks in envelopes of deeply embedded protostars.

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“…It is worth noting that this region does contain several outflows (e.g. Dionatos & Güdel 2017), including a second molecular flow detected at mm-wavelengths along the western edge of the HH 7-11 cavity (Lefévre et al 2017).…”

Section: Hh 11mentioning

confidence: 99%

Proper Motions and Shock Wave Dynamics in the HH 7-11 Stellar Jet

Hartigan

Holcomb

Frank

2019

ApJ

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We have used the Hubble Space Telescope to acquire new broad-band and narrow-band images of the optical line emission and red continuum associated with the HH 7-11 stellar jet in the NGC 1333 star formation region. Combining the new narrow-band images of Hα, [O I] λ6300 and [S II] λ6716 allows us to measure electron densities and excitations at each point in the outflow with the spatial resolution of HST, while the I-band image traces out the boundary of the cavity evacuated by the outflow. Comparing these images with those taken ∼ 20 years ago yields high precision proper motions for all the HH objects in the outflow. HH 11 is a bullet-like clump, and emerges from the exciting source SVS 13A towards the Earth at 24 degrees to line of sight. In contrast, HH 8 and HH 10 consist of two rings of shocked gas that show no bulk proper motions even though the emitting gas is blueshifted. The HH 8 rings are expanding with time.These shocks mark places where ambient material located along the path of the jet redirects the outflow. HH 7 consists of multiple shells, and emits strongly in H 2 in what appears to be a terminal bow shock for the outflow, implying that the jet has yet to fully break out of its nascent cloud core. The jet largely fragments into clumps by the time it reaches HH 7. As in the case of HH 110, deflection from ambient material plays a key role in producing observable shock waves in the HH 7-11 outflow.

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Feedback of atomic jets from embedded protostars in NGC 1333

Cited by 28 publications

References 49 publications

Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333

Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333

The Herschel-PACS Legacy of Low-mass Protostars: The Properties of Warm and Hot Gas Components and Their Origin in Far-UV Illuminated Shocks

Proper Motions and Shock Wave Dynamics in the HH 7-11 Stellar Jet

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