The CARMA–NRO Orion Survey: Protostellar Outflows, Energetics, and Filamentary Alignment

Feddersen, Jesse R.; Arce, Héctor G.; Kong, Shuo; Suri, S.; Sánchez-Monge, Á.; Ossenkopf-Okada, Volker; Dunham, Michael M.; Nakamura, Fúmitaka; Shimajiri, Yoshito; Bally, John

doi:10.3847/1538-4357/ab86a9

Cited by 37 publications

(57 citation statements)

References 82 publications

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“…Protostellar outflows inject a significant amount of energy and momentum into the surroundings (Arce et al 2010;Plunkett et al 2013;Feddersen et al 2020), and are likely to have a profound impact on their host cores. This is especially true in the context of low-mass star formation where other feedback mechanisms do not come into play.…”

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confidence: 99%

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

Rohde

Walch

Clarke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The accretion of material onto young protostars is accompanied by the launching of outflows. Observations show that accretion, and therefore also outflows, are episodic. However, the effects of episodic outflow feedback on the core-scale are not well understood. We have performed 88 Smoothed Particle Hydrodynamic simulations of turbulent dense $1 \, \rm {M}_{\odot }$ cores, to study the influence of episodic outflow feedback on the stellar multiplicity and the star formation efficiency (SFE). Protostars are represented by sink particles, which use a sub-grid model to capture stellar evolution, inner-disc evolution, episodic accretion and the launching of outflows. By comparing simulations with and without episodic outflow feedback, we show that simulations with outflow feedback reproduce the binary statistics of young stellar populations, including the relative proportions of singles, binaries, triples, etc. and the high incidence of twin binaries with q ≥ 0.95; simulations without outflow feedback do not. Entrainment factors (the ratio between total outflowing mass and initially ejected mass) are typically ∼7 ± 2, but can be much higher if the total mass of stars formed in a core is low and/or outflow episodes are infrequent. By decreasing both the mean mass of the stars formed and the number of stars formed, outflow feedback reduces the SFE by about a factor of 2 (as compared with simulations that do not include outflow feedback).

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mentioning

confidence: 99%

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

Rohde

Walch

Clarke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…FIR1a-b, MMS5, SIMBA-a, and FIR6c-a are sources for which the two properties are clearly observed as an outflow was detected towards these sources in previous studies (e.g. Aso et al 2000;Williams et al 2003;Takahashi et al 2008;Tobin et al 2016;Tanabe et al 2019;Feddersen et al 2020;Nagy et al 2020). A large outflow was also detected towards the MMS9 and CSO33 systems, but the angular resolution does not allow us to determine which of the components is actually the driving source (e.g.…”

Section: Sources Whose Previous Classification Is Confirmedmentioning

confidence: 84%

“…A large outflow was also detected towards the MMS9 and CSO33 systems, but the angular resolution does not allow us to determine which of the components is actually the driving source (e.g. Williams et al 2003;Takahashi et al 2008;Tanabe et al 2019;Feddersen et al 2020).…”

Section: Sources Whose Previous Classification Is Confirmedmentioning

confidence: 99%

“…An outflow has been detected towards the MMS2 system (e.g. Aso et al 2000;Williams et al 2003;Takahashi et al 2008;Tanabe et al 2019;Feddersen et al 2020), but we need high angular resolution studies to understand which of the two sources is the driving source, and thus which of the two sources is younger. Finally, in the case of CSO3-b, we can see that the 32.9 GHz emission is quite weak, but we cannot determine whether free-free emission is present.…”

Section: Sources Whose Previous Classification Is Confirmedmentioning

confidence: 99%

“…Outflows have been detected towards CSO33 and MMS9, but the angular resolution of the observations was insufficient to determine which of the sources actually drives them (e.g. Williams et al 2003;Takahashi et al 2008;Tanabe et al 2019;Feddersen et al 2020). The dust emissivity spectral indexes of these sources are very different, with β ≤ 0.7 for CSO33-a, β = 0 for MMS9-b, and β ∈ [0.3;1.8] for MMS9-c.…”

Section: Sources Whose Previous Classification Is Modifiedmentioning

confidence: 99%

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ORion Alma New GEneration Survey (ORANGES)

Bouvier

López-Sepulcre

Ceccarelli

et al. 2021

A&A

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Context. The spectral energy distribution (SED) in the millimetre to centimetre range is an extremely useful tool for characterising the dust in protostellar envelopes as well as free-free emission from the protostar and outflow. Actually, the evolutionary status of solar-type protostars is often based on their SED in the near-infrared to millimetre range. In addition, the presence or absence of free-free emission can be considered an indicator of the source evolutionary stage (Class 0/I versus Class II/III). While many studies have been carried out towards low- and high-mass protostars, little exists so far about solar-type protostars in high-mass star-forming regions, which are likely to be representatives of the conditions where the Solar System was born. Aims. In this work, we focus on the embedded solar-type protostars in the Orion Molecular Cloud (OMC) 2 and 3 filaments, which are bounded by nearby HII regions and which are, therefore, potentially affected by the high-UV illumination of the nearby OB stars. We use various dust parameters to understand whether the small-scale structure (≤1000 au) and the evolutionary status of these solar-type protostars are affected by the nearby HII regions, as is the case for the large-scale (≤104 au) gas chemical composition. Methods. We used the Atacama Large (sub-)Millimeter Array (ALMA) in the 1.3 mm band (246.2 GHz) to image the continuum of 16 young (Class 0/I) OMC-2/3 solar-type protostars, with an angular resolution of 0.25″ (100 au). We completed our data with archival data from the ALMA and VLA VANDAM survey of Orion Protostars at 333 and 32.9 GHz, respectively, to construct the dust SED and extract the dust temperature, the dust emissivity spectral index, the envelope plus disk mass of the sources and to assess whether free-free emission is contaminating their dust SED in the centimetre range. Results. From the millimetre to centimetre range dust SED, we found low dust emissivity spectral indexes (β < 1) for the majority of our source sample and free-free emission towards only 5 of the 16 sample sources. We were also able to confirm or correct the evolutionary status of the source sample reported in the literature. Finally, we did not find any dependence of the source dust parameters on their location in the OMC-2/3 filament. Conclusions. Our results show that the small-scale dust properties of the embedded OMC-2/3 protostars are not affected by the high-UV illumination from the nearby HII regions and that the formation of protostars likely takes place simultaneously throughout the filament.

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Gas phase Elemental abundances in Molecular cloudS (GEMS)

Fuente

Rivière-Marichalar

Beitia-Antero

et al. 2023

A&A

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Context. Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30m large program aimed at determining the elemental abundances of carbon (C), oxygen (O), nitrogen (N), and sulfur (S) in a selected set of prototypical star-forming filaments. In particular, the elemental abundance of S remains uncertain by several orders of magnitude, and its determination is one of the most challenging goals of this program. Aims. This paper aims to constrain the sulfur elemental abundance in Taurus, Perseus, and Orion A based on the GEMS molecular database. The selected regions are prototypes of low-mass, intermediate-mass, and high-mass star-forming regions, respectively, providing useful templates for the study of interstellar chemistry. Methods. We have carried out an extensive chemical modeling of the fractional abundances of CO, HCO + , HCN, HNC, CS, SO, H 2 S, OCS, and HCS + to determine the sulfur depletion toward the 244 positions in the GEMS database. These positions sample visual extinctions from A V ∼ 3 mag to >50 mag, molecular hydrogen densities ranging from a few ×10 3 cm −3 to 3×10 6 cm −3 , and T k ∼ 10−35 K. We investigate the possible relationship between sulfur depletion and the grain charge distribution in different environments. Results. Most of the positions in Taurus and Perseus are best fitted assuming early-time chemistry, t=0.1 Myr, ζ H 2 ∼ (0.5−1)×10 −16 s −1 , and [S/H]∼1.5×10 −6 . On the contrary, most of the positions in Orion are fitted with t=1 Myr and ζ H 2 ∼ 10 −17 s −1 . Moreover, ∼40% of the positions in Orion are best fitted assuming the undepleted sulfur abundance, [S/H]∼1.5×10 −5 . We find a tentative trend of sulfur depletion increasing with density. Conclusions. Our results suggest that sulfur depletion depends on the environment. While the abundances of sulfur-bearing species are consistent with undepleted sulfur in Orion, a depletion factor of ∼20 is required to explain those observed in Taurus and Perseus. We propose that differences in the grain charge distribution might explain these variations. Grains become negatively charged at a visual extinction of A V ∼ 3.5 mag in Taurus and Perseus. At this low visual extinction, the S + abundance is high, X(S + )>10 −6 , and the electrostatic attraction between S + and negatively charged grains could contribute to enhance sulfur depletion. In Orion, the net charge of grains remains approximately zero until higher visual extinctions (A V ∼ 5.5 mag), where the abundance of S + is already low because of the higher densities, thus reducing sulfur accretion. The shocks associated with past and ongoing star formation could also contribute to enhance [S/H].

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The CARMA–NRO Orion Survey: Protostellar Outflows, Energetics, and Filamentary Alignment

Cited by 37 publications

References 82 publications

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

The impact of episodic outflow feedback on stellar multiplicity and the star formation efficiency

ORion Alma New GEneration Survey (ORANGES)

Gas phase Elemental abundances in Molecular cloudS (GEMS)

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