The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. IV. Unveiling the Embedded Intermediate-Mass Protostar and Disk within OMC2-FIR3/HOPS-370

Tobin, John J.; Sheehan, Patrick; Reynolds, Nickalas; Megeath, S. Thomas; Osorio, M. R. Zapatero; Anglada, Guillem; Díaz-Rodríguez, A. K.; Furlan, Elise; Kratter, Kaitlin M.; Offner, Stella S. R.; Looney, Leslie W.; Kama, M.; Li, Zhi-Yun; Hoff, Merel L. R. van ’t; Sadavoy, Sarah; Karnath, Nicole

doi:10.3847/1538-4357/abc5bf

Cited by 32 publications

(46 citation statements)

References 127 publications

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“…A small amount of gas remains in the envelope around FIR 6b (Chini et al 1997;Furlan et al 2016;Shimajiri et al 2009). In addition, a disk-like structure with a size of ∼ 126 au and ∼ 56 au were also inferred from continuum observations at 0.87 mm by the Atacama Large Millimeter/submillimetre Array (ALMA) and 9 mm by the Very Large Array (VLA), respectively (Tobin et al 2020). Thus, FIR 6b is expected to be in the late main accretion phase and considered to be a Class 0 protostar.…”

Section: Introductionmentioning

confidence: 88%

“…FIR 6b is a Class 0 intermediate mass protostar (Chini et al 1997;Furlan et al 2016;Takahashi et al 2008). The distance to FIR 6b is d ∼392 pc (Tobin et al 2020) and the systemic velocity is v sys ∼ 11 km s −1 in the Local Standard of Rest (LSR) (Ikeda et al 2007). FIR 6b has a bolometric luminosity of L bol = 21.9 L (Furlan et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Super-fast Rotation in the OMC 2/FIR 6b Jet

Matsushita,

Takahashi,

Ishii

et al. 2021

Preprint

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We present ALMA CO (J=2-1) and 1.3 mm continuum observations of the high-velocity jet associated with the FIR 6b protostar located in the Orion Molecular Cloud-2. We detect a velocity gradient along the short axis of the jet in both the red-and blue-shifted components. The position-velocity diagrams along the short axis of the red-shifted jet show a typical characteristic of a rotating cylinder. We attribute the velocity gradient in the red-shifted component to rotation of the jet. The rotation velocity (> 20 km s −1 ) and specific angular momentum (> 10 22 cm 2 s −1 ) of the jet around FIR 6b are the largest among all jets in which rotation has been observed. By combining disk wind theory with our observations, the jet launching radius is estimated to be in the range of 2.18 − 2.96 au. The rapid rotation, large specific angular momentum, and a launching radius far from the central protostar can be explained by a magnetohydrodynamic disk wind that contributes to the angular momentum transfer in the late stages of protostellar accretion.

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Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Super-fast Rotation in the OMC 2/FIR 6b Jet

Matsushita,

Takahashi,

Ishii

et al. 2021

Preprint

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“…OMC-2 FIR4 is a protocluster located in the Orion Molecular Cloud 2 (OMC-2), at a distance of approximately 393±25 pc (Großschedl et al 2018). The source consists of several continuum sources embedded in an extended, diffuse envelope (Shimajiri et al 2008, López-Sepulcre et al 2013, Kainulainen et al 2017, Tobin et al 2019 and it is part of a long, pc-scale filament containing several young stellar objects (YSOs) and star-forming regions (e.g. Furlan et al 2016, Hacar et al 2018.…”

Section: Source Backgroundmentioning

confidence: 99%

“…There are two neighbouring far-infrared (FIR) sources: one to the south-east (FIR5), which is not included in our observations; and one to the north-west (FIR3), which is included in our observations. FIR3 itself is a Class I YSO (Tobin et al 2019). The envelope of OMC-2 FIR4, having an angular size of ∼ 10 − 15 or ∼ 4000-6000 au (e.g.…”

Section: Source Backgroundmentioning

confidence: 99%

Seeds of Life in Space (SOLIS). XIII. Nitrogen fractionation towards the protocluster OMC-2 FIR4

Evans,

Fontani,

Vastel

et al. 2021

Preprint

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Context. Isotopic fractionation is an important tool for investigating the chemical history of our Solar System. In particular, the isotopic fraction of nitrogen ( 14 N/ 15 N) is lower in comets and other pristine Solar System bodies with respect to the value measured for the protosolar nebula, suggesting a local chemical enrichment of 15 N during the formation of the Solar System. Therefore, interferometric studies of nitrogen fractionation in Solar System precursors are needed for us to obtain clues about our astrochemical origins. Aims. In this work we have investigated the variation in the 14 N/ 15 N ratio in one of the closest analogues of the environment in which the Solar System was born: the protocluster OMC-2 FIR4. We present the first comparison at high angular resolution between HCN and N 2 H + using interferometric data. Methods. We analysed observations of the HCN isotopologues H 13 CN and HC 15 N in the OMC-2 FIR4 protocluster. Specifically, we observed the transitions H 13 CN (1 − 0) and HC 15 N (1 − 0) with the NOrthern Extended Millimeter Array (NOEMA) within the context of the IRAM Seeds Of Life In Space (SOLIS) Large Program. We combined our results with analysis of archival data obtained with the Atacama Large Millimeter Array (ALMA) of N 2 H + and its 15 N isotopologues. Results. Our results show a small regional variation in the 14 N/ 15 N ratio for HCN, from ∼250 to 500. The ratios in the central regions of FIR4, where the candidate protostars are located, are largely consistent with one another and within that range (∼300). They also show little variation from the part of the protocluster known to harbour a high cosmic-ray ionisation rate to the portion with a lower rate. We also found a small variation in the 14 N/ 15 N ratio of N 2 H + across different regions, from ∼200 to ∼400. Conclusions. These results suggest that local changes in the physical parameters occurring on the small linear scales probed by our observations in the protocluster do not seem to affect the 14 N/ 15 N ratio in either HCN or N 2 H + and hence that this is independent of the molecule used. Moreover, the high level of irradiation due to cosmic rays does not affect the N fractionation either.

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“…Recent surveys by Tobin et al (2020) and Tychoniec et al (2020) studied the distribution of dust masses in Class 0, I, and II objects in Orion and Perseus with ALMA and the VLA and compared them to inferred exoplanet metallicities from Thorngren & Fortney (2019). They find that the average Class II disk does not contain enough total dust mass to reproduce the observed population of giant exoplanets.…”

Section: Introductionmentioning

confidence: 99%

Early planet formation in embedded protostellar disks: Setting the stage for the first generation of planetesimals

Cridland,

Rosotti,

Tabone

et al. 2021

Preprint

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Recent surveys of young star formation regions have shown that the average Class II object does not have enough dust mass to make the cores of giant planets. Younger Class 0/I objects have enough dust in their embedded disk, which begs the questions: can the first steps of planet formation occur in these younger systems? The first step is building the first planetesimals, generally believed to be the product of the streaming instability. Hence the question can be restated: are the physical conditions of embedded disks conducive to the growth of the streaming instability? The streaming instability requires moderately coupled dust grains and a dust-to-gas mass ratio near unity. Here we model the collapse of a 'dusty' proto-stellar cloud to show that if there is sufficient drift between the falling gas and dust, regions of the embedded disk can become sufficiently enhanced in dust to drive the streaming instability. We include four models, three with different dust grain sizes and one with a different initial cloud angular momentum to test a variety of collapse trajectories. We find a 'sweet spot' for planetesimal formation for grain sizes of a few 10s of micron since they fall sufficiently fast relative to the gas to build a high dust-to-gas ratio along the disk midplane, but have slow enough radial drift speeds in the embedded disk to maintain the high dust-to-gas ratio. Unlike the gas, which is held in hydrostatic equilibrium for a time due to gas pressure, the dust can begin collapsing from all radii at a much earlier time. The dust mass flux can thus be higher in Class 0/I systems than the gas flux, which builds an embedded dusty disk with a global dust-to-gas mass ratio that exceeds the ISM ratio by at least an order of magnitude. The streaming instability can produce at least between 7-35 M ⊕ of planetesimals in the Class 0/I phase of our smooth embedded disks, depending on the size of the falling dust grains. This mass is sufficient to build the core of the first giant planet in the system, and could be further enhanced by dust traps and/or pebble growth. This first generation of planetesimals could represent the first step in planet formation, and occurs earlier in the lifetime of the young star than is traditionally thought.

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The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. IV. Unveiling the Embedded Intermediate-Mass Protostar and Disk within OMC2-FIR3/HOPS-370

Cited by 32 publications

References 127 publications

Super-fast Rotation in the OMC 2/FIR 6b Jet

Super-fast Rotation in the OMC 2/FIR 6b Jet

Seeds of Life in Space (SOLIS). XIII. Nitrogen fractionation towards the protocluster OMC-2 FIR4

Early planet formation in embedded protostellar disks: Setting the stage for the first generation of planetesimals

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