Revised SED of the triple protostellar system VLA 1623−2417

Murillo, Nadia M.; Harsono, Daniel; McClure, Melissa; Lai, Shih-Ping; Hogerheijde, M. R.

doi:10.1051/0004-6361/201833420

Cited by 15 publications

(13 citation statements)

References 35 publications

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“…In all these cases, however, the binaries are separated by more than 40−50 au. Most binary sources observed to have a circumbinary disk/envelope structure show only a single outflow or parallel outflows, e.g., BHB07-11 (Alves et al 2017), L1448 IRS3B-a, b (Lee et al 2015;Tobin et al 2016a), and L1551NE (Reipurth et al 2000;Lim et al 2016). An exception is the case of VLA 1623A.…”

Section: Scenario 1: Two Outflows Driven By a Binary Systemmentioning

confidence: 99%

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

Okoda

Oya

Francis

et al. 2021

ApJ

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We have observed the very low-mass Class 0 protostar IRAS 15398−3359 at scales ranging from 50 to 1800 au, as part of the Atacama Large Millimeter/Submillimeter Array Large Program FAUST. We uncover a linear feature, visible in H 2 CO, SO, and C 18 O line emission, which extends from the source in a direction almost perpendicular to the known active outflow. Molecular line emission from H 2 CO, SO, SiO, and CH 3 OH further reveals an arc-like structure connected to the outer end of the linear feature and separated from the protostar, IRAS 15398−3359, by 1200 au. The arc-like structure is blueshifted with respect to the systemic velocity. A velocity gradient of 1.2 km s −1 over 1200 au along the linear feature seen in the H 2 CO emission connects the protostar and the arc-like structure

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Section: Scenario 1: Two Outflows Driven By a Binary Systemmentioning

confidence: 99%

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

Okoda

Oya

Francis

et al. 2021

ApJ

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“…The classification of VLA 1623W has been under debate (Maury et al 2012;Murillo et al 2018). The spectral energy distribution of the VLA 1623 core indicates that VLA 1623A/B protostars are deeply embedded (e.g., Evans et al 2009;Gutermuth et al 2009) with a prominent bipolar outflow (e.g., White et al 2015), but the spectral energy distribution of VLA 1623W peaks at shorter wavelengths.…”

Section: A Individual Sourcesmentioning

confidence: 99%

“…The spectral energy distribution of the VLA 1623 core indicates that VLA 1623A/B protostars are deeply embedded (e.g., Evans et al 2009;Gutermuth et al 2009) with a prominent bipolar outflow (e.g., White et al 2015), but the spectral energy distribution of VLA 1623W peaks at shorter wavelengths. VLA 1623W also has a lower envelope mass compared to VLA 1623A/B Murillo et al 2018), and it has no obvious outflow A1 except for IRAS 16293A and IRAS 16293B. We also added the criterion that P F /σ PF > 3 to remove spurious e-vectors at the edges and off source.…”

Section: A Individual Sourcesmentioning

confidence: 99%

Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. III. Survey Overview

Sadavoy

Stephens

Myers

et al. 2019

ApJS

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We present 0.25 resolution (35 au) ALMA 1.3 mm dust polarization observations for 37 young stellar objects (YSOs) in the Ophiuchus molecular cloud. These data encompass all the embedded protostars in the cloud and several Flat and Class II objects to produce the largest, homogeneous study of dust polarization on disk scales to date. The goal of this study is to study dust polarization morphologies down to disk scales. We find that 14/37 (38%) of the observed YSOs are detected in polarization at our sensitivity. Nine of these sources have uniform polarization angles and four sources have azimuthal polarization structure. We find that the sources with uniform polarization tend to have steeper inclinations (> 60 • ) than those with azimuthal polarization (< 60 • ). Overall, the majority (9/14) of the detected sources have polarization morphologies and disk properties consistent with dust self-scattering processes in optically thick disks. The remaining sources may be instead tracing magnetic fields. Their inferred field directions from rotating the polarization vectors by 90 • are mainly poloidal or hourglass shaped. We find no evidence of a strong toroidal field component toward any of our disks. For the 23 YSOs that are undetected in polarization, roughly half of them have 3-sigma upper limits of < 2%. These sources also tend to have inclinations < 60 • and they are generally compact. Since lower inclination sources tend to have azimuthal polarization, these YSOs may be undetected in polarization due to unresolved polarization structure within our beam. We propose that disks with inclinations > 60 • are the best candidates for future polarization studies of dust selfscattering as these systems will generally show uniform polarization vectors that do not require very high resolution to resolve. We release the continuum and polarization images for all the sources with this publication. Data from the entire survey can be obtained from Dataverse. † Hubble Fellow

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“…The envelope mass is substantially larger due to the younger nature of our source. In VLA 1623, Murillo et al (2018) derive an envelope mass of ∼ 1.0 M , assuming the two binary sources A & B share the same envelope. Pineda et al (2020) cite a dense core mass of 3.2 M for IRAS 03292+3039, the largest of all the sources.…”

Section: Mass-infall Ratementioning

confidence: 99%

Accretion Flows or Outflow Cavities? Uncovering the Gas Dynamics around Lupus 3-MMS

Thieme,

Lai,

Lin

et al. 2021

Preprint

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Understanding how material accretes onto the rotationally supported disk from the surrounding envelope of gas and dust in the youngest protostellar systems is important for describing how disks are formed. Magnetohydrodynamic simulations of magnetized, turbulent disk formation usually show spiral-like streams of material (accretion flows) connecting the envelope to the disk. However, accretion flows in these early stages of protostellar formation still remain poorly characterized due to their low intensity and possibly some extended structures are disregarded as being part of the outflow cavity. We use ALMA archival data of a young Class 0 protostar, Lupus 3-MMS, to uncover four extended accretion flow-like structures in C 18 O that follow the edges of the outflows. We make various types of position-velocity cuts to compare with the outflows and find the extended structures are not consistent with the outflow emission, but rather more consistent with a simple infall model. We then use a dendrogram algorithm to isolate five sub-structures in position-position-velocity space. Four out of the five sub-structures fit well (>95%) with our simple infall model, with specific angular momenta between 2.7 − 6.9 × 10 −4 km s −1 pc and mass-infall rates of 0.5 − 1.1 × 10 −6 M yr −1 . Better characterization of the physical structure in the supposed "outflow-cavities" is important to disentangle the true outflow cavities and accretion flows.

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Revised SED of the triple protostellar system VLA 1623−2417

Cited by 15 publications

References 35 publications

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

FAUST. II. Discovery of a Secondary Outflow in IRAS 15398−3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?

Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. III. Survey Overview

Accretion Flows or Outflow Cavities? Uncovering the Gas Dynamics around Lupus 3-MMS

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