ALMA Observations of the Protostellar Disk around the VeLLO IRAS 16253–2429

Hsieh, Tsung‐Hsin; Hirano, Naomi; Беллоче, А.; Lee, Chin-Fei; Aso, Yusuke; Lai, Shih-Ping

doi:10.3847/1538-4357/aaf4fe

Cited by 26 publications

(30 citation statements)

References 79 publications

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“…Since most of our disks are compact (< 2 beams), we may be biased to steeper inclinations. Nevertheless, higher resolution observations of WL 17, Oph-emb-1, and VLA 1623B (Sheehan & Eisner 2017;Harris et al 2018;Hsieh et al 2019b) give consistent inclinations within 5 • of our estimate, which suggest that our inclinations are broadly reliable. Figure 10 compares disk inclination with peak intensity (top) and deconvolved semi-major axis size (bottom) for the sources with uniform polarization (red diamonds), azimuthal polarization (blue diamonds), and undetected sources (open diamonds).…”

Section: Non-detected Polarizationsupporting

confidence: 78%

“…Such morphologies are generally expected in gravitationally dominated systems where the field is flux-frozen to the gas and dragged inward with the contraction (e.g., Mestel 1966;Mestel & Strittmatter 1967;Galli & Shu 1993). Indeed, each of these sources show evidence of infall or accretion (e.g., Mardones et al 1997;Pineda et al 2012;Evans et al 2015;Mottram et al 2017;Hsieh et al 2019b), which suggests that their larger cores and envelopes are collapsing. Poloidal fields are important for driving jets and outflows (e.g., Hennebelle & Ciardi 2009;Tomisaka 2011), but they can also remove angular momentum through magnetic braking and suppress the formation of disks or companion stars (e.g., Machida et al 2005;Price & Bate 2007;Hennebelle & Fromang 2008;Li et al 2011).…”

Section: Field Morphologiesmentioning

confidence: 95%

“…Previous high resolution observations of Oph-emb-1 (Chen et al 2013;Yen et al 2017;Hsieh et al 2019b) revealed a compact, elongated structure perpendicular to the outflow that is indicative of a disk. Hsieh et al (2019b) further show that this structure has red-and blue-shifted C 18 O (2-1) emission indicative of both infall and rotation. They suggest that Oph-emb-1 is likely to form a brown dwarf.…”

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confidence: 94%

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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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Section: Non-detected Polarizationsupporting

confidence: 78%

Section: Field Morphologiesmentioning

confidence: 95%

mentioning

confidence: 94%

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

Sadavoy

Stephens

Myers

et al. 2019

ApJS

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“…13 CS peaks at the same place as C 18 O, but is less spatially extended, and seems to be very well coupled with the dust emission in the SW outflow cavity wall. The kinematics of these two lines did not reveal any evidence of rotation in the inner core, which has been seen previously in molecular line observations of Class 0 disk-envelope systems (Ohashi et al 2014;Yen et al 2015;Lee et al 2016;Jacobsen et al 2018;Hsieh et al 2019). Rather, the kinematic information suggests that the gas is linked with the outflow motion.…”

Section: Serpens Emb 8(n)supporting

confidence: 59%

Characterizing Magnetic Field Morphologies in Three Serpens Protostellar Cores with ALMA

Gouellec

Hull

Maury

et al. 2019

ApJ

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With the aim of characterizing the dynamical processes involved in the formation of young protostars, we present high angular resolution ALMA dust polarization observations of the Class 0 protostellar cores Serpens SMM1, Emb 8(N), and Emb 8. With spatial resolutions ranging from 150 to 40 au at 870 µm, we find unexpectedly high values of the polarization fraction along the outflow cavity walls in Serpens Emb8(N). We use 3 mm and 1 mm molecular tracers to investigate outflow and dense gas properties and their correlation with the polarization. These observations allow us to investigate the physical processes involved in the Radiative Alignment Torques (RATs) acting on dust grains along the outflow cavity walls, which experience irradiation from accretion processes and outflow shocks. The inner core of SMM1-a presents a polarization pattern with a poloidal magnetic field at the bases of the two lobes of the bipolar outflow. To the south of SMM1-a we see two polarized filaments, one of which seems to trace the redshifted outflow cavity wall. The other may be an accretion streamer of material infalling onto the central protostar. We propose that the polarized emission we see at millimeter wavelengths along the irradiated cavity walls can be reconciled with the expectations of RAT theory if the aligned grains present at < 500 au scales in Class 0 envelopes have grown larger than the 0.1 µm size of ISM dust grains. Our observations allow us to constrain the star-forming sources' magnetic field morphologies within the central cores, along the outflow cavity walls, and in possible accretion streamers.

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“…So far, direct evidence of Keplerian motions has only been found in a few Class 0 protostars and that is thanks to high resolution (sub-)millimeter interferometric observations: L1527, a border-line Class 0 object (Tobin et al 2012b;Ohashi et al 2014;Aso et al 2017, disk radius of 74 au), VLA1623, the pro-Article number, page 1 of 24 arXiv:2001.06355v1 [astro-ph.SR] 17 Jan 2020 A&A proofs: manuscript no. ms totypical Class 0 protostar (Murillo et al 2013, disk radius of 150 au), HH212 (Codella et al 2014;Lee et al 2014, disk radius of 90-120 au), L1448-IRS3 (Tobin et al 2016a, disk radius of ∼400 au), Lupus 3 MMS (Yen et al 2017, disk radius of 100 au), and IRAS 16253-2429 (Hsieh et al 2019, disk radius of 8-32 au). On the other hand, no disks have been detected at scales larger than 100 au in NGC1333-IRAS2A (Maret et al 2014) and 10 au in B335 (Yen et al 2015b).…”

Section: Introductionmentioning

confidence: 99%

Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO

Maret

Maury

Беллоче

et al. 2020

A&A

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The formation of protoplanetary disks is not well understood. To understand how and when these disks are formed, it is crucial to characterize the kinematics of the youngest protostars at a high angular resolution. Here we study a sample of 16 Class 0 protostars to measure their rotation profile at scales from 50 to 500 au and search for Keplerian rotation. We used high-angular-resolution line observations obtained with the Plateau de Bure Interferometer as part of the CALYPSO large program. From 13 CO (J = 2 − 1), C 18 O (J = 2 − 1) and SO (N j = 5 6 − 4 5 ) moment maps, we find that seven sources show rotation about the jet axis at a few hundred au scales: SerpS-MM18, L1448-C, L1448-NB, L1527, NGC1333-IRAS2A, NGC1333-IRAS4B, and SVS13-B. We analyzed the kinematics of these sources in the uv plane to derive the rotation profiles down to 50 au scales. We find evidence for Keplerian rotation in only two sources, L1527 and L1448-C. Overall, this suggests that Keplerian disks larger than 50 au are uncommon around Class 0 protostars. However, in some of the sources, the line emission could be optically thick and dominated by the envelope emission. Due to the optical thickness of these envelopes, some of the disks could have remained undetected in our observations.

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ALMA Observations of the Protostellar Disk around the VeLLO IRAS 16253–2429

Cited by 26 publications

References 79 publications

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

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

Characterizing Magnetic Field Morphologies in Three Serpens Protostellar Cores with ALMA

Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO

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