Geometric and Kinematic Structure of the Outflow/Envelope System of L1527 Revealed by Subarcsecond-Resolution Observation of Cs

Oya, Yoko; Sakai, Nami; Leflóch, B.; López-Sepulcre, A.; Watanabe, Yoshimasa; Ceccarelli, C.; Yamamoto, Satoshi

doi:10.1088/0004-637x/812/1/59

Cited by 46 publications

(86 citation statements)

References 55 publications

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“…Meanwhile, velocity gradients are also seen in the PV diagram perpendicular to the disk direction (see Figure 8). Such behaviors are consistent with infalling-rotating motion in the envelope (e.g., Sakai et al 2014b;Oya et al 2015Oya et al , 2016, rather than pure rotation in the disk (see also Appendix C). The locations of the most blue and red-shifted emissions then correspond to the innermost radius of such an envelope (indicated by the blue arrows in Figure 6), where all the kinetic energy is converted to rotation (i.e., the centrifugal barrier; Sakai et al 2014a).…”

Section: Envelope/disk Tracerssupporting

confidence: 60%

An Ordered Envelope–Disk Transition in the Massive Protostellar Source G339.88-1.26

Zhang¹,

Tan²,

Sakai³

et al. 2019

ApJ

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We report molecular line observations of the massive protostellar source G339.88-1.26 with the Atacama Large Millimeter/Submillimeter Array. The observations reveal a highly collimated SiO jet extending from the 1.3 mm continuum source, which connects to a slightly wider but still highly collimated CO outflow. Rotational features perpendicular to the outflow axis are detected in various molecular emissions, including SiO, SO 2 , H 2 S, CH 3 OH, and H 2 CO emissions. Based on their spatial distributions and kinematics, we find that they trace different parts of the envelope-disk system. The SiO emission traces the disk and inner envelope in addition to the jet. The CH 3 OH and H 2 CO emissions mostly trace the infalling-rotating envelope, and are enhanced around the transition region between envelope and disk, i.e., the centrifugal barrier. The SO 2 and H 2 S emissions are enhanced around the centrifugal barrier, and also trace the outer part of the disk. Envelope kinematics are consistent with rotating-infalling motion, while those of the disk are consistent with Keplerian rotation. The radius and velocity of the centrifugal barrier are estimated to be about 530 au and 6 km s −1 , leading to a central mass of about 11 M , consistent with estimates based on spectral energy distribution fitting. These results indicate that an ordered transition from an infalling-rotating envelope to a Keplerian disk through a centrifugal barrier, accompanied by changes of types of molecular line emissions, is a valid description of this massive protostellar source. This implies that at least some massive stars form in a similar way as low-mass stars via Core Accretion.

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Section: Envelope/disk Tracerssupporting

confidence: 60%

An Ordered Envelope–Disk Transition in the Massive Protostellar Source G339.88-1.26

Zhang¹,

Tan²,

Sakai³

et al. 2019

ApJ

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“…• ; Oya et al 2015), its amplitude distribution shows different profiles along the major-and minor-axes, suggesting a pseudo disk-like envelope, while the envelope of SMM11 is more spherical. These may observationally imply that envelope morphology evolves from spherical shapes into more-disk like shapes.…”

Section: Continuum Visibilitymentioning

confidence: 98%

ALMA Observations of SMM11 Reveal an Extremely Young Protostar in Serpens Main Cluster

Aso¹,

Ohashi²,

Aikawa³

et al. 2017

ApJL

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We report the discovery of an extremely young protostar, SMM11, located in the associated submillimeter condensation in the Serpens Main cluster using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 3 at 1.3 mm and an angular resolution of ∼ 0.′′ 5 ∼ 210 AU. SMM11 is a Class 0 protostar without any counterpart at 70 µm or shorter wavelengths. The ALMA observations show 1.3 mm continuum emission associated with a collimated 12 CO bipolar outflow. Spitzer and Herschel data show that SMM11 is extremely cold (T bol =26 K) and faint (L bol 0.9L ⊙ ). We estimate the inclination angle of the outflow to be ∼ 80 • , almost parallel to the plane of the sky, from simple fitting using wind-driven-shell model. The continuum visibilities consist of Gaussian and power-law components, suggesting a spherical envelope with a radius of ∼ 600 AU around the protostar. The estimated low C 18 O abundance, X(C 18 O)=1.5-3×10 −10 , is also consistent with its youth. The high outflow velocity, a few 10 km s −1 at a few 1000 AU, is much higher than theoretical simulations of first hydrostatic cores and we suggest that SMM11 is a transitional object right after the second collapse of the first core.

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“…Using ALMA cycle 1 observations, Aso et al (2017) have recently confirmed Keplerian rotation at r < 56 au. The disk of L1527 is nearly edge-on (Tobin et al 2008;Oya et al 2015).…”

Section: L1527mentioning

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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Geometric and Kinematic Structure of the Outflow/Envelope System of L1527 Revealed by Subarcsecond-Resolution Observation of Cs

Cited by 46 publications

References 55 publications

An Ordered Envelope–Disk Transition in the Massive Protostellar Source G339.88-1.26

An Ordered Envelope–Disk Transition in the Massive Protostellar Source G339.88-1.26

ALMA Observations of SMM11 Reveal an Extremely Young Protostar in Serpens Main Cluster

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

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