A Chemical View of Protostellar-Disk Formation in L1527

Sakai, Nami; Oya, Yoko; Sakai, Takeshi; Watanabe, Yoshimasa; Hirota, Tomoya; Ceccarelli, C.; Kahane, C.; López-Sepulcre, A.; Leflóch, B.; Vastel, C.; Bottinelli, S.; Caux, E.; Coutens, A.; Aikawa, Yuri; Takakuwa, Shigehisa; Ohashi, Nagayoshi; Yen, Hsi-Wei; Yamamoto, Satoshi

doi:10.1088/2041-8205/791/2/l38

Cited by 114 publications

(185 citation statements)

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“…The PV diagram of the model prepared along the envelope reflects only the absolute value of its inclination angle, and it does not reflect the direction of its inclination from the plane of the sky. Hence, Sakai et al (2014a) did not consider the direction of the inclination in the analysis of the PV diagram. Therefore, we here examine the PV diagrams of the CS (J = 5-4) and c-C 3 H 2 (5 2,3 -4 3,2 ) lines prepared along various lines passing through the protostar position to investigate the direction of the inclination of the envelope.…”

Section: Envelopementioning

confidence: 99%

“…7,  which is the FWHM of the synthesized beam along the east-west axis. This value was derived using the RADEX code (van der Tak et al 2007), where the H 2 density and the kinetic temperature were assumed to be 10 6 -10 7 cm −3 and 30 K, respectively (Sakai et al 2014a(Sakai et al , 2014b. The H 2 column density is then roughly estimated to be (1-2) × 10 22 cm −2 by using a CS fractional abundance relative to H 2 of 10 −9 , a typical value for protostellar cores (e.g., van Dishoeck et al 1995;Watanabe et al 2012).…”

Section: Direction Of the Outflowmentioning

confidence: 99%

“…However, Sakai et al (2014a) pointed out that H 2 CO possibly resides inward of the centrifugal barrier. If so, the gas has to lose its angular momentum to fall beyond the centrifugal barrier.…”

Section: Angular Momentummentioning

confidence: 99%

“…In these models, the protostellar mass and the radius of the centrifugal barrier are assumed to be 0.18 M e and 100 AU, respectively, which are derived by Sakai et al (2014b). The outer radius of the envelope is fixed to be 1000 AU, which well reproduces the PV diagram of CCH (Sakai et al 2014a). The density profile is assumed to be proportional to r −1.5 .…”

Section: Comparison With Other Sourcesmentioning

confidence: 99%

“…On the other hand, the existence of a Keplerian disk was suggested by Tobin et al (2012) and Ohashi et al (2014) by observations of the 13 CO and 18 CO (J = 2-1) lines, respectively. Recently, Sakai et al (2014aSakai et al ( , 2014b presented a clear infalling rotating motion in its envelope at a resolution of 0. 6  with ALMA.…”

Section: Introductionmentioning

confidence: 99%

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

Oya

Sakai

Leflóch

et al. 2015

ApJ

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Subarcsecond-resolution images of the rotational line emissions of CS and c-C 3 H 2 obtained toward the low-mass protostar IRAS 04368+2557 in L1527 with the Atacama Large Millimeter/submillimeter Array are investigated to constrain the orientation of the outflow/envelope system. The distribution of CS consists of an envelope component extending from north to south and a faint butterfly shaped outflow component. The kinematic structure of the envelope is well reproduced by a simple ballistic model of an infalling rotating envelope. Although the envelope has a nearly edge-on configuration, we find that the western side of the envelope faces the observer. This configuration is opposite to the direction of the large-scale (∼10 4 AU) outflow suggested previously from the 12 CO (J = 3-2) observation, and to the morphology of infrared reflection near the protostar (∼200 AU). The latter discrepancy could originate from high extinction by the outflow cavity of the western side, or may indicate that the outflow axis is not parallel to the rotation axis of the envelope. Position-velocity diagrams show the accelerated outflow cavity wall, and its kinematic structure in the 2000 AU scale is explained by a standard parabolic model with the inclination angle derived from the analysis of the envelope. The different orientation of the outflow between the small and large scale implies a possibility of precession of the outflow axis. The shape and the velocity of the outflow in the vicinity of the protostar are compared with those of other protostars.

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Section: Envelopementioning

confidence: 99%