Shigehisa Takakuwa et al 2004 ApJ 616 L15 doi:10.1086/421939
Shigehisa Takakuwa1, Nagayoshi Ohashi2, Paul T. P. Ho3, Chunhua Qi3, David J. Wilner3, Qizhou Zhang3, Tyler L. Bourke1, Naomi Hirano4, Minho Choi4,5 and Ji Yang6
Show affiliationsWe have imaged the circumstellar envelope around the binary protostar L1551 IRS 5 in CS J = 7-6 and 343 GHz continuum emission at ~3'' resolution using the Submillimeter Array. The continuum emission shows an elongated structure (~220 × 100 AU) around the binary perpendicular to the axis of the associated radio jet. The CS emission extends over ~400 AU, appears approximately circularly symmetric, and shows a velocity gradient from southeast (blueshifted) to northwest (redshifted). The direction of the velocity gradient is different from that observed in C18O J = 1-0. This may be because rotation is more dominant in the CS envelope than the C18O envelope, in which both infall and rotation exist. The CS emission can be divided into two velocity components: (1) a "high"-velocity disklike structure surrounding the protostar ±1.0-1.5 km s-1 from the systemic velocity, and (2) a "low"-velocity structure located southwest of the protostar less than 1.0 km s-1 from the systemic velocity. The high-velocity component traces warm and dense gas with kinematics consistent with rotation around the protostar. The low-velocity component may arise from dense gas entrained in the outflow. Alternatively, this component may trace infalling and rotating gas in an envelope with a vertical structure.
ISM: individual (L1551 IRS 5); ISM: molecules; planetary systems: protoplanetary disks; stars: formation
Issue 1 (2004 November 20)
Received 2004 February 18, accepted for publication 2004 April 16
Published 2004 October 28
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