Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, J. K. Jørgensen, John Tobin, Yuri Aikawa, I. de Gregorio‐Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, S. Lai, Chang Won Lee, Jeong‐Eun Lee, Zhi‐Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyễn Thị Phương, Jinshi Sai, Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Abstract
Abstract Precise estimates of protostellar masses are crucial to characterize the formation of stars of low masses down to brown dwarfs (BDs; M * < 0.08 M ☉ ). The most accurate estimation of protostellar mass uses the Keplerian rotation in the circumstellar disk around the protostar. To apply the Keplerian rotation method to a protostar at the low-mass end, we have observed the Class 0 protostar IRAS 16253-2429 using the Atacama Large Millimeter/submillimeter Array (ALMA) in the 1.3 mm continuum at an angular resolution of 0.″07 (10 au), and in the 12 CO, C 18 O, 13 CO ( J = 2–1), and SO ( J N = 6 5 −5 4 ) molecular lines, as part of the ALMA Large Program Early Planet Formation in Embedded Disks project. The continuum emission traces a nonaxisymmetric, disk-like structure perpendicular to the associated 12 CO outflow. The position–velocity (PV) diagrams in the C 18 O and 13 CO lines can be interpreted as infalling and rotating motions. In contrast, the PV diagram along the major axis of the disk-like structure in the 12 CO line allows us to identify Keplerian rotation. The central stellar mass and the disk radius are estimated to be ∼0.12–0.17 M ☉ and ∼13–19 au, respectively. The SO line suggests the existence of an accretion shock at a ring ( r ∼ 28 au) surrounding the disk and a streamer from the eastern side of the envelope. IRAS 16253-2429 is not a proto-BD but has a central stellar mass close to the BD mass regime, and our results provide a typical picture of such very-low-mass protostars.