TY - JOUR
T1 - Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS
AU - Yamato, Yoshihide
AU - Aikawa, Yuri
AU - Ohashi, Nagayoshi
AU - Tobin, John J.
AU - Jørgensen, Jes K.
AU - Takakuwa, Shigehisa
AU - Aso, Yusuke
AU - Insa Choi, Jinshi Sai
AU - Flores, Christian
AU - de Gregorio-Monsalvo, Itziar
AU - Hirano, Shingo
AU - Han, Ilseung
AU - Kido, Miyu
AU - Koch, Patrick M.
AU - Kwon, Woojin
AU - Lai, Shih Ping
AU - Lee, Chang Won
AU - Lee, Jeong Eun
AU - Li, Zhi Yun
AU - Lin, Zhe Yu Daniel
AU - Looney, Leslie W.
AU - Mori, Shoji
AU - Narayanan, Suchitra
AU - Phuong, Nguyen Thi
AU - Saigo, Kazuya
AU - Santamaría-Miranda, Alejandro
AU - Sharma, Rajeeb
AU - Thieme, Travis J.
AU - Tomida, Kengo
AU - van ’t Hoff, Merel L.R.
AU - Yen, Hsi Wei
N1 - ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Y.Y. is supported by the International Graduate Program for Excellence in Earth-Space Science (IGPEES), World-leading Innovative Graduate Study (WINGS) Program of the University of Tokyo. Y.A. acknowledges support by NAOJ ALMA Scientific Research Grant code 2019-13B, Grant-in-Aid for Scientific Research (S) 18H05222, and Grant-in-Aid for Transformative Research Areas (A) 20H05844 and 20H05847. N.O. acknowledges support from National Science and Technology Council (NSTC) in Taiwan through the grants NSTC 109-2112-M-001-051 and 110-2112-M-001-031. J.J.T. acknowledges support from NASA XRP 80NSSC22K1159. J.K.J. and R.S. acknowledge support from the Independent Research Fund Denmark (grant No. 0135-00123B). S.T. is supported by JSPS KAKENHI grant No. 21H00048 and 21H04495. This work was supported by NAOJ ALMA Scientific Research Grant Code 2022-20A. I.d.G. acknowledges support from grant PID2020-114461GB-I00, funded by MCIN/AEI/10.13039/501100011033. P.M.K. acknowledges support from NSTC 108-2112- M-001-012, NSTC 109-2112-M-001-022 and NSTC 110-2112-M-001-057. W.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT; NRF-2021R1F1A1061794). S.P.L. and T.J.T. acknowledge grants from the National Science and Technology Council of Taiwan 106-2119-M-007-021-MY3 and 109-2112-M-007-010-MY3. C.W.L. is supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (NRF- 2019R1A2C1010851), and by the Korea Astronomy and Space Science Institute grant funded by the Korea government (MSIT; Project No. 2022-1-840-05). J.E.L. is supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIT; grant number 2021R1A2C1011718). Z.Y.L. is supported in part by NASA NSSC20K0533 and NSF AST-1910106. Z.Y.D.L. acknowledges support from NASA 80NSSC18K1095, the Jefferson Scholars Foundation, the NRAO ALMA Student Observing Support (SOS) SOSPA8-003, the Achievements Rewards for College Scientists (ARCS) Foundation Washington Chapter, the Virginia Space Grant Consortium (VSGC), and UVA research computing (RIVANNA). L.W.L. acknowledges support from NSF AST-2108794. S.M. is supported by JSPS KAKENHI grant No. JP21J00086 and 22K14081. S.N. acknowledges support from the National Science Foundation through the Graduate Research Fellowship Program under Grant No. 2236415. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. H.-W.Y. acknowledges support from the National Science and Technology Council (NSTC) in Taiwan through the grant NSTC 110-2628-M-001-003-MY3 and from the Academia Sinica Career Development Award (AS-CDA-111-M03). M.L.R.H. acknowledges support from the Michigan Society of Fellows.
This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.00261.L, ADS/JAO.ALMA#2019.A.00034.S.
PY - 2023/7/1
Y1 - 2023/7/1
N2 - Constraining the physical and chemical structure of young embedded disks is crucial for understanding the earliest stages of planet formation. As part of the Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Large Program, we present high spatial resolution (∼0.″1 or ∼15 au) observations of the 1.3 mm continuum and 13CO J = 2-1, C18O J = 2-1, and SO J N = 65-54 molecular lines toward the disk around the Class I protostar L1489 IRS. The continuum emission shows a ring-like structure at 56 au from the central protostar and tenuous, optically thin emission extending beyond ∼300 au. The 13CO emission traces the warm disk surface, while the C18O emission originates from near the disk midplane. The coincidence of the radial emission peak of C18O with the dust ring may indicate a gap-ring structure in the gaseous disk as well. The SO emission shows a highly complex distribution, including a compact, prominent component at ≲30 au, which is likely to originate from thermally sublimated SO molecules. The compact SO emission also shows a velocity gradient along a direction tilted slightly (∼15°) with respect to the major axis of the dust disk, which we interpret as an inner warped disk in addition to the warp around ∼200 au suggested by previous work. These warped structures may be formed by a planet or companion with an inclined orbit, or by a gradual change in the angular momentum axis during gas infall.
AB - Constraining the physical and chemical structure of young embedded disks is crucial for understanding the earliest stages of planet formation. As part of the Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Large Program, we present high spatial resolution (∼0.″1 or ∼15 au) observations of the 1.3 mm continuum and 13CO J = 2-1, C18O J = 2-1, and SO J N = 65-54 molecular lines toward the disk around the Class I protostar L1489 IRS. The continuum emission shows a ring-like structure at 56 au from the central protostar and tenuous, optically thin emission extending beyond ∼300 au. The 13CO emission traces the warm disk surface, while the C18O emission originates from near the disk midplane. The coincidence of the radial emission peak of C18O with the dust ring may indicate a gap-ring structure in the gaseous disk as well. The SO emission shows a highly complex distribution, including a compact, prominent component at ≲30 au, which is likely to originate from thermally sublimated SO molecules. The compact SO emission also shows a velocity gradient along a direction tilted slightly (∼15°) with respect to the major axis of the dust disk, which we interpret as an inner warped disk in addition to the warp around ∼200 au suggested by previous work. These warped structures may be formed by a planet or companion with an inclined orbit, or by a gradual change in the angular momentum axis during gas infall.
UR - http://www.scopus.com/inward/record.url?scp=85163832917&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85163832917&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/accd71
DO - 10.3847/1538-4357/accd71
M3 - Article
AN - SCOPUS:85163832917
SN - 0004-637X
VL - 951
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 11
ER -