Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247
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Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247. / Lin, Zhe Yu Daniel; Li, Zhi Yun; Tobin, John J.; Ohashi, Nagayoshi; Jørgensen, Jes Kristian; Looney, Leslie W.; Aso, Yusuke; Takakuwa, Shigehisa; Aikawa, Yuri; van’t Hoff, Merel L.R.; de Gregorio-Monsalvo, Itziar; Encalada, Frankie J.; Flores, Christian; Gavino, Sacha; Han, Ilseung; Kido, Miyu; Koch, Patrick M.; Kwon, Woojin; Lai, Shih Ping; Lee, Chang Won; Lee, Jeong Eun; Phuong, Nguyen Thi; Sai (Insa Choi), Jinshi; Sharma, Rajeeb; Sheehan, Patrick; Thieme, Travis J.; Williams, Jonathan P.; Yamato, Yoshihide; Yen, Hsi Wei.
I: Astrophysical Journal, Bind 951, Nr. 1, 9, 28.06.2023.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247
AU - Lin, Zhe Yu Daniel
AU - Li, Zhi Yun
AU - Tobin, John J.
AU - Ohashi, Nagayoshi
AU - Jørgensen, Jes Kristian
AU - Looney, Leslie W.
AU - Aso, Yusuke
AU - Takakuwa, Shigehisa
AU - Aikawa, Yuri
AU - van’t Hoff, Merel L.R.
AU - de Gregorio-Monsalvo, Itziar
AU - Encalada, Frankie J.
AU - Flores, Christian
AU - Gavino, Sacha
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 - Phuong, Nguyen Thi
AU - Sai (Insa Choi), Jinshi
AU - Sharma, Rajeeb
AU - Sheehan, Patrick
AU - Thieme, Travis J.
AU - Williams, Jonathan P.
AU - Yamato, Yoshihide
AU - Yen, Hsi Wei
N1 - Funding Information: We thank the reviewer for the constructive comments. 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). Z.-Y.L. is supported in part by NASA 80NSSC18K1095 and NSF AST-1910106. J.J.T. acknowledges support from NASA 21-XRP21-0064 and XRP 80NSSC22K1159. N.O. and C.F. acknowledge support from the National Science and Technology Council (NSTC) in Taiwan through grants NSTC 109-2112-M-001-051 and 110-2112-M-001-031. J.K.J. acknowledges support from the Independent Research Fund Denmark (grant No. 0135-00123B). L.W.L. acknowledges support from NSF AST-2108794. S.T. is supported by JSPS KAKENHI grant Nos. 21H00048 and 21H04495 and by NAOJ ALMA Scientific Research grant No. 2022-20A. 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. M.L.R.H. acknowledges support from the Michigan Society of Fellows. I.d.G. acknowledges support from grant PID2020-114461GB-I00, funded by MCIN/AEI/10.13039/501100011033. F.J.E. acknowledges support from NSF AST-2108794. S.G. acknowledges support from the Independent Research Fund Denmark (grant No. 0135-00123B). 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. 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. W.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) (NRF-2021R1F1A1061794). 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. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIT) (grant No. 2021R1A2C1011718). R.S. acknowledges support from the Independent Research Fund Denmark (grant No. 0135-00123B). P.D.S. acknowledges support from NSF AST-2001830 and NSF AST-2107784. J.P.W. acknowledges support from NSF AST-2107841. 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. H.-W.Y. acknowledges support from the National Science and Technology Council (NSTC) in Taiwan through grant NSTC 110-2628-M-001-003-MY3 and from the Academia Sinica Career Development Award (AS-CDA-111-M03). Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/6/28
Y1 - 2023/6/28
N2 - While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the “Butterfly Star.” With a resolution of 0.″05 (8 au), the 1.3 mm continuum shows an asymmetry along the minor axis that is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.″1 (16 au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for 12CO J = 2-1, 13CO J = 2-1, C18O J = 2-1, H 2CO J = 30,3-20,2, and SO J = 65-54, and constrain the CO midplane snow line to ∼130 au. We find Keplerian rotation around a protostar of 1.6 ± 0.4 M ⊙ using C18O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is ∼6 au at a radius of 100 au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class I source has yet to vertically settle significantly.
AB - While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the “Butterfly Star.” With a resolution of 0.″05 (8 au), the 1.3 mm continuum shows an asymmetry along the minor axis that is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.″1 (16 au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for 12CO J = 2-1, 13CO J = 2-1, C18O J = 2-1, H 2CO J = 30,3-20,2, and SO J = 65-54, and constrain the CO midplane snow line to ∼130 au. We find Keplerian rotation around a protostar of 1.6 ± 0.4 M ⊙ using C18O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is ∼6 au at a radius of 100 au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class I source has yet to vertically settle significantly.
U2 - 10.3847/1538-4357/acd5c9
DO - 10.3847/1538-4357/acd5c9
M3 - Journal article
AN - SCOPUS:85163853238
VL - 951
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 9
ER -
ID: 360822201