ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core

Shih-Ying Hsu; Chin-Fei Lee; Doug Johnstone; Sheng-Yuan Liu; Tie Liu; Leonardo Bronfman; Huei-Ru Vivien Chen; Somnath Dutta; David J. Eden; Naomi Hirano; Mika Juvela; Kee-Tae Kim; Yi-Jehng Kuan; Woojin Kwon; Chang Won Lee; Jeong-Eun Lee; Shanghuo Li; Sheng-Jun Lin; Chun-Fan Liu; Xunchuan Liu; J. A. López-Vázquez; Qiuyi Luo; Mark G. Rawlings; Dipen Sahu; Patricio Sanhueza; Hsien 賢 Shang 尚; Ken'ichi Tatematsu; Yao-Lun Yang

doi:10.3847/1538-4357/ade7fc

ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core

Shih-Ying Hsu, Chin-Fei Lee, Doug Johnstone, Sheng-Yuan Liu, Tie Liu, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Naomi Hirano, Mika Juvela, Kee-Tae Kim, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Sheng-Jun Lin, Chun-Fan Liu, Xunchuan LiuJ. A. López-Vázquez, Qiuyi Luo, Mark G. Rawlings, Dipen Sahu, Patricio Sanhueza, 尚 Hsien 賢 Shang, Ken'ichi Tatematsu, Yao-Lun Yang

Department of Physics

Research output: Contribution to journal › Article › peer-review

3 Citations (SciVal)

Abstract

Interstellar complex organic molecules (COMs) in solar-like young stellar objects (YSOs), particularly within protostellar disks, are of significant interest owing to their potential connection to prebiotic chemistry in emerging planetary systems. We report the discovery of a rotating feature enriched in COMs, including CH3OH, CH3CHO, and NH2CHO, in the protostellar core G192.12-11.10. By constructing a YSO model, we find that the COM-rich feature is likely located within or near the boundary of the Keplerian disk. The image synthesis results suggest that additional heating mechanisms leading to a warm ring or a warm inner disk are required to reproduce the observed emission. We discuss possible origins of the COM-rich feature, particularly accretion shocks as a plausible cause for a warm ring. Additionally, molecules such as C18O, H2CO, DCS, H2S, and OCS exhibit distinct behavior compared to CH3OH, indicating a range of physical and chemical conditions within the region. The observed kinematics of H2S and OCS suggest that OCS resides in regions closer to the central protostar than H2S, consistent with previous experimental studies.

Original language	English
Article number	56
Journal	The Astrophysical Journal
Volume	989
Issue number	1
Early online date	5 Aug 2025
DOIs	https://doi.org/10.3847/1538-4357/ade7fc
Publication status	Published - 10 Aug 2025

Bibliographical note

Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.

Funding

Acknowledgments a community-developed core Python package and an ecosystem of tools and resources for astronomy (Astropy Collaboration et al. ; A. M. Price-Whelan et al. ; Astropy Collaboration et al. ). S.-Y.H. acknowledges support from the Acadamia Sinica of Taiwan (grant No. AS-PD-1142-M02-2). S.-Y.H. and C.-F.L. acknowledge support from the National Science and Technology Council of Taiwan (grant No. 112-2112-M-001- 039-MY3). D.J. is supported by NRC Canada and by an NSERC Discovery Grant. X.L. acknowledges the support of the Strategic Priority Research Program of the Chinese Academy of Sciences under grant No. XDB0800303. The work of M.G.R. is supported by the international Gemini Observatory, a program of NSF NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the US National Science Foundation, on behalf of the Gemini partnership of Argentina, Brazil, Canada, Chile, the Republic of Korea, and the United States of America. L.B. gratefully acknowledges support by the ANID BASAL project FB210003. P.S. was partially supported by a Grant-in-Aid for Scientific Research (KAKENHI Nos. JP22H01271 and JP23H01221) of JSPS. W.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT; RS-2024-00342488 and RS-2024-00416859). M.J. acknowledges the support of the Research Council of Finland grant No. 348342. D.S. acknowledges the support from Ramanujan Fellowship (SERB) and PRL, India. J.-E.L. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) (grant numbers 2021R1A2C1011718 and RS-2024-00416859). CWL acknowledges support from the Basic Science Research Program through the 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. 2024-1-841-00). Y.-L.Y. acknowledges support from Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (20H05844 and 25H00676). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.00302.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSTC 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. This work made use of Astropy:2929 http://www.astropy.org a community-developed core Python package and an ecosystem of tools and resources for astronomy (Astropy Collaboration et al. 2013; A. M. Price-Whelan et al. 2018; Astropy Collaboration et al. 2022). S.-Y.H. acknowledges support from the Acadamia Sinica of Taiwan (grant No. AS-PD-1142-M02-2). S.-Y.H. and C.-F.L. acknowledge support from the National Science and Technology Council of Taiwan (grant No. 112-2112-M-001- 039-MY3). D.J. is supported by NRC Canada and by an NSERC Discovery Grant. X.L. acknowledges the support of the Strategic Priority Research Program of the Chinese Academy of Sciences under grant No. XDB0800303. The work of M.G.R. is supported by the international Gemini Observatory, a program of NSF NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the US National Science Foundation, on behalf of the Gemini partnership of Argentina, Brazil, Canada, Chile, the Republic of Korea, and the United States of America. L.B. gratefully acknowledges support by the ANID BASAL project FB210003. P.S. was partially supported by a Grant-in-Aid for Scientific Research (KAKENHI Nos. JP22H01271 and JP23H01221) of JSPS. W.K. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT; RS-2024-00342488 and RS-2024-00416859). M.J. acknowledges the support of the Research Council of Finland grant No. 348342. D.S. acknowledges the support from Ramanujan Fellowship (SERB) and PRL, India. J.-E.L. was supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) (grant numbers 2021R1A2C1011718 and RS-2024-00416859). CWL acknowledges support from the Basic Science Research Program through the 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. 2024-1-841-00). Y.-L.Y. acknowledges support from Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (20H05844 and 25H00676).

Funders	Funder number
National Research Foundation of Korea
Grant-in-Aid
National Science Foundation
Japan Society for the Promotion of Science
NSF
Natural Sciences and Engineering Research Council of Canada
Al Akhawayn University in Ifrane
National Institutes of Natural Sciences
National Radio Astronomy Observatory
ASIAA (Taiwan)
National Research Council Canada
KASI
National Astronomical Observatory of Japan	2022
Agencia Nacional de Investigación y Desarrollo	JP23H01221, JP22H01271, FB210003
Ministry of Science and ICT, South Korea	RS-2024-00416859, RS-2024-00342488
National Science and Technology Council	112-2112-M-001- 039-MY3
Science and Engineering Research Board	2021R1A2C1011718
Ministry of Education, Culture, Sports, Science and Technology	20H05844, 25H00676
Ministry of Education, Science and Technology	NRF- 2019R1A2C1010851
Acadamia Sinica of Taiwan	AS-PD-1142-M02-2
Chinese Academy of Sciences	XDB0800303
Korea Astronomy and Space Science Institute	2024-1-841-00
Research Council of Finland	348342

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Hsu, S.-Y., Lee, C.-F., Johnstone, D., Liu, S.-Y., Liu, T., Bronfman, L., Chen, H.-R. V., Dutta, S., Eden, D. J., Hirano, N., Juvela, M., Kim, K.-T., Kuan, Y.-J., Kwon, W., Lee, C. W., Lee, J.-E., Li, S., Lin, S.-J., Liu, C.-F., ... Yang, Y.-L. (2025). ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core. The Astrophysical Journal, 989(1), Article 56. https://doi.org/10.3847/1538-4357/ade7fc

Hsu, S-Y, Lee, C-F, Johnstone, D, Liu, S-Y, Liu, T, Bronfman, L, Chen, H-RV, Dutta, S, Eden, DJ, Hirano, N, Juvela, M, Kim, K-T, Kuan, Y-J, Kwon, W, Lee, CW, Lee, J-E, Li, S, Lin, S-J, Liu, C-F, Liu, X, López-Vázquez, JA, Luo, Q, Rawlings, MG, Sahu, D, Sanhueza, P, 尚H賢S, Tatematsu, K & Yang, Y-L 2025, 'ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core', The Astrophysical Journal, vol. 989, no. 1, 56. https://doi.org/10.3847/1538-4357/ade7fc

@article{21d1c600b8314428a813abf796cf0a53,

title = "ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core",

abstract = "Interstellar complex organic molecules (COMs) in solar-like young stellar objects (YSOs), particularly within protostellar disks, are of significant interest owing to their potential connection to prebiotic chemistry in emerging planetary systems. We report the discovery of a rotating feature enriched in COMs, including CH3OH, CH3CHO, and NH2CHO, in the protostellar core G192.12-11.10. By constructing a YSO model, we find that the COM-rich feature is likely located within or near the boundary of the Keplerian disk. The image synthesis results suggest that additional heating mechanisms leading to a warm ring or a warm inner disk are required to reproduce the observed emission. We discuss possible origins of the COM-rich feature, particularly accretion shocks as a plausible cause for a warm ring. Additionally, molecules such as C18O, H2CO, DCS, H2S, and OCS exhibit distinct behavior compared to CH3OH, indicating a range of physical and chemical conditions within the region. The observed kinematics of H2S and OCS suggest that OCS resides in regions closer to the central protostar than H2S, consistent with previous experimental studies. ",

author = "Shih-Ying Hsu and Chin-Fei Lee and Doug Johnstone and Sheng-Yuan Liu and Tie Liu and Leonardo Bronfman and Chen, \{Huei-Ru Vivien\} and Somnath Dutta and Eden, \{David J.\} and Naomi Hirano and Mika Juvela and Kee-Tae Kim and Yi-Jehng Kuan and Woojin Kwon and Lee, \{Chang Won\} and Jeong-Eun Lee and Shanghuo Li and Sheng-Jun Lin and Chun-Fan Liu and Xunchuan Liu and L{\'o}pez-V{\'a}zquez, \{J. A.\} and Qiuyi Luo and Rawlings, \{Mark G.\} and Dipen Sahu and Patricio Sanhueza and 尚, \{Hsien 賢 Shang\} and Ken'ichi Tatematsu and Yao-Lun Yang",

note = "Publisher Copyright: {\textcopyright} 2025. The Author(s). Published by the American Astronomical Society.",

year = "2025",

month = aug,

day = "10",

doi = "10.3847/1538-4357/ade7fc",

language = "English",

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T1 - ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core

AU - Hsu, Shih-Ying

AU - Lee, Chin-Fei

AU - Johnstone, Doug

AU - Liu, Sheng-Yuan

AU - Liu, Tie

AU - Bronfman, Leonardo

AU - Chen, Huei-Ru Vivien

AU - Dutta, Somnath

AU - Eden, David J.

AU - Hirano, Naomi

AU - Juvela, Mika

AU - Kim, Kee-Tae

AU - Kuan, Yi-Jehng

AU - Kwon, Woojin

AU - Lee, Chang Won

AU - Lee, Jeong-Eun

AU - Li, Shanghuo

AU - Lin, Sheng-Jun

AU - Liu, Chun-Fan

AU - Liu, Xunchuan

AU - López-Vázquez, J. A.

AU - Luo, Qiuyi

AU - Rawlings, Mark G.

AU - Sahu, Dipen

AU - Sanhueza, Patricio

AU - 尚, Hsien 賢 Shang

AU - Tatematsu, Ken'ichi

AU - Yang, Yao-Lun

PY - 2025/8/10

Y1 - 2025/8/10

N2 - Interstellar complex organic molecules (COMs) in solar-like young stellar objects (YSOs), particularly within protostellar disks, are of significant interest owing to their potential connection to prebiotic chemistry in emerging planetary systems. We report the discovery of a rotating feature enriched in COMs, including CH3OH, CH3CHO, and NH2CHO, in the protostellar core G192.12-11.10. By constructing a YSO model, we find that the COM-rich feature is likely located within or near the boundary of the Keplerian disk. The image synthesis results suggest that additional heating mechanisms leading to a warm ring or a warm inner disk are required to reproduce the observed emission. We discuss possible origins of the COM-rich feature, particularly accretion shocks as a plausible cause for a warm ring. Additionally, molecules such as C18O, H2CO, DCS, H2S, and OCS exhibit distinct behavior compared to CH3OH, indicating a range of physical and chemical conditions within the region. The observed kinematics of H2S and OCS suggest that OCS resides in regions closer to the central protostar than H2S, consistent with previous experimental studies.

AB - Interstellar complex organic molecules (COMs) in solar-like young stellar objects (YSOs), particularly within protostellar disks, are of significant interest owing to their potential connection to prebiotic chemistry in emerging planetary systems. We report the discovery of a rotating feature enriched in COMs, including CH3OH, CH3CHO, and NH2CHO, in the protostellar core G192.12-11.10. By constructing a YSO model, we find that the COM-rich feature is likely located within or near the boundary of the Keplerian disk. The image synthesis results suggest that additional heating mechanisms leading to a warm ring or a warm inner disk are required to reproduce the observed emission. We discuss possible origins of the COM-rich feature, particularly accretion shocks as a plausible cause for a warm ring. Additionally, molecules such as C18O, H2CO, DCS, H2S, and OCS exhibit distinct behavior compared to CH3OH, indicating a range of physical and chemical conditions within the region. The observed kinematics of H2S and OCS suggest that OCS resides in regions closer to the central protostar than H2S, consistent with previous experimental studies.

UR - https://www.scopus.com/pages/publications/105012742373

U2 - 10.3847/1538-4357/ade7fc

DO - 10.3847/1538-4357/ade7fc

M3 - Article

SN - 0004-637X

VL - 989

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 1

M1 - 56

ER -

ALMASOP. A Rotating Feature Rich in Complex Organic Molecules in a Protostellar Core

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