ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos
Hot corinos are of great interest due to their richness in interstellar complex organic molecules (COMs) and the consequent potential prebiotic connection to solar-like planetary systems. Recent surveys have reported an increasing number of detected hot corinos in Class 0/I protostars; however, the...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acefcf |
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| author | Shih-Ying Hsu Sheng-Yuan Liu Doug Johnstone Tie Liu Leonardo Bronfman Huei-Ru Vivien Chen Somnath Dutta David J. Eden Neal J. Evans II Naomi Hirano Mika Juvela Yi-Jehng Kuan Woojin Kwon Chin-Fei Lee Chang Won Lee Jeong-Eun Lee Shanghuo Li Chun-Fan Liu Xunchuan Liu Qiuyi Luo Sheng-Li Qin Mark G. Rawlings Dipen Sahu Patricio Sanhueza Hsien Shang Ken'ichi Tatematsu Yao-Lun Yang |
| author_facet | Shih-Ying Hsu Sheng-Yuan Liu Doug Johnstone Tie Liu Leonardo Bronfman Huei-Ru Vivien Chen Somnath Dutta David J. Eden Neal J. Evans II Naomi Hirano Mika Juvela Yi-Jehng Kuan Woojin Kwon Chin-Fei Lee Chang Won Lee Jeong-Eun Lee Shanghuo Li Chun-Fan Liu Xunchuan Liu Qiuyi Luo Sheng-Li Qin Mark G. Rawlings Dipen Sahu Patricio Sanhueza Hsien Shang Ken'ichi Tatematsu Yao-Lun Yang |
| author_sort | Shih-Ying Hsu |
| collection | DOAJ |
| description | Hot corinos are of great interest due to their richness in interstellar complex organic molecules (COMs) and the consequent potential prebiotic connection to solar-like planetary systems. Recent surveys have reported an increasing number of detected hot corinos in Class 0/I protostars; however, the relationships between their physical properties and the hot-corino signatures remain elusive. In this study, our objective is to establish a general picture of the detectability of hot corinos by identifying the origins of the hot-corino signatures in the sample of young stellar objects (YSOs) obtained from the Atacama Large Millimeter/submillimeter Array Survey of Orion Planck Galactic Cold Clumps project. We apply spectral energy distribution modeling to our sample and identify the physical parameters of the modeled YSOs directly, linking the detection of hot-corino signatures to the envelope properties of the YSOs. Imaging simulations of the methanol emission further support this scenario. We therefore posit that the observed COM emission originates from the warm inner envelopes of the sample YSOs, based on both the warm region size and the envelope density profile. The former is governed by the source luminosity and is additionally affected by the disk and cavity properties, while the latter is related to the evolutionary stages. This scenario provides a framework for detecting hot-corino signatures toward luminous Class 0 YSOs, with fewer detections being observed toward similarly luminous Class I sources. |
| first_indexed | 2024-03-11T17:20:32Z |
| format | Article |
| id | doaj.art-66b32b2f152a4dacb9a63f0c3c09c7d3 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T17:20:32Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-66b32b2f152a4dacb9a63f0c3c09c7d32023-10-19T13:58:42ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01956212010.3847/1538-4357/acefcfALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot CorinosShih-Ying Hsu0https://orcid.org/0000-0002-1369-1563Sheng-Yuan Liu1Doug Johnstone2https://orcid.org/0000-0002-6773-459XTie Liu3https://orcid.org/0000-0002-5286-2564Leonardo Bronfman4https://orcid.org/0000-0002-9574-8454Huei-Ru Vivien Chen5https://orcid.org/0000-0002-9774-1846Somnath Dutta6https://orcid.org/0000-0002-2338-4583David J. Eden7https://orcid.org/0000-0002-5881-3229Neal J. Evans II8https://orcid.org/0000-0001-5175-1777Naomi Hirano9https://orcid.org/0000-0001-9304-7884Mika Juvela10https://orcid.org/0000-0002-5809-4834Yi-Jehng Kuan11https://orcid.org/0000-0002-4336-0730Woojin Kwon12https://orcid.org/0000-0003-4022-4132Chin-Fei Lee13https://orcid.org/0000-0002-3024-5864Chang Won Lee14https://orcid.org/0000-0002-3179-6334Jeong-Eun Lee15https://orcid.org/0000-0003-3119-2087Shanghuo Li16https://orcid.org/0000-0003-1275-5251Chun-Fan Liu17https://orcid.org/0000-0002-1624-6545Xunchuan Liu18https://orcid.org/0000-0001-8315-4248Qiuyi Luo19https://orcid.org/0000-0003-4506-3171Sheng-Li Qin20https://orcid.org/0000-0003-2302-0613Mark G. Rawlings21https://orcid.org/0000-0002-6529-202XDipen Sahu22https://orcid.org/0000-0002-4393-3463Patricio Sanhueza23https://orcid.org/0000-0002-7125-7685Hsien Shang24https://orcid.org/0000-0001-8385-9838Ken'ichi Tatematsu25https://orcid.org/0000-0002-8149-8546Yao-Lun Yang26https://orcid.org/0000-0001-8227-2816National Taiwan University (NTU) , No. 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.); Institute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Institute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)NRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada; Department of Physics and Astronomy, University of Victoria , Victoria, BC, V8P 5C2, CanadaShanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaDepartamento de Astronomía, Universidad de Chile , Casilla 36-D, Santiago 83200000, ChileDepartment of Physics and Institute of Astronomy, National Tsing Hua University , Hsinchu, 30013, TaiwanInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Armagh Observatory and Planetarium , College Hill, Armagh, BT61 9DB, UKDepartment of Astronomy, The University of Texas at Austin , 2515 Speedway, Stop C1400, Austin, Texas 78712-1205, USAInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Department of Physics, P.O.Box 64, FI-00014, University of Helsinki , FinlandInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.); Department of Earth Sciences, National Taiwan Normal University , Taipei 11677, Taiwan (R.O.C.)Department of Earth Science Education, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; SNU Astronomy Research Center, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Korea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea; University of Science and Technology , Korea (UST), 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of KoreaDepartment of Physics and Astronomy, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaMax Planck Institute for Astronomy , Kstuhl 17, D-69117 Heidelberg, GermanyInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of ChinaShanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People's Republic of ChinaDepartment of Astronomy, Yunnan University , and Key Laboratory of Astroparticle Physics of Yunnan Province, Kunming, 650091, People's Republic of ChinaGemini Observatory/NSF NOIRLab , 670 N. Ahoku Place, Hilo, Hawai, 96720, USAInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.); Physical Research laboratory , Navrangpura, Ahmedabad, Gujarat 380009, IndiaNational Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute of Astronomy and Astrophysics , Academia Sinica, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 462-2 Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan; Department of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanRIKEN Cluster for Pioneering Research , Wako-shi, Saitama, 351-0198, JapanHot corinos are of great interest due to their richness in interstellar complex organic molecules (COMs) and the consequent potential prebiotic connection to solar-like planetary systems. Recent surveys have reported an increasing number of detected hot corinos in Class 0/I protostars; however, the relationships between their physical properties and the hot-corino signatures remain elusive. In this study, our objective is to establish a general picture of the detectability of hot corinos by identifying the origins of the hot-corino signatures in the sample of young stellar objects (YSOs) obtained from the Atacama Large Millimeter/submillimeter Array Survey of Orion Planck Galactic Cold Clumps project. We apply spectral energy distribution modeling to our sample and identify the physical parameters of the modeled YSOs directly, linking the detection of hot-corino signatures to the envelope properties of the YSOs. Imaging simulations of the methanol emission further support this scenario. We therefore posit that the observed COM emission originates from the warm inner envelopes of the sample YSOs, based on both the warm region size and the envelope density profile. The former is governed by the source luminosity and is additionally affected by the disk and cavity properties, while the latter is related to the evolutionary stages. This scenario provides a framework for detecting hot-corino signatures toward luminous Class 0 YSOs, with fewer detections being observed toward similarly luminous Class I sources.https://doi.org/10.3847/1538-4357/acefcfAstrochemistryInterstellar moleculesStar forming regionsLow mass starsProtostars |
| spellingShingle | Shih-Ying Hsu Sheng-Yuan Liu Doug Johnstone Tie Liu Leonardo Bronfman Huei-Ru Vivien Chen Somnath Dutta David J. Eden Neal J. Evans II Naomi Hirano Mika Juvela Yi-Jehng Kuan Woojin Kwon Chin-Fei Lee Chang Won Lee Jeong-Eun Lee Shanghuo Li Chun-Fan Liu Xunchuan Liu Qiuyi Luo Sheng-Li Qin Mark G. Rawlings Dipen Sahu Patricio Sanhueza Hsien Shang Ken'ichi Tatematsu Yao-Lun Yang ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos The Astrophysical Journal Astrochemistry Interstellar molecules Star forming regions Low mass stars Protostars |
| title | ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos |
| title_full | ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos |
| title_fullStr | ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos |
| title_full_unstemmed | ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos |
| title_short | ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos |
| title_sort | alma survey of orion planck galactic cold clumps almasop the warm envelope origin of hot corinos |
| topic | Astrochemistry Interstellar molecules Star forming regions Low mass stars Protostars |
| url | https://doi.org/10.3847/1538-4357/acefcf |
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