Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS
Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at \(\sim\)0.06" (8 au) resolution and molecular line em...
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creator | Merel L R van 't Hoff Tobin, John J Zhi-Yun, Li Ohashi, Nagayoshi Jørgensen, Jes K Zhe-Yu, Daniel Lin Aikawa, Yuri Aso, Yusuke Itziar de Gregorio-Monsalvo Gavino, Sacha Han, Ilseung Koch, Patrick M Kwon, Woojin Chang Won Lee Jeong-Eun, Lee Looney, Leslie W Narayanan, Suchitra Plunkett, Adele Jinshi Sai Santamaría-Miranda, Alejandro Sharma, Rajeeb Sheehan, Patrick D Takakuwa, Shigehisa Thieme, Travis J Williams, Jonathan P Shih-Ping, Lai Nguyen Thi Phuong Hsi-Wei Yen |
description | Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at \(\sim\)0.06" (8 au) resolution and molecular line emission at \(\sim\)0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures, but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of \(^{12}\)CO, \(^{13}\)CO, C\(^{18}\)O, H\(_2\)CO, c-C\(_3\)H\(_2\), SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in \(^{12}\)CO. The \(^{13}\)CO brightness temperature and the H\(_2\)CO line ratio confirm that the disk is too warm for CO freeze out, with the snowline located at \(\sim\)350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100" or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks. |
doi_str_mv | 10.48550/arxiv.2306.15407 |
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Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at \(\sim\)0.06" (8 au) resolution and molecular line emission at \(\sim\)0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures, but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of \(^{12}\)CO, \(^{13}\)CO, C\(^{18}\)O, H\(_2\)CO, c-C\(_3\)H\(_2\), SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in \(^{12}\)CO. The \(^{13}\)CO brightness temperature and the H\(_2\)CO line ratio confirm that the disk is too warm for CO freeze out, with the snowline located at \(\sim\)350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100" or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2306.15407</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Accretion disks ; Astrochemistry ; Asymmetry ; Brightness temperature ; Continuum radiation ; Emission analysis ; Initial conditions ; Misalignment ; Outflow ; Physics - Earth and Planetary Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planet formation ; Protostars ; Radio telescopes ; Star formation</subject><ispartof>arXiv.org, 2023-06</ispartof><rights>2023. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.3847/1538-4357/accf87$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.2306.15407$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Merel L R van 't Hoff</creatorcontrib><creatorcontrib>Tobin, John J</creatorcontrib><creatorcontrib>Zhi-Yun, Li</creatorcontrib><creatorcontrib>Ohashi, Nagayoshi</creatorcontrib><creatorcontrib>Jørgensen, Jes K</creatorcontrib><creatorcontrib>Zhe-Yu, Daniel Lin</creatorcontrib><creatorcontrib>Aikawa, Yuri</creatorcontrib><creatorcontrib>Aso, Yusuke</creatorcontrib><creatorcontrib>Itziar de Gregorio-Monsalvo</creatorcontrib><creatorcontrib>Gavino, Sacha</creatorcontrib><creatorcontrib>Han, Ilseung</creatorcontrib><creatorcontrib>Koch, Patrick M</creatorcontrib><creatorcontrib>Kwon, Woojin</creatorcontrib><creatorcontrib>Chang Won Lee</creatorcontrib><creatorcontrib>Jeong-Eun, Lee</creatorcontrib><creatorcontrib>Looney, Leslie W</creatorcontrib><creatorcontrib>Narayanan, Suchitra</creatorcontrib><creatorcontrib>Plunkett, Adele</creatorcontrib><creatorcontrib>Jinshi Sai</creatorcontrib><creatorcontrib>Santamaría-Miranda, Alejandro</creatorcontrib><creatorcontrib>Sharma, Rajeeb</creatorcontrib><creatorcontrib>Sheehan, Patrick D</creatorcontrib><creatorcontrib>Takakuwa, Shigehisa</creatorcontrib><creatorcontrib>Thieme, Travis J</creatorcontrib><creatorcontrib>Williams, Jonathan P</creatorcontrib><creatorcontrib>Shih-Ping, Lai</creatorcontrib><creatorcontrib>Nguyen Thi Phuong</creatorcontrib><creatorcontrib>Hsi-Wei Yen</creatorcontrib><title>Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS</title><title>arXiv.org</title><description>Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at \(\sim\)0.06" (8 au) resolution and molecular line emission at \(\sim\)0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures, but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of \(^{12}\)CO, \(^{13}\)CO, C\(^{18}\)O, H\(_2\)CO, c-C\(_3\)H\(_2\), SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in \(^{12}\)CO. The \(^{13}\)CO brightness temperature and the H\(_2\)CO line ratio confirm that the disk is too warm for CO freeze out, with the snowline located at \(\sim\)350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100" or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.</description><subject>Accretion disks</subject><subject>Astrochemistry</subject><subject>Asymmetry</subject><subject>Brightness temperature</subject><subject>Continuum radiation</subject><subject>Emission analysis</subject><subject>Initial conditions</subject><subject>Misalignment</subject><subject>Outflow</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planet formation</subject><subject>Protostars</subject><subject>Radio telescopes</subject><subject>Star formation</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkMtOwzAURCMkJKrSD2DFldjAIsWx48Rhh0oLkSqBoPvITm6oSxIX22npJ_GX9MFqNmdGoxMEVxEZx4Jzci_tj96MKSPJOOIxSc-CAWUsCkVM6UUwcm5FCKFJSjlng-B3Km2zg7dGduhhZmwrvTYd6A6mrcKqwgqetPtycIuHvIM8zx_gEWptnYel_lyGFp1p-mNto3ELpgbXq7BtoTSd113ftyC7ClrTYNk30kKjOwRstXOHkjdbaSvwS4RJI50DAmtrvHF-j84jTlPI3z8ug_NaNg5H_zkMFrPpYvISzl-f88njPJQZT0OmeCK4VFKwiEaCMs4wFUoxLOtMIU2YKpUQFZckIqnEStQJJxUKmnFFspoNg-vT7NFjsba6lXZXHHwWR5974uZE7E9-9-h8sTK97fafCioYibNMiIj9AZFRePc</recordid><startdate>20230627</startdate><enddate>20230627</enddate><creator>Merel L R van 't Hoff</creator><creator>Tobin, John J</creator><creator>Zhi-Yun, Li</creator><creator>Ohashi, Nagayoshi</creator><creator>Jørgensen, Jes K</creator><creator>Zhe-Yu, Daniel Lin</creator><creator>Aikawa, Yuri</creator><creator>Aso, Yusuke</creator><creator>Itziar de Gregorio-Monsalvo</creator><creator>Gavino, Sacha</creator><creator>Han, Ilseung</creator><creator>Koch, Patrick M</creator><creator>Kwon, Woojin</creator><creator>Chang Won Lee</creator><creator>Jeong-Eun, Lee</creator><creator>Looney, Leslie W</creator><creator>Narayanan, Suchitra</creator><creator>Plunkett, Adele</creator><creator>Jinshi Sai</creator><creator>Santamaría-Miranda, Alejandro</creator><creator>Sharma, Rajeeb</creator><creator>Sheehan, Patrick D</creator><creator>Takakuwa, Shigehisa</creator><creator>Thieme, Travis J</creator><creator>Williams, Jonathan P</creator><creator>Shih-Ping, Lai</creator><creator>Nguyen Thi Phuong</creator><creator>Hsi-Wei Yen</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20230627</creationdate><title>Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS</title><author>Merel L R van 't Hoff ; Tobin, John J ; Zhi-Yun, Li ; Ohashi, Nagayoshi ; Jørgensen, Jes K ; Zhe-Yu, Daniel Lin ; Aikawa, Yuri ; Aso, Yusuke ; Itziar de Gregorio-Monsalvo ; Gavino, Sacha ; Han, Ilseung ; Koch, Patrick M ; Kwon, Woojin ; Chang Won Lee ; Jeong-Eun, Lee ; Looney, Leslie W ; Narayanan, Suchitra ; Plunkett, Adele ; Jinshi Sai ; Santamaría-Miranda, Alejandro ; Sharma, Rajeeb ; Sheehan, Patrick D ; Takakuwa, Shigehisa ; Thieme, Travis J ; Williams, Jonathan P ; Shih-Ping, Lai ; Nguyen Thi Phuong ; Hsi-Wei Yen</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a957-3b5685aba8312182353e78bb3ecf9be263bcb88d5a0107aed8f650de8295b09f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Accretion disks</topic><topic>Astrochemistry</topic><topic>Asymmetry</topic><topic>Brightness temperature</topic><topic>Continuum radiation</topic><topic>Emission analysis</topic><topic>Initial conditions</topic><topic>Misalignment</topic><topic>Outflow</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planet formation</topic><topic>Protostars</topic><topic>Radio telescopes</topic><topic>Star formation</topic><toplevel>online_resources</toplevel><creatorcontrib>Merel L R van 't Hoff</creatorcontrib><creatorcontrib>Tobin, John J</creatorcontrib><creatorcontrib>Zhi-Yun, Li</creatorcontrib><creatorcontrib>Ohashi, Nagayoshi</creatorcontrib><creatorcontrib>Jørgensen, Jes K</creatorcontrib><creatorcontrib>Zhe-Yu, Daniel Lin</creatorcontrib><creatorcontrib>Aikawa, Yuri</creatorcontrib><creatorcontrib>Aso, Yusuke</creatorcontrib><creatorcontrib>Itziar de Gregorio-Monsalvo</creatorcontrib><creatorcontrib>Gavino, Sacha</creatorcontrib><creatorcontrib>Han, Ilseung</creatorcontrib><creatorcontrib>Koch, Patrick M</creatorcontrib><creatorcontrib>Kwon, Woojin</creatorcontrib><creatorcontrib>Chang Won Lee</creatorcontrib><creatorcontrib>Jeong-Eun, Lee</creatorcontrib><creatorcontrib>Looney, Leslie W</creatorcontrib><creatorcontrib>Narayanan, Suchitra</creatorcontrib><creatorcontrib>Plunkett, Adele</creatorcontrib><creatorcontrib>Jinshi Sai</creatorcontrib><creatorcontrib>Santamaría-Miranda, Alejandro</creatorcontrib><creatorcontrib>Sharma, Rajeeb</creatorcontrib><creatorcontrib>Sheehan, Patrick D</creatorcontrib><creatorcontrib>Takakuwa, Shigehisa</creatorcontrib><creatorcontrib>Thieme, Travis J</creatorcontrib><creatorcontrib>Williams, Jonathan P</creatorcontrib><creatorcontrib>Shih-Ping, Lai</creatorcontrib><creatorcontrib>Nguyen Thi Phuong</creatorcontrib><creatorcontrib>Hsi-Wei Yen</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Access via ProQuest (Open Access)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Merel L R van 't Hoff</au><au>Tobin, John J</au><au>Zhi-Yun, Li</au><au>Ohashi, Nagayoshi</au><au>Jørgensen, Jes K</au><au>Zhe-Yu, Daniel Lin</au><au>Aikawa, Yuri</au><au>Aso, Yusuke</au><au>Itziar de Gregorio-Monsalvo</au><au>Gavino, Sacha</au><au>Han, Ilseung</au><au>Koch, Patrick M</au><au>Kwon, Woojin</au><au>Chang Won Lee</au><au>Jeong-Eun, Lee</au><au>Looney, Leslie W</au><au>Narayanan, Suchitra</au><au>Plunkett, Adele</au><au>Jinshi Sai</au><au>Santamaría-Miranda, Alejandro</au><au>Sharma, Rajeeb</au><au>Sheehan, Patrick D</au><au>Takakuwa, Shigehisa</au><au>Thieme, Travis J</au><au>Williams, Jonathan P</au><au>Shih-Ping, Lai</au><au>Nguyen Thi Phuong</au><au>Hsi-Wei Yen</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS</atitle><jtitle>arXiv.org</jtitle><date>2023-06-27</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here, we present Atacama Large Millimeter/submillimeter Array (ALMA) observations of dust continuum at \(\sim\)0.06" (8 au) resolution and molecular line emission at \(\sim\)0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures, but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of \(^{12}\)CO, \(^{13}\)CO, C\(^{18}\)O, H\(_2\)CO, c-C\(_3\)H\(_2\), SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in \(^{12}\)CO. The \(^{13}\)CO brightness temperature and the H\(_2\)CO line ratio confirm that the disk is too warm for CO freeze out, with the snowline located at \(\sim\)350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk-envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk-envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100" or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2306.15407</doi><oa>free_for_read</oa></addata></record> |
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subjects | Accretion disks Astrochemistry Asymmetry Brightness temperature Continuum radiation Emission analysis Initial conditions Misalignment Outflow Physics - Earth and Planetary Astrophysics Physics - Solar and Stellar Astrophysics Planet formation Protostars Radio telescopes Star formation |
title | Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS |
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