300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution

We present an 870 μm continuum survey of 300 protostars from the Herschel Orion Protostar Survey using the Atacama Compact Array (ACA). These data measure protostellar flux densities on envelope scales ≤8000 au (20'') and resolve the structure of envelopes with 1600 au (4'') reso...

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Autores: Federman, Samuel, Megeath, S. Thomas, Tobin, John J., Sheehan, Patrick D., Pokhrel, Riwaj, Habel, Nolan, Stutz, Amelia M., Fischer, William J., Hartmann, Lee, Stanke, Thomas, Narang, Mayank, Osorio, Mayra, Atnagulov, Prabhani, Rahatgaonkar, Rohan
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/310298
Acceso en línea:http://hdl.handle.net/10261/310298
Access Level:acceso abierto
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spelling 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their EvolutionFederman, SamuelMegeath, S. ThomasTobin, John J.Sheehan, Patrick D.Pokhrel, RiwajHabel, NolanStutz, Amelia M.Fischer, William J.Hartmann, LeeStanke, ThomasNarang, MayankOsorio, MayraAtnagulov, PrabhaniRahatgaonkar, RohanWe present an 870 μm continuum survey of 300 protostars from the Herschel Orion Protostar Survey using the Atacama Compact Array (ACA). These data measure protostellar flux densities on envelope scales ≤8000 au (20'') and resolve the structure of envelopes with 1600 au (4'') resolution, a factor of 3–5 improvement in angular resolution over existing single-dish 870 μm observations. We compare the ACA observations to Atacama Large Millimeter/submillimeter Array 12 m array observations at 870 μm with ∼0farcs1 (40 au) resolution. Using the 12 m data to measure the fluxes from disks and the ACA data within 2500 au to measure the combined disk plus envelope fluxes, we calculate the 12 m/ACA 870 μm flux ratios. Our sample shows a clear evolution in this ratio. Class 0 protostars are mostly envelope-dominated with ratios <0.5. In contrast, Flat Spectrum protostars are primarily disk-dominated with ratios near 1, although with a number of face-on protostars dominated by their envelopes. Class I protostars span the range from envelope to disk-dominated. The increase in ratio is accompanied by a decrease in the envelope fluxes and estimated mass infall rates. We estimate that 80% of the mass is accreted during the envelope-dominated phase. We find that the 12 m/ACA flux ratio is an evolutionary indicator that largely avoids the inclination and foreground extinction dependence of spectral energy distribution-based indicators. © 2023. The Author(s). Published by the American Astronomical Society.This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01284.S. 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. A.S. gratefully acknowledges funding support through Fondecyt Regular (project code 1220610), from the ANID BASAL project FB210003, and from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. M.O. acknowledges support from the MCIN/AEI/10.13039/501100011033 through the PID2020-114461GB-I00), the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709) and the Consejería de Transformación Económica, Industria, Conocimiento y Universidades of the Junta de Andalucía, and the European Regional Development Fund from the European Union through the grant P20-00880.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (SEV-2017-0709).Peer reviewedIOP PublishingMinisterio de Ciencia, Innovación y Universidades (España)Junta de AndalucíaEuropean CommissionFondo Nacional de Desarrollo Científico y Tecnológico (Chile)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/310298reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-114461GB-I00info:eu-repo/grantAgreement/AEI//SEV-2017-0709http://dx.doi.org/10.3847/1538-4357/ac9f4bSíinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3102982026-05-22T06:33:51Z
dc.title.none.fl_str_mv 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
title 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
spellingShingle 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
Federman, Samuel
title_short 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
title_full 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
title_fullStr 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
title_full_unstemmed 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
title_sort 300: An ACA 870 μm Continuum Survey of Orion Protostars and Their Evolution
dc.creator.none.fl_str_mv Federman, Samuel
Megeath, S. Thomas
Tobin, John J.
Sheehan, Patrick D.
Pokhrel, Riwaj
Habel, Nolan
Stutz, Amelia M.
Fischer, William J.
Hartmann, Lee
Stanke, Thomas
Narang, Mayank
Osorio, Mayra
Atnagulov, Prabhani
Rahatgaonkar, Rohan
author Federman, Samuel
author_facet Federman, Samuel
Megeath, S. Thomas
Tobin, John J.
Sheehan, Patrick D.
Pokhrel, Riwaj
Habel, Nolan
Stutz, Amelia M.
Fischer, William J.
Hartmann, Lee
Stanke, Thomas
Narang, Mayank
Osorio, Mayra
Atnagulov, Prabhani
Rahatgaonkar, Rohan
author_role author
author2 Megeath, S. Thomas
Tobin, John J.
Sheehan, Patrick D.
Pokhrel, Riwaj
Habel, Nolan
Stutz, Amelia M.
Fischer, William J.
Hartmann, Lee
Stanke, Thomas
Narang, Mayank
Osorio, Mayra
Atnagulov, Prabhani
Rahatgaonkar, Rohan
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia, Innovación y Universidades (España)
Junta de Andalucía
European Commission
Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
description We present an 870 μm continuum survey of 300 protostars from the Herschel Orion Protostar Survey using the Atacama Compact Array (ACA). These data measure protostellar flux densities on envelope scales ≤8000 au (20'') and resolve the structure of envelopes with 1600 au (4'') resolution, a factor of 3–5 improvement in angular resolution over existing single-dish 870 μm observations. We compare the ACA observations to Atacama Large Millimeter/submillimeter Array 12 m array observations at 870 μm with ∼0farcs1 (40 au) resolution. Using the 12 m data to measure the fluxes from disks and the ACA data within 2500 au to measure the combined disk plus envelope fluxes, we calculate the 12 m/ACA 870 μm flux ratios. Our sample shows a clear evolution in this ratio. Class 0 protostars are mostly envelope-dominated with ratios <0.5. In contrast, Flat Spectrum protostars are primarily disk-dominated with ratios near 1, although with a number of face-on protostars dominated by their envelopes. Class I protostars span the range from envelope to disk-dominated. The increase in ratio is accompanied by a decrease in the envelope fluxes and estimated mass infall rates. We estimate that 80% of the mass is accreted during the envelope-dominated phase. We find that the 12 m/ACA flux ratio is an evolutionary indicator that largely avoids the inclination and foreground extinction dependence of spectral energy distribution-based indicators. © 2023. The Author(s). Published by the American Astronomical Society.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/310298
url http://hdl.handle.net/10261/310298
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-114461GB-I00
info:eu-repo/grantAgreement/AEI//SEV-2017-0709
http://dx.doi.org/10.3847/1538-4357/ac9f4b
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
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