The dynamical state of massive clumps

The dynamical state of massive clumps is key to our understanding of the formation of massive stars. In this work, we study the kinematic properties of massive clumps using synthetic observations. We have previously compiled a very large catalogue of synthetic dust-continuum compact sources from our...

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Detalles Bibliográficos
Autores: Lu, Zu-Jia, Pelkonen, Veli Matti, Juvela, Mika, Padoan, Paolo, Haugbølle, Troels, Nordlund, Åke
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/295995
Acceso en línea:http://hdl.handle.net/10261/295995
Access Level:acceso abierto
Palabra clave:MHD
Radiative transfer
Methods: numerical
Stars: formation
Infrared: stars
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spelling The dynamical state of massive clumpsLu, Zu-JiaPelkonen, Veli MattiJuvela, MikaPadoan, PaoloHaugbølle, TroelsNordlund, ÅkeMHDRadiative transferMethods: numericalStars: formationInfrared: starsThe dynamical state of massive clumps is key to our understanding of the formation of massive stars. In this work, we study the kinematic properties of massive clumps using synthetic observations. We have previously compiled a very large catalogue of synthetic dust-continuum compact sources from our 250 pc, SN-driven, star formation simulation. Here, we compute synthetic N2H+ line profiles for a subsample of those sources and compare their properties with the observations and with those of the corresponding three-dimensional (3D) clumps in the simulation. We find that the velocity dispersion of the sources estimated from the N2H+ line is a good estimate of that of the 3D clumps, although its correlation with the source size is weaker than the velocity–size correlation of the 3D clumps. The relation between the mass of the 3D clumps, Mmain, and that of the corresponding synthetic sources, MSED, has a large scatter and a slope of 0.5, Mmain∝M0.5SED⁠, due to uncertainties arising from the observational band-merging procedure and from projection effects along the line of sight. As a result, the virial parameters of the 3D clumps are not correlated with the clump masses, even if a negative correlation is found for the compact sources, and the virial parameter of the most massive sources may significantly underestimate that of the associated clumps.ZJL acknowledges financial support from China Scholarship Council (CSC) under grant no. 201606660003. PP and VMP acknowledge support by the grant PID2020-115892GB-I00 funded by MCIN/AEI/10.13039/501100011033. Computing resources for this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We acknowledge PRACE for awarding us access to Curie at GENCI@CEA, France. Storage and computing resources at the University of Copenhagen HPC centre, funded in part by Villum Fonden (VKR023406), were used to carry out part of the data analysis.Peer reviewedOxford University PressChina Scholarship CouncilAgencia Estatal de Investigación (España)Ministerio de Ciencia, Innovación y Universidades (España)NASAVillum FondenUniversity of Copenhagen202320232022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/295995reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-115892GB-I00Monthly Notices of the Royal Astronomical SocietyThe underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stab3323https://doi.org/10.1093/mnras/stab3323Noinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2959952026-05-22T06:33:51Z
dc.title.none.fl_str_mv The dynamical state of massive clumps
title The dynamical state of massive clumps
spellingShingle The dynamical state of massive clumps
Lu, Zu-Jia
MHD
Radiative transfer
Methods: numerical
Stars: formation
Infrared: stars
title_short The dynamical state of massive clumps
title_full The dynamical state of massive clumps
title_fullStr The dynamical state of massive clumps
title_full_unstemmed The dynamical state of massive clumps
title_sort The dynamical state of massive clumps
dc.creator.none.fl_str_mv Lu, Zu-Jia
Pelkonen, Veli Matti
Juvela, Mika
Padoan, Paolo
Haugbølle, Troels
Nordlund, Åke
author Lu, Zu-Jia
author_facet Lu, Zu-Jia
Pelkonen, Veli Matti
Juvela, Mika
Padoan, Paolo
Haugbølle, Troels
Nordlund, Åke
author_role author
author2 Pelkonen, Veli Matti
Juvela, Mika
Padoan, Paolo
Haugbølle, Troels
Nordlund, Åke
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv China Scholarship Council
Agencia Estatal de Investigación (España)
Ministerio de Ciencia, Innovación y Universidades (España)
NASA
Villum Fonden
University of Copenhagen
dc.subject.none.fl_str_mv MHD
Radiative transfer
Methods: numerical
Stars: formation
Infrared: stars
topic MHD
Radiative transfer
Methods: numerical
Stars: formation
Infrared: stars
description The dynamical state of massive clumps is key to our understanding of the formation of massive stars. In this work, we study the kinematic properties of massive clumps using synthetic observations. We have previously compiled a very large catalogue of synthetic dust-continuum compact sources from our 250 pc, SN-driven, star formation simulation. Here, we compute synthetic N2H+ line profiles for a subsample of those sources and compare their properties with the observations and with those of the corresponding three-dimensional (3D) clumps in the simulation. We find that the velocity dispersion of the sources estimated from the N2H+ line is a good estimate of that of the 3D clumps, although its correlation with the source size is weaker than the velocity–size correlation of the 3D clumps. The relation between the mass of the 3D clumps, Mmain, and that of the corresponding synthetic sources, MSED, has a large scatter and a slope of 0.5, Mmain∝M0.5SED⁠, due to uncertainties arising from the observational band-merging procedure and from projection effects along the line of sight. As a result, the virial parameters of the 3D clumps are not correlated with the clump masses, even if a negative correlation is found for the compact sources, and the virial parameter of the most massive sources may significantly underestimate that of the associated clumps.
publishDate 2022
dc.date.none.fl_str_mv 2022
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/10261/295995
url http://hdl.handle.net/10261/295995
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-115892GB-I00
Monthly Notices of the Royal Astronomical Society
The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stab3323
https://doi.org/10.1093/mnras/stab3323
No
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.812429

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