Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2

Context. High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest of these systems, making it an excellent target for case studies. Aims. We investigate the morphology, stability and dynamical pr...

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Autores: Trevino-Morales, S. P., Fuente, A., Sanchez-Monge, A., Kainulainen, J., Didelon, P., Suri, S., Schneider, Nicholas, Ballesteros-Paredes, Javier, Lee, Y. N., Hennebelle, Patrick, Pilleri, P., González García, Marta, Kramer, C., García-Burillo, Santiago, Luna, A., Goicoechea, Javier R., Tremblin, P., Geen, S.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2019
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/191924
Acceso en línea:http://hdl.handle.net/10261/191924
Access Level:acceso abierto
Palabra clave:ISM: kinematics and dynamics
ISM: structure
ISM: clouds
ISM: individual objects: Monoceros R2
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network_name_str España
repository_id_str
dc.title.none.fl_str_mv Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
title Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
spellingShingle Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
Trevino-Morales, S. P.
ISM: kinematics and dynamics
ISM: structure
ISM: clouds
ISM: individual objects: Monoceros R2
title_short Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
title_full Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
title_fullStr Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
title_full_unstemmed Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
title_sort Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2
dc.creator.none.fl_str_mv Trevino-Morales, S. P.
Fuente, A.
Sanchez-Monge, A.
Kainulainen, J.
Didelon, P.
Suri, S.
Schneider, Nicholas
Ballesteros-Paredes, Javier
Lee, Y. N.
Hennebelle, Patrick
Pilleri, P.
González García, Marta
Kramer, C.
García-Burillo, Santiago
Luna, A.
Goicoechea, Javier R.
Tremblin, P.
Geen, S.
author Trevino-Morales, S. P.
author_facet Trevino-Morales, S. P.
Fuente, A.
Sanchez-Monge, A.
Kainulainen, J.
Didelon, P.
Suri, S.
Schneider, Nicholas
Ballesteros-Paredes, Javier
Lee, Y. N.
Hennebelle, Patrick
Pilleri, P.
González García, Marta
Kramer, C.
García-Burillo, Santiago
Luna, A.
Goicoechea, Javier R.
Tremblin, P.
Geen, S.
author_role author
author2 Fuente, A.
Sanchez-Monge, A.
Kainulainen, J.
Didelon, P.
Suri, S.
Schneider, Nicholas
Ballesteros-Paredes, Javier
Lee, Y. N.
Hennebelle, Patrick
Pilleri, P.
González García, Marta
Kramer, C.
García-Burillo, Santiago
Luna, A.
Goicoechea, Javier R.
Tremblin, P.
Geen, S.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
Ministerio de Economía y Competitividad (España)
European Research Council
German Research Foundation
Centre National D'Etudes Spatiales (France)
Ministerio de Ciencia, Innovación y Universidades (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv ISM: kinematics and dynamics
ISM: structure
ISM: clouds
ISM: individual objects: Monoceros R2
topic ISM: kinematics and dynamics
ISM: structure
ISM: clouds
ISM: individual objects: Monoceros R2
description Context. High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest of these systems, making it an excellent target for case studies. Aims. We investigate the morphology, stability and dynamical properties of the Mon R2 hub-filament system. Methods. We employed observations of the (CO)-C-13 and (CO)-O-18 1 -> 0 and 2 -> 1 lines obtained with the IRAM-30m telescope. We also used H-2 column density maps derived from Herschel dust emission observations. Results. We identified the filamentary network in Mon R-2 with the DisPerSE algorithm and characterized the individual filaments as either main (converging into the hub) or secondary (converging to a main filament). The main filaments have line masses of 30-100 M-circle dot pc(-1) and show signs of fragmentation, while the secondary filaments have line masses of 12-60 M-circle dot pc(-1) and show fragmentation only sporadically. In the context of Ostriker's hydrostatic filament model, the main filaments are thermally supercritical. If non-thermal motions are included, most of them are transcritical. Most of the secondary filaments are roughly transcritical regardless of whether non-thermal motions are included or not. From the morphology and kinematics of the main filaments, we estimate a mass accretion rate of 10(-4)-10(-3) M-circle dot yr(-1) into the central hub. The secondary filaments accrete into the main filaments at a rate of 0.1-0.4 x 10(-4) M-circle dot yr(-1). The main filaments extend into the central hub. Their velocity gradients increase toward the hub, suggesting acceleration of the gas. We estimate that with the observed infall velocity, the mass-doubling time of the hub is similar to 2.5 Myr, ten times longer than the free-fall time, suggesting a dynamically old region. These timescales are comparable with the chemical age of the HII region. Inside the hub, the main filaments show a ring-or a spiral-like morphology that exhibits rotation and infall motions. One possible explanation for the morphology is that gas is falling into the central cluster following a spiral-like pattern.© ESO 2019.
publishDate 2019
dc.date.none.fl_str_mv 2019
2019
2019
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/191924
url http://hdl.handle.net/10261/191924
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
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dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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
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spelling Dynamics of cluster-forming hub-filament systems. The case of the high-mass star-forming complex Monoceros R2Trevino-Morales, S. P.Fuente, A.Sanchez-Monge, A.Kainulainen, J.Didelon, P.Suri, S.Schneider, NicholasBallesteros-Paredes, JavierLee, Y. N.Hennebelle, PatrickPilleri, P.González García, MartaKramer, C.García-Burillo, SantiagoLuna, A.Goicoechea, Javier R.Tremblin, P.Geen, S.ISM: kinematics and dynamicsISM: structureISM: cloudsISM: individual objects: Monoceros R2Context. High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest of these systems, making it an excellent target for case studies. Aims. We investigate the morphology, stability and dynamical properties of the Mon R2 hub-filament system. Methods. We employed observations of the (CO)-C-13 and (CO)-O-18 1 -> 0 and 2 -> 1 lines obtained with the IRAM-30m telescope. We also used H-2 column density maps derived from Herschel dust emission observations. Results. We identified the filamentary network in Mon R-2 with the DisPerSE algorithm and characterized the individual filaments as either main (converging into the hub) or secondary (converging to a main filament). The main filaments have line masses of 30-100 M-circle dot pc(-1) and show signs of fragmentation, while the secondary filaments have line masses of 12-60 M-circle dot pc(-1) and show fragmentation only sporadically. In the context of Ostriker's hydrostatic filament model, the main filaments are thermally supercritical. If non-thermal motions are included, most of them are transcritical. Most of the secondary filaments are roughly transcritical regardless of whether non-thermal motions are included or not. From the morphology and kinematics of the main filaments, we estimate a mass accretion rate of 10(-4)-10(-3) M-circle dot yr(-1) into the central hub. The secondary filaments accrete into the main filaments at a rate of 0.1-0.4 x 10(-4) M-circle dot yr(-1). The main filaments extend into the central hub. Their velocity gradients increase toward the hub, suggesting acceleration of the gas. We estimate that with the observed infall velocity, the mass-doubling time of the hub is similar to 2.5 Myr, ten times longer than the free-fall time, suggesting a dynamically old region. These timescales are comparable with the chemical age of the HII region. Inside the hub, the main filaments show a ring-or a spiral-like morphology that exhibits rotation and infall motions. One possible explanation for the morphology is that gas is falling into the central cluster following a spiral-like pattern.© ESO 2019.S.P.T.M. and J.K.acknowledge to the European Union's Horizon 2020 research and innovation program for funding support given under grant agreement No 639459 (PROMISE). A.F. thanks the Spanish MINECO for funding support from grants AYA2016-75 066-C2-2-P, and ERC under ERC-2013-SyG, G.A. 610 256 NANOCOSMOS. A.S.M. and S. S. thank the Deutsche Forschungsgemeinschaft (DFG) for funding support via the collaborative research grant SFB 956, projects A6 and A4. P. P. acknowledges financial support from the Center National de Etudes Spatiales (CNES). N.S. acknowledges support from the French ANR and the German DFG through the project "GENESIS" (ANR-16-CE92-0035-01/DFG1591/2-1). S. S. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Consolidator Grant CSF-648 505. S.G. is funded by the European Research Council under Grant Agreement no. 339 177 (STARLIGHT) of the European Community's Seventh Framework Programme (FP7/2007-2013). J.R.G. thanks the Spanish MICIU for funding support from grant AYA2017-85 111-P.Peer reviewedEDP SciencesEuropean CommissionMinisterio de Economía y Competitividad (España)European Research CouncilGerman Research FoundationCentre National D'Etudes Spatiales (France)Ministerio de Ciencia, Innovación y Universidades (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]201920192019info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/191924reponame:DIGITAL.CSIC. 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