ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4

Autores: Álvarez Gutiérrez, R. H.; Stutz, A. M.; Sandoval Garrido, N.; Louvet, F.; Motte, F.; Galván Madrid, R.; Cunningham, N.; Sanhueza, P.; Bonfand, M.; Bontemps, Sophie; Gusdorf, A.; Ginsburg, A.; Csengeri, T.; Reyes, S. D.; Salinas, J.; Baug, T.; Bronfman, L.; Busquets, Gabriel; Díaz González, D. J.; Fernandez Lopez, Manuel; Guzmán, A.; Koley, A.; Liu, H. L.; Olguin, F. A.; Valeille Manet, M.; Wyrowski, F.
Año de publicación: 2024
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N2H+ (1−0), with a spatial resolution of ~0.02 pc. G353.41, at a distance of ~2kpc, is embedded in a larger-scale (~8 pc) filament and has a mass of ~2.5 × 103 M⊙ within 1.3 × 1.3 pc2. We extracted the N2H+ (1−0) isolated line component and decomposed it by fitting up to three Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (~1 pc) and small scales (~0.2pc). We find good agreement between the N2H+ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled with the dense gas in which they form. We have measured nine converging “V-shaped” velocity gradients (VGs) (~20 km s−1 pc−1) that are well resolved (sizes ~0.1 pc), mostly located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimated the timescales associated with V-shapes as VG−1, and we interpret them as inflow timescales. The average inflow timescale is ~67 kyr, or about twice the free-fall time of cores in the same area (~33 kyr) but substantially shorter than protostar lifetime estimates (~0.5 Myr). We derived mass accretion rates in the range of (0.35–8.77) × 10−4 M⊙ yr−1. This feeding might lead to further filament collapse and the formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus, these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster’s lifetime.
Fil: Álvarez Gutiérrez, R. H.. Universidad de Concepción; Chile
Fil: Stutz, A. M.. Universidad de Concepción; Chile
Fil: Sandoval Garrido, N.. Universidad de Concepción; Chile
Fil: Louvet, F.. Universite Grenoble Alpes; Francia
Fil: Motte, F.. Universite Grenoble Alpes; Francia
Fil: Galván Madrid, R.. Universidad Nacional Autónoma de México; México
Fil: Cunningham, N.. Universite Grenoble Alpes; Francia
Fil: Sanhueza, P.. National Astronomical Observatory of Japan; Japón
Fil: Bonfand, M.. University of Virginia; Estados Unidos
Fil: Bontemps, Sophie. Universite de Bordeaux; Francia
Fil: Gusdorf, A.. Centre National de la Recherche Scientifique. Ecole Normale Supérieure; Francia
Fil: Ginsburg, A.. University of Florida; Estados Unidos
Fil: Csengeri, T.. Universite de Bordeaux; Francia
Fil: Reyes, S. D.. Universidad de Concepción; Chile
Fil: Salinas, J.. Universidad de Concepción; Chile
Fil: Baug, T.. S. N. Bose National Centre For Basic Sciences; India
Fil: Bronfman, L.. Universidad de Chile; Chile
Fil: Busquets, Gabriel. Universidad de Barcelona. Facultad de Física; España
Fil: Díaz González, D. J.. Universidad Nacional Autónoma de México; México
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Guzmán, A.. Joint ALMA Observatory; Chile
Fil: Koley, A.. Universidad de Concepción; Chile
Fil: Liu, H. L.. Universidad de Concepción; Chile
Fil: Olguin, F. A.. National Tsing Hua University; China
Fil: Valeille Manet, M.. Universite de Bordeaux; Francia
Fil: Wyrowski, F.. Max Planck Institute for Radio Astronomy; Alemania
Materia: ISM: clouds
ISM: molecules
Nivel de accesibilidad: acceso abierto
Condiciones de uso: https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
Institución: Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador: oai:ri.conicet.gov.ar:11336/268681

Acceder

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spelling	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4Álvarez Gutiérrez, R. H.Stutz, A. M.Sandoval Garrido, N.Louvet, F.Motte, F.Galván Madrid, R.Cunningham, N.Sanhueza, P.Bonfand, M.Bontemps, SophieGusdorf, A.Ginsburg, A.Csengeri, T.Reyes, S. D.Salinas, J.Baug, T.Bronfman, L.Busquets, GabrielDíaz González, D. J.Fernandez Lopez, ManuelGuzmán, A.Koley, A.Liu, H. L.Olguin, F. A.Valeille Manet, M.Wyrowski, F.ISM: cloudsISM: moleculeshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N2H+ (1−0), with a spatial resolution of ~0.02 pc. G353.41, at a distance of ~2kpc, is embedded in a larger-scale (~8 pc) filament and has a mass of ~2.5 × 103 M⊙ within 1.3 × 1.3 pc2. We extracted the N2H+ (1−0) isolated line component and decomposed it by fitting up to three Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (~1 pc) and small scales (~0.2pc). We find good agreement between the N2H+ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled with the dense gas in which they form. We have measured nine converging “V-shaped” velocity gradients (VGs) (~20 km s−1 pc−1) that are well resolved (sizes ~0.1 pc), mostly located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimated the timescales associated with V-shapes as VG−1, and we interpret them as inflow timescales. The average inflow timescale is ~67 kyr, or about twice the free-fall time of cores in the same area (~33 kyr) but substantially shorter than protostar lifetime estimates (~0.5 Myr). We derived mass accretion rates in the range of (0.35–8.77) × 10−4 M⊙ yr−1. This feeding might lead to further filament collapse and the formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus, these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster’s lifetime.Fil: Álvarez Gutiérrez, R. H.. Universidad de Concepción; ChileFil: Stutz, A. M.. Universidad de Concepción; ChileFil: Sandoval Garrido, N.. Universidad de Concepción; ChileFil: Louvet, F.. Universite Grenoble Alpes; FranciaFil: Motte, F.. Universite Grenoble Alpes; FranciaFil: Galván Madrid, R.. Universidad Nacional Autónoma de México; MéxicoFil: Cunningham, N.. Universite Grenoble Alpes; FranciaFil: Sanhueza, P.. National Astronomical Observatory of Japan; JapónFil: Bonfand, M.. University of Virginia; Estados UnidosFil: Bontemps, Sophie. Universite de Bordeaux; FranciaFil: Gusdorf, A.. Centre National de la Recherche Scientifique. Ecole Normale Supérieure; FranciaFil: Ginsburg, A.. University of Florida; Estados UnidosFil: Csengeri, T.. Universite de Bordeaux; FranciaFil: Reyes, S. D.. Universidad de Concepción; ChileFil: Salinas, J.. Universidad de Concepción; ChileFil: Baug, T.. S. N. Bose National Centre For Basic Sciences; IndiaFil: Bronfman, L.. Universidad de Chile; ChileFil: Busquets, Gabriel. Universidad de Barcelona. Facultad de Física; EspañaFil: Díaz González, D. J.. Universidad Nacional Autónoma de México; MéxicoFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Guzmán, A.. Joint ALMA Observatory; ChileFil: Koley, A.. Universidad de Concepción; ChileFil: Liu, H. L.. Universidad de Concepción; ChileFil: Olguin, F. A.. National Tsing Hua University; ChinaFil: Valeille Manet, M.. Universite de Bordeaux; FranciaFil: Wyrowski, F.. Max Planck Institute for Radio Astronomy; AlemaniaEDP Sciences2024-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/268681Álvarez Gutiérrez, R. H.; Stutz, A. M.; Sandoval Garrido, N.; Louvet, F.; Motte, F.; et al.; ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4; EDP Sciences; Astronomy and Astrophysics; 689; A74; 9-2024; 1-230004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202450321info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450321info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:26:41Zoai:ri.conicet.gov.ar:11336/268681instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:26:41.838CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
title	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
spellingShingle	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4 Álvarez Gutiérrez, R. H. ISM: clouds ISM: molecules
title_short	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
title_full	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
title_fullStr	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
title_full_unstemmed	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
title_sort	ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4
dc.creator.none.fl_str_mv	Álvarez Gutiérrez, R. H. Stutz, A. M. Sandoval Garrido, N. Louvet, F. Motte, F. Galván Madrid, R. Cunningham, N. Sanhueza, P. Bonfand, M. Bontemps, Sophie Gusdorf, A. Ginsburg, A. Csengeri, T. Reyes, S. D. Salinas, J. Baug, T. Bronfman, L. Busquets, Gabriel Díaz González, D. J. Fernandez Lopez, Manuel Guzmán, A. Koley, A. Liu, H. L. Olguin, F. A. Valeille Manet, M. Wyrowski, F.
author	Álvarez Gutiérrez, R. H.
author_facet	Álvarez Gutiérrez, R. H. Stutz, A. M. Sandoval Garrido, N. Louvet, F. Motte, F. Galván Madrid, R. Cunningham, N. Sanhueza, P. Bonfand, M. Bontemps, Sophie Gusdorf, A. Ginsburg, A. Csengeri, T. Reyes, S. D. Salinas, J. Baug, T. Bronfman, L. Busquets, Gabriel Díaz González, D. J. Fernandez Lopez, Manuel Guzmán, A. Koley, A. Liu, H. L. Olguin, F. A. Valeille Manet, M. Wyrowski, F.
author_role	author
author2	Stutz, A. M. Sandoval Garrido, N. Louvet, F. Motte, F. Galván Madrid, R. Cunningham, N. Sanhueza, P. Bonfand, M. Bontemps, Sophie Gusdorf, A. Ginsburg, A. Csengeri, T. Reyes, S. D. Salinas, J. Baug, T. Bronfman, L. Busquets, Gabriel Díaz González, D. J. Fernandez Lopez, Manuel Guzmán, A. Koley, A. Liu, H. L. Olguin, F. A. Valeille Manet, M. Wyrowski, F.
author2_role	author author author author author author author author author author author author author author author author author author author author author author author author author
dc.subject.none.fl_str_mv	ISM: clouds ISM: molecules
topic	ISM: clouds ISM: molecules
purl_subject.fl_str_mv	https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv	The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N2H+ (1−0), with a spatial resolution of ~0.02 pc. G353.41, at a distance of ~2kpc, is embedded in a larger-scale (~8 pc) filament and has a mass of ~2.5 × 103 M⊙ within 1.3 × 1.3 pc2. We extracted the N2H+ (1−0) isolated line component and decomposed it by fitting up to three Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (~1 pc) and small scales (~0.2pc). We find good agreement between the N2H+ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled with the dense gas in which they form. We have measured nine converging “V-shaped” velocity gradients (VGs) (~20 km s−1 pc−1) that are well resolved (sizes ~0.1 pc), mostly located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimated the timescales associated with V-shapes as VG−1, and we interpret them as inflow timescales. The average inflow timescale is ~67 kyr, or about twice the free-fall time of cores in the same area (~33 kyr) but substantially shorter than protostar lifetime estimates (~0.5 Myr). We derived mass accretion rates in the range of (0.35–8.77) × 10−4 M⊙ yr−1. This feeding might lead to further filament collapse and the formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus, these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster’s lifetime. Fil: Álvarez Gutiérrez, R. H.. Universidad de Concepción; Chile Fil: Stutz, A. M.. Universidad de Concepción; Chile Fil: Sandoval Garrido, N.. Universidad de Concepción; Chile Fil: Louvet, F.. Universite Grenoble Alpes; Francia Fil: Motte, F.. Universite Grenoble Alpes; Francia Fil: Galván Madrid, R.. Universidad Nacional Autónoma de México; México Fil: Cunningham, N.. Universite Grenoble Alpes; Francia Fil: Sanhueza, P.. National Astronomical Observatory of Japan; Japón Fil: Bonfand, M.. University of Virginia; Estados Unidos Fil: Bontemps, Sophie. Universite de Bordeaux; Francia Fil: Gusdorf, A.. Centre National de la Recherche Scientifique. Ecole Normale Supérieure; Francia Fil: Ginsburg, A.. University of Florida; Estados Unidos Fil: Csengeri, T.. Universite de Bordeaux; Francia Fil: Reyes, S. D.. Universidad de Concepción; Chile Fil: Salinas, J.. Universidad de Concepción; Chile Fil: Baug, T.. S. N. Bose National Centre For Basic Sciences; India Fil: Bronfman, L.. Universidad de Chile; Chile Fil: Busquets, Gabriel. Universidad de Barcelona. Facultad de Física; España Fil: Díaz González, D. J.. Universidad Nacional Autónoma de México; México Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Guzmán, A.. Joint ALMA Observatory; Chile Fil: Koley, A.. Universidad de Concepción; Chile Fil: Liu, H. L.. Universidad de Concepción; Chile Fil: Olguin, F. A.. National Tsing Hua University; China Fil: Valeille Manet, M.. Universite de Bordeaux; Francia Fil: Wyrowski, F.. Max Planck Institute for Radio Astronomy; Alemania
description	The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N2H+ (1−0), with a spatial resolution of ~0.02 pc. G353.41, at a distance of ~2kpc, is embedded in a larger-scale (~8 pc) filament and has a mass of ~2.5 × 103 M⊙ within 1.3 × 1.3 pc2. We extracted the N2H+ (1−0) isolated line component and decomposed it by fitting up to three Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (~1 pc) and small scales (~0.2pc). We find good agreement between the N2H+ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled with the dense gas in which they form. We have measured nine converging “V-shaped” velocity gradients (VGs) (~20 km s−1 pc−1) that are well resolved (sizes ~0.1 pc), mostly located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimated the timescales associated with V-shapes as VG−1, and we interpret them as inflow timescales. The average inflow timescale is ~67 kyr, or about twice the free-fall time of cores in the same area (~33 kyr) but substantially shorter than protostar lifetime estimates (~0.5 Myr). We derived mass accretion rates in the range of (0.35–8.77) × 10−4 M⊙ yr−1. This feeding might lead to further filament collapse and the formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus, these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster’s lifetime.
publishDate	2024
dc.date.none.fl_str_mv	2024-09
dc.type.none.fl_str_mv	info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo
format	article
status_str	publishedVersion
dc.identifier.none.fl_str_mv	http://hdl.handle.net/11336/268681 Álvarez Gutiérrez, R. H.; Stutz, A. M.; Sandoval Garrido, N.; Louvet, F.; Motte, F.; et al.; ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4; EDP Sciences; Astronomy and Astrophysics; 689; A74; 9-2024; 1-23 0004-6361 CONICET Digital CONICET
url	http://hdl.handle.net/11336/268681
identifier_str_mv	Álvarez Gutiérrez, R. H.; Stutz, A. M.; Sandoval Garrido, N.; Louvet, F.; Motte, F.; et al.; ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4; EDP Sciences; Astronomy and Astrophysics; 689; A74; 9-2024; 1-23 0004-6361 CONICET Digital CONICET
dc.language.none.fl_str_mv	eng
language	eng
dc.relation.none.fl_str_mv	info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202450321 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450321
dc.rights.none.fl_str_mv	info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv	openAccess
rights_invalid_str_mv	https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv	application/pdf application/pdf
dc.publisher.none.fl_str_mv	EDP Sciences
publisher.none.fl_str_mv	EDP Sciences
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repository.mail.fl_str_mv	dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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ALMA-IMF. XIII: N2H+ kinematic analysis of the intermediate protocluster G353.4

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