Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1

Autores
Busquet, G.; Girart, J. M.; Estalella, R.; Fernandez Lopez, Manuel; Galván Madrid, R.; Anglada, G.; Carrasco González, C.; Añez López, N.; Curiel, S.; Osorio, M.; Rodríguez, L. F.; Torrelles, J. M.
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Most stars form in clusters and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution. Specifically, it is critical to evaluate whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. We seek to investigate the properties of the protostellar disks in the GGD 27 cluster and compare these with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼56 au), and sensitivity (∼0.002 M·). Results. We detected a cluster of 25 continuum sources, most of which likely trace disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M·. The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result, combined with the dynamical timescale of the radio jet (∼104 years), suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this as well. We found a clear paucity of disks with Rdisk > 100 au. The median value of the radius is 34 au; this value is smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i.e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances <0.02 pc. Stars can only form larger and more massive disksfor distances >0.04 pc. This suggests that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass young stellar objects in distant and massive (still deeply embedded) clustered environments.
Fil: Busquet, G.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
Fil: Girart, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
Fil: Estalella, R.. Universidad de Barcelona; España
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: Galván Madrid, R.. Universidad Nacional Autónoma de México; México
Fil: Anglada, G.. Instituto de Astrofísica de Andalucía; España
Fil: Carrasco González, C.. Universidad Nacional Autónoma de México; México
Fil: Añez López, N.. Instituto de Ciencias del Espacio (ice); España
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
Fil: Osorio, M.. Instituto de Astrofísica de Andalucía; España
Fil: Rodríguez, L. F.. Universidad Nacional Autónoma de México; México
Fil: Torrelles, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
Materia
ACCRETION, ACCRETION DISKS
ISM: INDIVIDUAL OBJECTS: GGD 27
ISM: INDIVIDUAL OBJECTS: HH 80-81
ISM: INDIVIDUAL OBJECTS: IRAS 18162-2048
STARS: FORMATION
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/106138
Acceder
id CONICETDig_5866a724d446cb579e26edda701d57dd
oai_identifier_str oai:ri.conicet.gov.ar:11336/106138
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1Busquet, G.Girart, J. M.Estalella, R.Fernandez Lopez, ManuelGalván Madrid, R.Anglada, G.Carrasco González, C.Añez López, N.Curiel, S.Osorio, M.Rodríguez, L. F.Torrelles, J. M.ACCRETION, ACCRETION DISKSISM: INDIVIDUAL OBJECTS: GGD 27ISM: INDIVIDUAL OBJECTS: HH 80-81ISM: INDIVIDUAL OBJECTS: IRAS 18162-2048STARS: FORMATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Most stars form in clusters and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution. Specifically, it is critical to evaluate whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. We seek to investigate the properties of the protostellar disks in the GGD 27 cluster and compare these with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼56 au), and sensitivity (∼0.002 M·). Results. We detected a cluster of 25 continuum sources, most of which likely trace disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M·. The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result, combined with the dynamical timescale of the radio jet (∼104 years), suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this as well. We found a clear paucity of disks with Rdisk > 100 au. The median value of the radius is 34 au; this value is smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i.e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances <0.02 pc. Stars can only form larger and more massive disksfor distances >0.04 pc. This suggests that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass young stellar objects in distant and massive (still deeply embedded) clustered environments.Fil: Busquet, G.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); EspañaFil: Girart, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); EspañaFil: Estalella, R.. Universidad de Barcelona; EspañaFil: 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: Galván Madrid, R.. Universidad Nacional Autónoma de México; MéxicoFil: Anglada, G.. Instituto de Astrofísica de Andalucía; EspañaFil: Carrasco González, C.. Universidad Nacional Autónoma de México; MéxicoFil: Añez López, N.. Instituto de Ciencias del Espacio (ice); EspañaFil: Curiel, S.. Universidad Nacional Autónoma de México; MéxicoFil: Osorio, M.. Instituto de Astrofísica de Andalucía; EspañaFil: Rodríguez, L. F.. Universidad Nacional Autónoma de México; MéxicoFil: Torrelles, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); EspañaEDP Sciences2019-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/106138Busquet, G.; Girart, J. M.; Estalella, R.; Fernandez Lopez, Manuel; Galván Madrid, R.; et al.; Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1; EDP Sciences; Astronomy and Astrophysics; 623; L8; 3-2019; 1-110004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201833687info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2019/03/aa33687-18/aa33687-18.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:21:40Zoai:ri.conicet.gov.ar:11336/106138instacron: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 14:21:40.904CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
title Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
spellingShingle Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
Busquet, G.
ACCRETION, ACCRETION DISKS
ISM: INDIVIDUAL OBJECTS: GGD 27
ISM: INDIVIDUAL OBJECTS: HH 80-81
ISM: INDIVIDUAL OBJECTS: IRAS 18162-2048
STARS: FORMATION
title_short Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
title_full Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
title_fullStr Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
title_full_unstemmed Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
title_sort Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1
dc.creator.none.fl_str_mv Busquet, G.
Girart, J. M.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Anglada, G.
Carrasco González, C.
Añez López, N.
Curiel, S.
Osorio, M.
Rodríguez, L. F.
Torrelles, J. M.
author Busquet, G.
author_facet Busquet, G.
Girart, J. M.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Anglada, G.
Carrasco González, C.
Añez López, N.
Curiel, S.
Osorio, M.
Rodríguez, L. F.
Torrelles, J. M.
author_role author
author2 Girart, J. M.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Anglada, G.
Carrasco González, C.
Añez López, N.
Curiel, S.
Osorio, M.
Rodríguez, L. F.
Torrelles, J. M.
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ACCRETION, ACCRETION DISKS
ISM: INDIVIDUAL OBJECTS: GGD 27
ISM: INDIVIDUAL OBJECTS: HH 80-81
ISM: INDIVIDUAL OBJECTS: IRAS 18162-2048
STARS: FORMATION
topic ACCRETION, ACCRETION DISKS
ISM: INDIVIDUAL OBJECTS: GGD 27
ISM: INDIVIDUAL OBJECTS: HH 80-81
ISM: INDIVIDUAL OBJECTS: IRAS 18162-2048
STARS: FORMATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. Most stars form in clusters and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution. Specifically, it is critical to evaluate whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. We seek to investigate the properties of the protostellar disks in the GGD 27 cluster and compare these with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼56 au), and sensitivity (∼0.002 M·). Results. We detected a cluster of 25 continuum sources, most of which likely trace disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M·. The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result, combined with the dynamical timescale of the radio jet (∼104 years), suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this as well. We found a clear paucity of disks with Rdisk > 100 au. The median value of the radius is 34 au; this value is smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i.e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances <0.02 pc. Stars can only form larger and more massive disksfor distances >0.04 pc. This suggests that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass young stellar objects in distant and massive (still deeply embedded) clustered environments.
Fil: Busquet, G.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
Fil: Girart, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
Fil: Estalella, R.. Universidad de Barcelona; España
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: Galván Madrid, R.. Universidad Nacional Autónoma de México; México
Fil: Anglada, G.. Instituto de Astrofísica de Andalucía; España
Fil: Carrasco González, C.. Universidad Nacional Autónoma de México; México
Fil: Añez López, N.. Instituto de Ciencias del Espacio (ice); España
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
Fil: Osorio, M.. Instituto de Astrofísica de Andalucía; España
Fil: Rodríguez, L. F.. Universidad Nacional Autónoma de México; México
Fil: Torrelles, J. M.. Instituto de Estudios Espaciales de Cataluña; España. Instituto de Ciencias del Espacio (ice); España
description Context. Most stars form in clusters and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution. Specifically, it is critical to evaluate whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. We seek to investigate the properties of the protostellar disks in the GGD 27 cluster and compare these with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼56 au), and sensitivity (∼0.002 M·). Results. We detected a cluster of 25 continuum sources, most of which likely trace disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M·. The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result, combined with the dynamical timescale of the radio jet (∼104 years), suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this as well. We found a clear paucity of disks with Rdisk > 100 au. The median value of the radius is 34 au; this value is smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i.e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances <0.02 pc. Stars can only form larger and more massive disksfor distances >0.04 pc. This suggests that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass young stellar objects in distant and massive (still deeply embedded) clustered environments.
publishDate 2019
dc.date.none.fl_str_mv 2019-03
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/11336/106138
Busquet, G.; Girart, J. M.; Estalella, R.; Fernandez Lopez, Manuel; Galván Madrid, R.; et al.; Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1; EDP Sciences; Astronomy and Astrophysics; 623; L8; 3-2019; 1-11
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/106138
identifier_str_mv Busquet, G.; Girart, J. M.; Estalella, R.; Fernandez Lopez, Manuel; Galván Madrid, R.; et al.; Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1; EDP Sciences; Astronomy and Astrophysics; 623; L8; 3-2019; 1-11
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/doi/10.1051/0004-6361/201833687
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2019/03/aa33687-18/aa33687-18.html
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
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.221938

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