A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58

Autores
Maureira, María José; Arce, Héctor G.; Offner, Stella S. R.; Dunham, Michael M.; Pineda, Jaime E.; Fernandez Lopez, Manuel; Chen, Xuepeng; Mardones, Diego
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at ∼1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km s-1, which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of ∼0.5-0.6 , overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core.
Fil: Maureira, María José. University of Yale; Estados Unidos
Fil: Arce, Héctor G.. University of Yale; Estados Unidos
Fil: Offner, Stella S. R.. University of Texas at Austin; Estados Unidos
Fil: Dunham, Michael M.. State University of New York; Estados Unidos
Fil: Pineda, Jaime E.. Max Planck Institute for Extraterrestrial Physics; Alemania
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: Chen, Xuepeng. Chinese Academy of Sciences; República de China
Fil: Mardones, Diego. Universidad de Chile; Chile
Materia
ISM: INDIVIDUAL OBJECTS (PER-BOLO 58)
STARS: FORMATION
STARS: KINEMATICS AND DYNAMICS
STARS: LOW-MASS
STARS: PROTOSTARS
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:11336/56518
Acceder
id CONICETDig_552e31eb35455844549579deeed7cba0
oai_identifier_str oai:ri.conicet.gov.ar:11336/56518
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58Maureira, María JoséArce, Héctor G.Offner, Stella S. R.Dunham, Michael M.Pineda, Jaime E.Fernandez Lopez, ManuelChen, XuepengMardones, DiegoISM: INDIVIDUAL OBJECTS (PER-BOLO 58)STARS: FORMATIONSTARS: KINEMATICS AND DYNAMICSSTARS: LOW-MASSSTARS: PROTOSTARShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at ∼1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km s-1, which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of ∼0.5-0.6 , overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core.Fil: Maureira, María José. University of Yale; Estados UnidosFil: Arce, Héctor G.. University of Yale; Estados UnidosFil: Offner, Stella S. R.. University of Texas at Austin; Estados UnidosFil: Dunham, Michael M.. State University of New York; Estados UnidosFil: Pineda, Jaime E.. Max Planck Institute for Extraterrestrial Physics; AlemaniaFil: 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: Chen, Xuepeng. Chinese Academy of Sciences; República de ChinaFil: Mardones, Diego. Universidad de Chile; ChileIOP Publishing2017-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/56518Maureira, María José; Arce, Héctor G.; Offner, Stella S. R.; Dunham, Michael M.; Pineda, Jaime E.; et al.; A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58; IOP Publishing; Astrophysical Journal; 849; 2; 11-2017; 1-160004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa91ceinfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/1538-4357/aa91ce/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:04:46Zoai:ri.conicet.gov.ar:11336/56518instacron: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:34982025-10-22 12:04:47.03CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
title A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
spellingShingle A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
Maureira, María José
ISM: INDIVIDUAL OBJECTS (PER-BOLO 58)
STARS: FORMATION
STARS: KINEMATICS AND DYNAMICS
STARS: LOW-MASS
STARS: PROTOSTARS
title_short A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
title_full A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
title_fullStr A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
title_full_unstemmed A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
title_sort A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58
dc.creator.none.fl_str_mv Maureira, María José
Arce, Héctor G.
Offner, Stella S. R.
Dunham, Michael M.
Pineda, Jaime E.
Fernandez Lopez, Manuel
Chen, Xuepeng
Mardones, Diego
author Maureira, María José
author_facet Maureira, María José
Arce, Héctor G.
Offner, Stella S. R.
Dunham, Michael M.
Pineda, Jaime E.
Fernandez Lopez, Manuel
Chen, Xuepeng
Mardones, Diego
author_role author
author2 Arce, Héctor G.
Offner, Stella S. R.
Dunham, Michael M.
Pineda, Jaime E.
Fernandez Lopez, Manuel
Chen, Xuepeng
Mardones, Diego
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ISM: INDIVIDUAL OBJECTS (PER-BOLO 58)
STARS: FORMATION
STARS: KINEMATICS AND DYNAMICS
STARS: LOW-MASS
STARS: PROTOSTARS
topic ISM: INDIVIDUAL OBJECTS (PER-BOLO 58)
STARS: FORMATION
STARS: KINEMATICS AND DYNAMICS
STARS: LOW-MASS
STARS: PROTOSTARS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at ∼1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km s-1, which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of ∼0.5-0.6 , overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core.
Fil: Maureira, María José. University of Yale; Estados Unidos
Fil: Arce, Héctor G.. University of Yale; Estados Unidos
Fil: Offner, Stella S. R.. University of Texas at Austin; Estados Unidos
Fil: Dunham, Michael M.. State University of New York; Estados Unidos
Fil: Pineda, Jaime E.. Max Planck Institute for Extraterrestrial Physics; Alemania
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: Chen, Xuepeng. Chinese Academy of Sciences; República de China
Fil: Mardones, Diego. Universidad de Chile; Chile
description We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at ∼1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km s-1, which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of ∼0.5-0.6 , overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core.
publishDate 2017
dc.date.none.fl_str_mv 2017-11
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/11336/56518
Maureira, María José; Arce, Héctor G.; Offner, Stella S. R.; Dunham, Michael M.; Pineda, Jaime E.; et al.; A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58; IOP Publishing; Astrophysical Journal; 849; 2; 11-2017; 1-16
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/56518
identifier_str_mv Maureira, María José; Arce, Héctor G.; Offner, Stella S. R.; Dunham, Michael M.; Pineda, Jaime E.; et al.; A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58; IOP Publishing; Astrophysical Journal; 849; 2; 11-2017; 1-16
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa91ce
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/1538-4357/aa91ce/meta
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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 12.982451

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