SiO outflows in the most luminous and massive protostellar sources of the southern sky

Autores
Guerra Varas, N.; Merello, M.; Bronfman, L.; Duronea, Nicolas Urbano; Elia, D.; Finger, R.; Mendoza, E.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. High-mass star formation is far less understood than low-mass star formation. It entails the ejection of matter through molecular outflows, which disturbs the protostellar clump. Studying these outflows and the shocked gas caused by them is the key to a better understanding of this process. Aims: The present study aims to characterise the behaviour of molecular outflows in the most massive protostellar sources in the southern Galaxy by looking for evolutionary trends and associating the presence of shocked gas with outflow activity. Methods: We present APEX SEPIA180 (Band 5) observations (beamwidth ~36″) of SiO(4-3) molecular outflow candidates towards a well-selected sample of 32 luminous and dense clumps, which are candidates for harbouring hot molecular cores. We study the emission of the SiO(4-3) line, which is an unambiguous tracer of shocked gas, and recent and active outflow activity, as well as the HCO+(2-1) and H13CO+(2-1) lines. Results: Results show that 78% of our sample (25 sources) present SiO emission, revealing the presence of shocked gas. Nine of these sources are also found to have wings in the HCO+(2-1) line, indicating outflow activity. The SiO emission of these nine sources is generally more intense (Ta > 1 K) and wider (~61 km s−1 FWZP) than the rest of the clumps with SiO detection (~42 km s−1 FWZP), suggesting that the outflows in this group are faster and more energetic. This indicates that the shocked material gets dispersed as the core evolves and outflow activity decreases. Three positive linear correlations are found: a weak one (between the bolometric luminosity and outflow power) and two strong ones (one between the outflow power and the rate of matter expulsion and the other between the kinetic energy and outflow mass). These correlations suggest that more energetic outflows are able to mobilise more material. No correlation was found between the evolutionary stage indicator L/M and SiO outflow properties, supporting that molecular outflows happen throughout the whole high-mass star formation process. Conclusions: We conclude that sources with both SiO emission and HCO+ wings and sources with only SiO emission are in an advanced stage of evolution in the high-mass star formation process, and there is no clear evolutionary difference between them. The former present more massive and more powerful SiO outflows than the latter. Therefore, looking for more outflow signatures such as HCO+ wings could help identify more massive and active massive star-forming regions in samples of similarly evolved sources, and could also help identify sources with older outflow activity.
Fil: Guerra Varas, N.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Merello, M.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Bronfman, L.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Elia, D.. No especifíca;
Fil: Finger, R.. Universidad de Chile; Chile
Fil: Mendoza, E.. Universidad de Huelva; España
Materia
stars: formation
stars: massive
stars: jets and outflows
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:11336/236085

id CONICETDig_7a0782cb9cb844e6203877b44fed9585
oai_identifier_str oai:ri.conicet.gov.ar:11336/236085
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling SiO outflows in the most luminous and massive protostellar sources of the southern skyGuerra Varas, N.Merello, M.Bronfman, L.Duronea, Nicolas UrbanoElia, D.Finger, R.Mendoza, E.stars: formationstars: massivestars: jets and outflowshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. High-mass star formation is far less understood than low-mass star formation. It entails the ejection of matter through molecular outflows, which disturbs the protostellar clump. Studying these outflows and the shocked gas caused by them is the key to a better understanding of this process. Aims: The present study aims to characterise the behaviour of molecular outflows in the most massive protostellar sources in the southern Galaxy by looking for evolutionary trends and associating the presence of shocked gas with outflow activity. Methods: We present APEX SEPIA180 (Band 5) observations (beamwidth ~36″) of SiO(4-3) molecular outflow candidates towards a well-selected sample of 32 luminous and dense clumps, which are candidates for harbouring hot molecular cores. We study the emission of the SiO(4-3) line, which is an unambiguous tracer of shocked gas, and recent and active outflow activity, as well as the HCO+(2-1) and H13CO+(2-1) lines. Results: Results show that 78% of our sample (25 sources) present SiO emission, revealing the presence of shocked gas. Nine of these sources are also found to have wings in the HCO+(2-1) line, indicating outflow activity. The SiO emission of these nine sources is generally more intense (Ta > 1 K) and wider (~61 km s−1 FWZP) than the rest of the clumps with SiO detection (~42 km s−1 FWZP), suggesting that the outflows in this group are faster and more energetic. This indicates that the shocked material gets dispersed as the core evolves and outflow activity decreases. Three positive linear correlations are found: a weak one (between the bolometric luminosity and outflow power) and two strong ones (one between the outflow power and the rate of matter expulsion and the other between the kinetic energy and outflow mass). These correlations suggest that more energetic outflows are able to mobilise more material. No correlation was found between the evolutionary stage indicator L/M and SiO outflow properties, supporting that molecular outflows happen throughout the whole high-mass star formation process. Conclusions: We conclude that sources with both SiO emission and HCO+ wings and sources with only SiO emission are in an advanced stage of evolution in the high-mass star formation process, and there is no clear evolutionary difference between them. The former present more massive and more powerful SiO outflows than the latter. Therefore, looking for more outflow signatures such as HCO+ wings could help identify more massive and active massive star-forming regions in samples of similarly evolved sources, and could also help identify sources with older outflow activity.Fil: Guerra Varas, N.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; ChileFil: Merello, M.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; ChileFil: Bronfman, L.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; ChileFil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Elia, D.. No especifíca;Fil: Finger, R.. Universidad de Chile; ChileFil: Mendoza, E.. Universidad de Huelva; EspañaEDP Sciences2023-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/236085Guerra Varas, N.; Merello, M.; Bronfman, L.; Duronea, Nicolas Urbano; Elia, D.; et al.; SiO outflows in the most luminous and massive protostellar sources of the southern sky; EDP Sciences; Astronomy and Astrophysics; 677; A148; 9-2023; 1-230004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202245522info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/09/aa45522-22/aa45522-22.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 Técnicas2025-09-29T09:51:51Zoai:ri.conicet.gov.ar:11336/236085instacron: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:34982025-09-29 09:51:51.279CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv SiO outflows in the most luminous and massive protostellar sources of the southern sky
title SiO outflows in the most luminous and massive protostellar sources of the southern sky
spellingShingle SiO outflows in the most luminous and massive protostellar sources of the southern sky
Guerra Varas, N.
stars: formation
stars: massive
stars: jets and outflows
title_short SiO outflows in the most luminous and massive protostellar sources of the southern sky
title_full SiO outflows in the most luminous and massive protostellar sources of the southern sky
title_fullStr SiO outflows in the most luminous and massive protostellar sources of the southern sky
title_full_unstemmed SiO outflows in the most luminous and massive protostellar sources of the southern sky
title_sort SiO outflows in the most luminous and massive protostellar sources of the southern sky
dc.creator.none.fl_str_mv Guerra Varas, N.
Merello, M.
Bronfman, L.
Duronea, Nicolas Urbano
Elia, D.
Finger, R.
Mendoza, E.
author Guerra Varas, N.
author_facet Guerra Varas, N.
Merello, M.
Bronfman, L.
Duronea, Nicolas Urbano
Elia, D.
Finger, R.
Mendoza, E.
author_role author
author2 Merello, M.
Bronfman, L.
Duronea, Nicolas Urbano
Elia, D.
Finger, R.
Mendoza, E.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv stars: formation
stars: massive
stars: jets and outflows
topic stars: formation
stars: massive
stars: jets and outflows
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. High-mass star formation is far less understood than low-mass star formation. It entails the ejection of matter through molecular outflows, which disturbs the protostellar clump. Studying these outflows and the shocked gas caused by them is the key to a better understanding of this process. Aims: The present study aims to characterise the behaviour of molecular outflows in the most massive protostellar sources in the southern Galaxy by looking for evolutionary trends and associating the presence of shocked gas with outflow activity. Methods: We present APEX SEPIA180 (Band 5) observations (beamwidth ~36″) of SiO(4-3) molecular outflow candidates towards a well-selected sample of 32 luminous and dense clumps, which are candidates for harbouring hot molecular cores. We study the emission of the SiO(4-3) line, which is an unambiguous tracer of shocked gas, and recent and active outflow activity, as well as the HCO+(2-1) and H13CO+(2-1) lines. Results: Results show that 78% of our sample (25 sources) present SiO emission, revealing the presence of shocked gas. Nine of these sources are also found to have wings in the HCO+(2-1) line, indicating outflow activity. The SiO emission of these nine sources is generally more intense (Ta > 1 K) and wider (~61 km s−1 FWZP) than the rest of the clumps with SiO detection (~42 km s−1 FWZP), suggesting that the outflows in this group are faster and more energetic. This indicates that the shocked material gets dispersed as the core evolves and outflow activity decreases. Three positive linear correlations are found: a weak one (between the bolometric luminosity and outflow power) and two strong ones (one between the outflow power and the rate of matter expulsion and the other between the kinetic energy and outflow mass). These correlations suggest that more energetic outflows are able to mobilise more material. No correlation was found between the evolutionary stage indicator L/M and SiO outflow properties, supporting that molecular outflows happen throughout the whole high-mass star formation process. Conclusions: We conclude that sources with both SiO emission and HCO+ wings and sources with only SiO emission are in an advanced stage of evolution in the high-mass star formation process, and there is no clear evolutionary difference between them. The former present more massive and more powerful SiO outflows than the latter. Therefore, looking for more outflow signatures such as HCO+ wings could help identify more massive and active massive star-forming regions in samples of similarly evolved sources, and could also help identify sources with older outflow activity.
Fil: Guerra Varas, N.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Merello, M.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Bronfman, L.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
Fil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Elia, D.. No especifíca;
Fil: Finger, R.. Universidad de Chile; Chile
Fil: Mendoza, E.. Universidad de Huelva; España
description Context. High-mass star formation is far less understood than low-mass star formation. It entails the ejection of matter through molecular outflows, which disturbs the protostellar clump. Studying these outflows and the shocked gas caused by them is the key to a better understanding of this process. Aims: The present study aims to characterise the behaviour of molecular outflows in the most massive protostellar sources in the southern Galaxy by looking for evolutionary trends and associating the presence of shocked gas with outflow activity. Methods: We present APEX SEPIA180 (Band 5) observations (beamwidth ~36″) of SiO(4-3) molecular outflow candidates towards a well-selected sample of 32 luminous and dense clumps, which are candidates for harbouring hot molecular cores. We study the emission of the SiO(4-3) line, which is an unambiguous tracer of shocked gas, and recent and active outflow activity, as well as the HCO+(2-1) and H13CO+(2-1) lines. Results: Results show that 78% of our sample (25 sources) present SiO emission, revealing the presence of shocked gas. Nine of these sources are also found to have wings in the HCO+(2-1) line, indicating outflow activity. The SiO emission of these nine sources is generally more intense (Ta > 1 K) and wider (~61 km s−1 FWZP) than the rest of the clumps with SiO detection (~42 km s−1 FWZP), suggesting that the outflows in this group are faster and more energetic. This indicates that the shocked material gets dispersed as the core evolves and outflow activity decreases. Three positive linear correlations are found: a weak one (between the bolometric luminosity and outflow power) and two strong ones (one between the outflow power and the rate of matter expulsion and the other between the kinetic energy and outflow mass). These correlations suggest that more energetic outflows are able to mobilise more material. No correlation was found between the evolutionary stage indicator L/M and SiO outflow properties, supporting that molecular outflows happen throughout the whole high-mass star formation process. Conclusions: We conclude that sources with both SiO emission and HCO+ wings and sources with only SiO emission are in an advanced stage of evolution in the high-mass star formation process, and there is no clear evolutionary difference between them. The former present more massive and more powerful SiO outflows than the latter. Therefore, looking for more outflow signatures such as HCO+ wings could help identify more massive and active massive star-forming regions in samples of similarly evolved sources, and could also help identify sources with older outflow activity.
publishDate 2023
dc.date.none.fl_str_mv 2023-09
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/11336/236085
Guerra Varas, N.; Merello, M.; Bronfman, L.; Duronea, Nicolas Urbano; Elia, D.; et al.; SiO outflows in the most luminous and massive protostellar sources of the southern sky; EDP Sciences; Astronomy and Astrophysics; 677; A148; 9-2023; 1-23
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/236085
identifier_str_mv Guerra Varas, N.; Merello, M.; Bronfman, L.; Duronea, Nicolas Urbano; Elia, D.; et al.; SiO outflows in the most luminous and massive protostellar sources of the southern sky; EDP Sciences; Astronomy and Astrophysics; 677; A148; 9-2023; 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/doi/10.1051/0004-6361/202245522
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/09/aa45522-22/aa45522-22.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
_version_ 1844613592274436096
score 13.070432