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dc.contributor.author
Guerra Varas, N.
dc.contributor.author
Merello, M.
dc.contributor.author
Bronfman, L.
dc.contributor.author
Duronea, Nicolas Urbano
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dc.contributor.author
Elia, D.
dc.contributor.author
Finger, R.
dc.contributor.author
Mendoza, E.
dc.date.available
2024-05-27T13:38:14Z
dc.date.issued
2023-09
dc.identifier.citation
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
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/236085
dc.description.abstract
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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
stars: formation
dc.subject
stars: massive
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stars: jets and outflows
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
SiO outflows in the most luminous and massive protostellar sources of the southern sky
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2024-05-07T13:30:51Z
dc.journal.volume
677
dc.journal.number
A148
dc.journal.pagination
1-23
dc.journal.pais
Francia
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dc.journal.ciudad
Paris
dc.description.fil
Fil: Guerra Varas, N.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
dc.description.fil
Fil: Merello, M.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
dc.description.fil
Fil: Bronfman, L.. Universidad de Chile. Facultad de Ciencias Físicas y Matemáticas; Chile
dc.description.fil
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
dc.description.fil
Fil: Elia, D.. INAF. IAPS; Italia
dc.description.fil
Fil: Finger, R.. Universidad de Chile; Chile
dc.description.fil
Fil: Mendoza, E.. Universidad de Huelva; España
dc.journal.title
Astronomy and Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/https://doi.org/10.1051/0004-6361/202245522
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/09/aa45522-22/aa45522-22.html
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