870 μm continuum observations of the bubble-shaped nebula Gum 31

Autores
Duronea, Nicolás Urbano; Vasquez, Javier; Gómez, L.; Cappa, Cristina Elisabet; Firpo, Verónica; López Caraballo, C. H.; Rubio, Mónica
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We present here a study of the cold dust in the close environs of the ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, which was probably triggered by the expansion of the ionization front against its environment. Methods. We make use of 870 μm emission data obtained with the Large APEX Bolometer Camera (LABOCA) to map the dust emission. The 870 μm emission provides an excellent probe of mass and density of dense molecular clouds. The obtained LABOCA image was compared to archival infrared, radio continuum, and optical images. Results. The 870 μm emission follows the 8 μm (Spitzer), 250 μm, and 500 μm (Herschel) emission distributions showing the classical morphology of a two-dimensional projection of a spherical shell. We use the 870 μm and 250 μm images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 M and 2800 M, and volume densities between 1.1 × 103 cm-3 and ~2.04 × 105 cm-3. The total mass of the clumps is ~37 600 M. The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the Hii region it reaches ~40 K. The clump mass distribution for the sample is fitted by a power law dN/dlog (M/M) ∝ M, with α = 0.93 ± 0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 μm emission shows that only 37% of them lie in or above the high-mass star formation threshold. Most of this 37% have candidate YSOs projected inside their limits. A comparison of the dynamical age of the Hii region with the fragmentation time, allowed us to conclude that the collect-and-collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may be acting simultaneously. The position of the identified young stellar objects in the region is also a strong indicator that the collect-and-collapse process is acting.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
Materia
Ciencias Astronómicas
HII regions
Infrared: ISM
ISM: bubbles
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/86448

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/86448
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 870 μm continuum observations of the bubble-shaped nebula Gum 31Duronea, Nicolás UrbanoVasquez, JavierGómez, L.Cappa, Cristina ElisabetFirpo, VerónicaLópez Caraballo, C. H.Rubio, MónicaCiencias AstronómicasHII regionsInfrared: ISMISM: bubblesAims. We present here a study of the cold dust in the close environs of the ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, which was probably triggered by the expansion of the ionization front against its environment. Methods. We make use of 870 μm emission data obtained with the Large APEX Bolometer Camera (LABOCA) to map the dust emission. The 870 μm emission provides an excellent probe of mass and density of dense molecular clouds. The obtained LABOCA image was compared to archival infrared, radio continuum, and optical images. Results. The 870 μm emission follows the 8 μm (<i>Spitzer</i>), 250 μm, and 500 μm (<i>Herschel</i>) emission distributions showing the classical morphology of a two-dimensional projection of a spherical shell. We use the 870 μm and 250 μm images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 M<sub>⊙</sub> and 2800 M<sub>⊙</sub>, and volume densities between 1.1 × 10<SUP>3</SUP> cm<SUP>-3</SUP> and ~2.04 × 10<SUP>5</SUP> cm<SUP>-3</SUP>. The total mass of the clumps is ~37 600 M<sub>⊙</sub>. The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the Hii region it reaches ~40 K. The clump mass distribution for the sample is fitted by a power law dN/dlog (M/M<sub>⊙</sub>) ∝ M<SUP>-α</SUP>, with α = 0.93 ± 0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 μm emission shows that only 37% of them lie in or above the high-mass star formation threshold. Most of this 37% have candidate YSOs projected inside their limits. A comparison of the dynamical age of the Hii region with the fragmentation time, allowed us to conclude that the collect-and-collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may be acting simultaneously. The position of the identified young stellar objects in the region is also a strong indicator that the collect-and-collapse process is acting.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2015info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/86448enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201424724info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:54Zoai:sedici.unlp.edu.ar:10915/86448Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:54.54SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv 870 μm continuum observations of the bubble-shaped nebula Gum 31
title 870 μm continuum observations of the bubble-shaped nebula Gum 31
spellingShingle 870 μm continuum observations of the bubble-shaped nebula Gum 31
Duronea, Nicolás Urbano
Ciencias Astronómicas
HII regions
Infrared: ISM
ISM: bubbles
title_short 870 μm continuum observations of the bubble-shaped nebula Gum 31
title_full 870 μm continuum observations of the bubble-shaped nebula Gum 31
title_fullStr 870 μm continuum observations of the bubble-shaped nebula Gum 31
title_full_unstemmed 870 μm continuum observations of the bubble-shaped nebula Gum 31
title_sort 870 μm continuum observations of the bubble-shaped nebula Gum 31
dc.creator.none.fl_str_mv Duronea, Nicolás Urbano
Vasquez, Javier
Gómez, L.
Cappa, Cristina Elisabet
Firpo, Verónica
López Caraballo, C. H.
Rubio, Mónica
author Duronea, Nicolás Urbano
author_facet Duronea, Nicolás Urbano
Vasquez, Javier
Gómez, L.
Cappa, Cristina Elisabet
Firpo, Verónica
López Caraballo, C. H.
Rubio, Mónica
author_role author
author2 Vasquez, Javier
Gómez, L.
Cappa, Cristina Elisabet
Firpo, Verónica
López Caraballo, C. H.
Rubio, Mónica
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
HII regions
Infrared: ISM
ISM: bubbles
topic Ciencias Astronómicas
HII regions
Infrared: ISM
ISM: bubbles
dc.description.none.fl_txt_mv Aims. We present here a study of the cold dust in the close environs of the ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, which was probably triggered by the expansion of the ionization front against its environment. Methods. We make use of 870 μm emission data obtained with the Large APEX Bolometer Camera (LABOCA) to map the dust emission. The 870 μm emission provides an excellent probe of mass and density of dense molecular clouds. The obtained LABOCA image was compared to archival infrared, radio continuum, and optical images. Results. The 870 μm emission follows the 8 μm (<i>Spitzer</i>), 250 μm, and 500 μm (<i>Herschel</i>) emission distributions showing the classical morphology of a two-dimensional projection of a spherical shell. We use the 870 μm and 250 μm images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 M<sub>⊙</sub> and 2800 M<sub>⊙</sub>, and volume densities between 1.1 × 10<SUP>3</SUP> cm<SUP>-3</SUP> and ~2.04 × 10<SUP>5</SUP> cm<SUP>-3</SUP>. The total mass of the clumps is ~37 600 M<sub>⊙</sub>. The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the Hii region it reaches ~40 K. The clump mass distribution for the sample is fitted by a power law dN/dlog (M/M<sub>⊙</sub>) ∝ M<SUP>-α</SUP>, with α = 0.93 ± 0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 μm emission shows that only 37% of them lie in or above the high-mass star formation threshold. Most of this 37% have candidate YSOs projected inside their limits. A comparison of the dynamical age of the Hii region with the fragmentation time, allowed us to conclude that the collect-and-collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may be acting simultaneously. The position of the identified young stellar objects in the region is also a strong indicator that the collect-and-collapse process is acting.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
description Aims. We present here a study of the cold dust in the close environs of the ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, which was probably triggered by the expansion of the ionization front against its environment. Methods. We make use of 870 μm emission data obtained with the Large APEX Bolometer Camera (LABOCA) to map the dust emission. The 870 μm emission provides an excellent probe of mass and density of dense molecular clouds. The obtained LABOCA image was compared to archival infrared, radio continuum, and optical images. Results. The 870 μm emission follows the 8 μm (<i>Spitzer</i>), 250 μm, and 500 μm (<i>Herschel</i>) emission distributions showing the classical morphology of a two-dimensional projection of a spherical shell. We use the 870 μm and 250 μm images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 M<sub>⊙</sub> and 2800 M<sub>⊙</sub>, and volume densities between 1.1 × 10<SUP>3</SUP> cm<SUP>-3</SUP> and ~2.04 × 10<SUP>5</SUP> cm<SUP>-3</SUP>. The total mass of the clumps is ~37 600 M<sub>⊙</sub>. The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the Hii region it reaches ~40 K. The clump mass distribution for the sample is fitted by a power law dN/dlog (M/M<sub>⊙</sub>) ∝ M<SUP>-α</SUP>, with α = 0.93 ± 0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 μm emission shows that only 37% of them lie in or above the high-mass star formation threshold. Most of this 37% have candidate YSOs projected inside their limits. A comparison of the dynamical age of the Hii region with the fragmentation time, allowed us to conclude that the collect-and-collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may be acting simultaneously. The position of the identified young stellar objects in the region is also a strong indicator that the collect-and-collapse process is acting.
publishDate 2015
dc.date.none.fl_str_mv 2015
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/86448
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dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201424724
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
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