The interstellar medium surrounding the Scorpius-Centaurus association revisited

Autores
Pöppel, Wolfgang; Bajaja, Esteban; Arnal, Edmundo Marcelo; Morras, Ricardo
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We want to make a large-scale study of the morphology, kinematics, and origin of the HI, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern HI survey with the Leiden/Dwingeloo Survey, considering l = 240°-400°, b =-60° to +60°, and radial velocities of V =-41.8 to +40.8 kms-1.We point out the main HI branches surrounding the association and derive their kinematics. Kinematical HI-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical HI shells were fitted around each stellar subgroup. Results. The expanding ring of HI associated with the Gould Belt (GB) is very prominent. At each l, its radial velocity shifts ∼-7 kms-1 within an interval Δb ∼ 10°-25°. On the sky, the shifts occur within a narrow stripe extending between l. b ∼ 250°.-18° and 400°. +50°. The ranges of distances and radial thicknesses of most HI branches are nearly 70-160 pc and 40-90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocity V ∼-6.6 kms-1 at d = 76 pc from the Sun, covering about 102° × 65° (l. b), forming an "HI-wall". There are streamers at V ∼-15 to-35 km s-1, as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at Mt ∼ 368 000 M⊙ ± 60%, including ∼34 000 M⊙ of associated H2 and 30% of He. About 39% of the embedding gas was shocked by the association. At |b|≥35°, a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
open clusters and associations: individual: Sco-Cen association
open clusters and associations: individual: Gould Belt
ISM: clouds
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:10915/82506

id SEDICI_793c4031480cc8ca802a128a335dcc55
oai_identifier_str oai:sedici.unlp.edu.ar:10915/82506
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling The interstellar medium surrounding the Scorpius-Centaurus association revisitedPöppel, WolfgangBajaja, EstebanArnal, Edmundo MarceloMorras, RicardoCiencias Astronómicasopen clusters and associations: individual: Sco-Cen associationopen clusters and associations: individual: Gould BeltISM: cloudsAims. We want to make a large-scale study of the morphology, kinematics, and origin of the HI, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern HI survey with the Leiden/Dwingeloo Survey, considering l = 240°-400°, b =-60° to +60°, and radial velocities of V =-41.8 to +40.8 kms<SUP>-1</SUP>.We point out the main HI branches surrounding the association and derive their kinematics. Kinematical HI-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical HI shells were fitted around each stellar subgroup. Results. The expanding ring of HI associated with the Gould Belt (GB) is very prominent. At each l, its radial velocity shifts ∼-7 kms<SUP>-1</SUP> within an interval Δb ∼ 10°-25°. On the sky, the shifts occur within a narrow stripe extending between l. b ∼ 250°.-18° and 400°. +50°. The ranges of distances and radial thicknesses of most HI branches are nearly 70-160 pc and 40-90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocity V ∼-6.6 kms<SUP>-1</SUP> at d = 76 pc from the Sun, covering about 102° × 65° (l. b), forming an "HI-wall". There are streamers at V ∼-15 to-35 km s<SUP>-1</SUP>, as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at M<SUB>t</SUB> ∼ 368 000 M⊙ ± 60%, including ∼34 000 M⊙ of associated H<SUB>2</SUB> and 30% of He. About 39% of the embedding gas was shocked by the association. At |b|≥35°, a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.Facultad de Ciencias Astronómicas y Geofísicas2010info: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/10915/82506enginfo:eu-repo/semantics/altIdentifier/issn/00046361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200811290info: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:UNLP2025-09-29T11:15:31Zoai:sedici.unlp.edu.ar:10915/82506Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:31.372SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The interstellar medium surrounding the Scorpius-Centaurus association revisited
title The interstellar medium surrounding the Scorpius-Centaurus association revisited
spellingShingle The interstellar medium surrounding the Scorpius-Centaurus association revisited
Pöppel, Wolfgang
Ciencias Astronómicas
open clusters and associations: individual: Sco-Cen association
open clusters and associations: individual: Gould Belt
ISM: clouds
title_short The interstellar medium surrounding the Scorpius-Centaurus association revisited
title_full The interstellar medium surrounding the Scorpius-Centaurus association revisited
title_fullStr The interstellar medium surrounding the Scorpius-Centaurus association revisited
title_full_unstemmed The interstellar medium surrounding the Scorpius-Centaurus association revisited
title_sort The interstellar medium surrounding the Scorpius-Centaurus association revisited
dc.creator.none.fl_str_mv Pöppel, Wolfgang
Bajaja, Esteban
Arnal, Edmundo Marcelo
Morras, Ricardo
author Pöppel, Wolfgang
author_facet Pöppel, Wolfgang
Bajaja, Esteban
Arnal, Edmundo Marcelo
Morras, Ricardo
author_role author
author2 Bajaja, Esteban
Arnal, Edmundo Marcelo
Morras, Ricardo
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
open clusters and associations: individual: Sco-Cen association
open clusters and associations: individual: Gould Belt
ISM: clouds
topic Ciencias Astronómicas
open clusters and associations: individual: Sco-Cen association
open clusters and associations: individual: Gould Belt
ISM: clouds
dc.description.none.fl_txt_mv Aims. We want to make a large-scale study of the morphology, kinematics, and origin of the HI, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern HI survey with the Leiden/Dwingeloo Survey, considering l = 240°-400°, b =-60° to +60°, and radial velocities of V =-41.8 to +40.8 kms<SUP>-1</SUP>.We point out the main HI branches surrounding the association and derive their kinematics. Kinematical HI-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical HI shells were fitted around each stellar subgroup. Results. The expanding ring of HI associated with the Gould Belt (GB) is very prominent. At each l, its radial velocity shifts ∼-7 kms<SUP>-1</SUP> within an interval Δb ∼ 10°-25°. On the sky, the shifts occur within a narrow stripe extending between l. b ∼ 250°.-18° and 400°. +50°. The ranges of distances and radial thicknesses of most HI branches are nearly 70-160 pc and 40-90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocity V ∼-6.6 kms<SUP>-1</SUP> at d = 76 pc from the Sun, covering about 102° × 65° (l. b), forming an "HI-wall". There are streamers at V ∼-15 to-35 km s<SUP>-1</SUP>, as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at M<SUB>t</SUB> ∼ 368 000 M⊙ ± 60%, including ∼34 000 M⊙ of associated H<SUB>2</SUB> and 30% of He. About 39% of the embedding gas was shocked by the association. At |b|≥35°, a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.
Facultad de Ciencias Astronómicas y Geofísicas
description Aims. We want to make a large-scale study of the morphology, kinematics, and origin of the HI, which surrounds the Sco-Cen association. Methods. We combine our high-sensitivity southern HI survey with the Leiden/Dwingeloo Survey, considering l = 240°-400°, b =-60° to +60°, and radial velocities of V =-41.8 to +40.8 kms<SUP>-1</SUP>.We point out the main HI branches surrounding the association and derive their kinematics. Kinematical HI-maps were compared with spatial maps of interstellar (IS) Na I from the literature. Upper limits for distances d were derived from optical IS absorption components from the literature. Models of expanding spherical HI shells were fitted around each stellar subgroup. Results. The expanding ring of HI associated with the Gould Belt (GB) is very prominent. At each l, its radial velocity shifts ∼-7 kms<SUP>-1</SUP> within an interval Δb ∼ 10°-25°. On the sky, the shifts occur within a narrow stripe extending between l. b ∼ 250°.-18° and 400°. +50°. The ranges of distances and radial thicknesses of most HI branches are nearly 70-160 pc and 40-90 pc, respectively. The shell-models fit the main branches. Interactions between the shells built a large expanding bubble with a transverse diameter of nearly 250 pc around the association. The near face is approaching with a mean velocity V ∼-6.6 kms<SUP>-1</SUP> at d = 76 pc from the Sun, covering about 102° × 65° (l. b), forming an "HI-wall". There are streamers at V ∼-15 to-35 km s<SUP>-1</SUP>, as well as gas presumably overshot into Galactic Quadrant II. The receding gas is more tenuous. Conclusions. The association is traversing the ring since a time comparable to its age producing a significant disturbance on the expanding GB-ring of gas. The latter was almost totally shocked by the association, northerly of the stripe of velocity shifts. Southerly there are large amounts of preshocked gas, as well as smaller more localized shocked regions. Hot gas within the bubble produces most of the 1/4 keV radiation detected toward it by ROSAT. The total mass of the GB gas embedding the Sco-Cen association is estimated at M<SUB>t</SUB> ∼ 368 000 M⊙ ± 60%, including ∼34 000 M⊙ of associated H<SUB>2</SUB> and 30% of He. About 39% of the embedding gas was shocked by the association. At |b|≥35°, a comparison of the observations with test points moving on ballistic orbits is consistent with the formation of the Sco-Cen association within the gas ring of the GB and the presumable explosive origin of the latter. The rotation of the ring is assumed.
publishDate 2010
dc.date.none.fl_str_mv 2010
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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