The halo shape and evolution of polar disc galaxies

Autores
Snaith, O. N.; Gibson, B. K.; Brook, C. B.; Knebe, A.; Thacker, R. J.; Quinn, T. R.; Governato, F.; Tissera, Patricia Beatriz
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We examine the properties and evolution of a simulated polar disc galaxy. This galaxy is comprised of two orthogonal discs, one of which contains old stars (old stellar disc), and the other, containing both younger stars and the cold gas (polar disc) of the galaxy. By exploring the shape of the inner region of the dark matter halo, we are able to confirm that the halo shape is a oblate ellipsoid flattened in the direction of the polar disc. We also note that there is a twist in the shape profile, where the innermost 3 kpc of the halo flattens in the direction perpendicular to the old disc, and then aligns with the polar disc out until the virial radius. This result is then compared to the halo shape inferred from the circular velocities of the two discs. We also use the temporal information of the simulation to track the system’s evolution, and identify the processes which give rise to this unusual galaxy type. We confirm the proposal that the polar disc galaxy is the result of the last major merger, where the angular moment of the interaction is orthogonal to the angle of the infalling gas. This merger is followed by the resumption of coherent gas infall. We emphasis that the disc is rapidly restored after the major merger and that after this event the galaxy begins to tilt.A significant proportion of the infalling gas comes from filaments. This infalling gas from the filament gives the gas its angular momentum, and, in the case of the polar disc galaxy, the direction of the gas filament does not change before or after the last major merger.
Fil: Snaith, O. N.. University of Central Lancashire; Reino Unido
Fil: Gibson, B. K.. University of Central Lancashire; Reino Unido
Fil: Brook, C. B.. University of Central Lancashire; Reino Unido
Fil: Knebe, A.. Universidad Autónoma de Madrid; España
Fil: Thacker, R. J.. Saint Mary’s University; Canadá
Fil: Quinn, T. R.. University of Washington; Estados Unidos
Fil: Governato, F.. University of Washington; Estados Unidos
Fil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Materia
galaxy formation
galaxy evolution
cosmology
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:11336/19529
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/19529
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The halo shape and evolution of polar disc galaxiesSnaith, O. N.Gibson, B. K.Brook, C. B.Knebe, A.Thacker, R. J.Quinn, T. R.Governato, F.Tissera, Patricia Beatrizgalaxy formationgalaxy evolutioncosmologyhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We examine the properties and evolution of a simulated polar disc galaxy. This galaxy is comprised of two orthogonal discs, one of which contains old stars (old stellar disc), and the other, containing both younger stars and the cold gas (polar disc) of the galaxy. By exploring the shape of the inner region of the dark matter halo, we are able to confirm that the halo shape is a oblate ellipsoid flattened in the direction of the polar disc. We also note that there is a twist in the shape profile, where the innermost 3 kpc of the halo flattens in the direction perpendicular to the old disc, and then aligns with the polar disc out until the virial radius. This result is then compared to the halo shape inferred from the circular velocities of the two discs. We also use the temporal information of the simulation to track the system’s evolution, and identify the processes which give rise to this unusual galaxy type. We confirm the proposal that the polar disc galaxy is the result of the last major merger, where the angular moment of the interaction is orthogonal to the angle of the infalling gas. This merger is followed by the resumption of coherent gas infall. We emphasis that the disc is rapidly restored after the major merger and that after this event the galaxy begins to tilt.A significant proportion of the infalling gas comes from filaments. This infalling gas from the filament gives the gas its angular momentum, and, in the case of the polar disc galaxy, the direction of the gas filament does not change before or after the last major merger.Fil: Snaith, O. N.. University of Central Lancashire; Reino UnidoFil: Gibson, B. K.. University of Central Lancashire; Reino UnidoFil: Brook, C. B.. University of Central Lancashire; Reino UnidoFil: Knebe, A.. Universidad Autónoma de Madrid; EspañaFil: Thacker, R. J.. Saint Mary’s University; CanadáFil: Quinn, T. R.. University of Washington; Estados UnidosFil: Governato, F.. University of Washington; Estados UnidosFil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaOxford University Press2012-09-21info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19529Snaith, O. N.; Gibson, B. K.; Brook, C. B.; Knebe, A.; Thacker, R. J.; et al.; The halo shape and evolution of polar disc galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 425; 3; 21-9-2012; 1967-19790035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2012.21518.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/425/3/1967/981599/The-halo-shape-and-evolution-of-polar-disc?searchresult=1info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1206.5570info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:01:24Zoai:ri.conicet.gov.ar:11336/19529instacron: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:34982025-09-10 13:01:25.082CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The halo shape and evolution of polar disc galaxies
title The halo shape and evolution of polar disc galaxies
spellingShingle The halo shape and evolution of polar disc galaxies
Snaith, O. N.
galaxy formation
galaxy evolution
cosmology
title_short The halo shape and evolution of polar disc galaxies
title_full The halo shape and evolution of polar disc galaxies
title_fullStr The halo shape and evolution of polar disc galaxies
title_full_unstemmed The halo shape and evolution of polar disc galaxies
title_sort The halo shape and evolution of polar disc galaxies
dc.creator.none.fl_str_mv Snaith, O. N.
Gibson, B. K.
Brook, C. B.
Knebe, A.
Thacker, R. J.
Quinn, T. R.
Governato, F.
Tissera, Patricia Beatriz
author Snaith, O. N.
author_facet Snaith, O. N.
Gibson, B. K.
Brook, C. B.
Knebe, A.
Thacker, R. J.
Quinn, T. R.
Governato, F.
Tissera, Patricia Beatriz
author_role author
author2 Gibson, B. K.
Brook, C. B.
Knebe, A.
Thacker, R. J.
Quinn, T. R.
Governato, F.
Tissera, Patricia Beatriz
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv galaxy formation
galaxy evolution
cosmology
topic galaxy formation
galaxy evolution
cosmology
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 examine the properties and evolution of a simulated polar disc galaxy. This galaxy is comprised of two orthogonal discs, one of which contains old stars (old stellar disc), and the other, containing both younger stars and the cold gas (polar disc) of the galaxy. By exploring the shape of the inner region of the dark matter halo, we are able to confirm that the halo shape is a oblate ellipsoid flattened in the direction of the polar disc. We also note that there is a twist in the shape profile, where the innermost 3 kpc of the halo flattens in the direction perpendicular to the old disc, and then aligns with the polar disc out until the virial radius. This result is then compared to the halo shape inferred from the circular velocities of the two discs. We also use the temporal information of the simulation to track the system’s evolution, and identify the processes which give rise to this unusual galaxy type. We confirm the proposal that the polar disc galaxy is the result of the last major merger, where the angular moment of the interaction is orthogonal to the angle of the infalling gas. This merger is followed by the resumption of coherent gas infall. We emphasis that the disc is rapidly restored after the major merger and that after this event the galaxy begins to tilt.A significant proportion of the infalling gas comes from filaments. This infalling gas from the filament gives the gas its angular momentum, and, in the case of the polar disc galaxy, the direction of the gas filament does not change before or after the last major merger.
Fil: Snaith, O. N.. University of Central Lancashire; Reino Unido
Fil: Gibson, B. K.. University of Central Lancashire; Reino Unido
Fil: Brook, C. B.. University of Central Lancashire; Reino Unido
Fil: Knebe, A.. Universidad Autónoma de Madrid; España
Fil: Thacker, R. J.. Saint Mary’s University; Canadá
Fil: Quinn, T. R.. University of Washington; Estados Unidos
Fil: Governato, F.. University of Washington; Estados Unidos
Fil: Tissera, Patricia Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
description We examine the properties and evolution of a simulated polar disc galaxy. This galaxy is comprised of two orthogonal discs, one of which contains old stars (old stellar disc), and the other, containing both younger stars and the cold gas (polar disc) of the galaxy. By exploring the shape of the inner region of the dark matter halo, we are able to confirm that the halo shape is a oblate ellipsoid flattened in the direction of the polar disc. We also note that there is a twist in the shape profile, where the innermost 3 kpc of the halo flattens in the direction perpendicular to the old disc, and then aligns with the polar disc out until the virial radius. This result is then compared to the halo shape inferred from the circular velocities of the two discs. We also use the temporal information of the simulation to track the system’s evolution, and identify the processes which give rise to this unusual galaxy type. We confirm the proposal that the polar disc galaxy is the result of the last major merger, where the angular moment of the interaction is orthogonal to the angle of the infalling gas. This merger is followed by the resumption of coherent gas infall. We emphasis that the disc is rapidly restored after the major merger and that after this event the galaxy begins to tilt.A significant proportion of the infalling gas comes from filaments. This infalling gas from the filament gives the gas its angular momentum, and, in the case of the polar disc galaxy, the direction of the gas filament does not change before or after the last major merger.
publishDate 2012
dc.date.none.fl_str_mv 2012-09-21
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/11336/19529
Snaith, O. N.; Gibson, B. K.; Brook, C. B.; Knebe, A.; Thacker, R. J.; et al.; The halo shape and evolution of polar disc galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 425; 3; 21-9-2012; 1967-1979
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/19529
identifier_str_mv Snaith, O. N.; Gibson, B. K.; Brook, C. B.; Knebe, A.; Thacker, R. J.; et al.; The halo shape and evolution of polar disc galaxies; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 425; 3; 21-9-2012; 1967-1979
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2012.21518.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/425/3/1967/981599/The-halo-shape-and-evolution-of-polar-disc?searchresult=1
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1206.5570
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
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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 13.004268

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