Formation imprints in the kinematics of the Milky Way globular cluster system

Autores
Piatti, Andres Eduardo
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We report results on the kinematics of Milky Way (MW) globular clusters (GCs) based on updated space velocities for nearly the entire GC population. We found that a 3D space with the semimajor axis, the eccentricity, and the inclination of the orbit with respect to the MW plane as its axes, is helpful in order to dig into the formation of the GC system. We find that GCs formed in situ show a clear correlation between their eccentricities and their orbital inclination in the sense that clusters with large eccentricities also have large inclinations. These GCs also show a correlation between their distance to the MW center and their eccentricity. Accreted GCs do not exhibit a relationship between eccentricity and inclination, but span a wide variety of inclinations at eccentricities larger than ∼0.5. Finally, we computed the velocity anisotropy β of the GC system and found, for GCs formed in situ, that β decreases from ≈0.8 down to 0.3 from the outermost regions toward the MW center, but remains fairly constant (0.7-0.9) for accreted ones. These findings can be explained if GCs formed from gas that collapsed radially in the outskirts, with a preference for relatively high infall angles. As the material reached the rotating forming disk, it became more circular and moved with a lower inclination relative to the disk. Half of the GC population was accreted and deposited in orbits covering the entire range of energies from the outer halo to the bulge.
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Materia
GALAXY: FORMATION-GALAXY: STRUCTURE-GLOBULAR CLUSTERS: GENERAL
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:11336/128154

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spelling Formation imprints in the kinematics of the Milky Way globular cluster systemPiatti, Andres EduardoGALAXY: FORMATION-GALAXY: STRUCTURE-GLOBULAR CLUSTERS: GENERALhttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1We report results on the kinematics of Milky Way (MW) globular clusters (GCs) based on updated space velocities for nearly the entire GC population. We found that a 3D space with the semimajor axis, the eccentricity, and the inclination of the orbit with respect to the MW plane as its axes, is helpful in order to dig into the formation of the GC system. We find that GCs formed in situ show a clear correlation between their eccentricities and their orbital inclination in the sense that clusters with large eccentricities also have large inclinations. These GCs also show a correlation between their distance to the MW center and their eccentricity. Accreted GCs do not exhibit a relationship between eccentricity and inclination, but span a wide variety of inclinations at eccentricities larger than ∼0.5. Finally, we computed the velocity anisotropy β of the GC system and found, for GCs formed in situ, that β decreases from ≈0.8 down to 0.3 from the outermost regions toward the MW center, but remains fairly constant (0.7-0.9) for accreted ones. These findings can be explained if GCs formed from gas that collapsed radially in the outskirts, with a preference for relatively high infall angles. As the material reached the rotating forming disk, it became more circular and moved with a lower inclination relative to the disk. Half of the GC population was accreted and deposited in orbits covering the entire range of energies from the outer halo to the bulge.Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaIOP Publishing2019-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/128154Piatti, Andres Eduardo; Formation imprints in the kinematics of the Milky Way globular cluster system; IOP Publishing; Astrophysical Journal; 882; 2; 7-20190004-637X1538-4357CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ab3574info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/1907.09824info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ab3574info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:49:35Zoai:ri.conicet.gov.ar:11336/128154instacron: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 09:49:35.482CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Formation imprints in the kinematics of the Milky Way globular cluster system
title Formation imprints in the kinematics of the Milky Way globular cluster system
spellingShingle Formation imprints in the kinematics of the Milky Way globular cluster system
Piatti, Andres Eduardo
GALAXY: FORMATION-GALAXY: STRUCTURE-GLOBULAR CLUSTERS: GENERAL
title_short Formation imprints in the kinematics of the Milky Way globular cluster system
title_full Formation imprints in the kinematics of the Milky Way globular cluster system
title_fullStr Formation imprints in the kinematics of the Milky Way globular cluster system
title_full_unstemmed Formation imprints in the kinematics of the Milky Way globular cluster system
title_sort Formation imprints in the kinematics of the Milky Way globular cluster system
dc.creator.none.fl_str_mv Piatti, Andres Eduardo
author Piatti, Andres Eduardo
author_facet Piatti, Andres Eduardo
author_role author
dc.subject.none.fl_str_mv GALAXY: FORMATION-GALAXY: STRUCTURE-GLOBULAR CLUSTERS: GENERAL
topic GALAXY: FORMATION-GALAXY: STRUCTURE-GLOBULAR CLUSTERS: GENERAL
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We report results on the kinematics of Milky Way (MW) globular clusters (GCs) based on updated space velocities for nearly the entire GC population. We found that a 3D space with the semimajor axis, the eccentricity, and the inclination of the orbit with respect to the MW plane as its axes, is helpful in order to dig into the formation of the GC system. We find that GCs formed in situ show a clear correlation between their eccentricities and their orbital inclination in the sense that clusters with large eccentricities also have large inclinations. These GCs also show a correlation between their distance to the MW center and their eccentricity. Accreted GCs do not exhibit a relationship between eccentricity and inclination, but span a wide variety of inclinations at eccentricities larger than ∼0.5. Finally, we computed the velocity anisotropy β of the GC system and found, for GCs formed in situ, that β decreases from ≈0.8 down to 0.3 from the outermost regions toward the MW center, but remains fairly constant (0.7-0.9) for accreted ones. These findings can be explained if GCs formed from gas that collapsed radially in the outskirts, with a preference for relatively high infall angles. As the material reached the rotating forming disk, it became more circular and moved with a lower inclination relative to the disk. Half of the GC population was accreted and deposited in orbits covering the entire range of energies from the outer halo to the bulge.
Fil: Piatti, Andres Eduardo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza. Instituto Interdisciplinario de Ciencias Básicas. - Universidad Nacional de Cuyo. Instituto Interdisciplinario de Ciencias Básicas; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
description We report results on the kinematics of Milky Way (MW) globular clusters (GCs) based on updated space velocities for nearly the entire GC population. We found that a 3D space with the semimajor axis, the eccentricity, and the inclination of the orbit with respect to the MW plane as its axes, is helpful in order to dig into the formation of the GC system. We find that GCs formed in situ show a clear correlation between their eccentricities and their orbital inclination in the sense that clusters with large eccentricities also have large inclinations. These GCs also show a correlation between their distance to the MW center and their eccentricity. Accreted GCs do not exhibit a relationship between eccentricity and inclination, but span a wide variety of inclinations at eccentricities larger than ∼0.5. Finally, we computed the velocity anisotropy β of the GC system and found, for GCs formed in situ, that β decreases from ≈0.8 down to 0.3 from the outermost regions toward the MW center, but remains fairly constant (0.7-0.9) for accreted ones. These findings can be explained if GCs formed from gas that collapsed radially in the outskirts, with a preference for relatively high infall angles. As the material reached the rotating forming disk, it became more circular and moved with a lower inclination relative to the disk. Half of the GC population was accreted and deposited in orbits covering the entire range of energies from the outer halo to the bulge.
publishDate 2019
dc.date.none.fl_str_mv 2019-07
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/11336/128154
Piatti, Andres Eduardo; Formation imprints in the kinematics of the Milky Way globular cluster system; IOP Publishing; Astrophysical Journal; 882; 2; 7-2019
0004-637X
1538-4357
CONICET Digital
CONICET
url http://hdl.handle.net/11336/128154
identifier_str_mv Piatti, Andres Eduardo; Formation imprints in the kinematics of the Milky Way globular cluster system; IOP Publishing; Astrophysical Journal; 882; 2; 7-2019
0004-637X
1538-4357
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ab3574
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/1907.09824
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ab3574
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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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