The Sagittarius stellar stream embedded in a fermionic dark matter halo

Autores
Collazo, Santiago; Mestre, Martin Federico; Argüelles, Carlos Raúl
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Stellar streams are essential tracers of the gravitational potential of the Milky Way, with key implications for the problem of dark matter model distributions, either within or beyond phenomenological ΛCDM halos. Aims. For the first time in the literature, a dark matter (DM) halo model based on first physical principles such as (quantum) statistical mechanics and thermodynamics is used to try to reproduce the 6D observations of the Sagittarius (Sgr) stream. Thus, we aim to extract quantitative and qualitative conclusions on how well our assumptions stand with respect to the observations. We model both DM halos, the one of the Sgr dwarf and the one of its host, with a spherical self-gravitating system of neutral fermions that accounts for the effects of particle escape and fermion degeneracy (due to the Pauli exclusion principle), the latter causing a high-density core at the center of the halo. Full baryonic components for each galaxy are also considered. Methods. We used a spray algorithm with ∼ 10^5 particles to generate the Sgr tidal debris, which evolves in the combined gravitational potential of the host-progenitor system, to then make a direct comparison with the full phase-space data of the stream. We repeated this kind of simulation for different parameter setups of the fermionic model including the particle mass, with special attention to testing different DM halo morphologies allowed by the physics, including polytropic density tails as well as power-law-like trends. Results. We find that the fermionic halo models considered can only reproduce the trailing arm of the Sgr stream. Within the observationally allowed span of enclosed masses where the stream moves, neither the power-law-like nor the polytropic behavior of the fermionic halo models can answer for the observed trend of the leading tail ? a conclusion that is shared by former analyses using other types of spherically symmetric halos. Thus, we conclude that further model improvements, such as abandoning spherical symmetry and including the Large Magellanic Cloud perturber, are needed for the proper modeling of the overall Milky Way potential within this kind of first-principle halo model.
Fil: Collazo, Santiago. 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
Fil: Mestre, Martin Federico. 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
Fil: Argüelles, Carlos Raúl. 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
Materia
GALAXY: HALO
GALAXY: KINEMATICS & DYNAMICS
DARK MATTER
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:11336/290892
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The Sagittarius stellar stream embedded in a fermionic dark matter haloCollazo, SantiagoMestre, Martin FedericoArgüelles, Carlos RaúlGALAXY: HALOGALAXY: KINEMATICS & DYNAMICSDARK MATTERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Stellar streams are essential tracers of the gravitational potential of the Milky Way, with key implications for the problem of dark matter model distributions, either within or beyond phenomenological ΛCDM halos. Aims. For the first time in the literature, a dark matter (DM) halo model based on first physical principles such as (quantum) statistical mechanics and thermodynamics is used to try to reproduce the 6D observations of the Sagittarius (Sgr) stream. Thus, we aim to extract quantitative and qualitative conclusions on how well our assumptions stand with respect to the observations. We model both DM halos, the one of the Sgr dwarf and the one of its host, with a spherical self-gravitating system of neutral fermions that accounts for the effects of particle escape and fermion degeneracy (due to the Pauli exclusion principle), the latter causing a high-density core at the center of the halo. Full baryonic components for each galaxy are also considered. Methods. We used a spray algorithm with ∼ 10^5 particles to generate the Sgr tidal debris, which evolves in the combined gravitational potential of the host-progenitor system, to then make a direct comparison with the full phase-space data of the stream. We repeated this kind of simulation for different parameter setups of the fermionic model including the particle mass, with special attention to testing different DM halo morphologies allowed by the physics, including polytropic density tails as well as power-law-like trends. Results. We find that the fermionic halo models considered can only reproduce the trailing arm of the Sgr stream. Within the observationally allowed span of enclosed masses where the stream moves, neither the power-law-like nor the polytropic behavior of the fermionic halo models can answer for the observed trend of the leading tail ? a conclusion that is shared by former analyses using other types of spherically symmetric halos. Thus, we conclude that further model improvements, such as abandoning spherical symmetry and including the Large Magellanic Cloud perturber, are needed for the proper modeling of the overall Milky Way potential within this kind of first-principle halo model.Fil: Collazo, Santiago. 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; ArgentinaFil: Mestre, Martin Federico. 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; ArgentinaFil: Argüelles, Carlos Raúl. 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; ArgentinaEDP Sciences2025-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/290892Collazo, Santiago; Mestre, Martin Federico; Argüelles, Carlos Raúl; The Sagittarius stellar stream embedded in a fermionic dark matter halo; EDP Sciences; Astronomy and Astrophysics; 699; 7-2025; 1-140004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2025/07/aa50867-24/aa50867-24.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450867info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T14:44:27Zoai:ri.conicet.gov.ar:11336/290892instacron: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:34982026-08-25 14:44:27.522CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The Sagittarius stellar stream embedded in a fermionic dark matter halo
title The Sagittarius stellar stream embedded in a fermionic dark matter halo
spellingShingle The Sagittarius stellar stream embedded in a fermionic dark matter halo
Collazo, Santiago
GALAXY: HALO
GALAXY: KINEMATICS & DYNAMICS
DARK MATTER
title_short The Sagittarius stellar stream embedded in a fermionic dark matter halo
title_full The Sagittarius stellar stream embedded in a fermionic dark matter halo
title_fullStr The Sagittarius stellar stream embedded in a fermionic dark matter halo
title_full_unstemmed The Sagittarius stellar stream embedded in a fermionic dark matter halo
title_sort The Sagittarius stellar stream embedded in a fermionic dark matter halo
dc.creator.none.fl_str_mv Collazo, Santiago
Mestre, Martin Federico
Argüelles, Carlos Raúl
author Collazo, Santiago
author_facet Collazo, Santiago
Mestre, Martin Federico
Argüelles, Carlos Raúl
author_role author
author2 Mestre, Martin Federico
Argüelles, Carlos Raúl
author2_role author
author
dc.subject.none.fl_str_mv GALAXY: HALO
GALAXY: KINEMATICS & DYNAMICS
DARK MATTER
topic GALAXY: HALO
GALAXY: KINEMATICS & DYNAMICS
DARK MATTER
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. Stellar streams are essential tracers of the gravitational potential of the Milky Way, with key implications for the problem of dark matter model distributions, either within or beyond phenomenological ΛCDM halos. Aims. For the first time in the literature, a dark matter (DM) halo model based on first physical principles such as (quantum) statistical mechanics and thermodynamics is used to try to reproduce the 6D observations of the Sagittarius (Sgr) stream. Thus, we aim to extract quantitative and qualitative conclusions on how well our assumptions stand with respect to the observations. We model both DM halos, the one of the Sgr dwarf and the one of its host, with a spherical self-gravitating system of neutral fermions that accounts for the effects of particle escape and fermion degeneracy (due to the Pauli exclusion principle), the latter causing a high-density core at the center of the halo. Full baryonic components for each galaxy are also considered. Methods. We used a spray algorithm with ∼ 10^5 particles to generate the Sgr tidal debris, which evolves in the combined gravitational potential of the host-progenitor system, to then make a direct comparison with the full phase-space data of the stream. We repeated this kind of simulation for different parameter setups of the fermionic model including the particle mass, with special attention to testing different DM halo morphologies allowed by the physics, including polytropic density tails as well as power-law-like trends. Results. We find that the fermionic halo models considered can only reproduce the trailing arm of the Sgr stream. Within the observationally allowed span of enclosed masses where the stream moves, neither the power-law-like nor the polytropic behavior of the fermionic halo models can answer for the observed trend of the leading tail ? a conclusion that is shared by former analyses using other types of spherically symmetric halos. Thus, we conclude that further model improvements, such as abandoning spherical symmetry and including the Large Magellanic Cloud perturber, are needed for the proper modeling of the overall Milky Way potential within this kind of first-principle halo model.
Fil: Collazo, Santiago. 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
Fil: Mestre, Martin Federico. 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
Fil: Argüelles, Carlos Raúl. 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
description Context. Stellar streams are essential tracers of the gravitational potential of the Milky Way, with key implications for the problem of dark matter model distributions, either within or beyond phenomenological ΛCDM halos. Aims. For the first time in the literature, a dark matter (DM) halo model based on first physical principles such as (quantum) statistical mechanics and thermodynamics is used to try to reproduce the 6D observations of the Sagittarius (Sgr) stream. Thus, we aim to extract quantitative and qualitative conclusions on how well our assumptions stand with respect to the observations. We model both DM halos, the one of the Sgr dwarf and the one of its host, with a spherical self-gravitating system of neutral fermions that accounts for the effects of particle escape and fermion degeneracy (due to the Pauli exclusion principle), the latter causing a high-density core at the center of the halo. Full baryonic components for each galaxy are also considered. Methods. We used a spray algorithm with ∼ 10^5 particles to generate the Sgr tidal debris, which evolves in the combined gravitational potential of the host-progenitor system, to then make a direct comparison with the full phase-space data of the stream. We repeated this kind of simulation for different parameter setups of the fermionic model including the particle mass, with special attention to testing different DM halo morphologies allowed by the physics, including polytropic density tails as well as power-law-like trends. Results. We find that the fermionic halo models considered can only reproduce the trailing arm of the Sgr stream. Within the observationally allowed span of enclosed masses where the stream moves, neither the power-law-like nor the polytropic behavior of the fermionic halo models can answer for the observed trend of the leading tail ? a conclusion that is shared by former analyses using other types of spherically symmetric halos. Thus, we conclude that further model improvements, such as abandoning spherical symmetry and including the Large Magellanic Cloud perturber, are needed for the proper modeling of the overall Milky Way potential within this kind of first-principle halo model.
publishDate 2025
dc.date.none.fl_str_mv 2025-07
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/11336/290892
Collazo, Santiago; Mestre, Martin Federico; Argüelles, Carlos Raúl; The Sagittarius stellar stream embedded in a fermionic dark matter halo; EDP Sciences; Astronomy and Astrophysics; 699; 7-2025; 1-14
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/290892
identifier_str_mv Collazo, Santiago; Mestre, Martin Federico; Argüelles, Carlos Raúl; The Sagittarius stellar stream embedded in a fermionic dark matter halo; EDP Sciences; Astronomy and Astrophysics; 699; 7-2025; 1-14
0004-6361
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://www.aanda.org/articles/aa/full_html/2025/07/aa50867-24/aa50867-24.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450867
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
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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 13.265058

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