What does lie at the Milky Way centre? Insights from the S2-star orbit precession

Autores
Argüelles, Carlos Raúl; Mestre, Martin Federico; Becerra Vergara, E. A.; Crespi, Valentina; Krut, A.; Rueda, J. A.; Ruffini, R.
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
It has been recently demonstrated that both, a classical Schwarzschild black hole (BH), and a dense concentration of self-gravitating fermionic dark matter (DM) placed at the Galaxy centre, can explain the precise astrometric data (positions and radial velocities) of the S-stars orbiting Sgr A∗. This result encompasses the 17 best resolved S-stars, and includes the test of general relativistic effects such as the gravitational redshift in the S2-star. In addition, the DM model features another remarkable result: The dense core of fermions is the central region of a continuous density distribution of DM whose diluted halo explains the Galactic rotation curve. In this Letter, we complement the above findings by analysing in both models the relativistic periapsis precession of the S2-star orbit. While the Schwarzschild BH scenario predicts a unique prograde precession for S2, in the DM scenario, it can be either retrograde or prograde, depending on the amount of DM mass enclosed within the S2 orbit, which, in turn, is a function of the DM fermion mass. We show that all the current and publicly available data of S2 cannot discriminate between the two models, but upcoming S2 astrometry close to next apocentre passage could potentially establish if Sgr A∗ is governed by a classical BH or by a quantum DM system.
Fil: Argüelles, Carlos Raúl. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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: Becerra Vergara, E. A.. Universidad Industrial Santander; Colombia. Università degli studi di Roma "La Sapienza"; Italia
Fil: Crespi, Valentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Krut, A.. Università degli studi di Roma "La Sapienza"; Italia
Fil: Rueda, J. A.. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli studi di Roma "La Sapienza"; Italia
Fil: Ruffini, R.. Università degli studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Astrofisica; Italia. Università di Ferrara; Italia
Materia
DARK MATTER
GALAXY: CENTRE
GALAXY: STRUCTURE
STARS: KINEMATICS AND DYNAMICS
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:11336/211740

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spelling What does lie at the Milky Way centre? Insights from the S2-star orbit precessionArgüelles, Carlos RaúlMestre, Martin FedericoBecerra Vergara, E. A.Crespi, ValentinaKrut, A.Rueda, J. A.Ruffini, R.DARK MATTERGALAXY: CENTREGALAXY: STRUCTURESTARS: KINEMATICS AND DYNAMICShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1It has been recently demonstrated that both, a classical Schwarzschild black hole (BH), and a dense concentration of self-gravitating fermionic dark matter (DM) placed at the Galaxy centre, can explain the precise astrometric data (positions and radial velocities) of the S-stars orbiting Sgr A∗. This result encompasses the 17 best resolved S-stars, and includes the test of general relativistic effects such as the gravitational redshift in the S2-star. In addition, the DM model features another remarkable result: The dense core of fermions is the central region of a continuous density distribution of DM whose diluted halo explains the Galactic rotation curve. In this Letter, we complement the above findings by analysing in both models the relativistic periapsis precession of the S2-star orbit. While the Schwarzschild BH scenario predicts a unique prograde precession for S2, in the DM scenario, it can be either retrograde or prograde, depending on the amount of DM mass enclosed within the S2 orbit, which, in turn, is a function of the DM fermion mass. We show that all the current and publicly available data of S2 cannot discriminate between the two models, but upcoming S2 astrometry close to next apocentre passage could potentially establish if Sgr A∗ is governed by a classical BH or by a quantum DM system.Fil: Argüelles, Carlos Raúl. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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: Becerra Vergara, E. A.. Universidad Industrial Santander; Colombia. Università degli studi di Roma "La Sapienza"; ItaliaFil: Crespi, Valentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; ArgentinaFil: Krut, A.. Università degli studi di Roma "La Sapienza"; ItaliaFil: Rueda, J. A.. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli studi di Roma "La Sapienza"; ItaliaFil: Ruffini, R.. Università degli studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Astrofisica; Italia. Università di Ferrara; ItaliaOxford University Press2022-03info: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/11336/211740Argüelles, Carlos Raúl; Mestre, Martin Federico; Becerra Vergara, E. A.; Crespi, Valentina; Krut, A.; et al.; What does lie at the Milky Way centre? Insights from the S2-star orbit precession; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 1; 3-2022; 35-390035-87111745-3933CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnrasl/article/511/1/L35/6461107info:eu-repo/semantics/altIdentifier/doi/10.1093/mnrasl/slab126info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:06:01Zoai:ri.conicet.gov.ar:11336/211740instacron: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:34982025-10-15 15:06:02.001CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv What does lie at the Milky Way centre? Insights from the S2-star orbit precession
title What does lie at the Milky Way centre? Insights from the S2-star orbit precession
spellingShingle What does lie at the Milky Way centre? Insights from the S2-star orbit precession
Argüelles, Carlos Raúl
DARK MATTER
GALAXY: CENTRE
GALAXY: STRUCTURE
STARS: KINEMATICS AND DYNAMICS
title_short What does lie at the Milky Way centre? Insights from the S2-star orbit precession
title_full What does lie at the Milky Way centre? Insights from the S2-star orbit precession
title_fullStr What does lie at the Milky Way centre? Insights from the S2-star orbit precession
title_full_unstemmed What does lie at the Milky Way centre? Insights from the S2-star orbit precession
title_sort What does lie at the Milky Way centre? Insights from the S2-star orbit precession
dc.creator.none.fl_str_mv Argüelles, Carlos Raúl
Mestre, Martin Federico
Becerra Vergara, E. A.
Crespi, Valentina
Krut, A.
Rueda, J. A.
Ruffini, R.
author Argüelles, Carlos Raúl
author_facet Argüelles, Carlos Raúl
Mestre, Martin Federico
Becerra Vergara, E. A.
Crespi, Valentina
Krut, A.
Rueda, J. A.
Ruffini, R.
author_role author
author2 Mestre, Martin Federico
Becerra Vergara, E. A.
Crespi, Valentina
Krut, A.
Rueda, J. A.
Ruffini, R.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv DARK MATTER
GALAXY: CENTRE
GALAXY: STRUCTURE
STARS: KINEMATICS AND DYNAMICS
topic DARK MATTER
GALAXY: CENTRE
GALAXY: STRUCTURE
STARS: KINEMATICS AND DYNAMICS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv It has been recently demonstrated that both, a classical Schwarzschild black hole (BH), and a dense concentration of self-gravitating fermionic dark matter (DM) placed at the Galaxy centre, can explain the precise astrometric data (positions and radial velocities) of the S-stars orbiting Sgr A∗. This result encompasses the 17 best resolved S-stars, and includes the test of general relativistic effects such as the gravitational redshift in the S2-star. In addition, the DM model features another remarkable result: The dense core of fermions is the central region of a continuous density distribution of DM whose diluted halo explains the Galactic rotation curve. In this Letter, we complement the above findings by analysing in both models the relativistic periapsis precession of the S2-star orbit. While the Schwarzschild BH scenario predicts a unique prograde precession for S2, in the DM scenario, it can be either retrograde or prograde, depending on the amount of DM mass enclosed within the S2 orbit, which, in turn, is a function of the DM fermion mass. We show that all the current and publicly available data of S2 cannot discriminate between the two models, but upcoming S2 astrometry close to next apocentre passage could potentially establish if Sgr A∗ is governed by a classical BH or by a quantum DM system.
Fil: Argüelles, Carlos Raúl. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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: Becerra Vergara, E. A.. Universidad Industrial Santander; Colombia. Università degli studi di Roma "La Sapienza"; Italia
Fil: Crespi, Valentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina
Fil: Krut, A.. Università degli studi di Roma "La Sapienza"; Italia
Fil: Rueda, J. A.. Università di Ferrara; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli studi di Roma "La Sapienza"; Italia
Fil: Ruffini, R.. Università degli studi di Roma "La Sapienza"; Italia. Istituto Nazionale di Astrofisica; Italia. Università di Ferrara; Italia
description It has been recently demonstrated that both, a classical Schwarzschild black hole (BH), and a dense concentration of self-gravitating fermionic dark matter (DM) placed at the Galaxy centre, can explain the precise astrometric data (positions and radial velocities) of the S-stars orbiting Sgr A∗. This result encompasses the 17 best resolved S-stars, and includes the test of general relativistic effects such as the gravitational redshift in the S2-star. In addition, the DM model features another remarkable result: The dense core of fermions is the central region of a continuous density distribution of DM whose diluted halo explains the Galactic rotation curve. In this Letter, we complement the above findings by analysing in both models the relativistic periapsis precession of the S2-star orbit. While the Schwarzschild BH scenario predicts a unique prograde precession for S2, in the DM scenario, it can be either retrograde or prograde, depending on the amount of DM mass enclosed within the S2 orbit, which, in turn, is a function of the DM fermion mass. We show that all the current and publicly available data of S2 cannot discriminate between the two models, but upcoming S2 astrometry close to next apocentre passage could potentially establish if Sgr A∗ is governed by a classical BH or by a quantum DM system.
publishDate 2022
dc.date.none.fl_str_mv 2022-03
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/11336/211740
Argüelles, Carlos Raúl; Mestre, Martin Federico; Becerra Vergara, E. A.; Crespi, Valentina; Krut, A.; et al.; What does lie at the Milky Way centre? Insights from the S2-star orbit precession; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 1; 3-2022; 35-39
0035-8711
1745-3933
CONICET Digital
CONICET
url http://hdl.handle.net/11336/211740
identifier_str_mv Argüelles, Carlos Raúl; Mestre, Martin Federico; Becerra Vergara, E. A.; Crespi, Valentina; Krut, A.; et al.; What does lie at the Milky Way centre? Insights from the S2-star orbit precession; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 511; 1; 3-2022; 35-39
0035-8711
1745-3933
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://academic.oup.com/mnrasl/article/511/1/L35/6461107
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnrasl/slab126
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 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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