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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/211740
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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 |
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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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1846083203151953920 |
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13.22299 |