Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core

Autores
Becerra Vergara, E. A.; Argüelles, Carlos Raúl; Krut, A.; Rueda, J. A.; Ruffini, Remo
Año de publicación
2020
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The motion of S-stars around the Galactic center implies that the central gravitational potential is dominated by a compact source, Sagittarius A∗ (Sgr A∗), which has a mass of about 4 × 106 M⊠and is traditionally assumed to be a massive black hole (BH). The explanation of the multiyear accurate astrometric data of the S2 star around Sgr A∗, including the relativistic redshift that has recently been verified, is particularly important for this hypothesis and for any alternative model. Another relevant object is G2, whose most recent observational data challenge the scenario of a massive BH: its post-pericenter radial velocity is lower than expected from a Keplerian orbit around the putative massive BH. This scenario has traditionally been reconciled by introducing a drag force on G2 by an accretion flow. As an alternative to the central BH scenario, we here demonstrate that the observed motion of both S2 and G2 is explained in terms of the dense core-diluted halo fermionic dark matter (DM) profile, obtained from the fully relativistic Ruffini-Argüelles-Rueda (RAR) model. It has previously been shown that for fermion masses 48-345 keV, the RAR-DM profile accurately fits the rotation curves of the Milky Way halo. We here show that the solely gravitational potential of such a DM profile for a fermion mass of 56 keV explains (1) all the available time-dependent data of the position (orbit) and line-of-sight radial velocity (redshift function z) of S2, (2) the combination of the special and general relativistic redshift measured for S2, (3) the currently available data on the orbit and z of G2, and (4) its post-pericenter passage deceleration without introducing a drag force. For both objects, we find that the RAR model fits the data better than the BH scenario: The mean of reduced chi-squares of the time-dependent orbit and z data are â χ 2â.
Fil: Becerra Vergara, E. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Universidad Industrial Santander; Colombia
Fil: Argüelles, Carlos Raúl. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. 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.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia
Fil: Rueda, J. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; Italia
Fil: Ruffini, Remo. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; Italia
Materia
DARK MATTER
ELEMENTARY PARTICLES
GALAXY: CENTER
GALAXY: KINEMATICS AND DYNAMICS
GALAXY: STRUCTURE
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:11336/139914
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/139914
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic coreBecerra Vergara, E. A.Argüelles, Carlos RaúlKrut, A.Rueda, J. A.Ruffini, RemoDARK MATTERELEMENTARY PARTICLESGALAXY: CENTERGALAXY: KINEMATICS AND DYNAMICSGALAXY: STRUCTUREhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The motion of S-stars around the Galactic center implies that the central gravitational potential is dominated by a compact source, Sagittarius A∗ (Sgr A∗), which has a mass of about 4 × 106 M⊠and is traditionally assumed to be a massive black hole (BH). The explanation of the multiyear accurate astrometric data of the S2 star around Sgr A∗, including the relativistic redshift that has recently been verified, is particularly important for this hypothesis and for any alternative model. Another relevant object is G2, whose most recent observational data challenge the scenario of a massive BH: its post-pericenter radial velocity is lower than expected from a Keplerian orbit around the putative massive BH. This scenario has traditionally been reconciled by introducing a drag force on G2 by an accretion flow. As an alternative to the central BH scenario, we here demonstrate that the observed motion of both S2 and G2 is explained in terms of the dense core-diluted halo fermionic dark matter (DM) profile, obtained from the fully relativistic Ruffini-Argüelles-Rueda (RAR) model. It has previously been shown that for fermion masses 48-345 keV, the RAR-DM profile accurately fits the rotation curves of the Milky Way halo. We here show that the solely gravitational potential of such a DM profile for a fermion mass of 56 keV explains (1) all the available time-dependent data of the position (orbit) and line-of-sight radial velocity (redshift function z) of S2, (2) the combination of the special and general relativistic redshift measured for S2, (3) the currently available data on the orbit and z of G2, and (4) its post-pericenter passage deceleration without introducing a drag force. For both objects, we find that the RAR model fits the data better than the BH scenario: The mean of reduced chi-squares of the time-dependent orbit and z data are â χ 2â.Fil: Becerra Vergara, E. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Universidad Industrial Santander; ColombiaFil: Argüelles, Carlos Raúl. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. 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.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; ItaliaFil: Rueda, J. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; ItaliaFil: Ruffini, Remo. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; ItaliaEDP Sciences2020-09-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/139914Becerra Vergara, E. A.; Argüelles, Carlos Raúl; Krut, A.; Rueda, J. A.; Ruffini, Remo; Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core; EDP Sciences; Astronomy and Astrophysics; 641; 4-9-2020; 1-160004-63611432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/201935990info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935990info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:27:44Zoai:ri.conicet.gov.ar:11336/139914instacron: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 14:27:44.48CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
title Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
spellingShingle Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
Becerra Vergara, E. A.
DARK MATTER
ELEMENTARY PARTICLES
GALAXY: CENTER
GALAXY: KINEMATICS AND DYNAMICS
GALAXY: STRUCTURE
title_short Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
title_full Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
title_fullStr Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
title_full_unstemmed Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
title_sort Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core
dc.creator.none.fl_str_mv Becerra Vergara, E. A.
Argüelles, Carlos Raúl
Krut, A.
Rueda, J. A.
Ruffini, Remo
author Becerra Vergara, E. A.
author_facet Becerra Vergara, E. A.
Argüelles, Carlos Raúl
Krut, A.
Rueda, J. A.
Ruffini, Remo
author_role author
author2 Argüelles, Carlos Raúl
Krut, A.
Rueda, J. A.
Ruffini, Remo
author2_role author
author
author
author
dc.subject.none.fl_str_mv DARK MATTER
ELEMENTARY PARTICLES
GALAXY: CENTER
GALAXY: KINEMATICS AND DYNAMICS
GALAXY: STRUCTURE
topic DARK MATTER
ELEMENTARY PARTICLES
GALAXY: CENTER
GALAXY: KINEMATICS AND DYNAMICS
GALAXY: STRUCTURE
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The motion of S-stars around the Galactic center implies that the central gravitational potential is dominated by a compact source, Sagittarius A∗ (Sgr A∗), which has a mass of about 4 × 106 M⊠and is traditionally assumed to be a massive black hole (BH). The explanation of the multiyear accurate astrometric data of the S2 star around Sgr A∗, including the relativistic redshift that has recently been verified, is particularly important for this hypothesis and for any alternative model. Another relevant object is G2, whose most recent observational data challenge the scenario of a massive BH: its post-pericenter radial velocity is lower than expected from a Keplerian orbit around the putative massive BH. This scenario has traditionally been reconciled by introducing a drag force on G2 by an accretion flow. As an alternative to the central BH scenario, we here demonstrate that the observed motion of both S2 and G2 is explained in terms of the dense core-diluted halo fermionic dark matter (DM) profile, obtained from the fully relativistic Ruffini-Argüelles-Rueda (RAR) model. It has previously been shown that for fermion masses 48-345 keV, the RAR-DM profile accurately fits the rotation curves of the Milky Way halo. We here show that the solely gravitational potential of such a DM profile for a fermion mass of 56 keV explains (1) all the available time-dependent data of the position (orbit) and line-of-sight radial velocity (redshift function z) of S2, (2) the combination of the special and general relativistic redshift measured for S2, (3) the currently available data on the orbit and z of G2, and (4) its post-pericenter passage deceleration without introducing a drag force. For both objects, we find that the RAR model fits the data better than the BH scenario: The mean of reduced chi-squares of the time-dependent orbit and z data are â χ 2â.
Fil: Becerra Vergara, E. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Universidad Industrial Santander; Colombia
Fil: Argüelles, Carlos Raúl. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. 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.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia
Fil: Rueda, J. A.. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; Italia
Fil: Ruffini, Remo. International Center for Relativistic Astrophysics Network; Italia. Università di Roma; Italia. Università di Ferrara; Italia. Istituto de Astrofisica e Planetologia Spaziali; Italia
description The motion of S-stars around the Galactic center implies that the central gravitational potential is dominated by a compact source, Sagittarius A∗ (Sgr A∗), which has a mass of about 4 × 106 M⊠and is traditionally assumed to be a massive black hole (BH). The explanation of the multiyear accurate astrometric data of the S2 star around Sgr A∗, including the relativistic redshift that has recently been verified, is particularly important for this hypothesis and for any alternative model. Another relevant object is G2, whose most recent observational data challenge the scenario of a massive BH: its post-pericenter radial velocity is lower than expected from a Keplerian orbit around the putative massive BH. This scenario has traditionally been reconciled by introducing a drag force on G2 by an accretion flow. As an alternative to the central BH scenario, we here demonstrate that the observed motion of both S2 and G2 is explained in terms of the dense core-diluted halo fermionic dark matter (DM) profile, obtained from the fully relativistic Ruffini-Argüelles-Rueda (RAR) model. It has previously been shown that for fermion masses 48-345 keV, the RAR-DM profile accurately fits the rotation curves of the Milky Way halo. We here show that the solely gravitational potential of such a DM profile for a fermion mass of 56 keV explains (1) all the available time-dependent data of the position (orbit) and line-of-sight radial velocity (redshift function z) of S2, (2) the combination of the special and general relativistic redshift measured for S2, (3) the currently available data on the orbit and z of G2, and (4) its post-pericenter passage deceleration without introducing a drag force. For both objects, we find that the RAR model fits the data better than the BH scenario: The mean of reduced chi-squares of the time-dependent orbit and z data are â χ 2â.
publishDate 2020
dc.date.none.fl_str_mv 2020-09-04
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/11336/139914
Becerra Vergara, E. A.; Argüelles, Carlos Raúl; Krut, A.; Rueda, J. A.; Ruffini, Remo; Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core; EDP Sciences; Astronomy and Astrophysics; 641; 4-9-2020; 1-16
0004-6361
1432-0746
CONICET Digital
CONICET
url http://hdl.handle.net/11336/139914
identifier_str_mv Becerra Vergara, E. A.; Argüelles, Carlos Raúl; Krut, A.; Rueda, J. A.; Ruffini, Remo; Geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our Galactic core; EDP Sciences; Astronomy and Astrophysics; 641; 4-9-2020; 1-16
0004-6361
1432-0746
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/10.1051/0004-6361/201935990
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935990
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 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 13.22299

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