Testing dark matter distributions by neutrino–dark matter interactions

Penacchioni, A. V.; Civitarese, O.; Argüelles, Carlos

doi:10.1140/epjc/s10052-020-7744-x

Cited by 13 publications

(9 citation statements)

References 29 publications

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“…For the core-halo DM profiles, formation scenarios in which the quantum nature of the particle is considered (i.e., either bosonic or fermionic) are still an open field of research, and our aim here is to provide a further (precision) test for fermionic models. Joint observational tests based on additional physics, for example, strong lensing (Gómez et al 2016) or DM-active neutrino interactions (Penacchioni et al 2020), can help in unambiguously probing the existence of a central fermionic DM concentration in the allowed region of the extended RAR model parameter space. The results shown here imply that this free parameter space is slightly reduced with respect to the space described in Argüelles et al (2018).…”

Section: Discussionmentioning

confidence: 99%

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

Becerra-Vergara

Argüelles

Krut

et al. 2020

A&A

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116

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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 ⟨χ̄2⟩S2,RAR ≈ 3.1 and ⟨χ̄2⟩S2,BH ≈ 3.3 for S2 and ⟨χ̄2⟩G2,RAR ≈ 20 and ⟨χ̄2⟩G2,BH ≈ 41 for G2. The fit of the corresponding z data shows that while for S2 we find comparable fits, that is, χ̄2z,RAR ≈ 1.28 and χ̄2z,BH ≈ 1.04, for G2 the RAR model alone can produce an excellent fit of the data, that is, χ̄2z,RAR ≈ 1.0 and χ̄2z,BH ≈ 26. In addition, the critical mass for gravitational collapse of a degenerate 56 keV-fermion DM core into a BH is ∼ 108 M⊙. This result may provide the initial seed for the formation of the observed central supermassive BH in active galaxies, such as M 87.

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Section: Discussionmentioning

confidence: 99%

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

Becerra-Vergara

Argüelles

Krut

et al. 2020

A&A

Self Cite

116

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“…Remarkably, such a dense DM core is the central region of a continuous distribution of DM whose diluted halo explains the Galactic rotation curves (Argüelles & et al 2018;Becerra-Vergara et al 2020, 2021. Core-halo DM distributions of this kind are obtained from the solution of the Einstein equations for a self-gravitating, finite-temperature fluid of fermions in equilibrium following the Ruffini-Argüelles-Rueda (RAR) model (Ruffini et al 2015;Argüelles & et al 2016;Gómez et al 2016;Gómez & Rueda 2017;Argüelles & et al 2018Argüelles & et al , 2019Penacchioni & et al 2020;Yunis & et al 2020;Becerra-Vergara et al 2020, 2021Argüelles & et al 2021). These novel core-halo DM profiles, as the ones applied in this Letter, have been shown to form and remain stable in cosmological time-scales, when accounting for the quantum nature of the particles within proper relaxation mechanisms of collisionless fermions (Argüelles & et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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

Argüelles,

Mestre,

Becerra-Vergara

et al. 2021

Preprint

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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 analyzing 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 can not 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.

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“…Joint observational tests based on additional physics, e.g. strong lensing (Gómez et al 2016) or DM-active neutrino interactions (Penacchioni et al 2020), can help in unambiguously probing the existence of a central fermionic DM concentration in the allowed region of the extended RAR model parameter space. The results shown here imply that such free parameter space is slightly reduced with respect to the former one given in Argüelles et al (2018).…”

Section: Discussionmentioning

confidence: 99%

The geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our galactic core

Becerra-Vergara,

Arguelles,

Krut

et al. 2020

Preprint

View full text Add to dashboard Cite

The S-stars motion around the Galactic center implies that the central gravitational potential is dominated by a compact source, Sagittarius A* (Sgr A*), with a mass of about 4 × 10 6 M , traditionally assumed to be a massive black hole (BH). Particularly important for this hypothesis, and for any alternative model, is the explanation of the multiyear, accurate astrometric data of the S2 star around Sgr A*, including the relativistic redshift which has been recently verified. Another relevant object is G2, whose most recent observational data challenge the massive BH scenario: its post-pericenter radial velocity is lower than the expectation 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. Alternatively 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 been already 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 better the data than the BH scenario: the mean of reduced chi-squares of the time-dependent orbit and z data are, for S2, χ2 S2,RAR ≈ 3.1 and χ2 S2,BH ≈ 3.3 and, for G2, χ2 G2,RAR ≈ 20 and χ2 G2,BH ≈ 41. If we look at the fit of the corresponding z data, while for S2 we find comparable fits, i.e, χ2 z,RAR ≈ 1.28 and χ2 z,BH ≈ 1.04, for G2 only the RAR model can produce an excellent fit of the data, i.e. χ2 z,RAR ≈ 1.0 and χ2 z,BH ≈ 26. In addition, the critical mass for gravitational collapse of a degenerate 56 keV-fermion DM core into a BH is ∼ 10 8 M . This result may provide the initial seed for the formation of the observed central supermassive BH in active galaxies, such as M87.

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Testing dark matter distributions by neutrino–dark matter interactions

Cited by 13 publications

References 29 publications

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

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

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

The geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our galactic core

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