Constraints on parameters of dark matter and black hole in the Galactic Center

Paolis, F. De; Ingrosso, G.; Nucita, A. A.

doi:10.1134/s1063778810110086

Cited by 8 publications

(11 citation statements)

References 81 publications

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“…As it was noted earlier, observations of bright star trajectories near the Galactic Center could provide an efficient tool to evaluate a gravitational potential, in particular, analyzing these trajectories one can obtain constraints on parameters of black hole and stellar cluster [103] and on parameters of dark matter distribution [104][105][106][107].…”

Section: Observational Signatures Of Black Holesmentioning

confidence: 99%

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

2017

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Abstract. In February 2016 the LIGO & VIRGO collaboration reported the discovery of gravitational waves in merging black holes, therefore, the team confirmed GR predictions about an existence of black holes and gravitational waves in the strong gravitational field limit. Moreover, in their papers the joint LIGO & VIRGO team presented an upper limit on graviton mass such as m g < 1.2 × 10 −22 eV . So, the authors concluded that their observational data do not show any violation of classical general relativity. We show that an analysis of bright star trajectories could constrain graviton mass with a comparable accuracy with accuracies reached with gravitational wave interferometers and the estimate is consistent with the one obtained by the LIGO & VIRGO collaboration. This analysis gives an opportunity to treat observations of bright stars near the Galactic Center as a useful tool to obtain constraints on the fundamental gravity law such as modifications of the Newton gravity law in a weak field approximation. In that way, based on a potential reconstruction at the Galactic Center we obtain bounds on a graviton mass.

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Section: Observational Signatures Of Black Holesmentioning

confidence: 99%

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

2017

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“…The orbital effects of eq. (11) have been computed more or less explicitly and at various levels of approximations in [30,32,34,35,40,41]. Actually, also the averaged pericenter precession induced by eq.…”

Section: Power-law Dm Density Profilementioning

confidence: 99%

Exact Expressions for the Pericenter Precession Caused by Some Dark Matter Distributions and Constraints on Them from Orbital Motions in the Solar System, in the Double Pulsar and in the Galactic Center

Iorio¹

2013

Galaxies

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We analytically calculate the secular precession of the pericenter of a test particle orbiting a central body surrounded by a continuous distribution of Dark Matter (DM) by using some commonly adopted spherically symmetric density profiles for it. We obtain exact expressions without resorting to a-priori simplifying assumptions on the orbital geometry of the test particle. Our formulas allow us to put constraints on the parameters of the DM distributions considered in several local astronomical and astrophysical scenarios, such as the Sun's planetary system, the double pulsar, and the stellar system around the supermassive black hole in Sgr A∗, all characterized by a wide variety of orbital configuratio ns. As far as our Solar System is concerned, latest determinations of the supplementary perihelion precessions ̟˙ with the EPM2011 ephemerides and the common power-law DM density profile ρDM(r) = ρ0r−γ λγ yield 5 × 103 GeV cm−3 (γ = 0) ≤ ρ0 ≤ 8 × 103 GeV cm−3 (γ = 4), corresponding to 8.9 × 10−21 g cm−3 ≤ ρ0 ≤ 1.4 × 10−20 g cm−3, at the Saturn's distance. From the periastron of the pulsar PSR J0737-3039A and the same power-low DM density, one has 1.7 × 1016 GeV cm−3 (γ = 0) ≤ ρ0 ≤ 2 × 1016 (γ = 4) GeV cm−3, corresponding to 3.0 × 10−8 g cm−3 ≤ ρ0 ≤ 3.6 × 10−8 g cm−3. The perinigricon of the S0-2 star in Sgr A∗ and the power-law DM model give 1.2 × 1013 GeV cm−3 (γ = 0) ≤ ρ0 ≤ 1 × 1016 (γ = 4, λ = rmin) GeV cm−3, corresponding to 2.1 × 10−11 g cm−3 ≤ ρ0 ≤ 1.8 × 10−8 g cm−3

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“…This entails a dark envelope with gravitationally significant density near the event horizon. This envelope declines radially as a nuclear 'spike', though more steeply than the low-F spikes of previous modelling (Gondolo & Silk 1999;Mouawad et al 2005;Hall & Gondolo 2006;Zakharov et al 2010). For large F , the spike's steepness makes the combined DM envelope plus BH appear (from afar) as if it were a more massive black hole.…”

Section: Comparison To Observed Smbhmentioning

confidence: 70%

“…(i) The gravitational potential of the DM envelope will cause stellar orbits to deviate from the Keplerian orbits that are expected for motion around a bare spherically symmetric gravitating object (Rubilar & Eckart 2001;Hall & Gondolo 2006;Mouawad et al 2005;Zakharov et al 2007;Ghez et al 2008;Zakharov et al 2010;Iorio 2011). A possible means to detect this deviation is timing observations of pulsars, if present, around the central black holes in nearby galaxies (Wex & Kopeikin 1999;Pfahl & Loeb 2004;Kramer et al 2004;Liu et al 2012;Singh, Wu & Sarty 2014).…”

Section: Possible Observational Tests Of the Dark Matter Envelopementioning

confidence: 99%

Dark halo microphysics and massive black hole scaling relations in galaxies

Saxton

Soria

2014

Monthly Notices of the Royal Astronomical Society

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We investigate the black hole (BH) scaling relation in galaxies using a model in which the galaxy halo and central BH are a self-gravitating sphere of dark matter (DM) with an isotropic, adiabatic equation of state. The equipotential where the escape velocity approaches the speed of light defines the horizon of the BH. We find that the BH mass (m • ) depends on the DM entropy, when the effective thermal degrees of freedom (F ) are specified. Relations between BH and galaxy properties arise naturally, with the BH mass and DM velocity dispersion following m • ∝ σ F/2 (for global mean density set by external cosmogony). Imposing observationally derived constraints on F provides insight into the microphysics of DM. Given that DM velocities and stellar velocities are comparable, the empirical correlation between m • and stellar velocity dispersions σ ⋆ implies that 7 F < 10. A link between m • and globular cluster properties also arises because the halo potential binds the globular cluster swarm at large radii. Interestingly, for F > 6 the dense dark envelope surrounding the BH approaches the mean density of the BH itself, while the outer halo can show a nearly uniform kpc-scale core resembling those observed in galaxies.

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Constraints on parameters of dark matter and black hole in the Galactic Center

Cited by 8 publications

References 81 publications

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

Exact Expressions for the Pericenter Precession Caused by Some Dark Matter Distributions and Constraints on Them from Orbital Motions in the Solar System, in the Double Pulsar and in the Galactic Center

Dark halo microphysics and massive black hole scaling relations in galaxies

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