2020A&A...641A..34B


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.05CET01:09:49

2020A&A...641A..34B - Astronomy and Astrophysics, volume 641A, 34-34 (2020/9-1)

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

BECERRA-VERGARA E.A., ARGUELLES C.R., KRUT A., RUEDA J.A. and RUFFINI R.

Abstract (from CDS):

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 4x106M 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-Arguelles-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 <χ2>S2,RAR≃3.1 and <χ2>S2,BH≃3.3 for S2 and <χ2>G2,RAR≃20 and <χ2>G2,BH≃ 41 for G2. The fit of the corresponding z data shows that while for S2 we find comparable fits, that is, χ2z,RAR≃1.28 and χ2z,BH≃1.04, for G2 the RAR model alone can produce an excellent fit of the data, that is, χ2z,RAR≃1.0 and χ2z,BH≃26. In addition, the critical mass for gravitational collapse of a degenerate 56keV-fermion DM core into a BH is ∼108M. This result may provide the initial seed for the formation of the observed central supermassive BH in active galaxies, such as M 87.

Abstract Copyright: © ESO 2020

Journal keyword(s): Galaxy: center - Galaxy: kinematics and dynamics - Galaxy: structure - dark matter - elementary particles

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6301 3
2 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3548 3
3 NAME G2 Dust Cloud IR 17 45 40.04 -29 00 28.1           ~ 164 0
4 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11850 0
5 [EG97] S2 *i* 17 45 40.0442 -29 00 27.975           B0/2V 285 1

    Equat.    Gal    SGal    Ecl

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2020.12.05-01:09:50

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