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The geodesic motion of S2 and G2 as a test of the fermionic dark matter nature of our galactic core by Becerra-Vergara, E. A.; Arguelles, C. R.; Krut, A.; Rueda, J. A.; Ruffini, R. is a scholarly article available to read on EtoBox.

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

[Abridged] The S-stars motion around the Galactic center (Sgr A*) implies the existence of a compact source with a mass of about $4\times 10^6 M_\odot$, traditionally assumed to be a massive black hole (BH). Important for any model is the explanation of the multiyear, accurate astrometric data of S2 and the challenging G2: its post-pericenter velocity decelerates faster than expected from a Keplerian orbit around the putative BH. This has been reconciled in the literature by acting on G2 a drag force by an accretion flow. Alternatively, we show that the S2 and G2 motion is explained by the "core-halo" fermionic dark matter (DM) profile of the fully-relativistic Ruffini-Arg\"uelles-Rueda (RAR) model. It has been already shown that for 48-345 keV fermions, it accurately fits the rotation curves of the Milky-Way halo. We here show that, for a fermion mass of 56 keV, it explains the time-dependent data of the position (orbit) and light-of-sight radial velocity (redshift function $z$) of S2 and G2, the latter without a drag force. We find the RAR model fits better the data: the mean of reduced chi-squares of the orbit and $z$ data are, for S2, $\langle\bar{\chi}^2\rangle_{\rm S2, RAR}\a

Author

Becerra-Vergara, E. A.; Arguelles, C. R.; Krut, A.; Rueda, J. A.; Ruffini, R.

Published

2020

Language

EN