Conveners
Dark matter halos: its nature, modeling & tracers: Tuesday block 1
- Carlos Raúl Argüelles (Universidad Nacional de La Plata)
Dark matter halos: its nature, modeling & tracers: Tuesday block 2
- Carlos Raúl Argüelles (Universidad Nacional de La Plata)
Description
Actual attempts to explain the formation of DM halos and its final quasi-universal density profiles are mainly centered in N-body simulations. Despite its success in providing a fitting formula or law for the virialized distributions composed by collisionless particles, we still lack a clear understanding on both, its physical basis and in the very nature of the dark matter candidates. This session is devoted to different aspects of dark matter halos: (i) its modeling either from first principle physics or simulations; (ii) its nature either in terms of bosonic of fermionic particles; (iii) morphology constraints & tracers such as rotation curves or stellar streams among others.
The ESA Gaia astrometric mission has revolutionized our understanding of the Milky Way (MW) by providing six-dimensional phase-space measurements of its stars. Utilizing the third data release (Gaia DR3), we have derived a precise MW rotation curve (RC) extending up to 26.5 kpc. For the first time, we detect a Keplerian decline in the RC from 19 to 26.5 kpc. We estimate the MW dynamical mass...
In this talk I will describe novel techniques to simulate the nonlinear collapse of dark matter in the cosmos. I will then present simulations of the abundance of dark matter halos and subhalos as a function of the properties of dark matter. In addition, I will discuss simulations that focus on the first collapse of dark matter haloes and the emergence of single power law density profiles....
In the standard cosmological model the dark matter (DM) particles are collisionless and, because of this very nature, they develop halos with the characteristic central cusp known as NFW profile. Real galaxies do not show NFW profiles but, rather, have a DM mass distribution with a central plateau or core, characteristic of self-gravitating systems in thermodynamic equilibrium (SA+20). Within...
For the first time in the literature, a dark matter (DM) halo model based on first physical principles such as (quantum) statistical mechanics and thermodynamics is used to try to reproduce 6D phase-space observations in stellar streams. We model both DM haloes, the one of the progenitor and the one of its host with a spherical self-gravitating system of neutral fermions which accounts for the...
Observations with the Gaia satellite have confirmed that the satellite galaxies of the Milky Way are not distributed as homogeneously as expected. The same occurs in galaxies such as Andromeda and Centaurus A, where satellite galaxies around their host galaxies have been observed to have orbits aligned perpendicular to the galactic plane of the host galaxy. This problem is known for the Milky...
Using Low Brightness Surface Galaxies (LBSG) rotational curves we inferred the free parameters of l-boson stars as a dark matter component. The l-boson stars are numerical solutions to the non-relativistic limit of the Einstein-Klein-Gordon system, the Schrödinger-Poisson (SP) system. These solutions are parametrized by an angular momentum number l = (N −1)/2 and an excitation number n. We...
In spherical symmetry, the gravitational potential of galaxies and their halos are univocally derived from the rotational velocity profile. Thousands of galaxies are well-fitted by a universal velocity profile and thus, the gravitational profile is well known. By considering that dark matter can be treated either as an ideal gas, a Fermi, or a Bose gas, we found that only the latter can...
The halo of our Galaxy is populated with a significant number of high-velocity clouds (HVCs) moving with a speed up to $500$ km/s. It is suggested that these HVCs might contain a non-negligible fraction of the missing baryons. We aim to estimate the baryonic mass of the Milky Way halo in the form of HVCs to constrain a fraction of missing baryons in the form of these clouds. Such findings...
