Speaker
Description
Dark matter (DM), a large (~85%) non-baryonic and non-relativistic
component of the matter density of the Universe, likely consists of one
or several so-far undetected particles hypothesized in theories beyond
the Standard Model (SM). One of the most promising approaches to shed
light on the nature of DM particles is to search for signatures of their
annihilation or decay into SM particles - among which very-high energy
gamma-rays - from regions of the sky believed to be highly DM dominated,
such as the Galactic Center, the clusters of galaxies and local compact
objects such as the dwarf spheroidal galaxies (dSphs) and some globular
clusters around the Milky Way. In this context, the latter two are among
the most promising observational targets due to their relative proximity
and lack of astrophysical background sources, and are therefore
paramount targets to be pointed at with current (e.g., MAGIC) and
next-generation (e.g., CTA) Cherenkov telescopes to detect gamma-rays
produced by DM interactions or at least constrain the particle DM
parameter space. In this contribution, I will present new determinations
of the DM amount (i.e. the astrophysical factors for DM annihilation and
decay) in dSph and globular cluster halos obtained through the MCMC
Jeans analysis of their brightness and kinematic data through the CLUMPY
software. I will also discuss the systematic uncertainties affecting the
calculation of such quantities.
