Introduction to Xenon1t Excess

We utilize different detector efficiency and energy reconstruction models, but they primarily impact sub-keV energies and cannot explain the XENON1T excess.

8\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14}$ is consistent with the XENON1T excess, while accounting for the observed dark matter and satisfying astro/cosmo probes.

We provide a fit of the XENON1T excess in terms of a minimal low scale type-IIB string theory parameter space and present some benchmark points which provide a good fit to the data.

We argue that the Xenon1T excess can be explained by the emission of scalars from the Sun.

Finally, we show that such dark radiation can lead to a satisfactory explanation of the recently observed XENON1T excess in the electron recoil signal without being in conflict with other bounds.

Explaining the XENON1T excess with transition magnetic moments is marginally possible if very conservative assumptions are adopted regarding the supernova 1987 A and CMB constraints.

While being consistent with the required DM phenomenology along with sufficient self-interactions to address the small scale issues of cold dark matter, the model with GeV scale DM can explain the XENON1T excess via inelastic down scattering of heavier DM component into the lighter one.

In earlier attempts to explain XENON1T excess with inelastic DM in gauged Lμ − Lτ model [53] which can also explain (g − 2)μ, only a tiny parameter space was allowed from all requirements even while considering a much larger error bars in (g − 2)μ namely ∆aμ = (27.