Super-Heavy Dark Matter - Towards Predictive Scenarios from Inflation
  A generic prediction of the Coleman-Weinberg inflation is the existence of a
heavy particle sector whose interactions with the inflaton, the lightest state
in this sector, generate the inflaton potential at loop level. For typical
interactions the heavy sector may contain stable states whose relic abundance
is generated at the end of inflation by the gravity alone. This general
feature, and the absence of any particle physics signal of dark matter so far,
motivates us to look for new directions in the dark sector physics, including
scenarios in which dark matter is super-heavy. In this article we study the
possibility that the dark matter is even heavier than the inflaton, its
existence follows from the inflaton dynamics, and its abundance today is {\it
naturally} determined by the weakness of gravitational interaction. This
implies that the super-heavy dark matter scenarios can be tested via the
measurements of inflationary parameters and/or the CMB isocurvature
perturbations and non-Gaussianities. We explicitly work out details of three
Coleman-Weinberg inflation scenarios, study the systematics of super-heavy dark
matter production in those cases, and compute which parts of the parameter
spaces can be probed by the future CMB measurements.
