Dark energy and inflation invoked in CCGG by locally contorted
  space-time
  The cosmological implications of the Covariant Canonical Gauge Theory of
Gravity (CCGG) are investigated. We deduce that, in a metric compatible
geometry, the requirement of covariant conservation of matter invokes torsion
of space-time. In the Friedman model this leads to a scalar field built from
contortion and the metric with the property of dark energy, which transforms
the cosmological constant to a time-dependent function. Moreover, the
quadratic, scale invariant Riemann-Cartan term in the CCGG Lagrangian endows
space-time with kinetic energy, and in the field equations adds a geometrical
curvature correction to Einstein gravity. Applying in the Friedman model the
standard $\Lambda$CDM parameter set, those equations yield a cosmological field
depending just on one additional, dimensionless ``deformation'' parameter of
the theory that determines the strength of the quadratic term, viz. the
deviation from the Einstein-Hilbert ansatz. Moreover, the apparent curvature of
the universe differs from the actual curvature parameter of the metric. The
numerical analysis in that parameter space yields three cosmology types: (I) A
bounce universe starting off from a finite scale followed by a steady
inflation, (II) a singular Big Bang universe undergoing a secondary
inflation-deceleration phase, and (III) a solution similar to standard
cosmology but with a different temporal profile. The common feature of all
scenarios is the graceful exit to the current dark energy era. The value of the
deformation parameter can be deduced by comparing theoretical calculations with
observations, namely with the SNeIa Hubble diagram and the deceleration
parameter. That comparison implies a considerable admixture of scale invariant
quadratic gravity to Einstein gravity. This theory also sheds new light on the
resolution of the cosmological constant problem and of the Hubble tension.
