$\alpha$-attractor dark energy in view of next-generation cosmological
  surveys
  The $\alpha$-attractor inflationary models are nowadays favored by CMB Planck
observations. Their similarity with canonical quintessence models motivates the
exploration of a common framework that explains both inflation and dark energy.
We study the expected constraints that next-generation cosmological experiments
will be able to impose for the dark energy $\alpha$-attractor model. We
systematically account for the constraining power of SNIa from WFIRST, BAO from
DESI and WFIRST, galaxy clustering and shear from LSST and Stage-4 CMB
experiments. We assume a tensor-to-scalar ratio, $10^{-3} < r < 10^{-2}$, which
permits to explore the wide regime sufficiently close, but distinct, to a
cosmological constant, without need of fine tunning the initial value of the
field. We find that the combination S4CMB + LSST + SNIa will achieve the best
results, improving the FoM by almost an order of magnitude; respect to the
S4CMB + BAO + SNIa case. We find this is also true for the FoM of the $w_0 -
w_a$ parameters. Therefore, future surveys will be uniquely able to probe
models connecting early and late cosmic acceleration.
