Cosmological implications of ultralight axionlike fields

Cosmological observations are used to test for imprints of an ultralight axionlike field (ULA), with a range of potentials V(phi) proportional to [1 - cos(phi/f)](n) set by the axion-field value phi and decay constant f. Scalar field dynamics dictate that the field is initially frozen and then begins to oscillate around its minimum when the Hubble parameter drops below some critical value. For n = 1, once dynamical, the axion energy density dilutes as matter; for n = 2 it dilutes as radiation and for n = 3 it dilutes faster than radiation. Both the homogeneous evolution of the ULA and the dynamics of its linear perturbations are included, using an effective fluid approximation generalized from the usual n = 1 case. ULA models are parametrized by the redshift z(c) when the field becomes dynamical, the fractional energy density f(zc) equivalent to Omega(a) (z(c))/Omega(tot)(z(c)) in the axion field at z(c), and the effective sound speed c(s)(2). Using Planck, BAO and JLA data, constraints on f(zc) are obtained. ULAs are degenerate with dark energy for all three potentials if 1 + z(c) less than or similar to 10. When 3 x 10(4) greater than or similar to 1 + z(c) greater than or similar to 10, f(zc) is constrained to be. 0.004 for n = 1 and f(zc) less than or similar to 0.02 for the other two potentials. The constraints then relax with increasing z(c). These results have implications for ULAs as a resolution to cosmological tensions, such as discrepant measurements of the Hubble constant, or the EDGES measurement of the global 21 cm signal.