Constraints On Primordial Gravitational Waves From The Cosmic Microwave Background

Searches for primordial gravitational waves have resulted in constraints in a large frequency range from a variety of sources. The standard Cosmic Microwave Background (CMB) technique is to parameterise the tensor power spectrum in terms of the tensor-to-scalar ratio, r, and spectral index, n(t), and constrain these using measurements of the temperature and polarization power spectra. Another method, applicable to modes well inside the cosmological horizon at recombination, uses the shortwave approximation, under which gravitational waves behave as an effective neutrino species. In this paper we give model-independent CMB constraints on the energy density of gravitational waves, Omega(gw)h(2), for the entire range of observable frequencies. On large scales, f less than or similar to 10(-16) Hz, we reconstruct the initial tensor power spectrum in logarithmic frequency bins, finding maximal sensitivity for scales close to the horizon size at recombination. On small scales, f greater than or similar to 10(-15) Hz, we use the shortwave approximation, finding Omega(gw),h(2) < 1.7 x 10(-6) for adiabatic initial conditions and Omega(gw)h(2) < 2.9 x 10(-7) for homogeneous initial conditions (both 2 sigma upper limits). For scales close to the horizon size at recombination, we use second-order perturbation theory to calculate the back-reaction from gravitational waves, finding Omega(gw)h(2) < 8.4 x 10(-7), in the absence of neutrino anisotropic stress and Omega(gw)h(2) < 8.6 x 10(-7) when including neutrino anisotropic stress. These constraints are valid for 10(-15) Hz greater than or similar to f greater than or similar to 3 x 10(-16) Hz.