2015/08/12 by Zaven Arzoumanian, Adam Brazier, Sarah Burke-Spolaor +45 · 1 voice
Physics and Astronomy · #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.3847/0004-637x/821/1/13
21 pages, 12 figures. Please send any comments/questions to [email protected]
We compute upper limits on the nanohertz-frequency isotropic stochastic gravitational wave background (GWB) using the 9-year data release from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) collaboration. We set upper limits for a GWB from supermassive black hole binaries under power law, broken power law, and free spectral coefficient GW spectrum models. We place a 95% upper limit on the strain amplitude (at a frequency of yr-1) in the power law model of A\rm gw < 1.5× 10-15. For a broken power law model, we place priors on the strain amplitude derived from simulations of Sesana (2013) and McWilliams et al. (2014). We find that the data favor a broken power law to a pure power law with odds ratios of 22 and 2.2 to one for the McWilliams and Sesana prior models, respectively. The McWilliams model is essentially ruled out by the data, and the Sesana model is in tension with the data under the assumption of a pure power law. Using the broken power-law analysis we construct posterior distributions on environmental factors that drive the binary to the GW-driven regime including the stellar mass density for stellar-scattering, mass accretion rate for circumbinary disk interaction, and orbital eccentricity for eccentric binaries, marking the first time that the shape of the GWB spectrum has been used to make astrophysical inferences. We then place the most stringent limits so far on the energy density of relic GWs, Ωgw(f) h2 < 4.2 × 10-10, yielding a limit on the Hubble parameter during inflation of H_*=1.6×10-2~mPl, where mPl is the Planck mass. Our limit on the cosmic string GWB, Ωgw(f) h2 < 2.2 × 10-10, translates to a conservative limit of Gμ<3.3× 10-8 - a factor of 4 better than the joint Planck and high-l CMB data from other experiments.