This paper presents cosmological results from the final data release of the WiggleZ Dark Energy Survey. We perform full analyses of different cosmological models using the WiggleZ power spectra measured at $z=0.22$, 0.41, 0.60, and 0.78, combined with other cosmological data sets. The limiting factor in this analysis is the theoretical modeling of the galaxy power spectrum, including nonlinearities, galaxy bias, and redshift-space distortions. In this paper we assess several different methods for modeling the theoretical power spectrum, testing them against the Gigaparsec WiggleZ simulations (GiggleZ). We fit for a base set of six cosmological parameters, $\{{\Omega }_b{h}^2,{\Omega }_{\mathrm{CDM}}{h}^2,H_0,\tau ,A_s,n_s\}$, and five supplementary parameters $\{n_{\mathrm{run}},r,w,{\Omega }_k,\sum _{}^{}{m}_{\nu }\}$. In combination with the cosmic microwave background, our results are consistent with the $\Lambda \mathrm{CDM}$ concordance cosmology, with a measurement of the matter density of ${\Omega }_m=0.29\pm 0.016$ and amplitude of fluctuations ${\sigma }_8=0.825\pm 0.017$. Using WiggleZ data with cosmic microwave background and other distance and matter power spectra data, we find no evidence for any of the extension parameters being inconsistent with their $\Lambda \mathrm{CDM}$ model values. The power spectra data and theoretical modeling tools are available for use as a module for CosmoMC, which we here make publicly available at http://smp.uq.edu.au/wigglez-data. We also release the data and random catalogs used to construct the baryon acoustic oscillation correlation function.

The Majoron provides an attractive dark matter candidate, directly associated with the mechanism responsible for spontaneous neutrino mass generation within the standard model $\mathrm{SU}(3{)}_{\mathrm{c}}$\bigotimes${}\mathrm{SU}(2{)}_{\mathrm{L}}$\bigotimes${}\mathrm{U}(1{)}_{\mathrm{Y}}$ framework. Here we update the cosmological and astrophysical constraints on Majoron dark matter coming from the cosmic microwave background and a variety of x- and $$\gamma${}$-ray observations.

The primordial deuterium abundance probes fundamental physics during the Big Bang Nucleosynthesis and can be used to infer cosmological parameters. Observationally, the abundance can be measured using absorbing clouds along the lines of sight to distant quasars. Observations of the quasar PKS1937–101 contain two absorbers for which the deuterium abundance has previously been determined. Here we focus on the higher redshift one at z_abs = 3.572. We present new observations with significantly increased signal-to-noise ratio which enable a far more precise and robust measurement of the deuterium to hydrogen column density ratio, resulting in D i/H i = 2.62 ± 0.05 × 10⁻⁵. This particular measurement is of interest because it is among the most precise assessments to date and it has been derived from the second lowest column-density absorber [N(H i) = 17.9 cm⁻²] that has so-far been utilised for deuterium abundance measurements. The majority of existing high-precision measurements were obtained from considerably higher column density systems [i.e. N(H i) > 19.4 cm⁻²]. This bodes well for future observations as low column density systems are more common.

Astronomy & Astrophysics (A&A) is an international journal which publishes papers on all aspects of astronomy and astrophysics