DESI and other Dark Energy experiments in the era of neutrino mass measurements

By A. Font-Ribera, P. Mcdonald, N. Mostek, B. Reid, H. Seo, A. Slosar. 2013

302 citations recorded by the source corpus.

We present Fisher matrix projections for future cosmological parameter measurements, including neutrino masses, Dark Energy, curvature, modified gravity, the inflationary perturbation spectrum, non-Gaussianity, and dark radiation. We focus on DESI and generally redshift surveys (BOSS, HETDEX, eBOSS, Euclid, and WFIRST), but also include CMB (Planck) and weak gravitational lensing (DES and LSST) constraints. The goal is to present a consistent set of projections, for concrete experiments, which are otherwise scattered throughout many papers and proposals. We include neutrino mass as a free parameter in most projections, as it will inevitably be relevant — DESI and other experiments can measure the sum of neutrino masses to ∼ 0.02 eV or better, while the minimum possible sum is ∼ 0.06 eV. We note that constraints on Dark Energy are significantly degraded by the presence of neutrino mass uncertainty, especially when using galaxy clustering only as a probe of the BAO distance scale (because this introduces additional uncertainty in the background evolution after the CMB epoch). Using broadband galaxy power becomes relatively more powerful, and bigger gains are achieved by combining lensing survey constraints with redshift survey constraints. We do not try to be especially innovative, e.g., with complex treatments of potential systematic errors — these projections are intended as a straightforward baseline for comparison to more detailed analyses.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d1787ac4ac20f0253304504dc47b68eddebd77df

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Citations in the corpus

Nonlinear perturbation theory extension of the Boltzmann code CLASS (2020, background): “However, if one computes both the CMB power spectra C` and the non-linear power spectra P (k) in one CLASS call, one is encouraged to use the flag “output format=FAST.””
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The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, methodology): “This choice is motivated by the fact that this value is close to the amplitude of the BOSS power spectrum at k = 0.14 h Mpc−1, which is the effective scale suggested by Font-Ribera et al. (2014) to use for BOSS BAO measurements.”