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Neutrino mass without cosmic variance

Marilena LoVerde

  • C. N. Yang Institute for Theoretical Physics, Department of Physics & Astronomy, Stony Brook University, Stony Brook, New York 11794, USA

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Phys. Rev. D 93, 103526 – Published 23 May, 2016

DOI: https://doi.org/10.1103/PhysRevD.93.103526

Abstract

Measuring the absolute scale of the neutrino masses is one of the most exciting opportunities available with near-term cosmological data sets. Two quantities that are sensitive to neutrino mass, scale-dependent halo bias b(k) and the linear growth parameter f(k) inferred from redshift-space distortions, can be measured without cosmic variance. Unlike the amplitude of the matter power spectrum, which always has a finite error, the error on b(k) and f(k) continues to decrease as the number density of tracers increases. This paper presents forecasts for statistics of galaxy and lensing fields that are sensitive to neutrino mass via b(k) and f(k). The constraints on neutrino mass from the auto- and cross-power spectra of spectroscopic and photometric galaxy samples are weakened by scale-dependent bias unless a very high density of tracers is available. In the high-density limit, using multiple tracers allows cosmic variance to be beaten, and the forecasted errors on neutrino mass shrink dramatically. In practice, beating the cosmic-variance errors on neutrino mass with b(k) will be a challenge, but this signal is nevertheless a new probe of neutrino effects on structure formation that is interesting in its own right.

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Phys. Rev. D 93, 103526– Published 23 May, 2016
  • Received 29 February 2016
Article part of CHORUS

© 2016 American Physical Society

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