Cosmological parameter forecasts for H I intensity mapping experiments using the angular power spectrum

L. C. Olivari, C. Dickinson, R. A. Battye, Y.-Z. Ma, A. A. Costa, M. Remazeilles, S. Harper

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Abstract

H I intensity mapping is a new observational technique to survey the large-scale structure of matter using the 21 cm emission line of atomic hydrogen (H I). In this work, we simulate BINGO (BAO from Integrated Neutral Gas Observations) and SKA (Square Kilometre Array) phase-1 dish array operating in autocorrelation mode. For the optimal case of BINGO with no foregrounds, the combination of the H I angular power spectra with Planck results allows w to be measured with a precision of 4 per cent, while the combination of the BAO acoustic scale with Planck gives a precision of 7 per cent. We consider a number of potentially complicating effects, including foregrounds and redshift-dependent bias, which increase the uncertainty on w but not dramatically; in all cases, the final uncertainty is found to be Δw < 8 per cent for BINGO. For the combination of SKA–MID in autocorrelation mode with Planck, we find that, in ideal conditions, w can be measured with a precision of 4 per cent for the redshift range 0.35 < z < 3 (350–1050 MHz) and 2 per cent for 0 < z < 0.49 (950–1421 MHz). Extending the model to include the sum of neutrino masses yields a 95 per cent upper limit of ∑mν < 0.24 eV for BINGO and ∑mν < 0.08 eV for SKA phase 1, competitive with the current best constraints in the case of BINGO and significantly better than them in the case of SKA.
Original languageEnglish
Article number14
Pages (from-to)4242-4256
Number of pages15
JournalRoyal Astronomical Society. Monthly Notices
Volume473
Issue number3
Early online date11 Oct 2017
DOIs
Publication statusPublished - 21 Jan 2018

Keywords

  • methods: data analysis, cosmological parameters, dark energy, large-scale structure of Universe, radio continuum: galaxies, radio lines: galaxies

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