Olivari, L. C.
Battye, R. A.
Ma, Y. -Z.
Costa, A. A.
Total Authors: 7
 Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Oxford Rd, Manchester M13 9PL, Lancs - England
 Univ KwaZulu Natal, Sch Chem & Phys, Westville Campus, Private Bag X54001, ZA-4000 Durban - South Africa
 Univ Sao Paulo, Inst Fis, CP 66318, BR-05315970 Sao Paulo, SP - Brazil
Total Affiliations: 3
Monthly Notices of the Royal Astronomical Society;
Web of Science Citations:
HI intensity mapping is a new observational technique to survey the large-scale structure of matter using the 21 cm emission line of atomic hydrogen (HI). 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 HI 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 Delta w < 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 Sigma m(nu) < 0.24 eV for BINGO and Sigma m(nu) < 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. (AU)