| dc.description |
The designs of the first generation of cosmological 21-cm observatories are split between single dipole experiments which integrate over a large patch of sky in order to find the global (spectral) signature of reionization, and interferometers with arcminute-scale angular resolution whose goal is to measure the 3D power spectrum of ionized regions during reionization. We examine whether intermediate scale instruments with complete Fourier (uv) coverage are capable of placing new constraints on reionization. We find that even without using a full power spectrum analysis, the global redshift of reionization, z<sub>reion</sub>, can in principle be measured from the variance in the 21-cm signal among multiple beams as a function of frequency at a roughly 1 degree angular scale. At this scale, the beam-to-beam variance in the differential brightness temperature peaks when the average neutral fraction was ∼ 50%, providing a convenient flag of z<sub>reion</sub>. We choose a low angular resolution of order 1° to exploit the physical size of the ionized regions and maximize the signal-to-noise ratio. Thermal noise, foregrounds, and instrumental effects should also be manageable at this angular scale, as long as the uv coverage is complete within the compact core required for low-resolution imaging. For example, we find that z<sub>reion</sub> can potentially be detected to within a redshift uncertainty of Δz<sub>reion</sub>≲1 in ≳500 hours of integration on the existing MWA prototype (with only 32 × 16 dipoles), operating at an angular resolution of ∼ 1° and a spectral resolution of 2.4 MHz. |
