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The hyperfine transition of $^3$He$^+$ at 3.5cm has been thought as a probeof the high-z IGM since it offers a unique insight into the evolution of thehelium component of the gas, as well as potentially give an independentconstraint on the 21cm signal from neutral hydrogen. In this paper, we useradiative transfer simulations of reionization driven by sources such as stars,X-ray binaries, accreting black holes and shock heated interstellar medium, andsimulations of a high-z quasar to characterize the signal and analyze itsprospects of detection. We find that the peak of the signal lies in the range1-50 $\mu$K for both environments, but while around the quasar it is always inemission, in the case of cosmic reionization a brief period of absorption isexpected. As the evolution of HeII is determined by stars, we find that it isnot possible to distinguish reionization histories driven by more energeticsources. On the other hand, while a bright QSO produces a signal in 21cm thatis very similar to the one from a large collection of galaxies, its signaturein 3.5cm is very peculiar and could be a powerful probe to identify thepresence of the QSO. We analyze the prospects of the signal's detectabilityusing SKA1-mid as our reference telescope. We find that the noise powerspectrum dominates over the power spectrum of the signal, although a modest S/Nratio can be obtained when the wavenumber bin width and the survey volume aresufficiently large.

Probing the high-z IGM with the hyperfine transition of $^3$He$^+$