Optimal survey parameters: Ly$\alpha$ and H$\alpha$ intensity mapping for synergy with the 21cm signal during reionization

Abstract

Intensity mapping of multiple emission lines is emerging as a new branch to astronomy, to probe both properties of ionizing sources and the medium between, in particular the intergalactic medium. For Epoch of Reionization (EoR) studies, both multi-line experiments and analysis methods are still in their infancy. Here we explore optimal survey parameters for Ly$\alpha$ (and H$\alpha$) intensity mapping up to high redshifts of reionization, and requirements for optimised synergy with 21cm experiments. We investigate line sensitivity, spectral resolution and detector pixel size requirements for optimal (high signal-to-noise) mission output. Power and cross-power spectra in a fiducial setup are derived, as are mock intensity maps. For line power spectrum measurements a cumulative signal-to-noise of O$\left(10^3\right)$, and for respective cross-spectra with SKA 21cm observations of O$\left(10\right)$ to O$\left(10^2\right)$ are possible per redshift bin around the midpoint of reionization. These high signal-to-noise tomographic measurements are in reach for line sensitivities $>8\times 10^{-18}$ergs${}^{-1}$sr${}^{-1}$Hz${}^{-1}$, spectral resolution $R>250$ and detector pixel sizes $<2$arcsec; all three requirements are met by the proposed Cosmic Dawn Intensity Mapper (CDIM). For CDIM similar S/N values are in reach for H$\alpha$. Already the planned NASA mission SPHEREx will detect during the EoR Ly$\alpha$ autopower and cross power with 21cm, for sensitivities better than $10^{-18}$ergs${}^{-1}$sr${}^{-1}$Hz${}^{-1}$ in a moderate 21cm foreground scenario (better than $10^{-17}$ergs${}^{-1}$sr${}^{-1}$Hz${}^{-1}$ in an optimistic scenario). We advocate for IR missions in flavor of CDIM for a leap in IM and finish by providing a cookbook for successful multi-line IM during the EoR.

arXiv comment12 pages, 6 (+2) figures. Figure 4 and 6 as well as section 6 present main conclusions. v2 adds prospects for measurements with HERA, as well appendices with background on IGM attenuation, auto-power spectra, and the Knox criterion for optimised errors

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Cited by in corpus (13)

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