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Precision cosmology requires accurate galaxy redshifts, but next generationoptical surveys will observe unprecedented numbers of resolved galaxies,placing strain on the amount of spectroscopic follow-up required. We show howuseful information can be gained on the redshift distributions of opticalgalaxy samples from spatial cross-correlations with intensity maps ofunresolved HI (21cm) spectral line emission. We construct a redshiftdistribution estimator, which we test using simulations. We utilise the S3-SAXcatalogue which includes HI emission information for each galaxy, which we useto construct HI intensity maps. We also make use of simulated LSST andEuclid-like photometry enabling us to apply the HI clustering calibration torealistic simulated photometric redshifts. While taking into account importantlimitations to HI intensity mapping such as lost k-modes from foregroundcleaning and poor angular resolution due to large receiver beams, we show thatexcellent constraints on redshift distributions can be provided for an opticalphotometric sample.

HI Intensity Mapping for Clustering-Based Redshift Estimation