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HI intensity mapping for clustering-based redshift estimation

Research output: Contribution to journalArticle

Precision cosmology requires accurate galaxy redshifts, but next generation optical surveys will observe unprecedented numbers of resolved galaxies, placing strain on the amount of spectroscopic follow-up required. We show how useful information can be gained on the redshift distributions of optical galaxy samples from spatial cross-correlations with intensity maps of unresolved HI (21cm) spectral line emission. We construct a redshift distribution estimator, which we test using simulations. We utilise the S3-SAX catalogue which includes HI emission information for each galaxy, which we use to construct HI intensity maps. We also make use of simulated LSST and Euclid-like photometry enabling us to apply the HI clustering calibration to realistic simulated photometric redshifts. While taking into account important limitations to HI intensity mapping such as lost k-modes from foreground cleaning and poor angular resolution due to large receiver beams, we show that excellent constraints on redshift distributions can be provided for an optical photometric sample.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Early online date27 Oct 2018
DOIs
Publication statusEarly online - 27 Oct 2018

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  • HI intensity mapping

    Rights statement: This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Steven Cunnington, Ian Harrison, Alkistis Pourtsidou, David Bacon; HI Intensity Mapping for Clustering-Based Redshift Estimation, Monthly Notices of the Royal Astronomical Society, sty2928, DOI: 10.1093/mnras/sty2928, is available online at: https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/sty2928/5145866.

    Accepted author manuscript (Post-print), 1.66 MB, PDF document

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