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HI intensity mapping for clustering-based redshift estimation

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HI intensity mapping for clustering-based redshift estimation. / Cunnington, Steven; Harrison, Ian; Pourtsidou, Alkistis; Bacon, David.

In: Monthly Notices of the Royal Astronomical Society, 27.10.2018.

Research output: Contribution to journalArticlepeer-review

Harvard

Cunnington, S, Harrison, I, Pourtsidou, A & Bacon, D 2018, 'HI intensity mapping for clustering-based redshift estimation', Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/sty2928

APA

Cunnington, S., Harrison, I., Pourtsidou, A., & Bacon, D. (2018). HI intensity mapping for clustering-based redshift estimation. Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/sty2928

Vancouver

Cunnington S, Harrison I, Pourtsidou A, Bacon D. HI intensity mapping for clustering-based redshift estimation. Monthly Notices of the Royal Astronomical Society. 2018 Oct 27. https://doi.org/10.1093/mnras/sty2928

Author

Cunnington, Steven ; Harrison, Ian ; Pourtsidou, Alkistis ; Bacon, David. / HI intensity mapping for clustering-based redshift estimation. In: Monthly Notices of the Royal Astronomical Society. 2018.

Bibtex

@article{0e4aa506cfa74f33b7dd9f5aae7743cd,
title = "HI intensity mapping for clustering-based redshift estimation",
abstract = "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. ",
keywords = "astro-ph.CO, ST/N000668/1, RCUK, STFC",
author = "Steven Cunnington and Ian Harrison and Alkistis Pourtsidou and David Bacon",
year = "2018",
month = oct,
day = "27",
doi = "10.1093/mnras/sty2928",
language = "English",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",

}

RIS

TY - JOUR

T1 - HI intensity mapping for clustering-based redshift estimation

AU - Cunnington, Steven

AU - Harrison, Ian

AU - Pourtsidou, Alkistis

AU - Bacon, David

PY - 2018/10/27

Y1 - 2018/10/27

N2 - 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.

AB - 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.

KW - astro-ph.CO

KW - ST/N000668/1

KW - RCUK

KW - STFC

U2 - 10.1093/mnras/sty2928

DO - 10.1093/mnras/sty2928

M3 - Article

JO - MNRAS

JF - MNRAS

SN - 0035-8711

ER -

ID: 12062864