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    Effects of [N ii] and H α line blending on the WFIRST Galaxy redshift survey

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    Author
    Martens, Daniel
    Fang, Xiao
    Troxel, M A
    DeRose, Joe
    Hirata, Christopher M
    Wechsler, Risa H
    Wang, Yun
    Affiliation
    Univ Arizona, Dept Astron
    Univ Arizona, Steward Observ
    Issue Date
    2019-02-08
    Keywords
    line: identification
    surveys
    cosmology: observations
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    Daniel Martens, Xiao Fang, M A Troxel, Joe DeRose, Christopher M Hirata, Risa H Wechsler, Yun Wang, Effects of [N ii] and H α line blending on the WFIRST Galaxy redshift survey, Monthly Notices of the Royal Astronomical Society, Volume 485, Issue 1, May 2019, Pages 211–228, https://doi.org/10.1093/mnras/stz391
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    Copyright © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    The Wide Field Infrared Survey Telescope (WFIRST) will conduct a galaxy redshift survey using the H α emission line primarily for spectroscopic redshift determination. Due to the modest spectroscopic resolution of the grism, the H α and the neighbouring [N ii] lines are blended, leading to a redshift bias that depends on the [N ii]/H α ratio, which is correlated with a galaxy’s metallicity, hence mass and ultimately environment. We investigate how this bias propagates into the galaxy clustering and cosmological parameters obtained from the WFIRST. Using simulation, we explore the effect of line blending on redshift-space distortion and baryon acoustic oscillation (BAO) measurements. We measure the BAO parameters α∥, α⊥, the logarithmic growth factor fv, and calculate their errors based on the correlations between the line ratio and large-scale structure. We find Δα∥=0.31±0.23 per cent (⁠0.26±0.17 per cent⁠), Δα⊥=−0.10±0.10 per cent (⁠−0.12±0.11 per cent⁠), and Δfv=0.17±0.33 per cent (⁠−0.20±0.30 per cent⁠) for redshift 1.355–1.994 (0.700–1.345), which use approximately 18  per cent⁠, 9  per cent⁠, and 7  per cent of the systematic error budget in a root-sum-square sense. These errors may already be tolerable but further mitigations are discussed. Biases due to the environment-independent redshift error can be mitigated by measuring the redshift error probability distribution function. High-spectral-resolution reobservation of a few thousand galaxies would be required (if by direct approach) to reduce them to below 25  per cent of the error budget. Finally, we outline the next steps to improve the modelling of [N ii]-induced blending biases and their interaction with other redshift error sources.
    ISSN
    0035-8711
    DOI
    10.1093/mnras/stz391
    Version
    Final published version
    Sponsors
    Simons Foundation; U.S. Department of Energy [DE-AC02-76SF00515]; Packard Foundation; NSF; NASA [NNG16PJ25C]; NASA ROSES ATP [16-ATP16-0084]; U.S. Department of Energy Office
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz391
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