Joint analyses of 2D CMB lensing and 3D galaxy clustering in the spherical Fourier-Bessel basis

2021/10/31 by Yucheng Zhang, Anthony R. Pullen, Abhishek S. Maniyar
Mathematics · Physics and Astronomy · #Astrophysics #Basis (linear algebra) #Bessel function #Black Holes and Theoretical Physics #Cluster analysis #Cosmic microwave background #Cosmology and Gravitation Theories #Fourier transform #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geometry #Joint (building) #Mathematics #Optics #Physics #Statistics #astro-ph.CO

paper · pdf · doi:10.1103/physrevd.104.103523

published as Phys. Rev. D 104, 103523 (2021) · 21 pages, 14 figures, 3 tables; references added, published in PRD

openalex publication_date 2021/11/19 · arxiv created 2021/11/22 · arxiv updated 2021/11/23 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

Cross-correlating cosmic microwave background (CMB) lensing and galaxy clustering has been shown to greatly improve the constraints on the local primordial non-Gaussianity (PNG) parameter f_NL by reducing sample variance and also parameter degeneracies. To model the full use of the 3D information of galaxy clustering, we forecast f_NL measurements using the decomposition in the spherical Fourier-Bessel (SFB) basis, which can be naturally cross-correlated with 2D CMB lensing in spherical harmonics. In the meantime, such a decomposition would also enable us to constrain the growth rate of structure, a probe of gravity, through the redshift-space distortion (RSD). As a comparison, we also consider the tomographic spherical harmonic (TSH) analysis of galaxy samples with different bin sizes. Assuming galaxy samples that mimic a few future surveys, we perform Fisher forecasts using linear modes for f_NL and the growth-rate exponent \ensuremathγ, marginalized over standard \mathrm\ensuremathΛ cold dark matter (\mathrm\ensuremathΛCDM) cosmological parameters and two nuisance parameters that account for clustering bias and magnification bias. Compared to TSH analysis using only one bin, SFB analysis could improve \ensuremathσ(f_NL) by a factor of 3 to 12 thanks to large radial modes. With future wide-field and high-redshift photometric surveys like the LSST, the constraint \ensuremathσ(f_NL)<1 could be achieved using linear angular multipoles up to \ensuremathℓ_min\ensuremath≃20. Compared to using galaxy autopower spectra only, joint analyses with CMB lensing could improve \ensuremathσ(\ensuremathγ) by a factor of 2 to 5 by reducing degeneracies with other parameters, especially the clustering bias. For future spectroscopic surveys like the DESI or Euclid, using linear scales, \ensuremathγ could be constrained to 3% precision, assuming the GR fiducial value.

Citations

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