Linear relativistic corrections in the spherical Fourier-Bessel power spectrum
Abstract
The three-dimensional galaxy power spectrum is a powerful probe of primordial non-Gaussianity and additional general relativistic (GR) effects on large scales, which can be constrained by the current and upcoming large-scale structure surveys. In this work, we calculate the linear-order relativistic power spectrum in the spherical Fourier-Bessel (SFB) basis, a coordinate system that preserves the geometry of the curved sky and fully accounts for the wide-angle effect. In particular, we model the GR effects present in the discrete SFB power spectrum, which is a more efficient and stable decomposition of the galaxy density field compared to the continuous SFB basis in the presence of radial windows. To validate our GR calculations, we introduce a mapping between the angular power spectrum and the SFB power spectrum, and we compare our calculations with outputs from class. We discuss the rich pattern of GR effects in the SFB basis and compare the GR effects to the local primordial non-Gaussianity (PNG) effect. The Doppler and lensing effects have different angular and Fourier dependence compared to the PNG in the SFB basis, while the gravitational potential term is more degenerate with the PNG and comparable to a signal of 𝑓_(NL) ∼1. We also discuss the potential opportunities of extracting the lensing effect through SFB modes in upcoming LSS surveys.
Copyright and License
© 2024 American Physical Society.
Acknowledgement
We thank the SPHEREx cosmology team for useful discussions. We acknowledge support from the SPHEREx project under a contract from the NASA/GODDARD Space Flight Center to the California Institute of Technology. Part of this work was done at Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).
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Additional details
- Goddard Space Flight Center
- Jet Propulsion Laboratory
- National Aeronautics and Space Administration
- 80NM0018D0004
- Accepted
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2024-11-07Accepted
- Publication Status
- Published