Quijote-PNG: The Information Content of the Halo Mass Function
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arXiv
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2023
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| author | Jung, Gabriel Ravenni, Andrea Baldi, Marco Coulton, William R. Jamieson, Drew Karagiannis, Dionysios Liguori, Michele Shao, Helen Verde, Licia Villaescusa-Navarro, Francisco Wandelt, Benjamin D. |
| author_facet | Jung, Gabriel Ravenni, Andrea Baldi, Marco Coulton, William R. Jamieson, Drew Karagiannis, Dionysios Liguori, Michele Shao, Helen Verde, Licia Villaescusa-Navarro, Francisco Wandelt, Benjamin D. |
| contents | We study signatures of primordial non-Gaussianity (PNG) in the redshift-space halo field on non-linear scales, using a combination of three summary statistics, namely the halo mass function (HMF), power spectrum, and bispectrum. The choice of adding the HMF to our previous joint analysis of power spectrum and bispectrum is driven by a preliminary field-level analysis, in which we train graph neural networks on halo catalogues to infer the PNG $f_\mathrm{NL}$ parameter. The covariance matrix and the responses of our summaries to changes in model parameters are extracted from a suite of halo catalogues constructed from the Quijote-PNG N-body simulations. We consider the three main types of PNG: local, equilateral and orthogonal. Adding the HMF to our previous joint analysis of power spectrum and bispectrum produces two main effects. First, it reduces the equilateral $f_\mathrm{NL}$ predicted errors by roughly a factor $2$, while also producing notable, although smaller, improvements for orthogonal PNG. Second, it helps break the degeneracy between the local PNG amplitude, $f_\mathrm{NL}^\mathrm{local}$, and assembly bias, $b_ϕ$, without relying on any external prior assumption. Our final forecasts for PNG parameters are $Δf_\mathrm{NL}^\mathrm{local} = 40$, $Δf_\mathrm{NL}^\mathrm{equil} = 210$, $Δf_\mathrm{NL}^\mathrm{ortho} = 91$, on a cubic volume of $1 \left(h^{-1}{\rm Gpc}\right)^3$, with a halo number density of $\bar{n}\sim 5.1 \times 10^{-5}~h^3\mathrm{Mpc}^{-3}$, at $z = 1$, and considering scales up to $k_\mathrm{max} = 0.5~h\,\mathrm{Mpc}^{-1}$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2305_10597 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Quijote-PNG: The Information Content of the Halo Mass Function Jung, Gabriel Ravenni, Andrea Baldi, Marco Coulton, William R. Jamieson, Drew Karagiannis, Dionysios Liguori, Michele Shao, Helen Verde, Licia Villaescusa-Navarro, Francisco Wandelt, Benjamin D. Cosmology and Nongalactic Astrophysics We study signatures of primordial non-Gaussianity (PNG) in the redshift-space halo field on non-linear scales, using a combination of three summary statistics, namely the halo mass function (HMF), power spectrum, and bispectrum. The choice of adding the HMF to our previous joint analysis of power spectrum and bispectrum is driven by a preliminary field-level analysis, in which we train graph neural networks on halo catalogues to infer the PNG $f_\mathrm{NL}$ parameter. The covariance matrix and the responses of our summaries to changes in model parameters are extracted from a suite of halo catalogues constructed from the Quijote-PNG N-body simulations. We consider the three main types of PNG: local, equilateral and orthogonal. Adding the HMF to our previous joint analysis of power spectrum and bispectrum produces two main effects. First, it reduces the equilateral $f_\mathrm{NL}$ predicted errors by roughly a factor $2$, while also producing notable, although smaller, improvements for orthogonal PNG. Second, it helps break the degeneracy between the local PNG amplitude, $f_\mathrm{NL}^\mathrm{local}$, and assembly bias, $b_ϕ$, without relying on any external prior assumption. Our final forecasts for PNG parameters are $Δf_\mathrm{NL}^\mathrm{local} = 40$, $Δf_\mathrm{NL}^\mathrm{equil} = 210$, $Δf_\mathrm{NL}^\mathrm{ortho} = 91$, on a cubic volume of $1 \left(h^{-1}{\rm Gpc}\right)^3$, with a halo number density of $\bar{n}\sim 5.1 \times 10^{-5}~h^3\mathrm{Mpc}^{-3}$, at $z = 1$, and considering scales up to $k_\mathrm{max} = 0.5~h\,\mathrm{Mpc}^{-1}$. |
| title | Quijote-PNG: The Information Content of the Halo Mass Function |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2305.10597 |