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Similar

A. Slosar, C. Hirata, U. Seljak, S. Ho, and N. Padmanabhan, “Constraints on local primordial non-Gaussianity from large scale structure,” JCAP
Original
2008
Cited alongside, same era.
J. Tinker, A. V. Kravtsov, A. Klypin, K. Abazajian, M. Warren, G. Yepes, S. Gottlöber, and D. E. Holz, “Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality,” Astrophys. J
Original
2008
Cited alongside, same era.
A. Barreira, “On the impact of galaxy bias uncertainties on primordial non-Gaussianity constraints,” JCAP
Original
2009
Cited alongside, same era.
M. R. Krumholz, C. F. McKee, and J. Tumlinson, “The Atomic-to-Molecular Transition in Galaxies. II: H I and H 2
Original
2009
Cited alongside, same era.
X. Chen, “Primordial Non-Gaussianities from Inflation Models,” Advances in Astronomy

Then

D. Alonso and P. G. Ferreira, “Constraining ultralarge-scale cosmology with multiple tracers in optical and radio surveys,” Phys. Rev. D
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2015
Later among the works it cites.
V. Assassi, D. Baumann, and F. Schmidt, “Galaxy bias and primordial non-Gaussianity,” JCAP
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2015
Later among the works it cites.
Aug., 2016
Original
L. B. Newburgh and et al, “HIRAX: a probe of dark energy and radio transients,” in Ground-based and Airborne Telescopes VI · 2016
Later among the works it cites.
T. Lazeyras, C. Wagner, T. Baldauf, and F. Schmidt, “Precision measurement of the local bias of dark matter halos,” JCAP
Original
2016
Later among the works it cites.
E. D. Kovetz, M. P. Viero, A. Lidz, L. Newburgh, M. Rahman, E. Switzer, and et al, “Line-Intensity Mapping: 2017 Status Report,” arXiv e-prints

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2021

The local PNG bias of neutral Hydrogen, ${\rm H_I}$

Barreira, Alexandre

Understand

We use separate universe simulations with the IllustrisTNG galaxy formation model to predict the local PNG bias parameters $b_\phi$ and $b_{\phi\delta}$ of atomic neutral hydrogen, ${\rm H_I}$.

These parameters and their relation to the linear density bias parameter $b_1$ play a key role in observational constraints of the local PNG parameter $f_{\rm NL}$ using the ${\rm H_I}$ power spectrum and bispectrum.
Our results show that the popular calculation based on the universality of the halo mass function overpredicts the $b_\phi(b_1)$ and $b_{\phi\delta}(b_1)$ relations measured in the simulations.
In particular, our results show that at $z \lesssim 1$ the ${\rm H_I}$ power spectrum is more sensitive to $f_{\rm NL}$ compared to previously thought ($b_\phi$ is more negative), but is less sensitive at other epochs ($b_\phi$ is less positive).