User’s guide to extracting cosmological information from line-intensity maps

Bernal, José Luís; Breysse, Patrick C.; Gil-Marín, Héctor; Kovetz, Ely D.

doi:10.1103/physrevd.100.123522

Cited by 79 publications

(75 citation statements)

References 161 publications

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“…In future work we plan to investigate a suite of different models and perform fitting and cosmological parameter estimation analyses using MCMC, extending previous works (Pourtsidou et al 2017;Bacon et al 2018;Castorina & White 2019;Bernal et al 2019). This will also look into more detail of the optimal approach for dealing with the foreground contaminated regions.…”

Section: Resultsmentioning

confidence: 87%

Multipole expansion for H i intensity mapping experiments: simulations and modelling

Cunnington

Pourtsidou

Soares

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a framework and an open-source python toolkit to analyse the two-point statistics of 3D fluctuations in the context of H i intensity maps using the multipole expansion formalism. We include simulations of the cosmological H i signal using N-body and lognormal methods, foregrounds and their removal, as well as instrumental effects. Using these simulations and analytical modelling, we investigate the impact of foreground cleaning and the instrumental beam on the power spectrum multipoles as well as on the Fourier space clustering wedges. We find that both the instrumental beam and the foreground removal can produce a quadrupole (and a hexadecapole) signal, and demonstrate the importance of controlling and accurately modelling these effects for precision radio cosmology. We conclude that these effects can be modelled with reasonable accuracy using our multipole expansion technique. We also perform a Markov Chain Monte Carlo (MCMC) analysis to showcase the effect of foreground cleaning on the estimation of the H i abundance and bias parameters. The accompanying python toolkit is available at https://github.com/IntensityTools/MultipoleExpansion, and includes an interactive suite of examples to aid new users.

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Section: Resultsmentioning

confidence: 87%

Multipole expansion for H i intensity mapping experiments: simulations and modelling

Cunnington

Pourtsidou

Soares

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…As of yet, the era from (roughly) 2 z 1000 remains largely unconstrained. Future ground-based 21 cm surveys such as HERA [747] and SKA 20 , and other intensity mapping technics, will allow to extend constraints to the cosmic dawn epoch at z 20 [748,749,750,751,752], while future Moon-based experiments could probe the dark ages until z 200 [753,754,755]. At z > 1000, on the other hand, modifications of the expansion history affect the CMB spectra in ways that are much less subject to degeneracies.…”

Section: Effects Of Nonstandard Expansion Rate On the Cmbmentioning

confidence: 99%

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

Allahverdi¹,

Amin²,

Berlin³

et al. 2021

TheOJA

185

140

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It is commonly assumed that the energy density of the Universe was dominated by radiation between reheating after inflation and the onset of matter domination 54,000 years later. While the abundance of light elements indicates that the Universe was radiation dominated during Big Bang Nucleosynthesis (BBN), there is scant evidence that the Universe was radiation dominated prior to BBN. It is therefore possible that the cosmological history was more complicated, with deviations from the standard radiation domination during the earliest epochs. Indeed, several interesting proposals regarding various topics such as the generation of dark matter, matter-antimatter asymmetry, gravitational waves, primordial black holes, or microhalos during a nonstandard expansion phase have been recently made. In this paper, we review various possible causes and consequences of deviations from radiation domination in the early Universe -taking place either before or after BBN -and the constraints on them, as they have been discussed in the literature during the recent years.

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“…Instrument noise presents an additional term that adds variance to the intensity map. While this calculation depends on the specifics of the target line and instrument and is beyond the scope of the current proceeding, we refer the reader to Bernal et al (2019); Oxholm & Switzer (2021) for equations and background. These references also describe the formalism for cosmological forecasts with LIM experiments, relying on the Fisher matrix (Tegmark et al, 1997).…”

Section: Power Spectrum Statisticsmentioning

confidence: 99%

A Beginner’s Guide to Line Intensity Mapping Power Spectra

Oxholm

2022

Proc. Wisc. Space Conf.

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Line intensity mapping (LIM) is an emerging technique in measuring galaxy evolution and the large-scale structure of the universe. LIM surveys measure the cumulative emission from all galaxies emitting a given line at a particular redshift, which trace the distribution of dark matter throughout the universe. In this proceeding, we provide an introduction to LIM modeling, focusing on power spectrum calculation. Beyond these calculations, we describe how these power spectra may be used to constrain properties of galaxy evolution and large-scale structure cosmology. Throughout, we use the anticipated EXCLAIM signal of ionized carbon ([CII]) at redshift z=3 as a case study. Our goal is to provide a starting point to non-experts, e.g. upper-level undergraduate and graduate students familiar with the basics of cosmology, with the tools necessary to understand the literature and generate LIM power spectrum models themselves, while also describing a wide array of literature for continued studies.

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User’s guide to extracting cosmological information from line-intensity maps

Cited by 79 publications

References 161 publications

Multipole expansion for H i intensity mapping experiments: simulations and modelling

Multipole expansion for H i intensity mapping experiments: simulations and modelling

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

A Beginner’s Guide to Line Intensity Mapping Power Spectra

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