Forecasting constraints on the baryon mass fraction in the IGM from fast radio bursts and type Ia supernovae

Thais Lemos; Rodrigo Gonçalves; Joel Carvalho; Jailson Alcaniz

doi:10.1140/epjc/s10052-023-12248-6

2024 Impact factor 4.8

Particles and Fields

Open Access

Eur. Phys. J. C (2023) 83: 1128
https://doi.org/10.1140/epjc/s10052-023-12248-6

Regular Article - Theoretical Physics

Forecasting constraints on the baryon mass fraction in the IGM from fast radio bursts and type Ia supernovae

Thais Lemos¹^a, Rodrigo Gonçalves², Joel Carvalho¹ and Jailson Alcaniz¹

¹ Observatório Nacional, 20921-400, Rio de Janeiro, RJ, Brazil
² Departamento de Física, Universidade Federal Rural do Rio de Janeiro, 23897-000, Seropédica, RJ, Brazil

^a thaislemos@on.br

Received: 1 August 2023
Accepted: 10 November 2023
Published online: 14 December 2023

Abstract

Fast Radio Bursts (FRBs) are millisecond transient radio events with a high energy. By identifying the origin of the burst, it is possible to measure the redshift of the host galaxy, which can be used to constrain cosmological and astrophysical parameters and test aspects of fundamental physics when combined with the dispersion measure (DM). However, some factors limit the cosmological application of FRBs: (i) the poor modelling of the fluctuations in the DM due to spatial variation in the cosmic electrons density; (ii) the fact that the fraction of baryon mass in the intergalactic medium ( $f_{IGM}$ $f_{IGM}$ ) is degenerated with some cosmological parameters; (iii) the limited knowledge about host galaxy contribution ( $D M_{host}$ $DM_{host}$ ). In this work, we investigate the impact of different redshift distribution models of FRBs to constrain the baryon fraction in the IGM and host galaxy contribution. We use a cosmological model-independent method developed in previous work Lemos (EPJC 83:138, 2023) to perform the analysis and combine simulated FRB data from Monte Carlo simulation and supernovae data. We assume four distribution models for the FRBs: gamma-ray bursts (GRB), star formation rate (SFR), uniform and equidistant (ED). Also, we consider samples with $N = 15, 30, 100$ $$N = 15, 30, 100$$ and 500 points and different values of the fluctuations of electron density in the DM, $δ = 0, 100, 200, 400, 230 \sqrt{z}$ $\delta = 0, 100, 200, 400, 230\sqrt{z}$ pc/cm $^{3}$ $^{3}$ . Our analysis shows that all the distribution models present consistent results within $2 σ$ $2\sigma$ for the free parameters $f_{IGM}$ $f_{IGM}$ and $D M_{h o s t, 0}$ $DM_{host,0}$ and highlights the crucial role of DM fluctuations in obtaining more precise measurements.

Supplementary Information The online version contains supplementary material available at https://doi.org/10.1140/epjc/s10052-023-12248-6.

© The Author(s) 2023

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