The Dispersion of Fast Radio Bursts from a Structured Intergalactic Medium at Redshifts z &lt; 1.5

Shull, Michael; Danforth, Charles W.

doi:10.3847/2041-8213/aaa2fa

Cited by 51 publications

(57 citation statements)

References 49 publications

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“…where we adopt a rough median value for N OVII (see also Shull & Danforth 2018 and PZ19 for similar estimates). Meanwhile, our model predicts DM halo = 30-70 pc cm −3 over the same region of the sky.…”

Section: Absorption Line Measurementsmentioning

confidence: 99%

“…In general, the observed total dispersion for an extragalactic source DM obs can be split into the four components as DM obs = DM ISM + DM halo + DM IGM + DM host , (1) where DM ISM is the contribution from the warm ionized medium (WIM; T 10 4 K) of interstellar medium (ISM) in the MW disk, DM halo is that from the extended hot Galactic halo (T ∼ 10 6 -10 7 K), DM IGM is that from IGM, and DM host is that from the host galaxy including the local surrounding environment of the source. Here we neglected the contribution from intervening galaxy halos (McQuinn 2014;Shull & Danforth 2018;Prochaska & Neeleman 2018;Prochaska & Zheng 2019). In principle we can estimate the contribution of MW electrons to total DM (i.e., DM ISM and DM halo ) for the direction of an observed radio source, thereby obtaining a rough estimate of the maximum source distance through the analytic DM IGM -z relation (Ioka 2003;Inoue 2004;Deng & Zhang 2014;McQuinn 2014;Shull & Danforth 2018;Li et al 2019, for simulation study see also Dolag et al 2015;Pol et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…The distribution of hot gas (kT ∼ 0.3 keV) in the MW halo has been studied based on analytic gas density profile or numerical simulations, with observational constraints from oxygen absorption lines in UV or X-ray bands, emission measure (EM) of diffuse X-ray emission, and DM toward the Large Magellanic Cloud (LMC) (Maller & Bullock 2004;Sommer-Larsen 2006;Yao et al 2009;Fang et al 2013;Nuza et al 2014;Dolag et al 2015;Tepper-García et al 2015;Roca-Fàbrega et al 2016;Faerman et al 2017;Fielding et al 2017;Li & Bregman 2017;Nakashima et al 2018;Shull & Danforth 2018;Prochaska & Zheng 2019). The DM value estimated by these modelings is DM halo ∼ 30-80 pc cm −3 .…”

Section: Introductionmentioning

confidence: 99%

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The Galactic Halo Contribution to the Dispersion Measure of Extragalactic Fast Radio Bursts

Yamasaki

Totani

2020

ApJ

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A new model of the Milky Way (MW) halo component of the dispersion measure (DM) for extragalactic sources, such as fast radio bursts (FRBs), is presented in light of recent diffuse X-ray observations. In addition to the spherical component of isothermal gas (kT ∼ 0.3 keV) in hydrostatic equilibrium with the Galactic gravitational potential, our model includes a disk-like non-spherical hot gas component to reproduce the directional dependence of the observed X-ray emission measure (EM). The total gas mass (1.2 × 10 11 M ) is dominated by the spherical component, and is consistent with the total baryon mass of the MW expected from the dark matter mass and the cosmic baryon-to-dark-matter ratio. Our model predicts a mean halo DM of 43 pc cm −3 , with a full range of 30-245 pc cm −3 over the whole sky. The large scatter seen in the X-ray EM data implies a ∼ 0.2 dex (rms) fluctuation of the MW halo DM. We provide an analytic formula to estimate the MW halo DM of our model along any line of sight, which can be easily used to compute the total MW component of DM toward extragalactic sources, in combination with existing DM models of the warm ionized medium associated with the Galactic disk.

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Section: Absorption Line Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Galactic Halo Contribution to the Dispersion Measure of Extragalactic Fast Radio Bursts

Yamasaki

Totani

2020

ApJ

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“…Differences between sightline fluctuations of n e will cause sightline-to-sightline scatter in DM cos . It is expected the primary contribution to the scatter will come from dark matter halos that are overdense in baryons, while the scatter due to fluctuations in voids, sheets and filaments of the IGM will be subdominant [19,52]. Since halos with mass M h < 10 10 M are below the Jeans Mass of the IGM, and so are unlikely to be overdense in gas, only halos with mass M h ≥ 10 10 M will likely contribute to the scatter.…”

Section: B Distribution Of Dmsmentioning

confidence: 99%

“…Additional scatter is added to DM cos to account for sheets, filaments and voids in the IGM, as well as imperfect subtraction of Milky Way and host galaxy components. We assume these components take the form of zero mean Gaussian noise, with σ IGM = 10 pc cm −3 [19], σ MW = 15 pc cm −3 [54], and σ host = 50 pc cm −3 [49,53], which we add in quadrature to give σ = 53 pc cm −3 .…”

Section: Mock Datamentioning

confidence: 99%

Probing diffuse gas with fast radio bursts

Walters

Sievers

et al. 2019

Phys. Rev. D

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The dispersion measure -redshift relation of Fast Radio Bursts, DM(z), has been proposed as a potential new probe of the cosmos, complementary to existing techniques. In practice, however, the effectiveness of this approach depends on a number of factors, including (but not limited to) the intrinsic scatter in the data caused by intervening matter inhomogeneities. Here, we simulate a number of catalogues of mock FRB observations, and use MCMC techniques to forecast constraints, and assess which parameters will likely be best constrained. In all cases we find that any potential improvement in cosmological constraints are limited by the current uncertainty on the the diffuse gas fraction, f d (z). Instead, we find that the precision of current cosmological constraints allows one to constrain f d (z), and possibly its redshift evolution. Combining CMB + BAO + SNe + H0 constraints with just 100 FRBs (with redshifts), we find a typical constraint on the mean diffuse gas fraction of a few percent. A detection of this nature would alleviate the "missing baryon problem", and therefore highlights the value of localisation and spectroscopic followup of future FRB detections.

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Portraying the missing baryonic mass at the cosmic noon: the contribution of CUBES

D’Odorico

2022

Exp Astron

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The cosmological and galactic missing baryon problems are briefly reviewed with a particular focus on the contributions to the baryonic census derived from the analysis of quasar absorption spectra. The CUBES spectrograph foreseen for the ESO VLT, with its exceptional efficiency ($$> 40$$ > 40 %), blue wavelength coverage ($$\lambda \simeq 300-405$$ λ ≃ 300 - 405 nm) and intermediate resolution ($$R\simeq 24,000$$ R ≃ 24 , 000 ) will allow us to tackle this issue with two approaches: using H i Lyman-$$\alpha$$ α lines at $$z \simeq 1.5-2.3$$ z ≃ 1.5 - 2.3 , just after the peak of star formation, and using O vi absorbers at $$z \simeq 1.9-2.9$$ z ≃ 1.9 - 2.9 , at the cosmic noon. In both cases, in order to derive the baryonic masses it will be necessary to acquire also higher-resolution spectra of the same target quasars to cover the region at longer wavelengths. We simulate the observations with the CUBES E2E simulator considering a sample of 40 bright quasars at redshifts $$z_\mathrm{em}\sim 2-3$$ z em ∼ 2 - 3 observed for a total time of $$\sim 13$$ ∼ 13 h to reach a signal-to-noise ratio of $$\sim 15$$ ∼ 15 in the H i Lyman-$$\alpha$$ α , O vi forests.

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The Dispersion of Fast Radio Bursts from a Structured Intergalactic Medium at Redshifts z < 1.5

Cited by 51 publications

References 49 publications

The Galactic Halo Contribution to the Dispersion Measure of Extragalactic Fast Radio Bursts

The Galactic Halo Contribution to the Dispersion Measure of Extragalactic Fast Radio Bursts

Probing diffuse gas with fast radio bursts

Portraying the missing baryonic mass at the cosmic noon: the contribution of CUBES

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