Probing Galactic Halos with Fast Radio Bursts

Prochaska, J. Xavier; Zheng, Yong

doi:10.1093/mnras/stz261

Cited by 212 publications

(273 citation statements)

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“…As a function of the inferred flare energy E flare we show the Lorentz factor of the shocked gas (top), shock radius r sh (middle), and external density n ext immediately ahead of the shock (bottom). Green stars and triangle show the same results for the (apparently) non-repeating FRBs with host galaxy candidates identified by ASKAP and DSA-10, respectively Ravi et al 2019;Prochaska et al 2019;H. Cho et al in prep), while grey points show the other published non-repeating CHIME FRBs without host galaxy candidates (CHIME/FRB Collaboration et al 2019a).…”

Section: Rates and Energeticsmentioning

confidence: 64%

“…Equation (9) can also be re-expressed in terms of the upstream electron (positron) density, Figure 3 shows the values of Γ, r sh , and n ext (r sh ) as a function of E flare for all the bursts from our repeating sample, under the fiducial assumptions f ξ = 10 −3 , m * = m e , and f e = 0.5. Shown for comparison with green points are the same results for the (apparently) non-repeating FRBs with host galaxy candidates identified by ASKAP and DSA-10 Ravi et al 2019;Prochaska et al 2019;H. Cho et al in prep), while grey points show the other published non-repeating CHIME FRBs without host galaxy candidates (CHIME/FRB Collaboration et al 2019a).…”

Section: Properties Of the Flares And External Mediummentioning

confidence: 82%

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Constraints on the engines of fast radio bursts

Margalit

Metzger

Sironi

2020

Monthly Notices of the Royal Astronomical Society

112

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We model the sample of fast radio bursts (FRB), including the newly discovered CHIME repeaters, using the decelerating synchrotron blast wave model of Metzger, Margalit & Sironi (2019), which built on earlier work by Lyubarsky (2014), Beloborodov (2017). This model postulates that FRBs are precursor radiation from ultra-relativistic magnetized shocks generated as flare ejecta from a central engine collides with an effectively stationary external medium. Downward drifting of the burst frequency structure naturally arises from the deceleration of the blast-wave coupled with the dependence of the maser spectral energy distribution, and induced Compton scattering depth, on the upstream medium. The data are consistent with FRBs being produced by flares of energy E flare ∼ 10 43 − 10 46 ( f ξ /10 −3 ) −4/5 erg, where f ξ is the maser efficiency, and minimum bulk Lorentz factors Γ ≈ 10 2 − 10 3 , which generate the observed FRBs at shock radii r sh ∼ 10 12 − 10 13 cm. We infer upstream densities n ext (r sh ) ∼ 10 2 − 10 4 cm −3 and radial profiles n ext ∝ r −k showing a range of slopes k ≈ [−2, 1] (which are seen to evolve between bursts), both broadly consistent with the upstream medium being the inner edge of an ion-loaded shell released by a recent energetic flare. The burst timescales, energetics, rates, and external medium properties are consistent with repeating FRBs arising from young, hyper-active flaring magnetars, but the methodology presented is generally applicable to any central engine which injects energy impulsively into a dense magnetized medium. Several uncertainties and variations of the model regarding the composition and magnetization of the upstream medium, and the effects of the strong electric field of the FRB wave (strength parameter a 1) on the upstream medium and its scattering properties, are discussed. One-dimensional particle-in-cell simulations of magnetized shocks into a pair plasma are presented which demonstrate that high maser efficiency can be preserved, even in the limit a 1 in which the FRB wave accelerates the upstream electrons to ultra-relativistic speeds.

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Section: Rates and Energeticsmentioning

confidence: 64%

Section: Properties Of the Flares And External Mediummentioning

confidence: 82%

Constraints on the engines of fast radio bursts

Margalit

Metzger

Sironi

2020

Monthly Notices of the Royal Astronomical Society

112

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“…This sets the normalization in the above equation. We emphasize that neither f b nor the gas-density profile are well determined for galaxy halos (34,35,41,88,89).…”

Section: S211 the Dispersion Measure Contribution Of Galaxy Amentioning

confidence: 92%

“…as discussed in (34) where ρ 0 b is a normalizing density, y is dimensionless radial coordinate, with a steepness index set to α = 2 and (dimensionless) scale length y 0 = 2.; (ii) the halo contains a cosmic fraction of baryons, i.e.…”

Section: S211 the Dispersion Measure Contribution Of Galaxy Amentioning

confidence: 99%

A single fast radio burst localized to a massive galaxy at cosmological distance

Bannister

Deller

Phillips

et al. 2019

Science

400

353

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Fast Radio Bursts (FRBs) are brief radio emissions from distant astronomical sources. Some are known to repeat, but most are single bursts. Non-repeating FRB observations have had insufficient positional accuracy to localize them to an individual host galaxy. We report the interferometric localization of the single pulse FRB 180924 to a position 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst has not been observed to repeat. The properties of the burst and its host are markedly different from the only other accurately localized FRB source. The integrated electron column density along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.Cosmological observations have shown that baryons comprise 4% of the energy density of the Universe, of which only about 10% is in cold gas and stars (1), with the remainder residing in a diffuse plasma surrounding and in between galaxies and galaxy clusters. The location and density of this material has been challenging to characterize, and up to 50% of it remains unaccounted (2).Fast radio bursts (FRBs; ref.(3)) are bright bursts of radio waves with millisecond duration. They can potentially be used to detect, study, and map this medium, as bursts of emission are dispersed and scattered by their 1 arXiv:1906.11476v1 [astro-ph.HE] 27 Jun 2019 dual-polarization beams on the sky using digital beamforming, producing a total field-of-view of ∼ 30 deg 2 . For burst detection, the beamformers produces channelized autocorrelation spectra for both linear polarizations of all beams, with an integration time of 864 µs and channel bandwidth of 1 MHz in these observations. We used 336 channels centered at 1320 MHz. A real-time detection pipeline incoherently adds the spectra from all available antennas (24 antennas in these observations) and polarization channels, then searches (16) the result for dispersed pulses (17).Burst localization is completed with a second data product that utilizes both the amplitude and phase information of the burst radiation. The beamformers store samples of the complex electric field for all beams and both polarizations in a ring buffer of 3.1 s duration, with the oldest data being continuously overwritten by new data. The data are saved for offline interferometric analysis only when the pipeline identifies a candidate. For the searches reported here the triggering required pulses with widths less than 9 ms and S/N > 10.Previous searches with ASKAP used antennas pointed in different directions to maximize sky coverage (10,16). In contrast, our observations used antennas all pointed in the same direction, enabling the array to act as an interferometer capable of sub-arcsecond localization with a 30 deg 2 field of view. We targeted high Galactic latitude fields (Galactic latitude |b| ∼ 50 • ), that had been observed previously (10, 16), and Southern circumpolar fields. The high-latitude fields were observed regularly through 2017 and earl...

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“…For these four FRBs we use the spectroscopic redshifts instead of the redshift estimated from the dispersion measure. Recently another host galaxy was identified (FRB 181112 host; Prochaska et al 2019). This burst is not included in this work, since the burst information has not been listed in the FRBCAT as of 21 August 2019.…”

Section: Samplementioning

confidence: 99%

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

Hashimoto

Goto

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Fast radio bursts (FRBs) are mysterious radio bursts with a time scale of approximately milliseconds. Two populations of FRB, namely repeating and non-repeating FRBs, are observationally identified. However, the differences between these two and their origins are still cloaked in mystery. Here we show the time-integrated luminosityduration (L ν -w int,rest ) relations and luminosity functions (LFs) of repeating and nonrepeating FRBs in the FRB Catalogue project. These two populations are obviously separated in the L ν -w int,rest plane with distinct LFs, i.e., repeating FRBs have relatively fainter L ν and longer w int,rest with a much lower LF. In contrast with non-repeating FRBs, repeating FRBs do not show any clear correlation between L ν and w int,rest . These results suggest essentially different physical origins of the two. The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron-star mergers and accretion-induced collapse (AIC) of white dwarfs, and are consistent with those of soft gamma-ray repeaters (SGRs), type Ia supernovae, magnetars, and white-dwarf mergers. This indicates two possibilities: either (i) faint non-repeating FRBs originate in neutron-star mergers or AIC and are actually repeating during the lifetime of the progenitor, or (ii) faint non-repeating FRBs originate in any of SGRs, type Ia supernovae, magnetars, and white-dwarf mergers. The bright ends of LFs of repeating and non-repeating FRBs are lower than any candidates of progenitors, suggesting that bright FRBs are produced from a very small fraction of the progenitors regardless of the repetition. Otherwise, they might originate in unknown progenitors.

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Probing Galactic Halos with Fast Radio Bursts

Cited by 212 publications

References 130 publications

Constraints on the engines of fast radio bursts

Constraints on the engines of fast radio bursts

A single fast radio burst localized to a massive galaxy at cosmological distance

Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts

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