FRBCAT: The Fast Radio Burst Catalogue

Petroff, Emily; Barr, E. D.; Jameson, A.; Keane, E. F.; Bailes, M.; Krämer, M.; Morello, Vincent; Tabbara, D.; Straten, W. van

doi:10.1017/pasa.2016.35

Cited by 575 publications

(606 citation statements)

References 27 publications

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“…Fast radio bursts Fast Radio Bursts (FRBs) can be used to probe extragalactic magnetic fields across cosmological distances. So far, only a few dozen FRBs have been detected (Petroff et al, 2016), and the dispersion measure of their emission, defined as: 18 eV. Such a large anisotropy is hard to reconcile with any of our models, and it might be explained by a significantly dipolar distribution of sources, as we discuss in detail in Hackstein et al (2017).…”

Section: Ultra-high Energy Cosmic Rays (Uhecr) Cosmic Rays With Energmentioning

confidence: 75%

Simulations of extragalactic magnetic fields and of their observables

Vazza

Brüggen

Gheller³

et al. 2017

Class. Quantum Grav.

136

228

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Abstract. The origin of extragalactic magnetic fields is still poorly understood. Based on a dedicated suite of cosmological magneto-hydrodynamical simulations with the ENZO code we have performed a survey of different models that may have caused present-day magnetic fields in galaxies and galaxy clusters. The outcomes of these models differ in cluster outskirts, filaments, sheets and voids and we use these simulations to find observational signatures of magnetogenesis. With these simulations, we predict the signal of extragalactic magnetic fields in radio observations of synchrotron emission from the cosmic web, in Faraday Rotation, in the propagation of Ultra High Energy Cosmic Rays, in the polarized signal from Fast Radio Bursts at cosmological distance and in spectra of distant blazars. In general, primordial scenarios in which present-day magnetic fields originate from the amplification of weak (≤ nG) uniform seed fields result more homogeneous and relatively easier to observe magnetic fields than than astrophysical scenarios, in which present-day fields are the product of feedback processes triggered by stars and active galaxies. In the near future the best evidence for the origin of cosmic magnetic fields will most likely come from a combination of synchrotron emission and Faraday Rotation observed at the periphery of large-scale structures.

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Section: Ultra-high Energy Cosmic Rays (Uhecr) Cosmic Rays With Energmentioning

confidence: 75%

Simulations of extragalactic magnetic fields and of their observables

Vazza

Brüggen

Gheller³

et al. 2017

Class. Quantum Grav.

136

228

View full text Add to dashboard Cite

show abstract

“…The observed range of dispersion measures, DM ≡ n e d ≈ 300 − 1600 cm −3 pc (Petroff et al 2016) corresponds to column densities of intervening electrons N e ≈ (1 − 5) × 10 21 cm −2 . Most FRBs are isolated events, with the exception of the repeating FRB 121102 ) which was identified with a low-metallicity dwarf galaxy at z = 0.193 Bassa et al 2017).…”

Section: Introductionmentioning

confidence: 92%

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

Shull¹,

Danforth²

2018

ApJL

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We analyze the sources of free electrons that produce the large dispersion measures, DM ≈ 300 − 1600 (in units cm −3 pc), observed toward fast radio bursts (FRBs). Individual galaxies typically produce DM ∼ 25 − 60 cm −3 pc from ionized gas in their disk, disk-halo interface, and circumgalactic medium. Toward an FRB source at redshift z, a homogeneous IGM containing a fraction f IGM of cosmological baryons will produce DM = (935 cm. A structured IGM of photoionized Lyα absorbers in the cosmic web produces similar dispersion, modeled from the observed distribution, f b (N, z), of H I (Lyα-forest) absorbers in column density and redshift with ionization corrections and scaling relations from cosmological simulations. An analytic formula for DM(z) applied to observed FRB dispersions suggests that z FRB ≈ 0.2 − 1.5 for an IGM containing a significant baryon fraction, f IGM = 0.6 ± 0.1. Future surveys of the statistical distribution, DM(z), of FRBs identified with specific galaxies and redshifts can be used to calibrate the IGM baryon fraction and distribution of Lyα absorbers. Fluctuations in DM at the level ±10 cm −3 pc will arise from filaments and voids in the cosmic web.

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“…For an intrinsic pulse width W 5 i = ms, scattering time t 0 scatt = ms, and a DM of 756 pc cm −3 (mean DM of known FRBs; Petroff et al 2016), the minimum detectable flux density for the GBNCC survey is 0.63 Jy. We note that there is a reduction in sensitivity to high-DM events since the dispersive delay for these events across a bandwidth of 100 MHz is a large fraction of the observation time per pointing.…”

Section: Survey Sensitivitymentioning

confidence: 99%

“…At the time of writing, eighteen FRBs have been discovered (Lorimer et al 2007;Keane et al 2012;Thornton et al 2013;Burke-Spolaor & Bannister 2014;Masui et al 2015;Petroff et al 2015;Ravi et al 2015Ravi et al , 2016Champion et al 2016;Keane et al 2016), with only one source (Spitler et al 2014 known to repeat. A catalog of these bursts and their properties is made available by Petroff et al (2016).…”

Section: Introductionmentioning

confidence: 99%

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Chawla

Kaspi

Josephy

et al. 2017

ApJ

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We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm −3 , while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm −3 . No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of 3.6 10 3FRBs sky −1 day −1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index α by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for α>+0.35 in the absence of scattering and free-free absorption and α>−0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz).

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FRBCAT: The Fast Radio Burst Catalogue

Cited by 575 publications

References 27 publications

Simulations of extragalactic magnetic fields and of their observables

Simulations of extragalactic magnetic fields and of their observables

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

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

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