The dispersion–brightness relation for fast radio bursts from a wide-field survey

Shannon, R. M.; Macquart, Jean–Pierre; Bannister, K. W.; Ekers, R. D.; James, C. W.; Osłowski, S.; Qiu, Hao; Sammons, Mawson W.; Hotan, A. W.; Voronkov, M. A.; Beresford, Ron; Brown, Alex; Bunton, John D.; Chippendale, A. P.; Haskins, Christopher B.; Leach, M.; Marquarding, M.; McConnell, D.; Pilawa, M. A.; Sadler, E. M.; Troup, E. R.; Tuthill, J.; Whiting, M. T.; Allison, J. R.; Anderson, Craig S.; Bell, M. E.; Collier, J. D.; Gürkan, G.; Heald, G.; Riseley, C. J.

doi:10.1038/s41586-018-0588-y

Cited by 300 publications

(427 citation statements)

References 30 publications

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“…Some bursts have been detected with (sub-)millisecond temporal structure (Champion et al 2016;Farah et al 2018;Shannon et al 2018;Hessels et al 2019) thanks to (in some cases) real-time coherent de-dispersion or raw-voltage capture. However, the observed durations of most bursts are limited by the recorded time resolution, intra-channel dispersive smearing or scattering in some cases, making it difficult to study their spectro-temporal structure (Bhandari et al 2018).…”

Section: Introductionmentioning

confidence: 99%

A Sample of Low-energy Bursts from FRB 121102

Gourdji

Michilli

Spitler

et al. 2019

ApJL

181

214

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We present 41 bursts from the first repeating fast radio burst discovered (FRB 121102). A deep search has allowed us to probe unprecedentedly low burst energies during two consecutive observations (separated by one day) using the Arecibo telescope at 1.4 GHz. The bursts are generally detected in less than a third of the 580-MHz observing bandwidth, demonstrating that narrowband FRB signals may be more common than previously thought. We show that the bursts are likely faint versions of previously reported multi-component bursts. There is a striking lack of bursts detected below 1.35 GHz and simultaneous VLA observations at 3 GHz did not detect any of the 41 bursts, but did detect one that was not seen with Arecibo, suggesting preferred radio emission frequencies that vary with epoch. A power law approximation of the cumulative distribution of burst energies yields an index −1.8 ± 0.3 that is much steeper than the previously reported value of ∼ −0.7. The discrepancy may be evidence for a more complex energy distribution. We place constraints on the possibility that the associated persistent radio source is generated by the emission of many faint bursts (∼ 700 ms −1 ). We do not see a connection between burst fluence and wait time. The distribution of wait times follows a log-normal distribution centered around ∼ 200 s; however, some bursts have wait times below 1 s and as short as 26 ms, which is consistent with previous reports of a bimodal distribution. We caution against exclusively integrating over the full observing band during FRB searches, because this can lower signal-to-noise.

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Section: Introductionmentioning

confidence: 99%

A Sample of Low-energy Bursts from FRB 121102

Gourdji

Michilli

Spitler

et al. 2019

ApJL

181

214

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“…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.…”

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confidence: 99%

“…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.…”

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confidence: 99%

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

Bannister

Deller

Phillips

et al. 2019

Science

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413

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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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“…Each panel indicates FRBs detected with each telescope. Dashed lines correspond to detection limits reported in previous works (Spitler et al 2014;Keane & Petroff 2015;Caleb et al 2016;Shannon et al 2018;CHIME/FRB Collaboration et al 2019a). The reported detection limits of ASKAP, CHIME, and Arecibo include the duration dependency explicitly, while those of Parkes and UTMOST do not.…”

Section: Appendix B: Detection Limits Depending On Durationmentioning

confidence: 57%

“…d max is a maximum comoving distance for a FRB with a time-integrated luminosity, L ν rest , to be detected with a specific fluence limit, E lim . In previous studies, E lim is reported in terms of E ν for Parkes and UTMOST (Keane & Petroff 2015;Caleb et al 2016) and in terms of E ν × w 1/2 obs for ASKAP, CHIME, and Arecibo (Shannon et al 2018;CHIME/FRB Collaboration et al 2019a;Spitler et al 2014). To avoid systematic offsets in the luminosity functions due to the different definitions of E lim , we empirically derived E lim for each telescope with the same definition described in Appendix B.…”

Section: Calculation Of Luminosity Functionmentioning

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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The dispersion–brightness relation for fast radio bursts from a wide-field survey

Cited by 300 publications

References 30 publications

A Sample of Low-energy Bursts from FRB 121102

A Sample of Low-energy Bursts from FRB 121102

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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