Use of fast radio burst dispersion measures as distance measures

Kumar, Pawan; Linder, Eric V.

doi:10.1103/physrevd.100.083533

Cited by 36 publications

(20 citation statements)

References 74 publications

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“…The repeating rate above the threshold energy for each source r(E th ) is small in that P det 1 is well satisfied, so the detection probability is linearly proportional to the total observing time spent on each source, independent of the arrangement of observing runs as shown by equation (A14). 6 This is also supported by two other observations: (1) One of the ASKAP apparent non-repeaters is seen to repeat when observed with a more sensitive telescope (Kumar et al 2019); (2) CHIME has only detected one burst from FRB 121102 (Josephy et al 2019), so this well-known repeating source would be considered as a non-repeater if it were only detected by CHIME.…”

Section: Implications Of γmentioning

confidence: 57%

“…We use the following priors: 0.2 < k < 1.3, 1.2 < γ < 3, 0 < β < 3. The lower limit of k is motivated by the studies of FRB 121102 by Oppermann et al (2018) and by the fact that the detections of repetitions are often (but not always) spread over multiple observing sessions (C1-C4; Kumar et al 2019;Oostrum et al 2019). The motivation for the prior on redshift evolution is that the source number density is assumed to be somewhere between non-evolving (β = 0) and tracing star formation history (β 3).…”

Section: Single Populationmentioning

confidence: 99%

“…We adopt μ host = 100/(1 + z), σ host = 30/(1 + z), μ IGM (z) = 900z, and σ IGM = 200 √ z, all in units of pc cm −3 . These values are motivated by observational and theoretical studies of (potential) FRB host galaxies (Xu & Han 2015;Tendulkar et al 2017;Luo et al 2018;Bannister et al 2019;Prochaska et al 2019;Marcote et al 2020) and IGM electron density distribution (Deng & Zhang 2014;McQuinn 2014;Shull & Danforth 2018;Kumar & Linder 2019;Prochaska & Zheng 2019;. The σ IGM ∝ √ z behaviour can be roughly understood if one divides the line of sight into many short segments (of e.g.…”

Section: A P P E N D I X B : T H E S To C H a S T I C R E L At I O N B E T W E E N R E D S H I F T A N D Dm Exmentioning

confidence: 99%

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Implications of Canadian Hydrogen Intensity Mapping Experiment repeating fast radio bursts

Piro

Waxman

2020

Monthly Notices of the Royal Astronomical Society

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CHIME has now detected 18 repeating fast radio bursts (FRBs). We explore what can be learned about the energy distribution and activity level of the repeaters by fitting realistic FRB population models to the data. For a power-law energy distribution dN/dE∝E−γ for the repeating bursts, there is a critical index γcrit that controls whether the dispersion measure (DM, a proxy for source distance) distribution of repeaters is bottom or top-heavy. We find γcrit = 7/4 for Poisson wait-time distribution of repeaters in Euclidean space and further demonstrate how it is affected by temporal clustering of repetitions and cosmological effects. It is especially interesting that two of the CHIME repeaters (FRB 181017 and 190417) have large $\rm DM\sim 10^3\rm \, pc\, cm^{-3}$. These can be understood if: (i) the energy distribution is shallow $\gamma =1.7^{+0.3}_{-0.1}$ ($68\%$ confidence) or (ii) a small fraction of sources are extremely active. In the second scenario, these two high-DM sources should be repeating more than 100 times more frequently than FRB 121102, and the energy index is constrained to be $\gamma = 1.9^{+0.3}_{-0.2}$ ($68\%$ confidence). In either case, this γ is consistent with the energy dependence of the non-repeating ASKAP sample, which suggests that they are drawn from the same population. Finally, our model predicts how the CHIME repeating fraction should decrease with redshift, and this can be compared with observations to infer the distribution of activity level in the whole population.

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Section: Implications Of γmentioning

confidence: 57%

Section: Single Populationmentioning

confidence: 99%

Section: A P P E N D I X B : T H E S To C H a S T I C R E L At I O N B E T W E E N R E D S H I F T A N D Dm Exmentioning

confidence: 99%

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Implications of Canadian Hydrogen Intensity Mapping Experiment repeating fast radio bursts

Piro

Waxman

2020

Monthly Notices of the Royal Astronomical Society

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“…The extragalactic FRBs can be used as a cosmic probe to study the evolution of the universe and constrain cosmological parameters. A Combination of FRB with other cosmological probes will be a powerful tool in constraining the dark energy equation of state [249][250][251][252][253][254]. The Friedmann equation can be written as [255]:…”

Section: Dark Energymentioning

confidence: 99%

“…Zhou et al (2014) [249] constrained the equation of state of dark energy using type Ia supernovae (SNe Ia), simulated FRBs and BAO data in the optimistic case that in each narrow-redshift-bin tens of FRBs have been detected. FRB can also be associated with other cosmological probes to constrain the dark energy equation of state, such as GRB/FRB system [251], lensed FRBs/CMB/SNe Ia system [250], GW/FRB system [252], CMB+GW+FRB [254] and FRB/standard distance probes [253]. However, the effects of DMs contributed by host galaxies and fluctuations of IGM should be treated properly.…”

Section: Dark Energymentioning

confidence: 99%

The physics of fast radio bursts

Xiao

Wang

Dai

2021

Sci. China Phys. Mech. Astron.

147

107

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In 2007, a very bright radio pulse was identified in the archival data of the Parkes Telescope in Australia, marking the beginning of a new research branch in astrophysics. In 2013, this kind of millisecond bursts with extremely high brightness temperature takes a unified name, fast radio burst (FRB). Over the first few years, FRBs seemed very mysterious because the sample of known events was limited. With the improvement of instruments over the last five years, hundreds of new FRBs have been discovered. The field is now undergoing a revolution and understanding of FRB has rapidly increased as new observational data increasingly accumulate. In this review, we will summarize the basic physics of FRBs and discuss the current research progress in this area. We have tried to cover a wide range of FRB topics, including the observational property, propagation effect, population study, radiation mechanism, source model, and application in cosmology. A framework based on the latest observational facts is now under construction. In the near future, this exciting field is expected to make significant breakthroughs. fast radio burst, neutron star, cosmology

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A comparison of Galactic electron density models using PyGEDM

Price

Flynn

Deller

2021

Publ. Astron. Soc. Aust.

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Galactic electron density distribution models are crucial tools for estimating the impact of the ionised interstellar medium on the impulsive signals from radio pulsars and fast radio bursts. The two prevailing Galactic electron density models (GEDMs) are YMW16 (Yao et al. 2017, ApJ, 835, 29) and NE2001 (Cordes & Lazio 2002, arXiv e-prints, pp astro–ph/0207156). Here, we introduce a software package PyGEDM which provides a unified application programming interface for these models and the YT20 (Yamasaki & Totani 2020, ApJ, 888, 105) model of the Galactic halo. We use PyGEDM to compute all-sky maps of Galactic dispersion measure (DM) for YMW16 and NE2001 and compare the large-scale differences between the two. In general, YMW16 predicts higher DM values towards the Galactic anticentre. YMW16 predicts higher DMs at low Galactic latitudes, but NE2001 predicts higher DMs in most other directions. We identify lines of sight for which the models are most discrepant, using pulsars with independent distance measurements. YMW16 performs better on average than NE2001, but both models show significant outliers. We suggest that future campaigns to determine pulsar distances should focus on targets where the models show large discrepancies, so future models can use those measurements to better estimate distances along those line of sight. We also suggest that the Galactic halo should be considered as a component in future GEDMs, to avoid overestimating the Galactic DM contribution for extragalactic sources such as FRBs.

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Use of fast radio burst dispersion measures as distance measures

Cited by 36 publications

References 74 publications

Implications of Canadian Hydrogen Intensity Mapping Experiment repeating fast radio bursts

Implications of Canadian Hydrogen Intensity Mapping Experiment repeating fast radio bursts

The physics of fast radio bursts

A comparison of Galactic electron density models using PyGEDM

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