Search for Fast Radio Bursts in the Direction of the Galaxies M31 and M33

Fedorova, V. A.; Rodin, A. E.

doi:10.1134/s1063772919110039

Cited by 21 publications

(17 citation statements)

References 17 publications

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“…According to FRBCAT, there is a significant gap between ∼ 35 ms and ∼ 300 ms in pulse width. However, we notice that the measurements with pulse width larger than ∼ 300 ms all come from one radio facility, i.e., the radio telescope BSA LPI of the Pushchino Radio Astronomy Observatory, in which the time interval between samples is 100 ms (Fedorova & Rodin 2019). Considering that there may exist some observational bias effects in these data, we only include the pulses with a width shorter than ∼ 35 ms (80 non-repeaters).…”

Section: Frb Observation Datamentioning

confidence: 99%

Fast radio bursts: do repeaters and non-repeaters originate in statistically similar ensembles?

Cui

Zhang

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Fast Radio Bursts (FRBs) are the short, strong radio pulses lasting several milliseconds. They are subsequently identified, for the most part, as emanating from unknown objects at cosmological distances. At present, over one hundred FRBs have been verified, classified into two groups: repeating bursts (20 samples) and apparently non-repeating bursts (91 samples). Their origins, however, are still hotly debated. Here, we investigate the statistical classifications for the two groups of samples to see if the non-repeating and repeating FRBs have different origins by employing Anderson-Darling (A-D) test and Mann-Whitney-Wilcoxon (M-W-W) test. Firstly, by taking the pulse width as a statistical variant, we found that the repeating samples do not follow the Gaussian statistics (may belong to a χ-square distribution), although the overall data and non-repeating group do follow the Gaussian. Meanwhile, to investigate the statistical differences between the two groups, we turn to M-W-W test and notice that the two distributions have different origins. Secondly, we consider the FRB radio luminosity as a statistical variant, and find that both groups of samples can be regarded as the Gaussian distributions under the A-D test, although they have different origins according to M-W-W tests. Therefore, statistically, we can conclude that our classifications of both repeaters and non-repeaters are plausible, that the two FRB classes have different origins, or each has experienced distinctive phases or been subject to its own physical processes.

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Section: Frb Observation Datamentioning

confidence: 99%

Fast radio bursts: do repeaters and non-repeaters originate in statistically similar ensembles?

Cui

Zhang

Wang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We note that detection of 9 plus 51 bursts at 111 MHz using the Large Phased Array of the Pushchino Radio Astronomy Observatory has been claimed by [123,124]. However, the observational setup of their system (a coarse frequency resolution of 78 kHz over a tiny observation bandwidth of 2.5 MHz, and a sampling time not faster than 12.5 ms) required the use of a template matching approach in order to see the bursts.…”

Section: Large Phased Arraymentioning

confidence: 90%

The Low Frequency Perspective on Fast Radio Bursts

Pilia

2021

Universe

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Fast radio bursts (FRBs) represent one of the most exciting astrophysical discoveries of the recent past. The study of their low-frequency emission, which was only effectively picked up about ten years after their discovery, has helped shape the field thanks to some of the most important detections to date. Observations between 400 and 800 MHz, carried out by the CHIME/FRB telescope, in particular, have led to the detection of ∼500 FRBs in little more than 1 year and, among them, ∼20 repeating sources. Detections at low frequencies have uncovered a nearby population that we can study in detail via continuous monitoring and targeted campaigns. The latest, most important discoveries include: periodicity, both at the days level in repeaters and at the millisecond level in apparently non-repeating sources; the detection of an FRB-like burst from a galactic magnetar; and the localisation of an FRB inside a globular cluster in a nearby galaxy. The systematic study of the population at low frequencies is important for the characterisation of the environment surrounding the FRBs and, at a global level, to understand the environment of the local universe. This review is intended to give an overview of the efforts leading to the current rich variety of low-frequency studies and to put into a common context the results achieved in order to trace a possible roadmap for future progress in the field.

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“…In the work of Fedorova and Rodin [11] it was shown that the average rate of registration of bursts by the LPA LPI radio telescope at a frequency of 111 MHz is ∼ 2000 pulses/year.…”

Section: Catalog "Prao Frbs At 111 Mhz"mentioning

confidence: 99%

“…Nine more single pulses were detected, including one repeating pulse. All the events showed no apparent concentration towards the centers of the M31 and M33 galaxies [11]. In order to start making meaningful reliable conclusions about the properties of new pulses, it was necessary to increase their statistics to several dozen, so a search was started for the entire available area of the sky.…”

Section: Introductionmentioning

confidence: 99%

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Comparative Analysis of the Observational Properties of Fast Radio Bursts at the Frequencies of 111 and 1400 MHz

Fedorova,

Rodin

2021

Preprint

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A comparative analysis of the observational characteristics of fast radio bursts at the frequencies 111 and 1400 MHz is carried out. The distributions of radio bursts by the dispersion measure are constructed. At both frequencies, they are described by a lognormal distribution with the parameters µ = 6.2 σ = 0.7. The dependence τ sc (DM ) of the scattering value on the dispersion measure at 111 MHz and 1400 MHz is also constructed. This dependence is fundamentally different from the dependence for pulsars. A comparative analysis of the relationship between the scattering of pulses and the dispersion measure at 1400 MHz and 111 MHz showed that for both frequencies it has the form τ sc (DM ) ∼ DM k , where k = 0.49 ± 0.18 and k = 0.43 ± 0.15 for the frequencies 111 and 1400 MHz, respectively.The obtained dependence is explained within the framework of the assumption of the extragalactic occurrence of fast radio bursts and an almost uniform distribution of matter in intergalactic space. From the dependence τ sc (DM ) a total estimate of the contribution to the matter of the halo of our and the host galaxy to DM is obtained DM halo + DM host 1+z ≈ 60 pc/cm 3 . Based on the Log N -Log S dependence, the average spectral index of radio bursts is derived α = −0.63 ± 0.20 provided that the statistical properties of these samples at 111 and 1400 MHz are the same.

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Search for Fast Radio Bursts in the Direction of the Galaxies M31 and M33

Cited by 21 publications

References 17 publications

Fast radio bursts: do repeaters and non-repeaters originate in statistically similar ensembles?

Fast radio bursts: do repeaters and non-repeaters originate in statistically similar ensembles?

The Low Frequency Perspective on Fast Radio Bursts

Comparative Analysis of the Observational Properties of Fast Radio Bursts at the Frequencies of 111 and 1400 MHz

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