Piggyback search for fast radio bursts using Nanshan 26 m and Kunming 40 m radio telescopes – I. Observing and data analysis systems, discovery of a mysterious peryton

Men, Yunpeng; Luo, Rui; Chen, M. Z.; Hao, Longfei; Lee, K. J.; Li, J.; Li, Z. X.; Liu, Z. Y.; Xin, Pei; Wen, Z. G.; Wu, Jerry J.; Xu, Yang; Xu, R. X.; Yuan, Jianping; Zhang, C. F.

doi:10.1093/mnras/stz1931

Cited by 29 publications

(43 citation statements)

References 52 publications

(64 reference statements)

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“…We searched for the radio bursts with either a dispersion signature or instrumental saturation to all the FAST data collected during the observational campaign. We searched for dispersed bursts using the software package BEAR 31 . Four types of searches had been performed: 1) blind search, 2) dedicated search, 3) searching for saturation, and 4) windowed search.…”

Section: Methodsmentioning

confidence: 99%

No pulsed radio emission during a bursting phase of a Galactic magnetar

Lin,

Zhang,

Wang

et al. 2020

Preprint

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Fast radio bursts (FRBs) are mysterious millisecond-duration radio transients observed from extragalactic distances [1][2][3] . Magnetars have been long speculated as the possible engine to power repeating bursts from FRB sources [4][5][6][7][8][9][10][11][12][13] , but no convincing evidence has been collected so far 14 . Recently, a Galactic magnetar dubbed Soft Gamma-ray Repeater (SGR) J1935+2154 entered an active phase by emitting intense soft gamma-ray bursts 15 . One fast radio burst with two peaks (hereafter FRB 200428) and a luminosity comparable to those of extragalactic FRBs was detected from the source 16,17 in association with a soft γ-ray / hard X-ray flare [18][19][20][21] . Here we report an eight-hour targeted observational campaign with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in four observing sessions, assisted by multi-wavelength (optical and hard X-rays) observations. During the third session, twenty-nine SGR bursts were detected by the Fermi Gamma-ray Burst Monitor (GBM). Throughout the observing period, especially during the scrutinized epochs when SGR bursts reached the Earth, no single dispersed pulsed emission was detected by FAST. This places a fluence upper limit eight orders of magnitude deeper than the fluence of FRB 200428. Our results suggest that FRB -SGR burst associations are rather rare. FRBs may be highly relativistic and geometrically beamed or may carry narrow spectra with the characteristic frequencies of the most bursts far outside the FAST band. More intriguingly, it is also possible that the physical condition to achieve coherent radiation in SGR bursts is contrived. Only under extreme conditions could an FRB be made in association with an SGR burst.We have been closely monitoring SGR J1935+2154 with FAST, aiming at testing whether a magnetar can make FRBs or FRB-like events during its active phase. We observe the target for eight hours in the following four sessions: (1)

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Section: Methodsmentioning

confidence: 99%

No pulsed radio emission during a bursting phase of a Galactic magnetar

Lin,

Zhang,

Wang

et al. 2020

Preprint

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“…We used the BEAR(Burst Emission Automatic Roger) package 29 to perform the FRB searches. BEAR is capable of performing radio-frequency interference (RFI) mitigation, de-dispersion, and candidates score ranking in one run.…”

Section: Observations and Burst Detectionmentioning

confidence: 99%

Diverse polarization angle swings from a repeating fast radio burst source

Luo

Wang

Men

et al. 2020

Nature

158

149

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Fast radio bursts (FRBs) are mysterious millisecond-duration radio transients 1, 2. Two possible mechanisms that could generate extremely coherent emission from FRBs invoke neutron star magnetospheres 3-5 or relativistic shocks far from the central energy source 6-8. Detailed polarization observations may help us to understand the emission mechanism. However, the available FRB polarization data have been perplexing, because they show a host of polarimetric properties, including either a constant polarization angle during each burst for some repeaters 9, 10 , or variable polarization angles in some other apparently one-off events 11, 12. Here we report observations of 15 bursts from FRB 180301 and find various polarization

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“…Eleven telescopes are marked in the map. The fields of view and sensitivities come fromcorresponding references: Parkes (Staveley-Smith et al 1996), Arecibo (Spitler et al 2014), GBT (Masui et al 2015), UTMOST (Caleb et al 2017), ASKAP (Shannon et al 2018), CHIME (CHIME/FRB Collaboration et al 2018), TianLai (Chen 2012), FAST(Nan et al 2011), QTT(Wang 2017), NSRT and KM40(Men et al 2019). The extension of FoV using multibeam or phase array are considered if available at the site.…”

mentioning

confidence: 99%

On the FRB luminosity function – – II. Event rate density

Luo

Men

Lee

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

127

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The luminosity function of Fast Radio Bursts (FRBs), defined as the event rate per unit cosmic co-moving volume per unit luminosity, may help to reveal the possible origins of FRBs and design the optimal searching strategy. With the Bayesian modelling, we measure the FRB luminosity function using 46 known FRBs. Our Bayesian framework self-consistently models the selection effects, including the survey sensitivity, the telescope beam response, and the electron distributions from Milky Way / the host galaxy / local environment of FRBs. Different from the previous companion paper, we pay attention to the FRB event rate density and model the event counts of FRB surveys based on the Poisson statistics. Assuming a Schechter luminosity function form, we infer (at the 95% confidence level) that the characteristic FRB event rate density at the upper cut-off luminosity L * = 2.9 +11.9 −1.7 × 10 44 erg s −1 is φ * = 339 +1074 −313 Gpc −3 yr −1 , the power-law index is α = −1.79 +0.31 −0.35 , and the lower cut-off luminosity is L 0 ≤ 9.1 × 10 41 erg s −1 . The event rate density of FRBs is found to be 3.5 +5.7 −2.4 × 10 4 Gpc −3 yr −1 above 10 42 erg s −1 , 5.0 +3.2 −2.3 × 10 3 Gpc −3 yr −1 above 10 43 erg s −1 , and 3.7 +3.5 −2.0 × 10 2 Gpc −3 yr −1 above 10 44 erg s −1 . As a result, we find that, for searches conducted at 1.4 GHz, the optimal diameter of single-dish radio telescopes to detect FRBs is 30-40 m. The possible astrophysical implications of the measured event rate density are also discussed in the current paper.

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Piggyback search for fast radio bursts using Nanshan 26 m and Kunming 40 m radio telescopes – I. Observing and data analysis systems, discovery of a mysterious peryton

Cited by 29 publications

References 52 publications

No pulsed radio emission during a bursting phase of a Galactic magnetar

No pulsed radio emission during a bursting phase of a Galactic magnetar

Diverse polarization angle swings from a repeating fast radio burst source

On the FRB luminosity function – – II. Event rate density

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