PALFA Single-pulse Pipeline: New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst

Patel, C.; Agarwal, Devansh; Bhardwaj, Mohit; Boyce, M. M.; Brazier, A.; Chatterjee, Shami; Chawla, Pragya; Kaspi, V. M.; Lorimer, D. R.; McLaughlin, M. A.; Parent, E.; Pleunis, Ziggy; Ransom, S. M.; Scholz, Paul; Wharton, Robert; Zhu, Weiwei; Alam, Md Faisal; Valdez, K. Caballero; Camilo, F.; Cordes, J. M.; Crawford, F.; Deneva, J. S.; Ferdman, R. D.; Freire, P. C. C.; Hessels, J. W. T.; Nguyen, Benjamin M. X.; Stairs, I. H.; Stovall, K.; Leeuwen, J. van

doi:10.3847/1538-4357/aaee65

Cited by 42 publications

(36 citation statements)

References 48 publications

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“…For the surveys that did publish rates, we convert the published rates into rates per survey expressed as the number of FRBs detected per day of observing time. In this paper we adopt R htru ∼ 0.08 FRBs/day (Champion et al 2016), R askap−fly ∼ 0.12 FRBs/day (Shannon et al 2018) and R palfa ∼ 0.04 FRBs/day (Patel et al 2018) and R utmost ∼ 1/63 FRBs/day (Farah et al 2018). These rates encapsulate limits by their survey nature, whether in terms of observing frequency, fluence thresholds, sky coverage or any other selection effects.…”

Section: Frb Detection Ratesmentioning

confidence: 99%

Synthesising the intrinsic FRB population using frbpoppy

Gardenier

Leeuwen

Connor

et al. 2019

A&A

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Context. Fast Radio Bursts (FRBs) are radio transients of an unknown origin. Naturally, we are curious as to their nature. Enough FRBs have been detected for a statistical approach to parts of this challenge to be feasible. To understand the crucial link between detected FRBs and the underlying FRB source classes we perform FRB population synthesis, to determine how the underlying population behaves. The Python package we developed for this synthesis, frbpoppy, is open source and freely available. Aims. Our goal is to determine the current best fit FRB population model. Our secondary aim is to provide an easy-to-use tool for simulating and understanding FRB detections. It can compare surveys, or inform us of the intrinsic FRB population. Methods. frbpoppy simulates intrinsic FRB populations and the surveys that find them, to produce virtual observed populations. These resulting populations can then be compared with real data, allowing constrains to be placed on underlying physics and selection effects.Results. We are able to replicate real Parkes and ASKAP FRB surveys, in terms of both detection rates and distributions observed. We also show the effect of beam patterns on the observed dispersion measure (DM) distributions. We compare four types of source models. The "Complex" model, featuring a range of luminosities, pulse widths and spectral indices, reproduces current detections best. Conclusions. Using frbpoppy, an open-source FRB population synthesis package, we explain current FRB detections and offer a first glimpse of what the true population must be.

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Section: Frb Detection Ratesmentioning

confidence: 99%

Synthesising the intrinsic FRB population using frbpoppy

Gardenier

Leeuwen

Connor

et al. 2019

A&A

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“…The refurbished Molonglo Observatory Synthesis Telescope (MOST), utilised for the UTMOST project, has also detected a number of FRBs, most recently reported by Farah et al (2019), as has the Parkes Radio Telescope, most recently reported by Bhandari et al (2018). The Green Bank Telescope (GBT) has reported one FRB (Masui et al 2015) and Arecibo has reported two FRBs (Spitler et al 2014;Patel et al 2018). In all these cases, localisation precision is low.…”

Section: Introductionmentioning

confidence: 98%

A Search of TESS Full-frame Images for a Simultaneous Optical Counterpart to FRB 181228

Tingay

Yang

2019

ApJ

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FRB181228 was detected by the Molonglo Synthesis Radio Telescope (MOST) at a position and time coincident with Transiting Exoplanet Survey Satellite (TESS) observations, representing the first simultaneous multi-wavelength data collection for a Fast Radio Burst (FRB). The large imaged field-ofview of TESS allows a search over the uncertainty region produced by MOST. However, the TESS pixel scale of 21 and the Full Frame Image (FFI) cadence of 30 minutes is not optimal for the detection of an FOB with a possible millisecond duration. We search the TESS FFIs and find no events with a limiting TESS magnitude of 16, assuming a 30 minute event duration, corresponding to an optical flux density upper limit of approximately 2000 Jy for a ∼ 1 ms signal duration, assuming no signal loss. In addition, the cosmic ray mitigation method for TESS significantly reduces its sensitivity to short timescale transients, which we quantify. We compare our results to the predictions of Yang et al. (2019) and find that the upper limit is a factor of two thousand higher than the predicted maximum optical flux density. However, we find that if FRB181228 had occurred in the galaxy thought to host the nearest FRB detection to date (37 Mpc), an FOB may have been detectable by TESS. In the near future, when CHIME and ASKAP will detect hundreds to thousands of FRBs, TESS may be able to detect FOBs from those rare bright and nearby FRBs within this large population (if more sophisticated cosmic ray excision can be implemented).

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“…After about one decade, more than 60 FRBs have been found by terrestrial radio telescopes [2] 1 . FRBs have anomalously high dispersion measures (DMs), significantly exceeding the expected Milky Way contribution along the line of sight, which is contrary to Galactic pulsars [3,4,5,6,7,8,9,10] (but note that low DM has also been hinted from two FRBs [11,12] and a candidate (FRB 141113) [13]). It indicates that FRBs are of extragalactic or even cosmological origin, rather than of Galactic origin [14,15,16,17,18].…”

Section: Introductionmentioning

confidence: 93%

Statistical properties of the repeating fast radio burst source FRB 121102

Li¹,

Li²,

Zhang³

et al. 2019

Int J Cosmol Astron Astrophys

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Currently, FRB 121102 is the only fast radio burst source that was observed to give out bursts repeatedly. It shows a high repeating rate, with more than one hundred bursts being spotted, but with no obvious periodicity in the activities. Thanks to its repetition, the source was well localized with a subarcsecond accuracy, leading to a redshift measurement of about 0.2. FRB 121102 is a unique source that can help us understand the enigmatic nature of fast radio bursts. In this study, we analyze the characteristics of the waiting times between bursts from FRB 121102. It is found that there is a clear bimodal distribution for the waiting times. While most waiting times cluster at several hundred seconds, a small portion of the waiting times are strikingly in the range of 2 -40 millisecond. More interestingly, it is found that the waiting time does not correlate with the burst intensity, either for the preceding burst or for the subsequent burst. It strongly indicates that the repeating bursts should be generated by some external mechanisms, but not internal mechanisms. As a result, the models involving collisions between small bodies and neutron stars could be competitive mechanisms for this interesting source. * libing@ihep.ac.cn †

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PALFA Single-pulse Pipeline: New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst

Cited by 42 publications

References 48 publications

Synthesising the intrinsic FRB population using frbpoppy

Synthesising the intrinsic FRB population using frbpoppy

A Search of TESS Full-frame Images for a Simultaneous Optical Counterpart to FRB 181228

Statistical properties of the repeating fast radio burst source FRB 121102

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