Limits on fast radio bursts at 145 MHz with artemis, a real-time software backend

Karastergiou, A.; Chennamangalam, Jayanth; Armour, Wes; Williams, Christopher; Mort, Ben; Dulwich, Fred; Salvini, Stefano; Magro, Alessio; Roberts, Stephen; Serylak, M.; Doo, A.; Bilous, A. V.; Breton, R. P.; Falcke, H.; Grießmeier, Jean-Mathias; Hessels, J. W. T.; Keane, E. F.; Kondratiev, V. I.; Krämer, M.; Leeuwen, J. van; Noutsos, A.; Osłowski, S.; Sobey, C.; Stappers, B. W.; Weltevrede, P.

doi:10.1093/mnras/stv1306

Cited by 100 publications

(108 citation statements)

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“…Our simulations predict rates that are consistent with the upper limits reported for LOFAR (Coenen et al 2014;Karastergiou et al 2015), AO327 (Deneva et al 2016), MWA (Tingay et al 2015), VLA (Law et al 2015), and UTMOST (Caleb et al 2016). The simulations do not account for repeating sources, and the rate reported for the PALFA survey ) is based on the detection of a single event.…”

Section: Implications For Other Surveyssupporting

confidence: 88%

“…The constraints based on the GBNCC nondetection are not markedly different from the constraints evaluated by Rajwade & Lorimer (2017) based on nondetection with surveys such as AO327 (Deneva et al 2016), LOFAR (Karastergiou et al 2015), and UTMOST (Caleb et al 2016). The constraint we derive under the assumption of absence of scattering and freefree absorption, 1.18 lim a = , is stronger than the most constraining spectral index obtained from the above-mentioned surveys ( 0.7; lim a = AO327).…”

Section: Constant Comoving Number Density Distributioncontrasting

confidence: 57%

“…If intrinsic spectral index were the only reason for our nondetection, i.e., scattering and freefree absorption were absent, the nondetection with GBNCC would be compatible with the Parkes rate estimate reported by Crawford et al (2016) for 0.35 a > + . Karastergiou et al (2015) derived a constraint, α>+0.1, based on nondetection with LOFAR at 145 MHz. Nondetection with MWA at 155 MHz implied α>−1.2 (Tingay et al 2015).…”

Section: Discussionmentioning

confidence: 99%

“…Detection or stringent limits at lower frequencies are crucial for understanding properties of FRBs such as their spectral index and pulse profile evolution with frequency. Searches at low frequencies with telescopes such as LOFAR (Coenen et al 2014;Karastergiou et al 2015), Arecibo (Deneva et al 2016), and MWA (Tingay et al 2015;Rowlinson et al 2016) have so far not resulted in any detections. Deneva et al (2016) report an upper limit on the FRB rate at 327 MHz of 10 5 FRBs sky −1 day −1 for a flux density threshold of 83 mJy and pulse width of 10 ms. A nondetection with the LOFAR Pilot Pulsar Survey at 142 MHz allowed Coenen et al (2014) to place an upper limit of 150 FRBs sky −1 day −1…”

Section: Introductionmentioning

confidence: 99%

“…, for bursts brighter than 107 Jy at burst duration 0.66 ms. Karastergiou et al (2015) report an upper limit of 29 FRBs sky −1 day −1 for bursts with flux density above 62 Jy at 145 MHz and a pulse width of 5 ms, based on observations with the UK station of the LOFAR radio telescope. The upper limits on the FRB rate reported thus far from these low-frequency radio surveys are not particularly constraining because of limitations in total observing time and volume searched.…”

Section: Introductionmentioning

confidence: 99%

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A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Chawla

Kaspi

Josephy

et al. 2017

ApJ

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We report on a search for fast radio bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a dispersion measure (DM) of 3000 pc cm −3 , while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm −3 . No FRBs were detected in the pointings observed through 2016 May. We estimate a 95% confidence upper limit on the FRB rate of 3.6 10 3FRBs sky −1 day −1 above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index α by running simulations for different astrophysical scenarios and cumulative flux density distributions. The nondetection with GBNCC is consistent with the 1.4 GHz rate reported for the Parkes surveys for α>+0.35 in the absence of scattering and free-free absorption and α>−0.3 in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to ∼50 FRBs per day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log N-log S slope, and pulse profile evolution across its bandwidth (400-800 MHz).

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Section: Implications For Other Surveyssupporting

confidence: 88%

Section: Constant Comoving Number Density Distributioncontrasting

confidence: 57%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Chawla

Kaspi

Josephy

et al. 2017

ApJ

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Fast radio bursts

Petroff

Hessels

Lorimer

2019

Astron Astrophys Rev

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593

471

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The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar to the individual pulses from pulsars, their large dispersive delays suggest that they originate from far outside the Milky Way and hence are many ordersof-magnitude more luminous. While most FRBs appear to be one-off, perhaps cataclysmic events, two sources are now known to repeat and thus clearly have a longer-lived central engine. Beyond understanding how they are created, there is also the prospect of using FRBs -as with pulsars -to probe the extremes of the Universe as well as the otherwise invisible intervening medium. Such studies will be aided by the high implied all-sky event rate: there is a detectable FRB roughly once every minute occurring somewhere on the sky. The fact that less than a hundred FRB sources have been discovered in the last decade is largely due to the small fields-of-view of current radio telescopes. A new generation of wide-field instruments is now coming online, however, and these will be capable of detecting multiple FRBs per day. We are thus on the brink of further breakthroughs in the short-duration radio transient phase space, which will be critical for differentiating between the many proposed theories for the origin of FRBs. In this review, we give an observational and theoretical introduction at a level that is accessible to astronomers entering the field.

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A polyphase filter for many-core architectures

Adámek

Novotný

Armour

2016

Astronomy and Computing

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In this article we discuss our implementation of a polyphase filter for real-time data processing in radio astronomy. We describe in detail our implementation of the polyphase filter algorithm and its behaviour on three generations of NVIDIA GPU cards, on dual Intel Xeon CPUs and the Intel Xeon Phi (Knights Corner) platforms. All of our implementations aim to exploit the potential for data reuse that the algorithm offers. Our GPU implementations explore two different methods for achieving this, the first makes use of L1/Texture cache, the second uses shared memory. We discuss the usability of each of our implementations along with their behaviours. We measure performance in execution time, which is a critical factor for real-time systems, we also present results in terms of bandwidth (GB/s), compute (GFlop/s) and type conversions (GTc/s). We include a presentation of our results in terms of the sample rate which can be processed in real-time by a chosen platform, which more intuitively describes the expected performance in a signal processing setting. Our findings show that, for the GPUs considered, the performance of our polyphase filter when using lower precision input data is limited by type conversions rather than device bandwidth. We compare these results to an implementation on the Xeon Phi. We show that our Xeon Phi implementation has a performance that is 1.47x to 1.95x greater than our CPU implementation, however is not insufficient to compete with the performance of GPUs. We conclude with a comparison of our best performing code to two other implementations of the polyphase filter, showing that our implementation is faster in nearly all cases. This work forms part of the Astro-Accelerate project, a many-core accelerated real-time data processing library for digital signal processing of time-domain radio astronomy data.Comment: 19 pages, 20 figures, 5 table

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Limits on fast radio bursts at 145 MHz with artemis, a real-time software backend

Cited by 100 publications

References 35 publications

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Fast radio bursts

A polyphase filter for many-core architectures

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