The Apertif Radio Transient System (ARTS): Design, commissioning, data release, and detection of the first five fast radio bursts

Leeuwen, J. van; Kooistra, E.; Oostrum, L.; Connor, L.; Hargreaves, J. E.; Maan, Y.; Pastor-Marazuela, I.; Petroff, E.; Schuur, D. van der; Sclocco, A.; Straal, S. M.; Vohl, D.; Wijnholds, Stefan J.

doi:10.1051/0004-6361/202244107

Cited by 5 publications

(2 citation statements)

References 126 publications

(162 reference statements)

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“…This determination is crucial for a number of reasons. Firstly, it allows one to accurately estimate the redshift of the FRB, thus enabling estimation of the exact electron column depth between us and the source, which is paramount for estimating the baryon content of the Universe [6]. Secondly, it allows further follow-up of the host galaxy and the environs of the FRB, providing insight into the progenitor [34].…”

Section: Buffering Triggering and Alertingmentioning

confidence: 99%

“…All that was about to change when an extremely bright burst was discovered in 2007, with a dispersion much larger than what was expected from the Milky Way, in archival data from the Murriyang (Parkes) telescope. This seminal event in time-domain astronomy opened up a new parameter space of cosmological radio bursts with tremendous scientific potential [6].…”

Section: Introductionmentioning

confidence: 99%

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A Needle in a Cosmic Haystack: A Review of FRB Search Techniques

Rajwade,

van Leeuwen

2024

Universe

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Ephemeral Fast Radio Bursts (FRBs) must be powered by some of the most energetic processes in the Universe. That makes them highly interesting in their own right, and as precise probes for estimating cosmological parameters. This field thus poses a unique challenge: FRBs must be detected promptly and immediately localised and studied based only on that single millisecond-duration flash. The problem is that the burst occurrence is highly unpredictable and that their distance strongly suppresses their brightness. Since the discovery of FRBs in single-dish archival data in 2007, detection software has evolved tremendously. Pipelines now detect bursts in real time within a matter of seconds, operate on interferometers, buffer high-time and frequency resolution data, and issue real-time alerts to other observatories for rapid multi-wavelength follow-up. In this paper, we review the components that comprise a FRB search software pipeline, we discuss the proven techniques that were adopted from pulsar searches, we highlight newer, more efficient techniques for detecting FRBs, and we conclude by discussing the proposed novel future methodologies that may power the search for FRBs in the era of big data astronomy.

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Section: Buffering Triggering and Alertingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Needle in a Cosmic Haystack: A Review of FRB Search Techniques

Rajwade,

van Leeuwen

2024

Universe

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A fast radio burst with submillisecond quasi-periodic structure

Pastor-Marazuela,

van Leeuwen,

Bilous

et al. 2023

A&A

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Fast radio bursts (FRBs) are extragalactic radio transients of extraordinary luminosity. Studying the diverse temporal and spectral behaviour recently observed in a number of FRBs may help to determine the nature of the entire class. For example, a fast spinning or highly magnetised neutron star (NS) might generate the rotation-powered acceleration required to explain the bright emission. Periodic, subsecond components suggesting such rotation were recently reported in one FRB, and may also exist in two more. Here we report the discovery of FRB 20201020A with Apertif, an FRB that shows five components regularly spaced by 0.411 ms. This submillisecond structure in FRB 20201020A carries important clues about the progenitor of this FRB specifically, and potentially about the progenitors of FRBs in general. We therefore contrast its features to what is seen in other FRBs and pulsars, and to the predictions of some FRB models. We present a timing analysis of the FRB 20201020A components carried out in order to determine the significance of the periodicity. We compare these against the timing properties of the previously reported CHIME FRBs with subsecond quasi-periodic components, and against two Apertif bursts from repeating FRB 20180916B, which show complex time-frequency structure. We find the periodicity of FRB 20201020A to be marginally significant at 2.4σ. Its repeating subcomponents cannot be explained as pulsar rotation because the required spin rate of over 2 kHz exceeds the limits set by typical NS equations of state and observations. The fast periodicity is also in conflict with a compact object merger scenario. However, these quasi-periodic components could be caused by equidistant emitting regions in the magnetosphere of a magnetar. The submillisecond spacing of the components in FRB 20201020A, the smallest observed so far in a one-off FRB, may rule out both a NS spin period and binary mergers as the direct source of quasi-periodic FRB structure.

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The afterglow of GW170817 from every angle: prospects for detecting the afterglows of binary neutron star mergers

Morsony,

De Los Santos,

Hernandez

et al. 2024

Monthly Notices of the Royal Astronomical Society

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To date GW170817, produced by a binary neutron star (BNS) merger, is the only gravitational wave (GW) event with an electromagnetic counterpart. It was associated with a prompt short gamma-ray burst (GRB), an optical kilonova, and the afterglow of a structured off-axis relativistic jet. We model the prospects for future mergers discovered in gravitational waves to produce detectable afterglows. Using a model fit to GW170817, we assume all BNS mergers produce jets with the same parameters, and model the afterglow luminosity for a full distribution of observer angles, ISM densities, and distances. We find that in the LIGO/Virgo/KAGRA O4 run, 30 per cent–45 per cent of BNS mergers with a well-localized counterpart will have an afterglow detectable with current instrumentation in the X-ray, radio and optical. Without a previously detected counterpart, 10 per cent–15 per cent will have an afterglow detectable by wide-area radio and optical surveys, compared to only about 5 per cent–12 per cent of events expected to have bright (on-axis) gamma-ray emission. Most afterglows that are detected will be from off-axis jets. Further in the future, in the A + era (O5), 40 per cent–50 per cent of mergers will have afterglows detectable with next-generation X-ray and radio instruments. Future wide-area radio survey instruments, particularly DSA-2000, could detect 40 per cent of afterglows, even without a kilonova counterpart. Finding and monitoring these afterglows will provide valuable insight into the structure and diversity of relativistic jets, the rate at which mergers produce jets, and constrain the angle of the mergers relative to our line of sight.

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The Apertif Radio Transient System (ARTS): Design, commissioning, data release, and detection of the first five fast radio bursts

Cited by 5 publications

References 126 publications

A Needle in a Cosmic Haystack: A Review of FRB Search Techniques

A Needle in a Cosmic Haystack: A Review of FRB Search Techniques

A fast radio burst with submillisecond quasi-periodic structure

The afterglow of GW170817 from every angle: prospects for detecting the afterglows of binary neutron star mergers

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