A Simultaneous Search for Prompt Radio Emission Associated with the Short GRB 170112A Using the All-sky Imaging Capability of the OVRO-LWA

Anderson, Marin; Hallinan, Gregg; Eastwood, Michael; Monroe, Ryan; Vedantham, H. K.; Bourke, S.; Greenhill, L. J.; Kocz, J.; Lazio, T. Joseph W.; Price, Danny C.; Schinzel, F. K.; Wang, Yuankun; Woody, D. P.

doi:10.3847/1538-4357/aad2d7

Cited by 36 publications

(35 citation statements)

References 74 publications

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“…At extragalactic distances, potential transient sources at low frequencies include bright, coherent pulses predicted to accompany GRBs and neutron star mergers (see Anderson et al 2018, and references therein), as well as fast radio bursts (FRBs), highly dispersed millisecond pulses that have been detected at frequencies as low as 400 MHz (CHIME/FRB Collaboration et al 2019). The degree of scatter broadening from the current sample of FRBs indicates the potential for detecting this population even at very low frequencies (Ravi 2019).…”

Section: Introductionmentioning

confidence: 94%

New Limits on the Low-frequency Radio Transient Sky Using 31 hr of All-sky Data with the OVRO–LWA

Anderson

Hallinan

Eastwood

et al. 2019

ApJ

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We present the results of the first transient survey from the Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA) using 31 hr of data, in which we place the most constraining limits on the instantaneous transient surface density at timescales of 13 s to a few minutes and at frequencies below 100 MHz. The OVRO-LWA is a dipole array that images the entire viewable hemisphere with 58 MHz of bandwidth from 27 to 84 MHz at 13 s cadence. No transients are detected above a 6.5σ flux density limit of 10.5 Jy, implying an upper limit to the transient surface density of 2.5 × 10 −8 deg −2 at the shortest timescales probed, which is orders of magnitude deeper than has been achieved at sub-100 MHz frequencies and comparable flux densities to date. The nondetection of transients in the OVRO-LWA survey, particularly at minutes-long timescales, allows us to place further constraints on the rate of the potential population of transients uncovered by Stewart et al. 2016. From their transient rate, we expect a detection of 8.4 +31.8 −8.0 events, and the probability of our null detection is 1.9 +644 −1.9 × 10 −3 , ruling out a transient rate > 1.4 × 10 −4 days −1 deg −2 with 95% confidence at a flux density limit of 18.1 Jy, under the assumption of a flat spectrum and wide bandwidth. We discuss the implications of our nondetection for this population and further constraints that can be made on the source spectral index, intrinsic emission bandwidth, and resulting luminosity distribution.

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Section: Introductionmentioning

confidence: 94%

New Limits on the Low-frequency Radio Transient Sky Using 31 hr of All-sky Data with the OVRO–LWA

Anderson

Hallinan

Eastwood

et al. 2019

ApJ

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“…There have been several unsuccessful attempts to search for prompt radio emission from compact binary coalescence at low radio frequencies. Callister et al (2019) used the Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA, observing at 27-85 MHz) a to search for the prompt emission from the binary black hole merger GW170104, while Anderson et al (2018) used the OVRO-LWA to search for prompt emission from the cosmological short gamma-ray burst 170112A. Similarly, Rowlinson & Anderson (2019) examined data (Kaplan et al 2015) from the Murchison Widefield Array (MWA; Tingay et al 2013, observing at 70-300 MHz) from the short gamma-ray burst 150424A.…”

Section: Introductionmentioning

confidence: 99%

The capability of the Australian Square Kilometre Array Pathfinder to detect prompt radio bursts from neutron star mergers

Wang

Murphy

Kaplan

et al. 2020

Publ. Astron. Soc. Aust.

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We discuss observational strategies to detect prompt bursts associated with gravitational wave (GW) events using the Australian Square Kilometre Array Pathfinder (ASKAP). Many theoretical models of binary neutron stars mergers predict that bright, prompt radio emission would accompany the merger. The detection of such prompt emission would greatly improve our knowledge of the physical conditions, environment, and location of the merger. However, searches for prompt emission are complicated by the relatively poor localisation for GW events, with the 90% credible region reaching hundreds or even thousands of square degrees. Operating in fly’s eye mode, the ASKAP field of view can reach $\sim1\,000$ deg $^2$ at $\sim$ $888\,{\rm MHz}$ . This potentially allows observers to cover most of the 90% credible region quickly enough to detect prompt emission. We use skymaps for GW170817 and GW190814 from LIGO/Virgo’s third observing run to simulate the probability of detecting prompt emission for GW events in the upcoming fourth observing run. With only alerts released after merger, we find it difficult to slew the telescope sufficiently quickly as to capture any prompt emission. However, with the addition of alerts released before merger by negative-latency pipelines, we find that it should be possible to search for nearby, bright prompt fast radio burst-like emission from GW events. Nonetheless, the rates are low: we would expect to observe $\sim$ 0.012 events during the fourth observing run, assuming that the prompt emission is emitted microseconds around the merger.

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“…They have large fields of view (FOV) which allow them to efficiently search for poorly localised transients (e.g. Obenberger et al 2014;Howell et al 2015;Abbott et al 2016;Kaplan et al 2016;Anderson et al 2018;Callister et al 2019). Furthermore, the dispersive delay due to a distant radio signal's propagation through ionised gas in the ISM and intergalactic medium (IGM) can be minutes at low frequencies, providing extra time to re-point at a newly detected event (e.g.…”

Section: Introductionmentioning

confidence: 99%

Using negative-latency gravitational wave alerts to detect prompt radio bursts from binary neutron star mergers with the Murchison Widefield Array

James

Anderson

Wen

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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We examine how fast radio burst (FRB)-like signals predicted to be generated during the merger of a binary neutron star (BNS) may be detected in low-frequency radio observations triggered by the aLIGO/Virgo gravitational wave detectors. The rapidity, directional accuracy, and sensitivity of follow-up observations with the Murchison Widefield Array (MWA) are considered. We show that with current methodology, the rapidity criteria fails for triggered MWA observations above 136 MHz for BNS mergers within the aLIGO/Virgo horizon, for which little dispersive delay is expected. A calculation of the expected reduction in response time by triggering on 'negative latency' alerts from aLIGO/Virgo observations of gravitational waves generated by the BNS inspiral is presented. This allows for observations up to 300 MHz where the radio signal is expected to be stronger. To compensate for the poor positional accuracy expected from these alerts, we propose a new MWA observational mode that is capable of viewing one quarter of the sky. We show the sensitivity of this mode is sufficient to detect an FRB-like burst from an event similar to GW170817 if it occurred during the ongoing aLIGO/Virgo third science run (O3).

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A Simultaneous Search for Prompt Radio Emission Associated with the Short GRB 170112A Using the All-sky Imaging Capability of the OVRO-LWA

Cited by 36 publications

References 74 publications

New Limits on the Low-frequency Radio Transient Sky Using 31 hr of All-sky Data with the OVRO–LWA

New Limits on the Low-frequency Radio Transient Sky Using 31 hr of All-sky Data with the OVRO–LWA

The capability of the Australian Square Kilometre Array Pathfinder to detect prompt radio bursts from neutron star mergers

Using negative-latency gravitational wave alerts to detect prompt radio bursts from binary neutron star mergers with the Murchison Widefield Array

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