How Bright Are Fast Optical Bursts Associated With Fast Radio Bursts?

Yang, Yuan-Pei; Zhang, Bing; Wei, J. Y.

doi:10.3847/1538-4357/ab1fe2

Cited by 44 publications

(62 citation statements)

References 55 publications

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“…We cannot comment on the predictions from Beloborodov (2017) and Yang et al (2019), as their models only indicate the lower limits to á ñ n .…”

Section: How Many Multiwavelength Frb Counterparts Should Blindmentioning

confidence: 90%

“…We compare our most constraining result from Gaia (η10 3 , assuming nondetection and using the Gaia time resolution of 4.5 s) with predictions made by Yang et al (2019). These authors investigate the detectability of "fast optical bursts" (FOBs) associated with FRBs in two broad cases and five specific scenarios.…”

Section: Fast Optical Bursts Associated With Frbsmentioning

confidence: 99%

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The Multiwavelength Counterparts of Fast Radio Bursts

Chen

Ravi

2020

ApJ

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The engines that produce extragalactic fast radio bursts (FRBs), and the mechanism by which the emission is generated, remain unknown. Many FRB models predict prompt multiwavelength counterparts, which can be used to refine our knowledge of these fundamentals of the FRB phenomenon. However, several previous targeted searches for prompt FRB counterparts have yielded no detections and have additionally not reached sufficient sensitivity with respect to the predictions. In this work, we demonstrate a technique to estimate the ratio, η, between the energy outputs of FRB counterparts at various wavelengths and the radio-wavelength emission. Our technique combines the fluence distribution of the FRB population with results from several wide-field blind surveys for fast transients from the optical to the TeV bands. We present constraints on η that improve upon previous observations even in the case where all unclassified transient events in existing surveys are FRB counterparts. In some scenarios for the FRB engine and emission mechanism, we find that FRB counterparts should have already been detected, thus demonstrating that our technique can successfully test predictions for η. However, it is possible that FRB counterparts are lurking among catalogs of unclassified transient events. Although our technique is robust to the present uncertainty in the FRB fluence distribution, its ultimate application to accurately estimate or bound η will require the careful analysis of all candidate fast transient events in multiwavelength survey data sets.

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“…We cannot comment on the predictions from Beloborodov (2017) and Yang et al (2019), as their models only indicate the lower limits to á ñ n .…”

Section: How Many Multiwavelength Frb Counterparts Should Blindmentioning

confidence: 90%

Section: Fast Optical Bursts Associated With Frbsmentioning

confidence: 99%

The Multiwavelength Counterparts of Fast Radio Bursts

Chen

Ravi

2020

ApJ

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“…After the BNS merger, the newborn neutron star with a surface dipole magnetic field strength B and initial period P 0 would spin down due to magnetic torques, the spindown luminosity L sd is given by (e.g. Yang et al 2019)…”

Section: Frbs From Pulsar Magnetospherementioning

confidence: 99%

Fast Radio Bursts from Activity of Neutron Stars Newborn in BNS Mergers: Offset, Birth Rate, and Observational Properties

Wang

Yang

et al. 2020

ApJ

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Young neutron stars (NSs) born in core-collapse explosions are promising candidates for the central engines of fast radio bursts (FRBs), since the first localized repeating burst FRB 121102 happens in a star forming dwarf galaxy, which is similar to the host galaxies of superluminous supernovae (SLSNe) and long gamma-ray bursts (LGRBs). However, FRB 180924 and FRB 190523 are localized to massive galaxies with low rates of star formation, compared with the host of FRB 121102. Meanwhile, the offsets between the bursts and host centers are about 4 kpc and 29 kpc for FRB 180924 and FRB 190523, respectively. These properties of hosts are similar to short gamma-ray bursts (SGRBs), which are produced by mergers of binary neutron star (BNS) or neutron star-black hole (NS-BH). Therefore, the NSs powering FRBs may be formed in BNS mergers. In this paper, we study the BNS merger rates, merger times, and predict their most likely merger locations for different types of host galaxies using population synthesis method. We find that the BNS merger channel is consistent with the recently reported offsets of FRB 180924 and FRB 190523. The offset distribution of short GRBs is well reproduced by population synthesis using galaxy model which is similar to GRB hosts. The event rate of FRBs (including non-repeating and repeating), is larger than those of BNS merger and short GRBs, which requires a large fraction of observed FRBs emitting several bursts. Using curvature radiation by bunches in NS magnetospheres, we also predict the observational properties of FRBs from BNS mergers, including the dispersion measure, and rotation measure. At late times (t ≥ 1yr), the contribution to dispersion measure and rotation measure from BNS merger ejecta could be neglected.

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“…They find that under special conditions, optical emission from FRBs may be detectable under the Inverse Compton models. Overall, Yang et al (2019) find the detection probablility for optical emission from FRBs to be low, but that if optical emission from even a small number of FRBs was detected it would provide valuable insights into the physics of the progenitors.…”

Section: Introductionmentioning

confidence: 99%

“…From a theoretical modelling point of view, Yang, Zhang, & Wei (2019) predict the optical emission from the observed FRB radio emission, considering two different versions of Inverse Compton emission models plus an extension of the radio emission mechanism into the optical regime. They find that under special conditions, optical emission from FRBs may be detectable under the Inverse Compton models.…”

Section: Introductionmentioning

confidence: 99%

High-cadence optical transient searches using drift scan imaging I: Proof of concept with a pre-prototype system

Tingay

2020

Publ. Astron. Soc. Aust.

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An imaging technique with sensitivity to short duration optical transients is described. The technique is based on the use of wide-field cameras operating in a drift scanning mode, whereby persistent objects produce trails on the sensor and short duration transients occupy localised groups of pixels. A benefit of the technique is that sensitivity to short duration signals is not accompanied by massive data rates, because the exposure time >> transient duration. The technique is demonstrated using a pre-prototype system composed of readily available and inexpensive commercial components, coupled with common coding environments, commercially available software, and free web-based services. The performance of the technique and the pre-prototype system is explored, including aspects of photometric and astrometric calibration, detection sensitivity, characterisation of candidate transients, and the differentiation of astronomical signals from non-astronomical signals (primarily glints from satellites in Earth orbit and cosmic ray hits on sensor pixels). Test observations were made using the pre-prototype system, achieving sensitivity to transients with 21 ms duration, resulting in the detection of five candidate transients. An investigation of these candidates concludes they are most likely due to cosmic ray hits on the sensor and/or satellites. The sensitivity obtained with the pre-prototype system is such that, under some models for the optical emission from FRBs, the detection of a typical FRB, such as FRB181228, to a distance of approximately 100 Mpc is plausible. Several options for improving the system/technique in the future are described.

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How Bright Are Fast Optical Bursts Associated With Fast Radio Bursts?

Cited by 44 publications

References 55 publications

The Multiwavelength Counterparts of Fast Radio Bursts

The Multiwavelength Counterparts of Fast Radio Bursts

Fast Radio Bursts from Activity of Neutron Stars Newborn in BNS Mergers: Offset, Birth Rate, and Observational Properties

High-cadence optical transient searches using drift scan imaging I: Proof of concept with a pre-prototype system

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