Detection of Repeating FRB 180916.J0158+65 Down to Frequencies of 300 MHz

Chawla, Pragya; Andersen, Bridget C.; Bhardwaj, Mohit; Fonseca, Emmanuel; Josephy, Alexander; Kaspi, V. M.; Michilli, D.; Pleunis, Ziggy; Bandura, Kevin; Bassa, Cees; Boyle, P.J.; Brar, Charanjot; Cassanelli, Tomas; Čubranić, Davor; Dobbs, M.; Dong, Fengqiu Adam; Gaensler, B. M.; Good, Deborah C.; Hessels, J. W. T.; Landecker, T. L.; Leung, Calvin; Li, D.Z.; Lin, Hsiu-Hsien; Masui, Kiyoshi; Mckinven, Ryan; Mena-Parra, Juan; Merryfield, Marcus; Meyers, Bradley W.; Naidu, Arun; Ng, Cherry; Patel, C.; Rafiei-Ravandi, Masoud; Rahman, Mubdi; Sanghavi, Pranav; Scholz, Paul; Shin, Kaitlyn; Smith, Kendrick M.; Stairs, I. H.; Tendulkar, Shriharsh P.; Vanderlinde, K.

doi:10.3847/2041-8213/ab96bf

Cited by 95 publications

(118 citation statements)

References 62 publications

(88 reference statements)

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“…Like the decoherence time, the spatial coherence scale of the scintillation pattern scales as l d ∝ν. While the spatial scale thus decreases at lower frequencies, we would have to observe at frequencies 100 MHz, below the lowest-frequency FRB detections (300 MHz) to date (Chawla et al 2020;Pilia et al 2020), to resolve the spatial scintillation pattern we predict for SGR 1935+2154 using stations across the Earth. At 100 MHz, the scintillation bandwidth is predicted to be ∼24 kHz, requiring observations with fine spectral resolution.…”

Section: Discussionmentioning

confidence: 88%

Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154

Simard

Ravi

2020

ApJL

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The discovery of a fast radio burst (FRB) associated with a magnetar in the Milky Way by the Canadian Hydrogen Intensity Mapping Experiment FRB collaboration (CHIME/FRB) and the Survey for Transient Astronomical Radio Emission 2 has provided an unprecedented opportunity to refine FRB emission models. The burst discovered by CHIME/FRB shows two components with different spectra. We explore interstellar scintillation as the origin for this variation in spectral structure. Modeling a weak scattering screen in the supernova remnant associated with the magnetar, we find that a superluminal apparent transverse velocity of the emission region of >9.5c is needed to explain the spectral variation. Alternatively, the two components could have originated from independent emission regions >8.3×10 4 km apart. These scenarios may arise in "far-away" models where the emission originates from well beyond the magnetosphere of the magnetar (for example, through a synchrotron maser mechanism set up by an ultrarelativistic radiative shock), but not in "close-in" models of emission from within the magnetosphere. If further radio observations of the magnetar confirm scintillation as the source of the observed variation in spectral structure, this scattering model thus constrains the location of the emission region.

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Section: Discussionmentioning

confidence: 88%

Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154

Simard

Ravi

2020

ApJL

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“…In the four bursts presented here, the range of timescales is from a few µs to a few ms. In the literature, there are bursts detected from FRB 20180916B up to widths of 6 ms (at 300-800 MHz) 4,32 , although there could be a frequency dependence on burst width.…”

Section: Implications For Progenitor Modelsmentioning

confidence: 98%

“…The only other repeating FRB with published polarisation information from multiple bursts is FRB 20180916B 4,32 .…”

Section: Introductionmentioning

confidence: 99%

“…The PPA appears to be flat over the burst duration. The polarimetric properties of four bursts from FRB 20180916B, detected at 300-400 MHz using GBT, were presented in Chawla et al 32 . They report the same polarisation properties as the original discovery (∼100% linear, flat PPA, comparable RM) supporting the idea that repeating FRBs have consistent polarisation properties between bursts from the same source, and that the phenomenology is potentially consistent between different repeating FRB sources.…”

Section: Introductionmentioning

confidence: 99%

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Microsecond polarimetry of the repeating FRB 20180916B

Nimmo¹,

Hessels²,

Keimpema³

et al. 2020

Preprint

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Fast radio bursts (FRBs) exhibit a wide variety of spectral, temporal and polarimetric properties, which can unveil clues into their emission physics and propagation effects in the local medium. FRBs are challenging to study at very high time resolution due to the precision needed to constrain the dispersion measure, signal-to-noise limitations, and also scattering from the intervening medium. Here we present the high-time-resolution (down to 1 μs) polarimetric properties of four 1.7-GHz bursts from the repeating FRB 20180916B, which were detected in voltage data during observations with the European VLBI Network. In these bursts we observe a range of emission timescales spanning three orders of magnitude, the shortest component width reaching 3-4 μs (below which we are limited by scattering). We demonstrate that all four bursts are highly linearly polarised (≥ 80%), show no evidence for significant circular polarisation (≤ 15%), and exhibit a constant polarisation position angle during and between bursts. On short timescales (≤ 100 μs), however, there appear to be subtle (few degree) polarisation position angle variations across the burst profiles. These observational results are most naturally explained in an FRB model where the emission is magnetospheric in origin, as opposed to models where the emission originates at larger distances in a relativistic shock.

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“…Fast radio bursts (FRBs) are a new class of radio transient with unknown origins (see Cordes & Chatterjee 2019;Petroff et al 2019, for reviews). They are millisecond-long, bright (peak flux densities ∼0.1-10 Jy at ∼1 GHz) bursts and have been observed at frequencies from 300 MHz (Chawla et al 2020) to 8 GHz (Gajjar et al 2018). Their distances, both based on their dispersion measure (DM) excesses (in comparison to the expected Milky Way contributions; Cordes & Lazio 2002;Yao et al 2017) and measured host-galaxy redshifts for a few sources (Chatterjee et al 2017;Bannister et al 2019;Ravi et al 2019;Prochaska et al 2019;Marcote et al 2020), are extragalactic, and the most distant sources appear to come from cosmological distances (i.e., z 0.5; Thornton et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB ∼ 180916.J0158+65

Scholz

Cook

Cruces

et al. 2020

ApJ

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We report on simultaneous radio and X-ray observations of the repeating fast radio burst source FRB180916. J0158+65 using the Canadian Hydrogen Intensity Mapping Experiment (CHIME), Effelsberg, and Deep Space Network (DSS-14 and DSS-63) radio telescopes and the Chandra X-ray Observatory. During 33 ks of Chandra observations, we detect no radio bursts in overlapping Effelsberg or Deep Space Network observations and a single burst during CHIME/FRB source transits. We detect no X-ray events in excess of the background during the Chandra observations. These non-detections imply a 5σ limit of <5×10 −10 erg cm −2 for the 0.5-10 keV fluence of prompt emission at the time of the radio burst and 1.3×10 −9 erg cm −2 at any time during the Chandra observations. Given the host-galaxy redshift of FRB180916.J0158+65 (z∼0.034), these correspond to energy limits of <1.6×10 45 erg and <4×10 45 erg, respectively. We also place a 5σ limit of <8×10 −15 erg s −1 cm −2 on the 0.5-10 keV absorbed flux of a persistent source at the location of FRB180916.J0158+65. This corresponds to a luminosity limit of <2×10 40 erg s −1. Using an archival set of radio bursts from FRB180916.J0158+65, we search for prompt gamma-ray emission in Fermi/GBM data but find no significant gamma-ray bursts, thereby placing a limit of 9×10 −9 erg cm −2 on the 10-100 keV fluence. We also search Fermi/LAT data for periodic modulation of the gamma-ray brightness at the 16.35 days period of radio burst activity and detect no significant modulation. We compare these deep limits to the predictions of various fast radio burst models, but conclude that similar X-ray constraints on a closer fast radio burst source would be needed to strongly constrain theory.

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Detection of Repeating FRB 180916.J0158+65 Down to Frequencies of 300 MHz

Cited by 95 publications

References 62 publications

Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154

Scintillation Can Explain the Spectral Structure of the Bright Radio Burst from SGR 1935+2154

Microsecond polarimetry of the repeating FRB 20180916B

Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB ∼ 180916.J0158+65

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