The Multiwavelength Counterparts of Fast Radio Bursts

Chen, Ge; Ravi, Vikram; Lu, W.

doi:10.3847/1538-4357/ab982b

Cited by 38 publications

(40 citation statements)

References 67 publications

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“…Extending the same model to the shock properties derived for the observed populations of cosmological FRBs predicts that the afterglow emission for these more energetic bursts will occur at much higher energies,  E peak MeV-GeV, in the gamma-ray band (Figure 8). Unfortunately, gamma-ray satellites like Swift and Fermi are generally not sensitive enough to detect this emission to the cosmological distances of most FRB sources (Metzger et al 2019;Chen et al 2020;Margalit et al 2020). We furthermore emphasize that this predicted short (∼milliseconds duration) gamma-ray signal from the shocks is distinct from the longer-lasting and typically softer gamma-ray emission observed from giant Galactic magnetar flares (e.g., Hurley et al 2005;Palmer et al 2005), which is instead well explained as a pair fireball generated by dissipation very close to the NS surface.…”

Section: Baryonic Shellmentioning

confidence: 99%

“…In curvature models, the FRB is produced by curvature radiation from bunched electrons streaming along the magnetic field lines of the magnetar (e.g., Kumar et al 2017;Lu & Kumar 2018). These models predict fluence ratios h~1 in all bands (Chen et al 2020) and thus cannot explain the properties of the observed X-ray burst of SGR 1935+2154(whose fluence ratio is  h~-10 1…”

Section: Additional Modelsmentioning

confidence: 99%

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Implications of a Fast Radio Burst from a Galactic Magnetar

Margalit

Beniamini

Sridhar

et al. 2020

ApJL

151

123

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A luminous radio burst was recently detected in temporal coincidence with a hard X-ray flare from the Galactic magnetar SGR 1935+2154with a time and frequency structure consistent with cosmological fast radio bursts (FRBs) and a fluence within a factor of 10 of the least energetic extragalactic FRB previously detected. Although active magnetars are commonly invoked FRB sources, several distinct mechanisms have been proposed for generating the radio emission that make different predictions for the accompanying higher-frequency radiation. We show that the properties of the coincident radio and X-ray flares from SGR 1935+2154, including their approximate simultaneity and relative fluence~-E E 10 radio X 5 , as well as the duration and spectrum of the X-ray emission, are consistent with extant predictions for the synchrotron maser shock model. Rather than arising from the inner magnetosphere, the X-rays are generated by (incoherent) synchrotron radiation from thermal electrons heated at the same internal shocks that produce the coherent maser emission as ultrarelativistic flare ejecta collides with a slower particle outflow (e.g., as generated by earlier flaring activity) on a radial scale of~10 11 cm. Although the rate of SGR 1935+2154-like bursts in the local universe is not sufficient to contribute appreciably to the extragalactic FRB rate, the inclusion of an additional population of more active magnetars with stronger magnetic fields than the Galactic population can explain both the FRB rate and the repeating fraction, but only if the population of active magnetars are born at a rate that is at least 2 orders of magnitude lower than that of the SGR 1935+2154-like magnetars. This may imply that the more active magnetar sources are not younger magnetars formed in a similar way to the Milky Way population (e.g., via ordinary supernovae) but are instead formed through more exotic channels, such as superluminous supernovae, accretion-induced collapse, or neutron star mergers.

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Section: Baryonic Shellmentioning

confidence: 99%

Section: Additional Modelsmentioning

confidence: 99%

Implications of a Fast Radio Burst from a Galactic Magnetar

Margalit

Beniamini

Sridhar

et al. 2020

ApJL

151

123

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“…Since the theoretical predictions for multiwavelength counterparts are not well constrained enough to interpret our upper limits directly, we only briefly compare them to our NIR observational data. Chen et al (2020) provide a summary of the predictions for the fluence in the aforementioned models. In the case of the relativistic shock interaction model by Beloborodov (2020), if the the blast wave strikes a wind bubble in the tail of a previous flare, a bright optical flare could result with an optical to radio fluence ratio of    10 opt radio 5 (Chen et al 2020).…”

Section: Comparison To Theoretical Modelsmentioning

confidence: 99%

“…Chen et al (2020) provide a summary of the predictions for the fluence in the aforementioned models. In the case of the relativistic shock interaction model by Beloborodov (2020), if the the blast wave strikes a wind bubble in the tail of a previous flare, a bright optical flare could result with an optical to radio fluence ratio of    10 opt radio 5 (Chen et al 2020). If some X-ray bursts from SGR 1935+2154 during the PGIR campaign were accompanied by a radio burst similar to FRB 200428, then we have the corresponding prediction of R NIR 0.1 for ).…”

Section: Comparison To Theoretical Modelsmentioning

confidence: 99%

Constraining the X-Ray–Infrared Spectral Index of Second-timescale Flares from SGR 1935+2154 with Palomar Gattini-IR

Ashley

Andreoni

et al. 2020

ApJL

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The Galactic magnetar SGR 1935+2154 has been reported to produce the first example of a bright millisecondduration radio burst (FRB 200428) similar to the cosmological population of fast radio bursts (FRBs). The detection of a coincident bright X-ray burst represents the first observed multiwavelength counterpart of an FRB. However, the search for similar emission at optical wavelengths has been hampered by the high inferred extinction on the line of sight. Here, we present results from the first search for second-timescale emission from the source at near-infrared (NIR) wavelengths using the Palomar Gattini-IR observing system in the J band, enabled by a novel detector readout mode that allows short exposure times of ≈0.84 s with 99.9% observing efficiency. With a total observing time of ≈12 hr (≈47,728 images) during its 2020 outburst, we place median 3σ limits on the secondtimescale NIR fluence of 18Jy ms (13.1 AB mag). The corresponding extinction-corrected limit is 125Jy ms for an estimated extinction of A J =2.0 mag. Our observations were sensitive enough to easily detect an NIR counterpart of FRB 200428 if the NIR emission falls on the same power law as observed across its radio to X-ray spectrum. We report nondetection limits from epochs of four simultaneous X-ray bursts detected by the Insight-HXMT and NuSTAR telescopes during our observations. These limits provide the most stringent constraints to date on fluence of flares at ∼10 14 Hz, and constrain the fluence ratio of the NIR emission to coincident X-ray bursts to R NIR 0.025 (fluence index 0.35).

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“…The first decade of FRB searches was undertaken with telescopes that had localization regions ?1 arcmin 2 . This is inhibited by the seeming lack of "afterglows" analogous to those observed for GRBs (Petroff et al 2017;Bhandari et al 2018;Chen et al 2020) and associated supernova-like transient counterparts (Marnoch et al 2020). A precise localization (∼1″) of the burst itself is thus required to robustly identify the associated host galaxy (Eftekhari & Berger 2017).…”

Section: Introductionmentioning

confidence: 99%

Host Galaxy Properties and Offset Distributions of Fast Radio Bursts: Implications for Their Progenitors

Heintz

Prochaska

Simha

et al. 2020

ApJ

207

280

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We present observations and detailed characterizations of five new host galaxies of fast radio bursts (FRBs) discovered with the Australian Square Kilometre Array Pathfinder (ASKAP) and localized to 1″. Combining these galaxies with FRB hosts from the literature, we introduce criteria based on the probability of chance coincidence to define a subsample of 10 highly confident associations (at z=0.03-0.52), 3 of which correspond to known repeating FRBs. Overall, the FRB-host galaxies exhibit a broad, continuous range of color (M u −M r =0.9-2.0), stellar mass (M å =10 8 −6×10 10 M e), and star formation rate (SFR=0.05-10 M e yr −1) spanning the full parameter space occupied by z<0.5 galaxies. However, they do not track the color-magnitude, SFR-M å , nor BPT diagrams of field galaxies surveyed at similar redshifts. There is an excess of "green valley" galaxies and an excess of emission-line ratios indicative of a harder radiation field than that generated by star formation alone. From the observed stellar mass distribution, we rule out the hypothesis that FRBs strictly track stellar mass in galaxies (>99% c.l.). We measure a median offset of 3.3 kpc from the FRB to the estimated center of the host galaxies and compare the host-burst offset distribution and other properties with the distributions of long-and short-duration gamma-ray bursts (LGRBs and SGRBs), core-collapse supernovae (CC-SNe), and SNe Ia. This analysis rules out galaxies hosting LGRBs (faint, star-forming galaxies) as common hosts for FRBs (>95% c.l.). Other transient channels (SGRBs, CC-, and SNe Ia) have host-galaxy properties and offsets consistent with the FRB distributions. All of the data and derived quantities are made publicly available on a dedicated website and repository.

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The Multiwavelength Counterparts of Fast Radio Bursts

Cited by 38 publications

References 67 publications

Implications of a Fast Radio Burst from a Galactic Magnetar

Implications of a Fast Radio Burst from a Galactic Magnetar

Constraining the X-Ray–Infrared Spectral Index of Second-timescale Flares from SGR 1935+2154 with Palomar Gattini-IR

Host Galaxy Properties and Offset Distributions of Fast Radio Bursts: Implications for Their Progenitors

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