On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

Zhong, S. Q.; Dai, Z. G.; Zhang, H. M.; Deng, C. M.

doi:10.48550/arxiv.2005.11109

Cited by 6 publications

(10 citation statements)

References 29 publications

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“…This non-detection, together with the relatively low inferred extinction towards the source at NIR wavelengths (A J ≈ 2.0 ± 0.3 mag) allows us to place the most stringent extinction-corrected constraints till date on second-timescale flares from the source of ≈ 85 − 150 Jy ms at optical/NIR wavelengths (ν ∼ 10 14 Hz). The NIR limit corresponds to an energy E 3 × 10 36 erg at a distance of 9 kpc (Zhong et al 2020), and is within an order of magnitude of that reported in the radio for FRB 200428 at 1.25 GHz (≈ 2 × 10 35 erg; Bochenek et al 2020). It is also several orders of magnitude deeper than reported optical limits from nearby well-localized FRBs (∼ 10 43−46 erg; Hardy et al 2017;Andreoni et al 2020).…”

Section: Discussionsupporting

confidence: 76%

Constraining the X-ray - Infrared spectral index of second-timescale flares from SGR1935+2154 with Palomar Gattini-IR

De,

Ashley,

Andreoni

et al. 2020

Preprint

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The Galactic magnetar SGR 1935+2154 has been reported to produce the first known example of a bright millisecond duration radio burst (FRB 200428) similar to the cosmological population of fast radio bursts (FRBs), bolstering the association of FRBs to active magnetars. The detection of a coincident bright X-ray burst has revealed the first observed multi-wavelength counterpart of a 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 wavelengths using the Palomar Gattini-IR observing system in J-band, made possible by a recently implemented detector read-out mode that allowed for short exposure times of ≈ 0.84 s with 99.9% observing efficiency. With a total observing time of ≈ 12 hours (≈ 47728 images) on source during its 2020 outburst, we place median 3 σ limits on the second-timescale emission of 20 mJy (13.1 AB mag). We present non-detection limits from epochs of four simultaneous X-ray bursts detected by the Insight-HXMT and NuSTAR telescopes during our observing campaign. The limits translate to an observed fluence limit of 18 Jy ms, while the corresponding extinction corrected limit is 125 Jy ms for an estimated extinction of A J = 2.0 mag. These limits provide the most stringent constraints (energy 3×10 36 erg at 9 kpc) to date on the fluence of flares at frequencies of ∼ 10 14 Hz, and constrain the ratio of the near-infrared (NIR) fluence to that of coincident X-ray bursts to R NIR 2.5 × 10 −2 . Our observations were sensitive enough to easily detect a near-infrared counterpart of FRB 200428 if the NIR emission falls on the same power law as that observed across its radio to X-ray spectrum. The non-detection of NIR emission around the coincident X-ray bursts constrains the fluence index of the brightest burst to be steeper than ≈ 0.35.

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Section: Discussionsupporting

confidence: 76%

Constraining the X-ray - Infrared spectral index of second-timescale flares from SGR1935+2154 with Palomar Gattini-IR

De,

Ashley,

Andreoni

et al. 2020

Preprint

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“…Identification of FRB with rotating neutron stars predicts that FRB activity should be modulated, at some level, at the rotation rate. Periodicity has not been observed in FRB 121102, the only FRB for which abundant data exist (Zhang et al 2018); see discussion in Katz (2019). If "cosmological" and Galactic FRB are qualitatively similar phenomena, periodicity should be detectable in any FRB that repeats frequently.…”

Section: Discussionmentioning

confidence: 99%

“…A past argument (Katz 2020) against a neutron star origin of FRB was the absence of periodicity in repeating FRB, particularly in the well-studied FRB 121102 (Zhang et al 2018). SGR 1935+2154 has a period of 3.245 s (Israel et al 2016), which would be expected to modulate the observable activity of FRB 200428, whatever its mechanism of emission, unless its magnetic field be a dipole aligned with the spin axis.…”

Section: Frbmentioning

confidence: 99%

The FRB-SGR Connection

Katz

2020

Preprint

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The discovery that the Galactic SGR 1935+2154 emitted FRB 200428 simultaneous with a gamma-ray flare demonstrated the common source and association of these phenomena. If FRB radio emission is the result of coherent curvature radiation, the net charge of the radiating "bunches" or waves may be estimated. A statistical argument indicates that the radiating bunches must have a Lorentz factor 10. The observed radiation frequencies indicate that their phase velocity (pattern speed) corresponds to Lorentz factors 100. Coulomb repulsion implies that the electrons making up these bunches may have yet larger Lorentz factors, limited by their incoherent curvature radiation. These electrons also Compton scatter in the soft gamma-ray field of the SGR. In FRB 200428 the power radiated coherently at radio frequencies exceeded that of Compton scattering, but in more luminous SGR outbursts Compton scattering dominates, precluding the acceleration of energetic electrons. This explains the absence of a FRB associated with the giant 27 December 2004 outburst of SGR 1806−20. SGR with luminosity 10 42 ergs/s do not emit FRB, while those of lesser luminosity can do so.

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“…SGR 1935+2154 is a magnetar with rotational period P = 3.24 s (Stamatikos et al 2014), a surface dipolar magnetic field B NS 2.2 × 10 14 G derived from the spin-down rate Ṗ 1.43 × 10 −11 s s −1 (Israel et al 2016). It is associated with supernova remnant (SNR) G57.2+0.8 (Gaensler 2014), of which the distance is roughly within a range of 6-15 kpc (Sun et al 2011;Pavlović et al 2013;Kothes et al 2018;Zhong et al 2020;Zhou et al 2020). In this work, we adopt D L = 10 kpc for SGR 1935+2154, and the uncertainty of D L will not affect our results significantly.…”

Section: Magnetar-asteroid Interactionmentioning

confidence: 99%

FRB 200428: an Impact between an Asteroid and a Magnetar

Geng,

Li,

et al. 2020

Preprint

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A fast radio burst was recently detected to be associated with a hard X-ray burst from the Galactic magnetar SGR 1935+2154. Scenarios involving magnetars for FRBs are hence highly favored. In this work, we suggest that the impact between an asteroid and a magnetar could explain such a detection. According to our calculations, an asteroid of mass 10 20 g will be disrupted at 7 × 10 9 cm when approaching the magnetar, the accreted material will flow along the magnetic field lines at Alfvén radius ∼ 10 7 cm. After falling onto the magnetar surface, an instant accretion column will be formed, producing a Comptonized X-ray burst and an FRB in the magnetosphere. We show that all the observational features could be interpreted self-consistently in our scenario. Quasi-periodic oscillations in this specific X-ray burst may help to verify our scenario.

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On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

Cited by 6 publications

References 29 publications

Constraining the X-ray - Infrared spectral index of second-timescale flares from SGR1935+2154 with Palomar Gattini-IR

Constraining the X-ray - Infrared spectral index of second-timescale flares from SGR1935+2154 with Palomar Gattini-IR

The FRB-SGR Connection

FRB 200428: an Impact between an Asteroid and a Magnetar

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