Magnetic Fields in Gamma-Ray Bursts and Their Polarised Emission

Kobayashi, S.

doi:10.1007/978-3-030-19715-5_13

Cited by 2 publications

(2 citation statements)

References 175 publications

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“…For this GRB, the GISP is estimated to be 0.07%, 0.08%, and 0.09% for 𝐼, 𝑅, and 𝑉 bands thus contribution from GISP is negligible. Since we are observing forward shock dominated emission, the low level of polarization detection is in line with theoretical predictions (Rossi et al 2004;Kobayashi 2019).…”

Section: Grb 141220asupporting

confidence: 89%

“…One of the most puzzling aspects of GRBs is the magnetic field properties of their jets which can shed light on the driving mechanism of the explosion (Lazzati 2006;Toma 2013; Covino & Gotz ★ E-mail: m.shrestha@ljmu.ac.uk 2016; Kobayashi 2019). Since GRBs are cosmological in nature, we cannot obtain the spatial resolution to understand the magnetic field strength and structure of the jets with most observational methods.…”

Section: Introductionmentioning

confidence: 99%

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Polarimetry and photometry of gamma-ray bursts afterglows with RINGO3

Shrestha

Steele

Kobayashi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present photometric and polarimetric measurements of gamma-ray burst (GRB) optical afterglows observed by the RINGO3 imaging polarimeter over its ∼7 year lifetime mounted on the Liverpool Telescope. During this time, RINGO3 responded to 67 GRB alerts. Of these, 28 had optical afterglows and a further ten were sufficiently bright for photometric and polarimetric analysis (R⪅17). We present high quality multicolour light curves of ten sources: GRB 130606A, GRB 130610A, GRB 130612A, GRB 140430A, GRB 141220A, GRB 151215A, GRB 180325A, GRB 180618A, GRB 190114C, and GRB 191016A and polarimetry for seven of these (excluding GRB 130606A, GRB 130610A, and GRB 130612A, which were observed before the polarimetry mode was fully commissioned). Eight of these ten GRBs are classical long GRBs, one sits at the short-long duration interface with a T90 ∼ 4 seconds and one is a classical short, hard burst with extended emission. We detect polarization for GRB 190114C and GRB 191016A. While detailed analyses of several of these GRBs have been published previously, here we present a uniform re-reduction and analysis of the whole sample and investigation of the population in a broad context relative to the current literature. We use survival analysis to fully include the polarization upper limits in the comparison with other GRB properties, such as temporal decay rate, isotropic energy and redshift. We find no clear correlation between polarization properties and wider sample properties and conclude that larger samples of early time polarimetry of GRB afterglows are required to fully understand GRB magnetic fields.

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Section: Grb 141220asupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Polarimetry and photometry of gamma-ray bursts afterglows with RINGO3

Shrestha

Steele

Kobayashi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Spectropolarimetry and photometry of the early afterglow of the gamma-ray burst GRB 191221B

Buckley

Bagnulo

Britto

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report on results of spectropolarimetry of the afterglow of the long gamma-ray burst GRB 191221B, obtained with SALT/RSS and VLT/FORS2, as well as photometry from two telescopes in the MASTER Global Robotic Network, at the MASTER-SAAO (South Africa) and MASTER-OAFA (Argentina) stations. Prompt optical emission was detected by MASTER-SAAO 38 s after the alert, which dimmed from a magnitude (white-light) of ∼10 to 16.2 mag over a period of ∼10 ks, followed by a plateau phase lasting ∼10 ks and then a decline to ∼18 mag after 80 ks. The light curve shows complex structure, with four or five distinct breaks in the power-law decline rate. SALT/RSS linear spectropolarimetry of the afterglow began ∼2.9 h after the burst, during the early part of the plateau phase of the light curve. Absorption lines seen at ∼6010 Å and 5490 Å are identified with the Mg II 2799 Å line from the host galaxy at z = 1.15 and an intervening system located at z = 0.96. The mean linear polarisation measured over 3400 − 8000 Å was ∼1.5% and the mean equatorial position angle (θ) ∼65○. VLT/FORS2 spectropolarimetry was obtained ∼10 h postburst, during a period of slow decline (α = −0.44), and the polarisation was measured to be p = 1.2% and θ = 60○. Two observations with the MeerKAT radio telescope, taken 30 and 444 days after the GRB trigger, detected radio emission from the host galaxy only. We interpret the light curve and polarisation of this long GRB in terms of a slow-cooling forward-shock.

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Magnetic Fields in Gamma-Ray Bursts and Their Polarised Emission

Cited by 2 publications

References 175 publications

Polarimetry and photometry of gamma-ray bursts afterglows with RINGO3

Polarimetry and photometry of gamma-ray bursts afterglows with RINGO3

Spectropolarimetry and photometry of the early afterglow of the gamma-ray burst GRB 191221B

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