The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data

Kienlin, A. von; Meegan, C.; Pačiesas, W. S.; Bhat, P. N.; Bissaldi, E.; Briggs, M. S.; Burns, E.; Cleveland, W. H.; Gibby, M. H.; Giles, M. M.; Goldstein, A.; Hamburg, R.; Hui, C. M.; Kocevski, D.; Mailyan, B.; Malacaria, C.; Poolakkil, S.; Preece, R. D.; Roberts, O. J.; Vereš, P.; Wilson-Hodge, C.

doi:10.3847/1538-4357/ab7a18

Cited by 262 publications

(192 citation statements)

References 41 publications

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“…4.6). The emission is characterized by a total duration of $ 0:01À5 s predominantly in the $ 10 keV to $ 10 MeV, with peak isotropic luminosities $ 10 51 erg =s (e.g., von Kienlin et al 2020;Abbott et al 2017b).…”

Section: Jetsmentioning

confidence: 99%

Neutron star mergers and how to study them

Burns

2020

Living Rev Relativ

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Neutron star mergers are the canonical multimessenger events: they have been observed through photons for half a century, gravitational waves since 2017, and are likely to be sources of neutrinos and cosmic rays. Studies of these events enable unique insights into astrophysics, particles in the ultrarelativistic regime, the heavy element enrichment history through cosmic time, cosmology, dense matter, and fundamental physics. Uncovering this science requires vast observational resources, unparalleled coordination, and advancements in theory and simulation, which are constrained by our current understanding of nuclear, atomic, and astroparticle physics. This review begins with a summary of our current knowledge of these events, the expected observational signatures, and estimated detection rates for the next decade. I then present the key observations necessary to advance our understanding of these sources, followed by the broad science this enables. I close with a discussion on the necessary future capabilities to fully utilize these enigmatic sources to understand our universe.

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Section: Jetsmentioning

confidence: 99%

Neutron star mergers and how to study them

Burns

2020

Living Rev Relativ

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“…The spectral and timing properties for both short and long GRBs suggest that the gamma-ray component of the prompt emission is produced in highly relativistic jets (Gehrels & Razzaque 2013). However, the physical properties of these jets, such as their structure and magnetic topology, remain poorly understood despite the plethora of flux, spectral, and timing measurements produced over the last five decades; see for example Kienlin et al (2020), Lien et al (2016), Meegan et al (1997) and Tsvetkova et al (2017c).…”

Section: Introductionmentioning

confidence: 99%

The POLAR gamma-ray burst polarization catalog

Kole

Angelis²,

Berlato³

et al. 2020

A&A

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Context. Despite over 50 years of research, many open questions remain about the origin and nature of gamma-ray bursts (GRBs). Linear polarization measurements of the prompt emission of these extreme phenomena have long been thought to be key to answering a range of these questions. The POLAR detector was designed to produce the first set of detailed and reliable linear polarization measurements in the 50 − 500 keV energy range. During late 2016 and early 2017, POLAR detected a total of 55 GRBs. The analysis results of 5 of these GRBs have been reported, and were found to be consistent with a low or unpolarized flux. However, previous reports by other collaborations found high levels of linear polarization, including some as high as 90%. Aims. We study the linear polarization for the 14 GRBs observed by POLAR for which statistically robust inferences are possible. Additionally, time-resolved polarization studies are performed on GRBs with sufficient apparent flux. Methods. A publicly available polarization analysis tool, developed within the Multi-Mission Maximum Likelihood framework (3ML), was used to produce statistically robust results. The method allows spectral and polarimetric data from POLAR to be combined with spectral data from the Fermi Gamma-ray Burst Monitor (Fermi-GBM) and the Neil Gehrels Swift Observatory (hereafter Swift) to jointly model the spectral and polarimetric parameters. Results. The time-integrated analysis finds all results to be compatible with low or zero polarization with the caveat that, when timeresolved analysis is possible within individual pulses, we observe moderate linear polarization with a rapidly changing polarization angle. Therefore, time-integrated polarization results, while pointing to lower polarization, are potentially an artifact of summing over the changing polarization signal and thus washing out the true moderate polarization. We therefore caution against overinterpretation of any time-integrated results inferred herein and encourage the community to wait for more detailed polarization measurements from forthcoming missions such as POLAR-2 and LEAP.

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“…The accompanying plasma continues its outward flow with a bulk Lorentz factor G ej ⇠ 100 and kinetic energy ⇠ 3 ⇥ 10 46 erg 21,22 . Such a high Lotentz factor is in contrast to the MGFs observed in the Milky Way that powered only mildly relativistic outflows observed as radio nebulae 23,24 expanding at ⇠ .7c, where the much lower expansion velocity can be attributed to entrainment of a larger baryon mass. The inferred kinetic energy of the outflow from the MGF in Sculptor is, however, comparable with the total radiated energy in the initial spike, as also inferred for the previous local MGFs.…”

Section: /7mentioning

confidence: 57%

High-energy emission from a magnetar giant flare in the Sculptor galaxy

Ajello¹,

Atwood²,

Axelsson³

et al. 2021

Nat Astron

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Magnetars are the most highly-magnetized neutron stars in the cosmos (B ⇠ 10 13 15 G). Giant flares from magnetars are rare, short-duration (about 0.1 s) bursts of hard X-rays and soft g rays 1, 2. We report here the discovery of GeV emission from a magnetar giant flare (MGF) on 15 April, 2020 3-5. The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope detected GeV g rays from 19 s until 284 s after the initial detection of a signal in the MeV band. Our analysis shows that these g rays are spatially associated with the nearby (3.5 Mpc) Sculptor galaxy and are unlikely to originate from a cosmological gray burst. Thus, we infer that the g rays originated with the MGF in Sculptor. We suggest that the GeV signal is generated by an ultra-relativistic outflow that first radiates the prompt MeV-band photons, and then deposits its energy far from the stellar magnetosphere. After a propagation delay, the outflow interacts with environmental gas, produces shock waves that accelerate electrons to very high energies and these then emit GeV g rays as optically thin synchrotron radiation. On 15 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200415A 4 initially classified as a short (duration<2 seconds) Gamma-ray Burst (SGRB). The Interplanetary Network of gray detectors (IPN 1) reduced the uncertainty on the GBM position to 20 sq. arcmin suggesting that the GRB originated from the nearby Sculptor galaxy 3 , located at a distance of ⇠3.5 Mpc 6. This, with the resemblance of the GBM sub-MeV light curve 7 to the extragalactic Soft Gamma Repeater (SGR) giant flare candidates GRB 051103 3, 8 and GRB 070201 9 , and the detection of quasi-periodic oscillations (QPOs) by the Atmosphere-Space Interaction Monitor (ASIM) 5 , led to the identification of GRB 200415A as a Magnetar Giant Flare (MGF) in Sculptor. GRB 200415A was 43 from the LAT boresight at the GBM trigger time T 0 (08:48:05.563746 UTC) and remained well within the LAT field of view (FOV) until 500 seconds after T 0. Three g rays were detected by the LAT, allowing the localization of GRB 200415A at high energies (>100 MeV): this represents the first detection of high-energy gamma-ray emission from an MGF, and suggests that magnetars can power the relativistic outflows observed in some SGRBs. To study the localization of the gray signal observed by the LAT we perform a likelihood analysis and compute a test statistic (TS) for the presence of the source at different positions. The best position is obtained from the maximum of the TS (TS max = 29, corresponding to a detection significance close to 5 s , see the Method section). Then, the variation of the TS around this position provides the map of localization contours shown in Figure 1. The iso-contours in red encompass localization probabilities of 68% and 90%. Four galaxies (IC 1576, IC 1578, IC 1582 and NGC 253) from the NGC 2000 catalog 10 are located within a circular region of radius r 99 , whose area is equivalent to the 99% c.l., and which is centered on the maximum of...

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The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data

Cited by 262 publications

References 41 publications

Neutron star mergers and how to study them

Neutron star mergers and how to study them

The POLAR gamma-ray burst polarization catalog

High-energy emission from a magnetar giant flare in the Sculptor galaxy

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