Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Oates, S. R.

doi:10.3390/universe9030113

Cited by 6 publications

(4 citation statements)

References 267 publications

(383 reference statements)

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“…Such profiles generally exhibit structured features on timescales of up to 10 3 s. At early times, they may also be directly related to the prompt activity of the central engine of the GRB. The class of decays corresponds to about 50% of events (Oates 2023). These GRBs are characterized by a simple power-law decay of the optical flux with time.…”

Section: Temporal Profilesmentioning

confidence: 99%

Detecting the Early Optical Flashes of Gamma-Ray Bursts with Small Telescope Arrays

Sadeh

2024

ApJ

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We present an observational approach for the independent detection of the early optical emission of long gamma-ray bursts (GRBs). For this purpose, we explore the potential of the Large Array Survey Telescope (LAST). This array of small optical telescopes can be used to scan a wide region of the sky, and to focus on a smaller field of view with increased sensitivity, as needed. The modularity of the array facilitates dynamic scanning of multiple fields, by shifting telescope pointing directions with high cadence. This can significantly increase the effective sky-coverage of a blind survey on short timescales. For events associated with gamma-ray counterparts, the valuable early time data can supplement high-energy observations. Regardless of gamma-ray association, detections can potentially be used to explore various phenomena associated with GRBs, such as orphan afterglows; dirty fireballs; and choked jets. We simulate a sample of GRBs and their respective optical signals at early times. After accounting for dynamic cadence, the light curves are given as input to a machine-learning classifier, used to identify astrophysical transients. We find that, by dedicating half of an LAST array to a blind search, one would expect to independently detect 7–11 GRBs yr–1, corresponding to an approximate intrinsic event rate of 0.12 deg–2 yr–1.

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Section: Temporal Profilesmentioning

confidence: 99%

Detecting the Early Optical Flashes of Gamma-Ray Bursts with Small Telescope Arrays

Sadeh

2024

ApJ

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“…Thanks to this configuration, its rapid reaction capability and its long life time (already about 20 years), several new results have already been obtained with this mission, with reviews of the most important ones, inclusive of those obtained from statistical studies, already reported (see [110][111][112][113][114][115][116][117][118][119]). Among them, two important results, left open by Bep-poSAX and solved with Swift thanks to its rapid reaction capability, are the early afterglow properties of long GRBs and the afterglow of short GRBs (no afterglow of short GRBs was discovered with BeppoSAX).…”

Section: Swift and Its Role In The Progress Of The Grb Phenomenonmentioning

confidence: 99%

A Short History of the First 50 Years: From the GRB Prompt Emission and Afterglow Discoveries to the Multimessenger Era

Frontera

2024

Universe

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More than fifty years have elapsed from the first discovery of gamma-ray bursts (GRBs) with American Vela satellites, and more than twenty-five years from the discovery with the BeppoSAX satellite of the first X-ray afterglow of a GRB. Thanks to the afterglow discovery and to the possibility given to the optical and radio astronomers to discover the GRB optical counterparts, the long-time mystery about the origin of these events has been solved. Now we know that GRBs are huge explosions, mainly ultra relativistic jets, in galaxies at cosmological distances. Starting from the first GRB detection with the Vela satellites, I will review the story of these discoveries, those obtained with BeppoSAX, the contribution to GRBs by other satellites and ground experiments, among them being Venera, Compton Gamma Ray Observatory, HETE-2, Swift, Fermi, AGILE, MAGIC, H.E.S.S., which were, and some of them are still, very important for the study of GRB properties. Then, I will review the main results obtained thus far and the still open problems and prospects of GRB astronomy.

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“…The burst was localised by the Neil Gehrels Swift Observatory's Burst Alert Telescope (Dichiara et al 2022) and followed up by the Very Large Telescope (VLT) X-shooter instrument (de Ugarte Postigo et al 2022;Malesani et al 2023), which determined that it occurred at a redshift of 0.151 and belongs to very near long GRBs (Oates 2023). It was also detected by a multitude of other instruments: AGILE/GRID (Piano et al 2022), AGILE/MCAL (Ursi et al 2022), BepiColombo/MGNS Send offprint requests to: J. Řípa, e-mail: ripa.jakub@gmail.com (Kozyrev et al 2022), Insight-HXMT & SATech-01/GECAM-C (HEBS; An et al 2023), INTEGRAL/SPI-ACS (Gotz et al 2022), Konus-WIND & SRG/ART-XC (Frederiks et al 2023), MAXI & NICER (Williams et al 2023), Solar Orbiter/STIX (Xiao et al 2022), STPSat-6/SIRI-2 (Mitchell et al 2022), and XMM-Newton (Tiengo et al 2023).…”

Section: Introductionmentioning

confidence: 99%

The peak flux of GRB 221009A measured with GRBAlpha

Ripa¹,

Takahashi²,

Fukazawa³

et al. 2023

A&A

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Context. On 2022 October 9 the brightest gamma-ray burst (GRB) ever observed lit up the high-energy sky. It was detected by a multitude of instruments, attracting the close attention of the GRB community, and saturated many detectors. Aims. GRBAlpha, a nano-satellite with a form factor of a 1U CubeSat, detected this extraordinarily bright long-duration GRB, GRB 221009A, without saturation but affected by pile-up. We present light curves of the prompt emission in 13 energy bands, from 80 keV to 950 keV, and performed a spectral analysis to calculate the peak flux and peak isotropic-equivalent luminosity. Methods. Since the satellite's attitude information is not available for the time of this GRB, more than 200 incident directions were probed in order to find the median luminosity and its systematic uncertainty. Results. We find that the peak flux in the 80−800 keV range (observer frame) was F p ph = 1300 +1200 −200 ph cm −2 s −1 , or F p erg = 5.7 +3.7 −0.7 ×10 −4 erg cm −2 s −1 , and the fluence in the same energy range of the first GRB episode, which lasted 300 s and was observable by GRBAlpha, was S = 2.2 +1.4 −0.3 × 10 −2 erg cm −2 , or S bol = 4.9 +0.8 −0.5 × 10 −2 erg cm −2 for the extrapolated range of 0.9 − 8, 690 keV. We infer the isotropic-equivalent released energy of the first GRB episode to be E bol iso = 2.8 +0.8 −0.5 × 10 54 erg in the 1 − 10, 000 keV band (rest frame at z = 0.15). The peak isotropic-equivalent luminosity in the 92 − 920 keV range (rest frame) was L p iso = 3.7 +2.5 −0.5 × 10 52 erg s −1 , and the bolometric peak isotropic-equivalent luminosity was L p,bol iso = 8.4 +2.5 −1.5 × 10 52 erg s −1 (4 s scale) in the 1 − 10, 000 keV range (rest frame). The peak emitted energy is E * p = E p (1 + z) = 1120 ± 470 keV. Our measurement of L p,bol iso is consistent with the Yonetoku relation. It is possible that, due to the spectral evolution of this GRB and the orientation of GRBAlpha at the peak time, the true values of peak flux, fluence, L iso , and E iso are even higher.

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Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Cited by 6 publications

References 267 publications

Detecting the Early Optical Flashes of Gamma-Ray Bursts with Small Telescope Arrays

Detecting the Early Optical Flashes of Gamma-Ray Bursts with Small Telescope Arrays

A Short History of the First 50 Years: From the GRB Prompt Emission and Afterglow Discoveries to the Multimessenger Era

The peak flux of GRB 221009A measured with GRBAlpha

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