scholarly journals GRB 090926A AND BRIGHT LATE-TIME FERMI LARGE AREA TELESCOPE GAMMA-RAY BURST AFTERGLOWS

2010 ◽  
Vol 718 (1) ◽  
pp. L14-L18 ◽  
Author(s):  
C. A. Swenson ◽  
A. Maxham ◽  
P. W. A. Roming ◽  
P. Schady ◽  
L. Vetere ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Late Time ◽  
Large Area ◽  
Gamma Ray Burst

scholarly journals X-Ray Astronomy Satellite Ginga

1990 ◽  
Vol 123 ◽  
pp. 41-48
Author(s):  
F. Makino
Keyword(s):  
Gamma Ray ◽  
Effective Area ◽  
X Rays ◽  
Scientific Instruments ◽  
Large Area ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Proportional Counters ◽  
Main Instrument

AbstractThe X-ray astronomy satellite Ginga carries three scientific instruments, the Large Area proportional Counters (LAC), All Sky X-ray Monitor (ASM) and Gamma-ray Burst Detector (GBD). The LAC is the main instrument with an effective area of 4000 cm2 giving it the highest sensitivity to hard X-rays so far achieved. Ginga observed about 250 targets up to the end of 1989.

Balloon Observations of Several Southern X-Ray Sources

1979 ◽  
Vol 3 (5) ◽  
pp. 349-350 ◽  
Author(s):  
J. G. Greenhill ◽  
M. L Duldig ◽  
M. W. Emery ◽  
A. G. Fenton ◽  
K. B. Fenton ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Transient Increase ◽  
Large Area ◽  
Gamma Ray Burst ◽  
X Ray ◽  
The University ◽  
Area X

The University of Tasmania balloon-borne large area X-ray telescope was flown from Alice Springs on 20 November 1978. A number of known X-ray sources were observed and a transient increase believed to be a gamma ray burst was detected.

scholarly journals Late-time Evolution and Modeling of the Off-axis Gamma-Ray Burst Candidate FIRST J141918.9+394036

2022 ◽  
Vol 924 (1) ◽  
pp. 16
Author(s):  
K. P. Mooley ◽  
B. Margalit ◽  
C. J. Law ◽  
D. A. Perley ◽  
A. T. Deller ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Optical Data ◽  
Host Galaxy ◽  
Opening Angle ◽  
Late Time ◽  
Gamma Ray Burst ◽  
Very Large Array ◽  
Long Baseline ◽  
New Radio ◽  
Low Metallicity

Abstract We present new radio and optical data, including very-long-baseline interferometry, as well as archival data analysis, for the luminous, decades-long radio transient FIRST J141918.9+394036. The radio data reveal a synchrotron self-absorption peak around 0.3 GHz and a radius of around 1.3 mas (0.5 pc) 26 yr post-discovery, indicating a blastwave energy ∼5 × 1050 erg. The optical spectrum shows a broad [O iii]λ4959,5007 emission line that may indicate collisional excitation in the host galaxy, but its association with the transient cannot be ruled out. The properties of the host galaxy are suggestive of a massive stellar progenitor that formed at low metallicity. Based on the radio light curve, blastwave velocity, energetics, nature of the host galaxy and transient rates, we find that the properties of J1419+3940 are most consistent with long gamma-ray burst (LGRB) afterglows. Other classes of (optically discovered) stellar explosions as well as neutron star mergers are disfavored, and invoking any exotic scenario may not be necessary. It is therefore likely that J1419+3940 is an off-axis LGRB afterglow (as suggested by Law et al. and Marcote et al.), and under this premise the inverse beaming fraction is found to be f b − 1 ≃ 280 − 200 + 700 , corresponding to an average jet half-opening angle < θ j > ≃ 5 − 2 + 4 degrees (68% confidence), consistent with previous estimates. From the volumetric rate we predict that surveys with the Very Large Array, Australian Square Kilometre Array Pathfinder, and MeerKAT will find a handful of J1419+3940-like events over the coming years.

scholarly journals GRB 190114C: from prompt to afterglow?

2019 ◽  
Vol 626 ◽  
pp. A12 ◽  
Author(s):  
M. E. Ravasio ◽  
G. Oganesyan ◽  
O. S. Salafia ◽  
G. Ghirlanda ◽  
G. Ghisellini ◽  
...  
Keyword(s):  
Energy Range ◽  
Power Law ◽  
Gamma Ray ◽  
Spectral Energy Distribution ◽  
Onset Time ◽  
Lorentz Factor ◽  
Spectral Energy ◽  
Large Area ◽  
Spectral Evolution ◽  
Gamma Ray Burst

GRB 190114C is the first gamma-ray burst detected at very high energies (VHE, i.e., > 300 GeV) by the MAGIC Cherenkov telescope. The analysis of the emission detected by the Fermi satellite at lower energies, in the 10 keV–100 GeV energy range, up to ∼50 s (i.e., before the MAGIC detection) can hold valuable information. We analyze the spectral evolution of the emission of GRB 190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV–40 MeV energy range up to ∼60 s. The first 4 s of the burst feature a typical prompt emission spectrum, which can be fit by a smoothly broken power-law function with typical parameters. Starting on ∼4 s post-trigger, we find an additional nonthermal component that can be fit by a power law. This component rises and decays quickly. The 10 keV–40 MeV flux of the power-law component peaks at ∼6 s; it reaches a value of 1.7 × 10−5 erg cm−2 s−1. The time of the peak coincides with the emission peak detected by the Large Area Telescope (LAT) on board Fermi. The power-law spectral slope that we find in the GBM data is remarkably similar to that of the LAT spectrum, and the GBM+LAT spectral energy distribution seems to be consistent with a single component. This suggests that the LAT emission and the power-law component that we find in the GBM data belong to the same emission component, which we interpret as due to the afterglow of the burst. The onset time allows us to estimate that the initial jet bulk Lorentz factor Γ0 is about 500, depending on the assumed circum-burst density.

Anatomy of a merger

2019 ◽  
pp. 541-580
Author(s):  
Nils Andersson
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binary System ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Tidal Effects ◽  
Gamma Ray Burst ◽  
Love Numbers ◽  
Star Binary

This chapter discusses the different stages of an inspiralling neutron star binary system, through the formation of a black hole and the possible emergence of a gamma-ray burst. Tidal effects and the information encoded in the so-called Love numbers are explored. The violent dynamics of the merger is considered and models of gamma-ray bursts and the late time kilonova emission are also explored.

scholarly journals Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

Science ◽  
2013 ◽  
Vol 343 (6166) ◽  
pp. 42-47 ◽  
Author(s):  
M. Ackermann ◽  
M. Ajello ◽  
K. Asano ◽  
W. B. Atwood ◽  
M. Axelsson ◽  
...  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Synchrotron Emission ◽  
Large Area ◽  
Energy Photon ◽  
Isotropic Energy ◽  
Spectral Analyses ◽  
Gamma Ray Burst ◽  
Γ Ray ◽  
High Energy Emission

The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of these unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest γ-ray duration (20 hours), and one of the largest isotropic energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the nonthermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock.

scholarly journals Gamma-ray burst detection prospects for next generation ground-based VHE facilities

2021 ◽  
Author(s):  
G La Mura ◽  
U Barres de Almeida ◽  
R Conceição ◽  
A De Angelis ◽  
F Longo ◽  
...  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Large Area ◽  
Gamma Ray Burst ◽  
Cherenkov Telescopes ◽  
200 Gev ◽  
Energy Domain ◽  
Very High Energy ◽  
Γ Ray ◽  
Very High

Abstract Gamma-ray Bursts (GRB) were discovered by satellite-based detectors as powerful sources of transient γ-ray emission. The Fermi satellite detected an increasing number of these events with its dedicated Gamma-ray Burst Monitor (GBM), some of which were associated with high energy photons (E &gt; 10 GeV), by the Large Area Telescope (LAT). More recently, follow-up observations by Cherenkov telescopes detected very high energy emission (E &gt; 100 GeV) from GRBs, opening up a new observational window with implications on the interpretation of their central engines and on the propagation of very energetic photons across the Universe. Here, we use the data published in the 2nd Fermi-LAT Gamma Ray Burst Catalogue to characterise the duration, luminosity, redshift and light curve of the high energy GRB emission. We extrapolate these properties to the very high energy domain, comparing the results with available observations and with the potential of future instruments. We use observed and simulated GRB populations to estimate the chances of detection with wide-eld ground-based γ-ray instruments. Our analysis aims to evaluate the opportunities of the Southern Wide-eld-of-view Gamma-ray Observatory (SWGO), to be installed in the Southern Hemisphere, to complement CTA. We show that a low-energy observing threshold (Elow &lt; 200 GeV), with good point source sensitivity (Flim ≈ 10−11erg cm−2 s−1 in 1 yr), are optimal requirements to work as a GRB trigger facility and to probe the burst spectral properties down to time scales as short as 10 s, accessing a time domain that will not be available to IACT instruments.

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