Viewing Short Gamma-Ray Bursts From a Different Angle

Burgess, J.; Greiner, J.; Bégué, Damien; Giannios, Dimitrios; Berlato, F.; Lipunov, V.

doi:10.3389/fspas.2020.00040

Cited by 6 publications

(10 citation statements)

References 48 publications

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“…We conclude that the overall properties of GRB150101B are naturally accounted for by a structured jet viewed off-axis. This implies that in the nearby (z<0.2) Universe, where off-axis explosions are detectable by current gamma-ray facilities 54 , the true-to-observed ratio of short GRBs is much smaller than the beaming correction factor (∼300) of the uniform jet model 51,55 . Based on our model of a Gaussian jet, we show in Figure 7 some predictions for X-ray searches of GW counterparts.…”

Section: Discussionmentioning

confidence: 99%

A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341

et al. 2018

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The recent discovery of a gamma-ray burst (GRB) coincident with the gravitational-wave (GW) event GW170817 revealed the existence of a population of low-luminosity short duration gamma-ray transients produced by neutron star mergers in the nearby Universe. These events could be routinely detected by existing gamma-ray monitors, yet previous observations failed to identify them without the aid of GW triggers. Here we show that GRB150101B is an analogue of GRB170817A located at a cosmological distance. GRB150101B is a faint short burst characterized by a bright optical counterpart and a long-lived X-ray afterglow. These properties are unusual for standard short GRBs and are instead consistent with an explosion viewed off-axis: the optical light is produced by a luminous kilonova, while the observed X-rays trace the GRB afterglow viewed at an angle of ~13°. Our findings suggest that these properties could be common among future electromagnetic counterparts of GW sources.

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Section: Discussionmentioning

confidence: 99%

A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341

et al. 2018

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“…We identified a group of similar GRBs and suggested that a good fraction of the previously detected faint short GRBs is not at large redshifts, but local, at redshift smaller than 0.1, seen off-axis (Fig. 36, [23]). We incorporated off-axis emission in the estimate of the rates of short GRBs and predicted that the majority of future GW-detections of NS-NS mergers will be accompanied by faint γ-ray emission [23], contrary to previous thinking and still open for an observational test.…”

Section: Glast/fermimentioning

confidence: 71%

“…36, [23]). We incorporated off-axis emission in the estimate of the rates of short GRBs and predicted that the majority of future GW-detections of NS-NS mergers will be accompanied by faint γ-ray emission [23], contrary to previous thinking and still open for an observational test. Overall, this event was a confirmation of MPE's previous successful scientific strategy, as the only two gamma-ray measurements were taken with detectors built under MPE leadership (on INTEGRAL-SPI/ACS and Fermi/GBM), and additionally important kilonova observations could be provided with MPE's GROND imager [144].…”

Section: Glast/fermimentioning

confidence: 99%

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Half-a-century of gamma-ray astrophysics at the Max-Planck Institute for Extraterrestrial Physics

Schönfelder

Greiner

2021

EPJ H

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Gamma-ray astronomy has been one of the prime scientific research fields of the Max-Planck Institute for Extraterrestrial Physics (MPE) from its beginning. Over the years, the entire gamma-ray energy range accessible from space was explored. The purpose of this review article is to summarise the achievements of the gamma-ray group at MPE during the last 50+ years. This covers a substantial part of the general history of space-based gamma-ray astronomy, for which both, general review articles (e.g. Pinkau in Exp Astron 5: 157, 2009; Schönfelder in AN 323: 524, 2002; Trimble in AIP Conf Proc 304: 40, 1994) and a detailed tabular list of events and missions (Leonard and Gehrels in https://heasarc.gsfc.nasa.gov/docs/history, version 1.0.8, 2009), have been compiled. Here, we describe the gamma-ray activities at MPE from the beginning till the present, reviewing the tight interplay between new technological developments towards new instruments and scientific progress in understanding gamma-ray sources in the sky. This covers (i) the early development of instruments and their tests on half a dozen balloon flights, (ii) the involvement in the most important space missions at the time, i.e. ESA’s COS-B satellite, NASA’s Compton Gamma-ray Observatory and Fermi Space Telescope, as well as ESA’s INTEGRAL observatory, (iii) the participation in several other missions such as TD-1, Solar Maximum Mission, or Ulysses, and (iv) the complementary ground-based optical instruments OPTIMA and GROND to enhance selected science topics (pulsars, gamma-ray bursts). With the gradual running-out of institutional support since 2010, gamma-ray astrophysics as a main research field has now come to an end at MPE.

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“…The distribution also hints that a small fraction of Fermi bursts may contain nearby events viewed at large angles. There have been claims of such local events from archival Fermi and Swift data (Burgess et al 2017;Troja et al 2018;von Kienlin et al 2019).…”

Section: Detected Populationmentioning

confidence: 99%

Detectability of Electromagnetic counterparts from Neutron Star mergers: prompt emission vs afterglow

Mohan,

Saleem,

Resmi

2019

Preprint

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Electromagnetic observations of the first binary Neutron Star (BNS) merger GW170817 has established that relativistic jets can be successfully launched in BNS mergers. Typically, such jets produce emission in two phases: γ-ray prompt emission and multi-wavelength afterglow. Due to relativistic de-boosting, the detectability of both these counterparts are dependent on the angle (θ v ) between the observer's line of sight and the jet axis. We compare the detectability of prompt and afterglow emission from off-axis jets, assuming standard detector thresholds. We find that for top-hat jets, afterglow is a more potential counterpart than the prompt emission even with unfavourable afterglow parameters. For structured jets with a Gaussian profile, prompt emission is more promising than the afterglows at extreme viewing angles, under the assumption that the energy emitted in the prompt phase equals the kinetic energy of the outflow. Assuming a Gaussian jet profile, we forecast the population of γ-ray detections and find that extreme viewing angle events like GRB170817A will be rare. In our simulated sample, the observed isotropic equivalent energy in γ-rays is moderately correlated with the viewing angle, such that a low E iso,γ is almost always associated with a high off-axis viewing angle.

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Viewing Short Gamma-Ray Bursts From a Different Angle

Cited by 6 publications

References 48 publications

A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341

A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341

Half-a-century of gamma-ray astrophysics at the Max-Planck Institute for Extraterrestrial Physics

Detectability of Electromagnetic counterparts from Neutron Star mergers: prompt emission vs afterglow

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