The Jet Structure and the Intrinsic Luminosity Function of Short Gamma-Ray Bursts

Tan, Wei-Wei; Yu, Yun-Wei

doi:10.3847/1538-4357/abb404

Cited by 17 publications

(9 citation statements)

References 82 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…90% and 50% credible intervals as functions of L log 10 and compares them to other estimations performed in other works (Ghirlanda et al 2016;Salafia et al 2020;Tan & Yu 2020). It illustrates how the short GRB luminosity function in our model peaks around L ∼ L GRB 170817A , considering this the only short GRB event observed at such a low luminosity.…”

Section: Population Studiessupporting

confidence: 81%

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3b

Abbott

Acernese

et al. 2022

ApJ

View full text Add to dashboard Cite

We search for gravitational-wave signals associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (2019 November 1 15:00 UTC–2020 March 27 17:00 UTC). We conduct two independent searches: a generic gravitational-wave transients search to analyze 86 GRBs and an analysis to target binary mergers with at least one neutron star as short GRB progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these GRBs. A weighted binomial test of the combined results finds no evidence for subthreshold gravitational-wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each GRB. Finally, we constrain the population of low-luminosity short GRBs using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate.

show abstract

Section: Population Studiessupporting

confidence: 81%

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3b

Abbott

Acernese

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…By assuming a single-Gaussian structured jet model (e.g., Zhang & Mészáros 2002), we have shown that GW170817-like events, which can be simultaneously observed as an off-axis sGRB and a clear kilonova, may be scarce. In order to explain the sGRB signal of GW170817/GRB170817A, a two-Gaussian structured jet model may be required (Tan & Yu 2020). Future multi-messenger detection rates of sGRBs, kilonovae and afterglows can be used for constraining the jet structure.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Zhu¹,

Wu²,

Yang³

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

In the second work of this series, we explore the optimal search strategy for serendipitous and gravitational-wave-triggered target-of-opportunity observations of kilonovae and optical short-duration gamma-ray burst (sGRB) afterglows from binary neutron star (BNS) mergers, assuming that cosmological kilonovae are AT2017gfo-like (but with viewing-angle dependence) and that the properties of afterglows are consistent with those of cosmological sGRB afterglows. A one-day cadence serendipitous search strategy with an exposure time of ∼ 30 s can always achieve an optimal search strategy of kilonovae and afterglows for various survey projects. We show that the optimal detection rates of the kilonova-dominated (afterglow-dominated) events are ∼ 0.2/0.5/0.8/20 yr −1 (∼ 500/300/600/3000 yr −1 ) for ZTF/Mephisto/WFST/LSST, respectively. A better search strategy for SiTian is to increase the exposure time. SiTian can find ∼ 5(6000) yr −1 kilonova-dominated (afterglow-dominated) events. We predict abundant off-axis orphan afterglows may be recorded in the survey database although not been identified. For target-of-opportunity observations, we simulate the maximum BNS gravitational-wave (GW) detection rates, which are ∼ 27/210/1800/2.0 × 10 5 yr −1 , in the networks of 2nd/2.5th/3rd(Voyager)/3rd(ET&CE)-generation GW detectors. In the upcoming 2nd-generation networks, follow-up observations with a limiting magnitude of m limit 22 − 23 mag can discover all EM signals from BNS GW events. Among these detected GW events, ∼ 60% events (∼ 16 yr −1 ) can detect clear kilonova signals, while afterglow-dominated events would account for the other ∼ 40% events (∼ 11 yr −1 ). In the 2.5th-and 3rd(Voyager)-generation era, the critical magnitudes for the detection of EM emissions from all BNS GW events would be ∼ 23.5 mag and ∼ 25 mag, respectively. Foreseeable optical survey projects cannot detect all EM signals of GW events detected during the ET&CE era.

show abstract

“…In a statistical view, by denoting the event rate of GRBs and their luminosity function as ṘGRB and Φ(L), the detectable numbers of GRBs in different flux and redshift ranges can be calculated by [93] N…”

Section: Luminosity Functionmentioning

confidence: 99%

“…As usual, without considering the jet structure, the luminosity function is found to have a broken-power-law form. However, when a Gaussian jet structure is invoked, it can be found that a single-power-law luminosity function would become a better choice [93]. This hints that the usual low-energy power law in the luminosity function could be a result of off-axis observations.…”

Section: Luminosity Functionmentioning

confidence: 99%

Gamma-Ray Bursts

Yu¹,

He²,

Wang³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Gamma-ray bursts (GRBs) are short and intense bursts of ∼100 keV−1MeV photons, usually followed by long-lasting decaying afterglow emission in a wide range of electromagnetic wavelengths from radio to Xray and, sometimes, even to GeV gamma-rays. These emissions are believed to originate from a relativistic jet, which is driven due to the collapse of special massive stars and the mergers of compact binaries (i.e., double neutron stars or a neutron star and a black hole). This chapter first briefly introduces the basic observational facts of the GRB phenomena, including the prompt emission, afterglow emission, and host galaxies. Secondly, a general theoretical understanding of the GRB phenomena is described based on a relativistic jet's overall dynamical evolution, including the acceleration, propagation, internal dissipation, and deceleration phases. Here a long-lasting central engine of the GRBs can substantially influence the dynamical evolution of the jet. In addition, a supernova/kilonova emission can appear in the optical afterglow of some nearby GRBs, which can provide an important probe to the

show abstract

The Jet Structure and the Intrinsic Luminosity Function of Short Gamma-Ray Bursts

Cited by 17 publications

References 82 publications

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3b

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3b

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Gamma-Ray Bursts

Contact Info

Product

Resources

About