A kilonova following a long-duration gamma-ray burst at 350 Mpc

Rastinejad, J.; Gompertz, B.; Levan, A. J.; Fong, W.; Nicholl, Matt; Lamb, Gavin P.; Malesani, D.; Nugent, Anya E.; Oates, S. R.; Tanvir, N. R.; Postigo, A. de Ugarte; Kilpatrick, C. D.; Moore, C. J.; Metzger, Brian D.; Ravasio, M. E.; Rossi, A.; Schroeder, G.; Jencson, J.; Sand, David J.; Smith, Nathan; Fernández, J. F. Agüı́; Berger, E.; Blanchard, P. K.; Chornock, R.; Kung, Bethany Cobb; Pasquale, M. de; Fynbo, J. P. U.; Izzo, L.; Канн, Д. А.; Laskar, T.; Marini, E.; Paterson, K.; Escorial, A. Rouco; Sears, Huei; Thöne, C. C.

doi:10.1038/s41586-022-05390-w

Cited by 128 publications

(140 citation statements)

References 154 publications

(81 reference statements)

Supporting

Mentioning

126

Contrasting

Order By: Relevance

“…The light curve of prompt emission is composed of an initial hard-main emission (with a duration ∼13 s) followed by a series of soft gamma-ray extended emission with a duration ∼55 s, and the structure of the light curve is similar to the particularly interesting case GRB 060614 (Xiao & Zhang 2022;Yang & Zhang 2022) and GRB 211227A (Lü et al 2022). More interestingly, no associated supernova signature is detected for GRB 211211A, even down to very stringent limits at such a low redshift, but associated with kilonova is observed by several optical telescopes (Rastinejad et al 2022). That observed evidence suggests that GRB 211211A originated from a binary compact star merger (Gompertz et al 2022;Rastinejad et al 2022;Xiao & Zhang 2022;Yang & Zhang 2022).…”

Section: Introductionmentioning

confidence: 56%

“…More interestingly, no associated supernova signature is detected for GRB 211211A, even down to very stringent limits at such a low redshift, but associated with kilonova is observed by several optical telescopes (Rastinejad et al 2022). That observed evidence suggests that GRB 211211A originated from a binary compact star merger (Gompertz et al 2022;Rastinejad et al 2022;Xiao & Zhang 2022;Yang & Zhang 2022). However, how to produce such long-duration emission within the compact star merger scenario remains an open question.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Thermal and Nonthermal Emission from a Peculiar Long-duration GRB 211211A

Xue-Zhao

Lü

Yang

et al. 2023

ApJ

View full text Add to dashboard Cite

Long-duration GRB 211211A that lacks a supernova emission even down to very stringent limits at such a low redshift z = 0.076 and is associated with kilonova emission, suggests that its physical origin is from a binary compact star merger. By reanalyzing its data observed with the Gamma-Ray Burst Monitor on board the Fermi mission, we find that both time-integrated and time-resolved spectra can be fitted well by using a 2SBPL plus blackbody (2SBPL+BB) model in the prompt emission. The bulk Lorentz factors (Γph) of the outflow can be inferred by invoking the observed thermal emission at the photosphere radius within a pure fireball model, and we find out that the temporal evolution of Γph seems to be tracking with the light curve. The derived values of Γph are also consistent with the Γph–L γ,iso/E γ,iso correlations that had been found in other bursts. Moreover, we also calculate the magnetization factor σ 0 in the central engine and σ ph at the photosphere radius within the framework of a hybrid jet model, and find that the values of both 1 + σ 0 and 1 + σ ph are larger than 1 for different time slices. It suggests that at least the Poynting-flux component is indeed existent in the outflow. If this is the case, one possible physical interpretation of thermal and nonthermal emissions in GRB 211211A is from the contributions of both ν ν ¯ annihilation and the Blandford–Znajek mechanisms in the relativistic jet when a stellar mass black hole resides in the central engine.

show abstract

Section: Introductionmentioning

confidence: 56%

Section: Introductionmentioning

confidence: 99%

Thermal and Nonthermal Emission from a Peculiar Long-duration GRB 211211A

Xue-Zhao

Lü

Yang

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…To date, except for AT2017gfo, other kilonova candidates were all detected in superposition with decaying sGRB afterglows (e.g., Berger et al 2013;Fan et al 2013;Tanvir et al 2013;Gao et al 2015Gao et al , 2017Jin et al 2015Jin et al , 2016Jin et al , 2020Yang et al 2015;Gompertz et al 2018;Ascenzi et al 2019;Rossi et al 2020;Fong et al 2021;Ma et al 2021;Wu et al 2021;Yuan et al 2021). Interestingly, a bright kilonova candidate was recently found to be associated with a longduration GRB 211211A (e.g., Rastinejad et al 2022;Troja et al 2022;Yang et al 2022b;Zhu et al 2022a). One possible reason why almost all kilonova candidates were detected in GRB afterglows is that most BNS and NSBH mergers are far away from us.…”

Section: Introductionmentioning

confidence: 99%

Kilonovae and Optical Afterglows from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational Wave Triggers

Zhu

Yang

et al. 2023

ApJ

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 (ToO) 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 kilonovae (afterglows) are ∼0.3/0.6/1/20 yr−1 (∼50/60/100/800 yr−1) for Zwicky the Transient Facility (ZTF)/Multi-channel Photometric Survey Telescope (Mephisto)/Wide Field Survey Telescope (WFST)/Large Synoptic Survey Telescope (LSST), respectively. A better search strategy for SiTian than the current design is to increase the exposure time. In principle, a fully built SiTian can detect ∼7(2000) yr−1 kilonovae (afterglows). Population properties of electromagnetic (EM) signals detected by serendipitous observations are studied in detail. For ToO observations, we predict that one can detect ∼11 yr−1 BNS gravitational wave (GW) events during the fourth observing run (O4) by considering an exact duty cycle of the third observing run. The median GW sky localization area is expected to be ∼10 deg2 for detectable BNS GW events. For O4, we predict that ZTF/Mephisto/WFST/LSST can detect ∼5/4/3/3 kilonovae (∼1/1/1/1 afterglows) per year, respectively. The GW detection rates, GW population properties, GW sky localizations, and optimistic ToO detection rates of detectable EM counterparts for BNS GW events at the Advanced Plus, LIGO Voyager, and ET&CE eras are detailedly simulated in this paper.

show abstract

“…The recent discoveries of short GRBs (GRB 200826A, GRB 211227A) from the collapse of massive stars (Ahumada et al 2021;Lü et al 2022) and a long GRB (GRB 211211A) from binary mergers (Rastinejad et al 2022) challenge our understanding about the progenitor systems of GRBs. In this section, we examine the possible progenitors of GRB 201015A and GRB 201216C.…”

Section: Progenitors Of Grb 201015a and Grb 201216cmentioning

confidence: 99%

“…On the other hand, SGRBs are believed to originate from the merging of compact binaries like two neutron stars or a neutron star and a black hole (Perna & Belczynski 2002;Abbott et al 2017). However, recent discoveries of a few GRBs exhibiting hybrid properties from the collapse of massive stars (Ahumada et al 2021) as well as from binary mergers (Rastinejad et al 2022;Troja et al 2022) challenge current understanding and provide valuable clues about the physical nature of progenitors of GRBs.…”

Section: Introductionmentioning

confidence: 99%

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror

Gupta

Jelínek

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

We present a detailed prompt emission and early optical afterglow analysis of the two very-high-energy (VHE) detected bursts GRB 201015A and GRB 201216C, and their comparison with a subset of similar bursts. Time-resolved spectral analysis of multistructured GRB 201216C using the Bayesian binning algorithm revealed that during the entire duration of the burst, the low-energy spectral index (α pt) remained below the limit of the synchrotron line of death. However, statistically some of the bins supported the additional thermal component. Additionally, the evolution of spectral parameters showed that both the peak energy (E p) and α pt tracked the flux. These results were further strengthened using the values of the physical parameters obtained by synchrotron modeling of the data. Our earliest optical observations of both bursts using the F/Photometric Robotic Atmospheric Monitor Observatorio del Roque de los Muchachos and Burst Observer and Optical Transient Exploring System robotic telescopes displayed a smooth bump in their early optical light curves, consistent with the onset of the afterglow due to synchrotron emission from an external forward shock. Using the observed optical peak, we constrained the initial bulk Lorentz factors of GRB 201015A and GRB 201216C to Γ0 = 204 and Γ0 = 310, respectively. The present early optical observations are the earliest known observations constraining outflow parameters and our analysis indicate that VHE detected bursts could have a diverse range of observed luminosity within the detectable redshift range of present VHE facilities.

show abstract

A kilonova following a long-duration gamma-ray burst at 350 Mpc

Cited by 128 publications

References 154 publications

Thermal and Nonthermal Emission from a Peculiar Long-duration GRB 211211A

Thermal and Nonthermal Emission from a Peculiar Long-duration GRB 211211A

Kilonovae and Optical Afterglows from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational Wave Triggers

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Contact Info

Product

Resources

About