Physical Implications of the Subthreshold GRB GBM-190816 and Its Associated Subthreshold Gravitational-wave Event

Yang, Yu-Han; Zhong, Shuangling; Zhang, Bin-Bin; Wu, Shichao; Yang, Yuhan; Cao, Zhoujian; Wang, Jie-Shuang; Lü, Hou-Jun; Cang, Jirong; Dai, Z. G.

doi:10.3847/1538-4357/ab9ff5

Cited by 15 publications

(10 citation statements)

References 65 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Goldstein et al (2019a) reported a sub-threshold GRB candidate,GBM-190816, which was potentially associated with a sub-threshold LVC compact binary coalescence candidate Yang et al (2020). investigated the physical implications of this potential association and indicated this GW candidate could be a NSBH merger with the mass ratio Q = 2.26+2.75 −1.43 .…”

mentioning

confidence: 99%

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Zhu

Yang

et al. 2021

ApJ

Self Cite

View full text Add to dashboard Cite

We analyse the tidal disruption probability of potential neutron star-black hole (NSBH) merger gravitational wave (GW) events, including GW190426 152155, GW190814, GW200105 162426 and GW200115 042309, detected during the third observing run of the LIGO/Virgo Collaboration, and the detectability of kilonova emission in connection with these events. The posterior distributions of GW190814 and GW200105 162426 show that they must be plunging events and hence no kilonova signal is expected from these events. With the stiffest NS equation of state allowed by the constraint of GW170817 taken into account, the probability that GW190426 152155 and GW200115 042309 can make tidal disruption is ∼ 24% and ∼ 3%, respectively. However, the predicted kilonova brightness is too faint to be detected for present follow-up search campaigns, which explains the lack of electromagnetic (EM) counterpart detection after triggers of these GW events. Based on the best constrained population synthesis simulation results, we find that disrupted events account for only 20% of cosmological NSBH mergers since most of the primary BHs could have low spins. The associated kilonovae for those disrupted events are still difficult to be discovered by LSST after GW triggers in the future, because of their low brightness and larger distances. For future GW-triggered multi-messenger observations, potential short-duration gamma-ray bursts and afterglows are more probable EM counterparts of NSBH GW events.

show abstract

mentioning

confidence: 99%

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Zhu

Yang

et al. 2021

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Some controversial GW-associated electromagnetic (EM) counterparts have been reported, e.g. a sub-threshold GRB candidate GBM 190816 occurring at 1.57 s after a sub-threshold GW event candidate(Goldstein et al 2019;Yang et al 2020), and a plausible EM flare associated with a candidate binary black hole (BBH) merger S190521g(Graham et al 2020). …”

mentioning

confidence: 99%

Kilonova Emission From Black Hole-Neutron Star Mergers. II. Luminosity Function and Implications for Target-of-opportunity Observations of Gravitational-wave Triggers and Blind Searches

Zhu,

Wu,

Yang

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

We present detailed simulations of kilonova and GRB afterglow emission originating from black holeneutron star (BH-NS) mergers. We present kilonova luminosity function and discuss the detectability of kilonova and GRB afterglow in connection with gravitational wave (GW) detections, GW-triggered target-of-opportunity follow-up observations, and blind searches in time-domain survey observations. The predicted absolute magnitude of the radioactive-powered BH-NS merger kilonovae at 0.5 day after the merger falls in the range of [−10, −15.5]. The simulated luminosity function contains the potential viewing angle distribution information of the anisotropic kilonova emission. We simulate the GW detection rates, detectable distances and signal duration, for the future networks of 2nd, 2.5th, and 3rd generation GW detectors. BH-NS mergers tend to produce brighter kilonovae and afterglows if the primary BH has a high aligned-spin, and the NS companion is less-massive with a stiff equation of state. The detectability of kilonova emission is especially sensitive to the spin of the primary BH. If primary BHs typically have a low spin, the electromagnetic (EM) counterpart of BH-NS mergers are hard to discover. For the 2nd generation GW detector networks, a limiting magnitude of m limit ∼ 23 − 24 mag is required to detect the kilonovae from triggered BH-NS mergers even if BH high spin is assumed. This could provide a plausible explanation for the lack of kilonova detection from BH-NS candidates during LIGO/Virgo O3 (early 2nd generation detectors): either there is no EM counterpart (plunging events), or the current follow-up observations are too shallow to make a detection. On the other hand, these observations may still have the chance to detect the on-axis jet afterglow associated with a shortduration gamma-ray burst or an orphan afterglow, if the line of sight is not too far away from the jet axis (presumably the axis of binary merger). In future GW detection eras, more remote GW signals can be detected, but their associated kilonovae are more difficult to detect. Follow up observations can in any case detect possible associated sGRB afterglows, from which kilonova signatures may be studied. For time-domain blind survey observations, a high-cadence search in redder filters is recommended to detect more BH-NS merger kilonovae and afterglows in the current and future GW detection eras.

show abstract

“…Following Yang et al (2020b) and Yang et al (2020a), we calculate the burst duration, T 90 , in 8 keV -800 keV energy band using the continuous time-tagged event (CTTE) data of the Fermi/GBM detector n0. The results are shown in Figure 2.…”

Section: Light Curvesmentioning

confidence: 99%

GRB 210121A: A Typical Fireball Burst Detected by Two Small Missions

Wang,

Zheng,

Xiao

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

The Chinese CubeSat Mission, Gamma Ray Integrated Detectors (GRID), recently detected its first gamma-ray burst, GRB 210121A, which was jointly observed by the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM). This burst is confirmed by several other missions, including Fermi and Insight-HXMT. We combined multi-mission observational data and performed a comprehensive analysis of the burst's temporal and spectral properties. Our results show that the burst is special in its high peak energy, thermal-like low energy indices, and large fluence. By putting it to the E p -E γ,iso relation diagram with assumed distance, we found this burst can be constrained at the redshift range of [0.3,3.0]. The thermal spectral component is also confirmed by the direct fit of the physical models to the observed spectra. Interestingly, the physical photosphere model also constrained a redshift of z ∼ 0.3 for this burst, which help us to identify a host galaxy candidate at such a distance within the location error box. Assuming the host galaxy is real, we found the burst can be best explained by the photosphere emission of a typical fireball with an initial radius of r 0 ∼ 6.7 × 10 7 cm.

show abstract

Physical Implications of the Subthreshold GRB GBM-190816 and Its Associated Subthreshold Gravitational-wave Event

Cited by 15 publications

References 65 publications

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Kilonova Emission From Black Hole-Neutron Star Mergers. II. Luminosity Function and Implications for Target-of-opportunity Observations of Gravitational-wave Triggers and Blind Searches

GRB 210121A: A Typical Fireball Burst Detected by Two Small Missions

Contact Info

Product

Resources

About