Short GRB 160821B: a reverse shock, a refreshed shock, and a well-sampled 
kilonova

Lamb, G. P.; Tanvir, N. R.; Levan, A. J.; Postigo, A. de Ugarte; Kawaguchi, Kyohei; Corsi, A.; Evans, P. A.; Malesani, D. B.; Page, K. L.; Wiersema, K.; Fruchter, A. S.; Gompertz, B.; Rosswog, S.; Shibata, M.; Tanaka, M.; van der Horst, A. J.; Cano, Z.; Fynbo, J. P. U.; Greiner, J.; Heintz, K.; Higgins, A.; Hjorth, J.; Izzo, L.; Jakobsson, P.; Kann, D. A.; O'Brien, P. T.; Perley, D. A.; Pian, E.; Pugliese, G.; Starling, R. L. C.; Thöne, C. C.; Watson, D.; Wijers, R. A. M. J.; Xu, D.

doi:10.3847/1538-4357/ab38bb

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Short GRB 160821B: a reverse shock, a refreshed shock, and a well-sampled kilonova

MPS-Authors

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Kawaguchi, Kyohei
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Shibata, M.
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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引用

Lamb, G. P., Tanvir, N. R., Levan, A. J., Postigo, A. d. U., Kawaguchi, K., Corsi, A., Evans, P. A., Malesani, D. B., Page, K. L., Wiersema, K., Fruchter, A. S., Gompertz, B., Rosswog, S., Shibata, M., Tanaka, M., van der Horst, A. J., Cano, Z., Fynbo, J. P. U., Greiner, J., Heintz, K., Higgins, A., Hjorth, J., Izzo, L., Jakobsson, P., Kann, D. A., O'Brien, P. T., Perley, D. A., Pian, E., Pugliese, G., Starling, R. L. C., Thöne, C. C., Watson, D., Wijers, R. A. M. J., & Xu, D. (2019). Short GRB 160821B: a reverse shock, a refreshed shock, and a well-sampled kilonova. The Astrophysical Journal, 883(1):. doi:10.3847/1538-4357/ab38bb.

引用: https://hdl.handle.net/21.11116/0000-0004-4504-A

要旨

We report our identification of the optical afterglow and host galaxy of the
short-duration gamma-ray burst sGRB 160821Bb. The spectroscopic redshift of the
host is $z=0.162$, making it one of the lowest redshift sGRBs identified by
Swift. Our intensive follow-up campaign using a range of ground-based
facilities as well as HST, XMM and Swift, shows evidence for a late-time excess
of optical and near-infrared emission in addition to a complex afterglow. The
afterglow light-curve at X-ray frequencies reveals a narrow jet,
$\theta_j\sim1.9$ deg, that is refreshed at $>1$ day post-burst by a slower
outflow with significantly more energy than the initial outflow that produced
the main GRB. Observations of the 5 GHz radio afterglow shows a reverse shock
into a mildly magnetised shell. The optical and near-infrared excess is fainter
than AT2017gfo associated with GW170817, and is well explained by a kilonova
with dynamic ejecta mass $M_{\rm dyn}=(2.0\pm1.2)\times10^{-3}$\,M$_{\odot}$
and a secular ejecta mass with $M_{\rm pm}=
1.0\pm0.6)\times10^{-2}$\,M$_\odot$, consistent with a binary neutron star
merger resulting in a short-lived massive neutron star. This optical and
near-infrared dataset provides the best-sampled kilonova light-curve without a
gravitational wave trigger to date.