Published in

American Astronomical Society, Astrophysical Journal Letters, 2(850), p. L22, 2017

DOI: 10.3847/2041-8213/aa97d2

arXiv, 2017

DOI: 10.48550/arxiv.1710.05862

Links

Tools

Export citation

Search in Google Scholar

TeV Gamma-Ray Observations of the Binary Neutron Star Merger GW170817 with H.E.S.S.

Journal article published in 2017 by N. Żywucka, D. J. van der Walt, H. Abdalla, P. deWilt, A. Abramowski, R. de los Reyes, F. Aharonian ORCID, M. Arrieta, P. Aubert, F. Ait Benkhali, M. Backes, E. O. Angüner, A. Balzer, :., M. Barnard ORCID and other authors.
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

Full text: Download

Red circle
Preprint: archiving forbidden
Red circle
Postprint: archiving forbidden
Green circle
Published version: archiving allowed
Data provided by SHERPA/RoMEO

Abstract

We search for high-energy gamma-ray emission from the binary neutron star merger GW170817 with the H.E.S.S. Imaging Air Cherenkov Telescopes. The observations presented here have been obtained starting only 5.3h after GW170817. The H.E.S.S. target selection identified regions of high probability to find a counterpart of the gravitational wave event. The first of these regions contained the counterpart SSS17a that has been identified in the optical range several hours after our observations. We can therefore present the first data obtained by a ground-based pointing instrument on this object. A subsequent monitoring campaign with the H.E.S.S. telescopes extended over several days, covering timescales from 0.22 to 5.2 days and energy ranges between $270\,\mathrm{GeV}$ to $8.55\,\mathrm{TeV}$. No significant gamma-ray emission has been found. The derived upper limits on the very-high-energy gamma-ray flux for the first time constrain non-thermal, high-energy emission following the merger of a confirmed binary neutron star system.