ABDALLA, H.; AHARONIAN, F.; BENKHALI, F. Ait; ANGÜNER, E.O.; ASHKAR, H.; BACKES, M.; BAGHMANYAN, V.; MARTINS, V. Barbosa; BATZOFIN, R.; BECHERINI, Y.; BERGE, D.; BERNLÖHR, K.; BI, B.; BÖTTCHER, M.; BOISSON, C.; BOLMONT, J.; DE BONY DE LAVERGNE, M.; BROSE, R.; BRUN, F.; BULIK, T.; BYLUND, T.; CANGEMI, F.; CAROFF, S.; CASANOVA, S.; CHAND, T.; CHEN, A.; COTTER, G.; MBARUBUCYEYE, J. Damascene; DEVIN, J.; DJANNATI-ATAÏ, A.; EGBERTS, K.; ERNENWEIN, J.-P.; FEGAN, S.; FIASSON, A.; DE CLAIRFONTAINE, G. Fichet; FONTAINE, G.; FUNK, S.; GABICI, S.; GIAVITTO, G.; GIUNTI, L.; GLAWION, D.; GLICENSTEIN, J.F.; GRONDIN, M.-H.; HINTON, J.A.; HÖRBE, M.; HOFMANN, W.; HOLCH, T.L.; HOLLER, M.; HUANG, Zhiqiu; HUBER, D.; JAMROZY, M.; JANKOWSKY, F.; JUNG-RICHARDT, I.; KASAI, E.; KATARZYŃSKI, K.; KATZ, U.; KHÉLIFI, B.; KOMIN, Nu.; KONNO, R.; KOSACK, K.; KOSTUNIN, D.; KUNDU, A.; LAMANNA, G.; STUM, S. Le; LEMIÈRE, A.; LEMOINE-GOUMARD, M.; LENAIN, J.-P.; LEUSCHNER, F.; LOHSE, T.; LUASHVILI, A.; LYPOVA, I.; MACKEY, J.; MAJUMDAR, J.; MALYSHEV, D.; MARANDON, V.; MARCHEGIANI, P.; MARTÍ-DEVESA, G.; MARX, R.; MAURIN, G.; MEINTJES, P.J.; MITCHELL, A.; MOHRMANN, L.; MONTANARI, A.; MOULIN, E.; MULLER, J.; MURACH, T.; DE NAUROIS, M.; NAYERHODA, A.; NIEMIEC, J.; NOEL, A. Priyana; O'BRIEN, P.; OHM, S.; OLIVERA-NIETO, L.; WILHELMI, E. De Ona; OSTROWSKI, M.; PANTER, M.; PARSONS, R.D.; PERON, G.; POIREAU, V.; PROKHOROV, D.A.; PROKOPH, H.; PÜHLHOFER, G.; PUNCH, M.; QUIRRENBACH, A.; REICHHERZER, P.; RENAUD, M.; RIEGER, F.; ROWELL, G.; RUDAK, B.; RICARTE, H. Rueda; VELASCO, E. Ruiz; SAHAKIAN, V.; SAILER, S.; SALZMANN, H.; SANCHEZ, D.A.; SANTANGELO, A.; SASAKI, M.; SCHÜSSLER, F.; SCHUTTE, H.M.; SCHWANKE, U.; SENNIAPPAN, M.; SHAPOPI, J.N. S.; SINHA, A.; SOL, H.; SPECOVIUS, A.; SPENCER, S.; STAWARZ, L.; STEINMASSL, S.; STEPPA, C.; SUN, L.; TAKAHASHI, T.; TANAKA, T.; TERRIER, R.; THORPE-MORGAN, C.; TSIROU, M.; TSUJI, N.; UCHIYAMA, Y.; VAN ELDIK, C.; VEH, J.; VINK, J.; WAGNER, S.J.; WERNER, F.; WHITE, R.; WIERZCHOLSKA, A.; WONG, Yu Wun; ZACHARIAS, M.; ZARGARYAN, D.; ZDZIARSKI, A.A.; ZECH, A.; ZHU, S.J.; ZOUARI, S.; ZYWUCKA, N.

doi:10.3847/1538-4357/ac2e04

The system will be going down for regular maintenance. Please save your work and logout.

Metadata

Show full item record

License

ABDALLA, H.
University of Namibia [UNAM]

AHARONIAN, F.
Dublin Institute of Technology [DIT]
Max-Planck-Institut für Kernphysik [MPIK]
Russian-Armenian University [RAU]

BENKHALI, F. Ait
Max-Planck-Institut für Kernphysik [MPIK]

Language

Article de revue

This item was published in

Astrophys.J. 2021, vol. 923, n° 1, p. 109

English Abstract

We report on the observations of four well-localized binary black hole (BBH) mergers by the High Energy Stereoscopic System (H.E.S.S.) during the second and third observing runs of Advanced LIGO and Advanced Virgo, O2 and O3. H.E.S.S. can observe 20 deg$^{2}$ of the sky at a time and follows up gravitational-wave (GW) events by “tiling” localization regions to maximize the covered localization probability. During O2 and O3, H.E.S.S. observed large portions of the localization regions, between 35% and 75%, for four BBH mergers (GW170814, GW190512_180714, GW190728_064510, and S200224ca). For these four GW events, we find no significant signal from a pointlike source in any of the observations, and we set upper limits on the very high energy (>100 GeV) γ-ray emission. The 1–10 TeV isotropic luminosity of these GW events is below 10$^{45}$ erg s$^{−1}$ at the times of the H.E.S.S. observations, around the level of the low-luminosity GRB 190829A. Assuming no changes are made to how follow-up observations are conducted, H.E.S.S. can expect to observe over 60 GW events per year in the fourth GW observing run, O4, of which eight would be observable with minimal latency.Read less <

English Keywords

localization

gravitational radiation

LIGO

VIRGO

GeV

gamma ray: VHE

TeV

energy: high

black hole: binary: coalescence

gamma ray: burst

black hole: binary

HESS

Metadata

License

H.E.S.S. follow-up observations of binary black hole coalescence events during the second and third gravitational-wave observing runs of advanced LIGO and advanced Virgo

Language

This item was published in

English Abstract

English Keywords

DOI

Origin

Collections