ABDALLA, H.; ADAM, R.; AHARONIAN, F.; AIT BENKHALI, F.; ANGÜNER, E. O.; ARAKAWA, M.; ARCARO, C.; ARMAND, C.; ARMSTRONG, T.; ASHKAR, H.; BACKES, M.; BAGHMANYAN, V.; BARBOSA-MARTINS, V.; BARNACKA, A.; BARNARD, M.; BECHERINI, Y.; BERGE, D.; BERNLÖHR, K.; BLACKWELL, R.; BÖTTCHER, M.; BOISSON, C.; BOLMONT, J.; BONNEFOY, S.; BREGEON, J.; BREUHAUS, M.; BRUN, F.; BRUN, P.; BRYAN, M.; BÜCHELE, M.; BULIK, T.; BYLUND, T.; CAROFF, S.; CAROSI, A.; CASANOVA, S.; CERRUTI, M.; CHAND, T.; CHANDRA, S.; CHEN, A.; COTTER, G.; CURYŁO, M.; DAVIDS, I. D.; DAVIES, J.; DEIL, C.; DEVIN, J.; DEWILT, P.; DIRSON, L.; DJANNATI-ATAÏ, A.; DMYTRIIEV, A.; DONATH, A.; DOROSHENKO, V.; DYKS, J.; EGBERTS, K.; EICHHORN, F.; EMERY, G.; ERNENWEIN, J. -P.; ESCHBACH, S.; FEIJEN, K.; FEGAN, S.; FIASSON, A.; FONTAINE, G.; FUNK, S.; FÜSSLING, M.; GABICI, S.; GALLANT, Y. A.; GIAVITTO, G.; GIUNTI, L.; GLAWION, D.; GLICENSTEIN, J. F.; GOTTSCHALL, D.; GRONDIN, M. -H.; HAHN, J.; HAUPT, M.; HEINZELMANN, G.; HERMANN, G.; HINTON, J. A.; HOFMANN, W.; HOISCHEN, C.; HOLCH, T. L.; HOLLER, M.; HÖRBE, M.; HORNS, D.; HUBER, D.; IWASAKI, H.; JAMROZY, M.; JANKOWSKY, D.; JANKOWSKY, F.; JARDIN-BLICQ, A.; JOSHI, V.; JUNG-RICHARDT, I.; KASTENDIECK, M. A.; KATARZYŃSKI, K.; KATSURAGAWA, M.; KATZ, U.; KHANGULYAN, D.; KHÉLIFI, B.; KLEPSER, S.; KLUŹNIAK, W.; KOMIN, Nu.; KONNO, R.; KOSACK, K.; KOSTUNIN, D.; KRETER, M.; LAMANNA, G.; LEMIÈRE, A.; LEMOINE-GOUMARD, M.; LENAIN, J.-P.; LESER, E.; LEVY, C.; LOHSE, T.; LYPOVA, I.; MACKEY, J.; MAJUMDAR, J.; MALYSHEV, D.; MALYSHEV, D.; MARANDON, V.; MARCHEGIANI, P.; MARCOWITH, A.; MARES, A.; MARTÍ-DEVESA, G.; MARX, R.; MAURIN, G.; MEINTJES, P. J.; MODERSKI, R.; MOHAMED, M.; MOHRMANN, L.; MOORE, C.; MORRIS, P.; MOULIN, E.; MULLER, J.; MURACH, T.; NAKASHIMA, S.; NAKASHIMA, K.; DE NAUROIS, M.; NDIYAVALA, H.; NIEDERWANGER, F.; NIEMIEC, J.; OAKES, L.; O'BRIEN, P.; ODAKA, H.; OHM, S.; DE ONA WILHELMI, E.; OSTROWSKI, M.; PANTER, M.; PARSONS, R. D.; PEYAUD, B.; PIEL, Q.; PITA, S.; POIREAU, V.; NOEL, A. Priyana; PROKHOROV, D. A.; PROKOPH, H.; PÜHLHOFER, G.; PUNCH, M.; QUIRRENBACH, A.; RAAB, S.; RAUTH, R.; REIMER, A.; REIMER, O.; REMY, Q.; RENAUD, M.; RIEGER, F.; RINCHIUSO, L.; ROMOLI, C.; ROWELL, G.; RUDAK, B.; RUIZ-VELASCO, E.; SAHAKIAN, V.; SAILER, S.; SAITO, S.; SANCHEZ, D. A.; SANTANGELO, A.; SASAKI, M.; SCALICI, M.; SCHLICKEISER, R.; SCHÜSSLER, F.; SCHULZ, A.; SCHUTTE, H. M.; SCHWANKE, U.; SCHWEMMER, S.; SEGLAR-ARROYO, M.; SENNIAPPAN, M.; SEYFFERT, A. S.; SHAFI, N.; SHININGAYAMWE, K.; SIMONI, R.; SINHA, A.; SOL, H.; SPECOVIUS, A.; SPENCER, S.; SPIR-JACOB, M.; STAWARZ, Ł.; STEENKAMP, R.; STEGMANN, C.; STEPPA, C.; TAKAHASHI, T.; TAVERNIER, T.; TAYLOR, A. M.; TERRIER, R.; TIZIANI, D.; TLUCZYKONT, M.; TOMANKOVA, L.; TRICHARD, C.; TSIROU, M.; TSUJI, N.; TUFFS, R.; UCHIYAMA, Y.; VAN DER WALT, D. J.; VAN ELDIK, C.; VAN RENSBURG, C.; VAN SOELEN, B.; VASILEIADIS, G.; VEH, J.; VENTER, C.; VINCENT, P.; VINK, J.; VÖLK, H. J.; VUILLAUME, T.; WADIASINGH, Z.; WAGNER, S. J.; WATSON, J.; WERNER, F.; WHITE, R.; WIERZCHOLSKA, A.; YANG, R.; YONEDA, H.; ZACHARIAS, M.; ZANIN, R.; ZDZIARSKI, A. A.; ZECH, A.; ZORN, J.; ŻYWUCKA, N.; RODRIGUES, X.

doi:10.3847/2041-8213/ab8b59

Métadonnées

Afficher la notice complète

Licence d’utilisation du document

ABDALLA, H.

ADAM, R.
Laboratoire Leprince-Ringuet [LLR]

AHARONIAN, F.

Langue

Article de revue

Ce document a été publié dans

The Astrophysical journal letters. 2020, vol. 894, n° 2, p. L16

Bristol : IOP Publishing

Résumé en anglais

The detection of the first electromagnetic counterpart to the binary neutron star (BNS) merger remnant GW170817 established the connection between short $\gamma$-ray bursts and BNS mergers. It also confirmed the forging of heavy elements in the ejecta (a so-called $kilonova$) via the $r-process\ nucleosynthesis$. The appearance of nonthermal radio and X-ray emission, as well as the brightening, which lasted more than 100 days, were somewhat unexpected. Current theoretical models attempt to explain this temporal behavior as either originating from a relativistic off-axis jet or a kilonova-like outflow. In either scenario, there is some ambiguity regarding how much energy is transported in the nonthermal electrons versus the magnetic field of the emission region. Combining the Very Large Array (radio) and Chandra (X-ray) measurements with observations in the GeV-TeV domain can help break this ambiguity, almost independently of the assumed origin of the emission. Here we report for the first time on deep H.E.S.S. observations of GW170817/GRB 170817A between 124 and 272 days after the BNS merger with the full H.E.S.S. array of telescopes, as well as on an updated analysis of the prompt (<5 days) observations with the upgraded H.E.S.S. phase-I telescopes. We discuss implications of the H.E.S.S. measurement for the magnetic field in the context of different source scenarios.< Réduire

Mots clés en anglais

Gamma-ray transient sources

Stellar mergers

Gamma-ray bursts

Gamma-ray astronomy

Ejecta

1853

2157

629

628

453

High Energy Astrophysical Phenomena

Métadonnées

Partager cette publication !

Licence d’utilisation du document

Probing the magnetic field in the GW170817 outflow using H.E.S.S. observations

Langue

Ce document a été publié dans

Résumé en anglais

Mots clés en anglais

URI

DOI

Origine

Unités de recherche