ABDALLA, H.; AHARONIAN, F.; AIT BENKHALI, F.; ANGÜNER, E.O.; ARAKAWA, M.; ARCARO, C.; ARMAND, C.; BACKES, M.; BARNARD, M.; BECHERINI, Y.; BECKER TJUS, J.; BERGE, D.; BERNLÖHR, K.; BLACKWELL, R.; BÖTTCHER, M.; BOISSON, C.; BOLMONT, J.; BONNEFOY, S.; BORDAS, P.; BREGEON, J.; BRUN, F.; BRUN, P.; BRYAN, M.; BÜCHELE, M.; BULIK, T.; BYLUND, T.; CAPASSO, M.; CAROFF, S.; CAROSI, A.; CASANOVA, S.; CERRUTI, M.; CHAKRABORTY, N.; CHAND, T.; CHANDRA, S.; CHAVES, R.C.G.; CHEN, A.; COLAFRANCESCO, S.; CONDON, B.; DAVIDS, I.D.; DEIL, C.; DEVIN, J.; DEWILT, P.; DIRSON, L.; DJANNATI-ATAÏ, A.; DMYTRIIEV, A.; DONATH, A.; DOROSHENKO, V.; DRURY, L.O'C.; DYKS, J.; EGBERTS, K.; EMERY, G.; ERNENWEIN, J.P.; ESCHBACH, S.; FEGAN, S.; FIASSON, A.; FONTAINE, G.; FUNK, S.; FÜSSLING, M.; GABICI, S.; GALLANT, Y.A.; GATÉ, F.; GIAVITTO, G.; GLAWION, D.; GLICENSTEIN, J.F.; GOTTSCHALL, D.; GRONDIN, M.H.; HAHN, J.; HAUPT, M.; HEINZELMANN, G.; HENRI, G.; HERMANN, G.; HINTON, J.A.; HOFMANN, W.; HOISCHEN, C.; HOLCH, T.L.; HOLLER, M.; HORNS, D.; HUBER, D.; IWASAKI, H.; JACHOLKOWSKA, A.; JAMROZY, M.; JANKOWSKY, D.; JANKOWSKY, F.; JOUVIN, L.; JUNG-RICHARDT, I.; KASTENDIECK, M.A.; KATARZYŃSKI, K.; KATSURAGAWA, M.; KATZ, U.; KHANGULYAN, D.; KHÉLIFI, B.; KING, J.; KLEPSER, S.; KLUŹNIAK, W.; KOMIN, Nu.; KOSACK, K.; KRAUS, M.; LAMANNA, G.; LAU, J.; LEFAUCHEUR, J.; LEMIÈRE, A.; LEMOINE-GOUMARD, M.; LENAIN, J.P.; LESER, E.; LOHSE, T.; LÓPEZ-COTO, R.; LYPOVA, I.; MALYSHEV, D.; MARANDON, V.; MARCOWITH, A.; MARIAUD, C.; MARTÍ-DEVESA, G.; MARX, R.; MAURIN, G.; MEINTJES, P.J.; MITCHELL, A.M.W.; MODERSKI, R.; MOHAMED, M.; MOHRMANN, L.; MOORE, C.; MOULIN, E.; MURACH, T.; NAKASHIMA, S.; DE NAUROIS, M.; NDIYAVALA, H.; NIEDERWANGER, F.; NIEMIEC, J.; OAKES, L.; O'BRIEN, P.; ODAKA, H.; OHM, S.; OSTROWSKI, M.; OYA, I.; PANTER, M.; PARSONS, R.D.; PERENNES, C.; PETRUCCI, P.O.; PEYAUD, B.; PIEL, Q.; PITA, S.; POIREAU, V.; PRIYANA NOEL, A.; PROKHOROV, D.A.; PROKOPH, H.; PÜHLHOFER, G.; PUNCH, M.; QUIRRENBACH, A.; RAAB, S.; RAUTH, R.; REIMER, A.; REIMER, O.; RENAUD, M.; RIEGER, F.; RINCHIUSO, L.; ROMOLI, C.; ROWELL, G.; RUDAK, B.; RUIZ-VELASCO, E.; SAHAKIAN, V.; SAITO, S.; SANCHEZ, D.A.; SANTANGELO, A.; SASAKI, M.; SCHLICKEISER, R.; SCHÜSSLER, F.; SCHULZ, A.; SCHUTTE, H.; SCHWANKE, U.; SCHWEMMER, S.; SEGLAR-ARROYO, M.; SENNIAPPAN, M.; SEYFFERT, A.S.; SHAFI, N.; SHILON, I.; SHININGAYAMWE, K.; SIMONI, R.; SINHA, A.; SOL, H.; SPECOVIUS, A.; SPIR-JACOB, M.; STAWARZ, L.; STEENKAMP, R.; STEGMANN, C.; STEPPA, C.; TAKAHASHI, T.; TAVERNET, J.P.; TAVERNIER, T.; TAYLOR, A.M.; TERRIER, R.; TIZIANI, D.; TLUCZYKONT, M.; 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.; VOISIN, F.; VÖLK, H.J.; VUILLAUME, T.; WADIASINGH, Z.; WAGNER, S.J.; WAGNER, R.M.; WHITE, R.; WIERZCHOLSKA, A.; YANG, R.; YONEDA, H.; ZABOROV, D.; ZACHARIAS, M.; ZANIN, R.; ZDZIARSKI, A.A.; ZECH, A.; ZIEGLER, A.; ZORN, J.; ŻYWUCKA, N.

doi:10.1038/s41550-019-0910-0

Métadonnées

Afficher la notice complète

Licence d’utilisation du document

Langue

Article de revue

Ce document a été publié dans

Nature Astron.. 2020, vol. 4, n° 2, p. 167-173

Résumé en anglais

The Crab nebula is one of the most-studied cosmic particle accelerators, shining brightly across the entire electromagnetic spectrum up to very-high-energy gamma rays1,2. It is known from observations in the radio to gamma-ray part of the spectrum that the nebula is powered by a pulsar, which converts most of its rotational energy losses into a highly relativistic outflow. This outflow powers a pulsar wind nebula, a region of up to ten light-years across, filled with relativistic electrons and positrons. These particles emit synchrotron photons in the ambient magnetic field and produce very-high-energy gamma rays by Compton up-scattering of ambient low-energy photons. Although the synchrotron morphology of the nebula is well established, it has not been known from which region the very-high-energy gamma rays are emitted3,4,5,6,7,8. Here we report that the Crab nebula has an angular extension at gamma-ray energies of 52 arcseconds (assuming a Gaussian source width), much larger than at X-ray energies. This result closes a gap in the multi-wavelength coverage of the nebula, revealing the emission region of the highest-energy gamma rays. These gamma rays enable us to probe a previously inaccessible electron and positron energy range. We find that simulations of the electromagnetic emission reproduce our measurement, providing a non-trivial test of our understanding of particle acceleration in the Crab nebula.< Réduire

Mots clés en anglais

gamma ray: VHE

gamma ray: energy

positron: energy

particle: acceleration

electron: relativistic

radio wave

energy loss: rotation

pulsar

electromagnetic

synchrotron

photon

magnetic field

accelerator

X-ray

gap

Métadonnées

Licence d’utilisation du document

Resolving the Crab pulsar wind nebula at teraelectronvolt energies

Langue

Ce document a été publié dans

Résumé en anglais

Mots clés en anglais

DOI

Origine

Unités de recherche