ABDALLA, H.; ADAM, R.; AHARONIAN, F.; AIT BENKHALI, F.; ANGÜNER, E.O.; 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.; BI, B.; BÖTTCHER, M.; BOISSON, C.; BOLMONT, J.; DE BONY DE LAVERGNE, M.; BORDAS, P.; BREUHAUS, M.; BRUN, F.; BRUN, P.; BRYAN, M.; BÜCHELE, M.; BULIK, T.; BYLUND, T.; CAROFF, S.; CAROSI, A.; CASANOVA, S.; CHAND, T.; CHANDRA, S.; CHEN, A.; COTTER, G.; CURYŁO, M.; DAMASCENE MBARUBUCYEYE, J.; DAVIDS, I.; DAVIES, J.; DEIL, C.; DEVIN, J.; DEWILT, P.; DIRSON, L.; DJANNATI-ATAÏ, A.; DMYTRIIEV, A.; DONATH, A.; DOROSHENKO, V.; DUFFY, C.; DYKS, J.; EGBERTS, K.; EICHHORN, F.; EINECKE, S.; EMERY, G.; ERNENWEIN, J.-P.; FEIJEN, K.; FEGAN, S.; FIASSON, A.; FICHET DE CLAIRFONTAINE, G.; FONTAINE, G.; FUNK, S.; FÜSSLING, M.; GABICI, S.; GALLANT, Y.; GIAVITTO, G.; GIUNTI, L.; GLAWION, D.; GLICENSTEIN, J.; GOTTSCHALL, D.; GRONDIN, M.-H.; HAHN, J.; HAUPT, M.; HERMANN, G.; HINTON, J.; HOFMANN, W.; HOISCHEN, C.; HOLCH, T.; HOLLER, M.; HÖRBE, M.; HORNS, D.; HUBER, D.; JAMROZY, M.; JANKOWSKY, D.; JANKOWSKY, F.; JARDIN-BLICQ, A.; JOSHI, V.; JUNG-RICHARDT, I.; KASAI, E.; KASTENDIECK, M.; KATARZYŃSKI, K.; 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.; LEVY, C.; LOHSE, T.; LYPOVA, I.; MACKEY, J.; MAJUMDAR, J.; MALYSHEV, D.; MARANDON, V.; MARCHEGIANI, ¶.; MARCOWITH, Alexandre; MARES, A.; MARTÍ-DEVESA, G.; MARX, R.; MAURIN, G.; MEINTJES, P.; MEYER, M.; MITCHELL, A.; MODERSKI, R.; MOHAMED, M.; MOHRMANN, L.; MONTANARI, A.; MOORE, C.; MORRIS, P.; MOULIN, E.; MULLER, J.; MURACH, T.; NAKASHIMA, K.; NAYERHODA, A.; DE NAUROIS, M.; NDIYAVALA, H.; NIEDERWANGER, F.; NIEMIEC, J.; OAKES, L.; O’BRIEN, P.; ODAKA, H.; OHM, S.; OLIVERA-NIETO, L.; DE ONA WILHELMI, E.; OSTROWSKI, M.; OYA, I.; PANTER, M.; PANNY, S.; PARSONS, R.; PERON, G.; PEYAUD, B.; PIEL, Q.; PITA, S.; POIREAU, V.; PRIYANA NOEL, A.; PROKHOROV, D.; PROKOPH, H.; PÜHLHOFER, G.; PUNCH, M.; QUIRRENBACH, A.; RAAB, S.; RAUTH, R.; REICHHERZER, P.; REIMER, A.; REIMER, O.; REMY, Q.; RENAUD, Matthieu; RIEGER, F.; RINCHIUSO, L.; ROMOLI, C.; ROWELL, G.; RUDAK, B.; RUIZ-VELASCO, E.; SAHAKIAN, V.; SAILER, S.; SANCHEZ, D.; SANTANGELO, A.; SASAKI, M.; SCALICI, M.; SCHÜSSLER, F.; SCHUTTE, H.; SCHWANKE, U.; SCHWEMMER, S.; SEGLAR-ARROYO, M.; SENNIAPPAN, M.; SEYFFERT, A.; SHAFI, N.; SHININGAYAMWE, K.; SIMONI, R.; SINHA, A.; SOL, H.; SPECOVIUS, A.; SPENCER, S.; SPIR-JACOB, M.; STAWARZ, Ł.; SUN, L.; STEENKAMP, R.; STEGMANN, C.; STEINMASSL, S.; STEPPA, C.; TAKAHASHI, T.; TAVERNIER, T.; TAYLOR, A.; TERRIER, R.; TIZIANI, D.; TLUCZYKONT, M.; TOMANKOVA, L.; TRICHARD, C.; TSIROU, M.; TUFFS, R.; UCHIYAMA, Y.; VAN DER WALT, D.; VAN ELDIK, C.; VAN RENSBURG, C.; VAN SOELEN, B.; VASILEIADIS, George; VEH, J.; VENTER, C.; VINCENT, P.; VINK, J.; VÖLK, H.; VUILLAUME, T.; WADIASINGH, Z.; WAGNER, S.; WATSON, J.; WERNER, F.; WHITE, R.; WIERZCHOLSKA, A.; WONG, Yu Wun; YUSAFZAI, A.; ZACHARIAS, M.; ZANIN, R.; ZARGARYAN, D.; ZDZIARSKI, A.; ZECH, A.; ZHU, S.; ZIEGLER, A.; ZORN, J.; ZOUARI, S.; ŻYWUCKA, N.

doi:10.1051/0004-6361/202038851

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ABDALLA, H.

ADAM, R.
Laboratoire de Physique Nucléaire et de Hautes Énergies [LPNHE (UMR_7585)]

AHARONIAN, F.

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Astronomy and Astrophysics - A&A. 2020-12, vol. 644, p. A112

EDP Sciences

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The unidentified very-high-energy (VHE; E > 0.1 TeV) γ -ray source, HESS J1826−130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady γ -ray flux from HESS J1826−130, which appears extended with a half-width of 0.21° ± 0.02 stat ° ± 0.05 sys °. The source spectrum is best fit with either a power-law function with a spectral index Γ = 1.78 ± 0.10 stat ± 0.20 sys and an exponential cut-off at 15.2 −3.2 +5.5 TeV, or a broken power-law with Γ 1 = 1.96 ± 0.06 stat ± 0.20 sys , Γ 2 = 3.59 ± 0.69 stat ± 0.20 sys for energies below and above E br = 11.2 ± 2.7 TeV, respectively. The VHE flux from HESS J1826−130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825−137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826−130 VHE emission related to PSR J1826−1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826−130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to ≳200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.< Réduire

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Gamma rays

general -gamma rays

observations -gamma rays

individual objects

HESS J1826−130 -ISM

clouds -ISM

cosmic rays

ISM: supernova remnants

ISM: clouds

gamma rays: general

gamma rays: ISM

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An extreme particle accelerator in the Galactic plane: HESS J1826−130

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