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Aharonian, F.; Aschersleben, J.; Backes, M.; Martins, V. Barbosa; Batzofin, R.; Becherini, Y.; Bernlöhr, K.; Böttcher, M.; Bolmont, J.; de Bony de Lavergne, M.; Borowska, J.; Brose, R.; Brown, A.; Bruno, B.; Burger-Scheidlin, C.; Casanova, S.; Celic, J.; Chandra, S.; Chen, A.; Chibueze, J.; Cotter, G.; Cristofari, P.; Devin, J.; Djannati-Ataï, A.; Egberts, K.; Feijen, K.; Filipovic, M.; Fontaine, G.; Gallant, Y. A.; Glicenstein, J. F.; Glombitza, J.; Grolleron, G.; Haerer, L.; Heß, B.; Hinton, J. A.; Holch, T. L.; Horns, D.; Huang, Zhiqiu; Jamrozy, M.; Jankowsky, F.; Jung-Richardt, I.; Kasai, E.; Katarzyński, K.; Khélifi, B.; Kostunin, D.; Kundu, A.; Lang, R. G.; Le Stum, S.; Lemière, A.; Lemoine-Goumard, M.; Mackey, J.; Marandon, V.; Martí-Devesa, G.; Mehta, A.; Moderski, R.; Moghadam, M. O.; Mohrmann, L.; Niemiec, J.; Ohm, S.; Olivera-Nieto, L.; de Ona Wilhelmi, E.; Ostrowski, M.; Panny, S.; Pensec, U.; Peron, G.; Pühlhofer, G.; Quirrenbach, A.; Ravikularaman, S.; Regeard, M.; Reimer, A.; Reimer, O.; Ren, H.; Renaud, M.; Rieger, F.; Ruiz-Velasco, E.; Sahakian, V.; Salzmann, H.; Sasaki, M.; Schäfer, J.; Schüssler, F.; Sol, H.; Spencer, S.; Stawarz, Ł.; Steinmassl, S.; Streil, K.; Sushch, I.; Taylor, A. M.; Terrier, R.; Tsirou, M.; Tsuji, N.; van Eldik, C.; Vecchi, M.; Venter, C.; Vink, J.; White, R.; Wierzcholska, A.; Zacharias, M.; Zdziarski, A. A.; Zech, A.; Żywucka, N.
Astrophysical journal. Letters, 2024, Letnik: 970, Številka: 1Journal Article
Abstract The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce very high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy γ -ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the γ -ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The γ -ray luminosity above 0.5 TeV of both sources is (2–3) × 10 35 erg s −1 . This exceeds by more than a factor of 2 the luminosity of HESS J1646−458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the γ -ray emission from each source is extended with a significance of >3 σ and a Gaussian width of about 30 pc. For 30 Dor C, a connection between the γ -ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the γ -ray signal from R136 are discussed.
