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000640718 1001_ $$00000-0002-2028-9230$$aAcharyya, Atreya$$b0
000640718 245__ $$aAn In-depth Study of Gamma Rays from the Starburst Galaxy M82 with VERITAS
000640718 260__ $$aLondon$$bInstitute of Physics Publ.$$c2025
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000640718 500__ $$a15 pages, 7 figures; Accepted for the publication in The Astrophysical Journal (ApJ)
000640718 520__ $$aAssuming Galactic cosmic rays originate in supernovae and the winds of massive stars, starburst galaxies should produce very-high-energy (VHE; E > 100 GeV) gamma-ray emission via the interaction of their copious quantities of cosmic rays with the large reservoirs of dense gas within the galaxies. Such VHE emission was detected by VERITAS from the starburst galaxy M82 in 2008–09. An extensive, multiyear campaign followed these initial observations, yielding a total of 254 hr of good-quality VERITAS data on M82. Leveraging modern analysis techniques and the larger exposure, these VERITAS data show a more statistically significant VHE signal (∼6.5 standard deviations, σ). The corresponding photon spectrum is well fit by a power law (Γ = 2.3 ± 0.3$_{stat}$ ± 0.2$_{sys}$), and the observed integral flux is F (>450 GeV) = (3.2 ± 0.6$_{stat}$ ± 0.6$_{sys}$) × 10$^{−13}$ cm$^{−2}$ s$^{−1}$, or ∼0.4% of the Crab Nebula flux above the same energy threshold. The improved VERITAS measurements, when combined with various multiwavelength data, enable modeling of the underlying emission and transport processes. A purely leptonic scenario is found to be a poor representation of the gamma-ray spectral energy distribution (SED). A lepto-hadronic scenario with cosmic rays following a power-law spectrum in momentum (index s ≃ 2.25) and with significant bremsstrahlung below 1 GeV provides a good match to the observed SED. The synchrotron emission from the secondary electrons indicates that efficient nonradiative losses of cosmic-ray electrons may be related to advective escape from the starburst core.
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000640718 7001_ $$00000-0001-6391-9661$$aBuckley, J. H.$$b5
000640718 7001_ $$aChen, Yu$$b6
000640718 7001_ $$aChristiansen, Jodi L.$$b7
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000640718 7001_ $$00000-0003-1716-4119$$aDuerr, Anne$$b9
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000640718 7001_ $$aGodoy, Miguel E.$$b11
000640718 7001_ $$00000-0002-5068-7344$$aFalcone, Abe$$b12
000640718 7001_ $$aFeldman, Sydney$$b13
000640718 7001_ $$aFeng, Qi$$b14
000640718 7001_ $$00000-0002-2944-6060$$aFoote, Juniper$$b15
000640718 7001_ $$00000-0002-1067-8558$$aFortson, Lucy$$b16
000640718 7001_ $$00000-0003-1614-1273$$aFurniss, Amy$$b17
000640718 7001_ $$00000-0002-0109-4737$$aHanlon, William$$b18
000640718 7001_ $$00000-0002-8513-5603$$aHanna, David$$b19
000640718 7001_ $$00000-0003-3878-1677$$aHervet, Olivier$$b20
000640718 7001_ $$00000-0001-6951-2299$$aHinrichs, Claire E.$$b21
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000640718 7001_ $$00000-0002-1432-7771$$aHumensky, Thomas B.$$b23
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000640718 7001_ $$aSembroski, Glenn H.$$b55
000640718 7001_ $$00000-0002-9856-989X$$aShang, Ruo$$b56
000640718 7001_ $$00000-0003-3407-9936$$aSplettstoesser, Megan$$b57
000640718 7001_ $$aTak, D.$$b58
000640718 7001_ $$aTalluri, Anjana K.$$b59
000640718 7001_ $$aTucci, James V.$$b60
000640718 7001_ $$aVassiliev, Vladimir V.$$b61
000640718 7001_ $$00000-0003-2740-9714$$aWilliams, David A.$$b62
000640718 7001_ $$00000-0002-2730-2733$$aWong, Samantha L.$$b63
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000640718 773__ $$0PERI:(DE-600)1473835-1$$a10.3847/1538-4357/adab71$$gVol. 981, no. 2, p. 189 -$$n2$$p189 $$tThe astrophysical journal / Part 1$$v981$$x0004-637X$$y2025
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