Home > Publications database > Multiwavelength Investigation of γ-Ray Source MGRO J1908+06 Emission Using Fermi-LAT, VERITAS and HAWC > print

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024 7 _ |a 10.3847/1538-4357/ad698d
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024 7 _ |a inspire:2814548
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024 7 _ |a 0004-637X
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024 7 _ |a 1538-4357
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024 7 _ |a arXiv:2408.01625
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024 7 _ |a 10.3204/PUBDB-2025-00618
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088 _ _ |a arXiv:2408.01625
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100 1 _ |a Acharyya, A.
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245 _ _ |a Multiwavelength Investigation of γ-Ray Source MGRO J1908+06 Emission Using Fermi-LAT, VERITAS and HAWC
260 _ _ |a London
|c 2024
|b Institute of Physics Publ.
336 7 _ |a article
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336 7 _ |a ARTICLE
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336 7 _ |a Journal Article
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500 _ _ |a Grants DE-AC02-76SF00515; DE-AC02-05CH11231
520 _ _ |a This paper investigates the origin of the γ-ray emission from MGRO J1908+06 in the GeV–TeV energy band. By analyzing the data collected by the Fermi Large Area Telescope, the Very Energetic Radiation Imaging Telescope Array System, and High Altitude Water Cherenkov, with the addition of spectral data previously reported by LHAASO, a multiwavelength study of the morphological and spectral features of MGRO J1908+06 provides insight into the origin of the γ-ray emission. The mechanism behind the bright TeV emission is studied by constraining the magnetic field strength, the source age, and the distance through detailed broadband modeling. Both spectral shape and energy-dependent morphology support the scenario that inverse Compton emission of an evolved pulsar wind nebula associated with PSR J1907+0602 is responsible for the MGRO J1908+06 γ-ray emission with a best-fit true age of T = 22 ± 9 kyr and a magnetic field of B = 5.4 ± 0.8 μG, assuming the distance to the pulsar d$_{PSR}$ = 3.2 kpc.
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