Multiwavelength Investigation of γ-ray Source MGRO J1908+06 Emission Using Fermi--LAT, VERITAS, and HAWC

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https://iopscience.iop.org/article/10.3847/1538-4357/ad698d

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https://doi.org/10.3847/1538-4357/ad698d
 http://hdl.handle.net/11603/35793

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
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2024-08-02

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journal articles
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Citation of Original Publication

Acharyya, A., C. B. Adams, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, J. L. Christiansen, et al. “Multiwavelength Investigation of γ-Ray Source MGRO J1908+06 Emission Using Fermi-LAT, VERITAS and HAWC.” The Astrophysical Journal 974, no. 1 (October 2024): 61. https://doi.org/10.3847/1538-4357/ad698d.

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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Astrophysics - Astrophysics of Galaxies
Astrophysics - High Energy Astrophysical Phenomena

Abstract

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 Fermi--LAT, VERITAS, and HAWC, with the addition of spectral data previously reported by LHAASO, a multiwavelength (MW) 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 (IC) emission of an evolved pulsar wind nebula (PWN) 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 dₚₛᵣ=3.2 kpc.