HAWC, VERITAS, Fermi-LAT and XMM-Newton follow-up observations of the unidentified ultra-high-energy gamma-ray source LHAASO J2108+5157

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dc.contributor.authorKumar, Sajan
dc.contributor.authorValverde, Janeth
dc.contributor.authorAdams, C. B.
dc.contributor.authorBangale, P.
dc.contributor.authorBenbow, W.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorChen, Y.
dc.contributor.authorHarding, J. P.
dc.contributor.authorVERITAS collaboration
dc.contributor.authorHAWC collaboration
dc.contributor.authorXMM-Newton collaboration
dc.contributor.authoret al
dc.date.accessioned2025-08-28T16:10:50Z
dc.date.issued2025-08-03
dc.descriptionAuthors at The VERITAS collaboration : C. B. Adams, P. Bangale, W. Benbow, J. H. Buckley, Y. Chen, J. L. Christiansen, A. J. Chromey, M. Escobar Godoy, S. Feldman, Q. Feng, J. Foote, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, S. Kumar, M. J. Lang, M. Lundy, G. Maier, M. J. Millard, P. Moriarty, R. Mukherjee, W. Ning, R. A. Ong, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, I. Sadeh, L. Saha, G. H. Sembroski, R. Shang, D. Tak, A. K. Talluri, J. V. Tucci, J. Valverde, D. A. Williams, S. L. Wong, and J. Woo. Authors at The HAWC collaboration: R. Alfaro, C. Alvarez, J.C. Arteaga-Velazquez, D. Avila Rojas, R. Babu, E. Belmont-Moreno, A. Bernal, K.S. Caballero-Mora, A. Carraminana, S. Casanova, U. Cotti, J. Cotzomi, E. De la Fuente, C. de Leon, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M.A. DuVernois, K. Engel, T. Ergin, C. Espinoza, K.L. Fan, N. Fraija, S. Fraija, J.A. García-Gonzalez, F. Garfias, A. Gonzalez Munoz, M.M. Gonzalez, J.A. Goodman, S. Groetsch, J.P. Harding, S. Hernandez-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Huntemeyer, A. Iriarte, S. Kaufmann, A. Lara, J. Lee, H. Leon Vargas, A.L. Longinotti, and G. Luis-Raya. K. Malone, O. Martinez, J. Martínez-Castro, J.A. Matthews, P. Miranda-Romagnoli, J.A. Morales-Soto, E. Moreno, M. Araya, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, E. Ponce, E.G. Pérez-Pérez, C.D. Rho, D. Rosa-Gonzalez, M. Roth, H. Salazar, A. Sandoval, M. Schneider, J. Serna-Franco, A.J. Smith, Y. Son, R.W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I.J. Watson, H. Wu, S. Yu, S. Yun-Carcamo, and H. Zhou. Authors at The XMM-Newton collaboration: Kaya Mori, Charles J. Hailey, Samar Safi-Harb, and Shuo Zhang.
dc.description.abstractWe report observations of the ultra-high-energy gamma-ray source LHAASO J2108+5157, utilizing VERITAS, HAWC, Fermi-LAT, and XMM-Newton. VERITAS has collected ∼ 40 hours of data that we used to set ULs to the emission above 200 GeV. The HAWC data, collected over ∼ 2400 days, reveal emission between 3 and 146 TeV, with a significance of 7.5 σ, favoring an extended source model. The best-fit spectrum measured by HAWC is characterized by a simple power-law with a spectral index of 2.45 ± 0.11ₛₜₐₜ. Fermi-LAT analysis finds a point source with a very soft spectrum in the LHAASO J2108+5157 region, consistent with the 4FGL-DR3 catalog results. The XMM-Newton analysis yields a null detection of the source in the 2 - 7 keV band. The broadband spectrum can be interpreted as a pulsar and a pulsar wind nebula system, where the GeV gamma-ray emission originates from an unidentified pulsar, and the X-ray and TeV emission is attributed to synchrotron radiation and inverse Compton scattering of electrons accelerated within a pulsar wind nebula. In this leptonic scenario, our X-ray upper limit provides a stringent constraint on the magnetic field, which is ≲ 1.5 µG.
dc.description.sponsorshipThis research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, and by the Helmholtz Association in Germany. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science, and resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. We acknowledge the support from: the US National Science Foundation (NSF); the US Department of Energy Office of High-Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnolog´a (CONACyT), M´exico, grants LNC-2023-117, 271051, 232656, 260378, 179588, 254964, 258865, 243290, 132197, A1-S-46288, A1-S22784, CF-2023-I-645, c´atedras 873, 1563, 341, 323, Red HAWC, M´exico; DGAPA-UNAM grants IG101323, IN111716-3, IN111419, IA102019, IN106521, IN114924, IN110521 , IN102223; VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015; the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Polish Science Centre grant, 2024/53/B/ST9/02671; Coordinaci´on de la Investigaci´on Cient´fica de la Universidad Michoacana; Royal Society - Newton Advanced Fellowship 180385; Gobierno de Espa˜na and European Union - NextGenerationEU, grant CNS2023- 144099; The Program Management Unit for Human Resources & Institutional Development, Research and Innovation, NXPO (grant number B16F630069); Coordinaci´on General Acad´emica e Innovaci´on (CGAI-UdeG), PRODEP-SEP UDG-CA499; Institute of Cosmic Ray Research (ICRR), University of Tokyo. H.F. acknowledges support by NASA under award number 80GSFC21M0002. C.R. acknowledges support from National Research Foundation of Korea (RS-2023-00280210). We also acknowledge the 11 significant contributions over many years of Stefan Westerhoff, Gaurang Yodh and Arnulfo Zepeda Dom´nguez, all deceased members of the HAWC collaboration. Thanks to Scott Delay, Luciano D´az and Eduardo Murrieta for technical support. The XMM-Newton observation and data analysis are supported by NASA grant XMMNC22.
dc.description.urihttp://arxiv.org/abs/2508.01934
dc.format.extent12 pages
dc.genrejournal articles
dc.genrepreprints
dc.identifierdoi:10.13016/m2sz7q-1woi
dc.identifier.urihttps://doi.org/10.48550/arXiv.2508.01934
dc.identifier.urihttp://hdl.handle.net/11603/40047
dc.language.isoen
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis 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.
dc.rightsPublic Domain
dc.rights.urihttps://creativecommons.org/publicdomain/mark/1.0/
dc.subjectAstrophysics - High Energy Astrophysical Phenomena
dc.titleHAWC, VERITAS, Fermi-LAT and XMM-Newton follow-up observations of the unidentified ultra-high-energy gamma-ray source LHAASO J2108+5157
dc.typeText

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