Search for joint multimessenger signals from potential Galactic
PeVatrons with HAWC and IceCube
R. Alfaro,C. Alvarez,J. C. Arteaga-Velázquez,D. Avila Rojas,H. A. Ayala Solares,R. Babu,E. Belmont-Moreno,K. S. Caballero-Mora,T. Capistrán,A. Carramiñana,S. Casanova,U. Cotti,J. Cotzomi,S. Coutiño de León,E. De la Fuente,D. Depaoli,N. Di Lalla,R. Diaz Hernandez,J. C. Díaz-Vélez,K. Engel,T. Ergin,K. L. Fan,K. Fang,N. Fraija,S. Fraija,J. A. García-González,F. Garfias,M. M. González,J. A. Goodman,S. Groetsch,J. P. Harding,S. Hernández-Cadena,I. Herzog,D. Huang,F. Hueyotl-Zahuantitla,P. Hüntemeyer,A. Iriarte,S. Kaufmann,J. Lee,H. León Vargas,A. L. Longinotti,G. Luis-Raya,K. Malone,J. Martínez-Castro,J. A. Matthews,P. Miranda-Romagnoli,J. A. Montes,E. Moreno,M. Mostafá,L. Nellen,N. Omodei,M. Osorio,Y. Pérez Araujo,E. G. Pérez-Pérez,C. D. Rho,D. Rosa-González,H. Salazar,D. Salazar-Gallegos,A. Sandoval,M. Schneider,J. Serna-Franco,A. J. Smith,Y. Son,O. Tibolla,K. Tollefson,I. Torres,R. Torres-Escobedo,R. Turner,F. Ureña-Mena,X. Wang,I. J. Watson,K. Whitaker,E. Willox,H. Wu,S. Yun-Cárcamo,H. Zhou,C. de León,R. Abbasi,M. Ackermann,J. Adams,S. K. Agarwalla,J. A. Aguilar,M. Ahlers,J. M. Alameddine,N. M. Amin,K. Andeen,C. Argüelles,Y. Ashida,S. Athanasiadou,L. Ausborm,S. N. Axani,X. Bai,A. Balagopal V.,M. Baricevic,S. W. Barwick,S. Bash,V. Basu,R. Bay,J. J. Beatty,J. Becker Tjus,J. Beise,C. Bellenghi,C. Benning,S. BenZvi,D. Berley,E. Bernardini,D. Z. Besson,E. Blaufuss,L. Bloom,S. Blot,F. Bontempo,J. Y. Book Motzkin,C. Boscolo Meneguolo,S. Böser,O. Botner,J. Böttcher,J. Braun,B. Brinson,J. Brostean-Kaiser,L. Brusa,R. T. Burley,D. Butterfield,M. A. Campana,I. Caracas,K. Carloni,J. Carpio,S. Chattopadhyay,N. Chau,Z. Chen,D. Chirkin,S. Choi,B. A. Clark,A. Coleman,G. H. Collin,A. Connolly,J. M. Conrad,P. Coppin,R. Corley,P. Correa,D. F. Cowen,P. Dave,C. De Clercq,J. J. DeLaunay,D. Delgado,S. Deng,A. Desai,P. Desiati,K. D. de Vries,G. de Wasseige,T. DeYoung,A. Diaz,J. C. Díaz-Vélez,P. Dierichs,M. Dittmer,A. Domi,L. Draper,H. Dujmovic,K. Dutta,M. A. DuVernois,T. Ehrhardt,L. Eidenschink,A. Eimer,P. Eller,E. Ellinger,S. El Mentawi,D. Elsässer,R. Engel,H. Erpenbeck,J. Evans,P. A. Evenson,K. Farrag,A. R. Fazely,A. Fedynitch,N. Feigl,S. Fiedlschuster,C. Finley,L. Fischer,D. Fox,A. Franckowiak,S. Fukami,P. Fürst,J. Gallagher,E. Ganster,A. Garcia,M. Garcia,G. Garg,E. Genton,L. Gerhardt,A. Ghadimi,C. Girard-Carillo,C. Glaser,T. Glüsenkamp,J. G. Gonzalez,S. Goswami,A. Granados,D. Grant,S. J. Gray,O. Gries,S. Griffin,S. Griswold,K. M. Groth,C. Günther,P. Gutjahr,C. Ha,C. Haack,A. Hallgren,L. Halve,F. Halzen,H. Hamdaoui,M. Ha Minh,M. Handt,K. Hanson,J. Hardin,A. A. Harnisch,P. Hatch,A. Haungs,J. Häußler,K. Helbing,J. Hellrung,J. Hermannsgabner,L. Heuermann,N. Heyer,S. Hickford,A. Hidvegi,C. Hill,G. C. Hill,K. D. Hoffman,S. Hori,K. Hoshina,M. Hostert,W. Hou,T. Huber,K. Hultqvist,M. Hünnefeld,R. Hussain,K. Hymon,A. Ishihara,W. Iwakiri,M. Jacquart,O. Janik,M. Jansson,G. S. Japaridze,M. Jeong,M. Jin,B. J. P. Jones,N. Kamp,D. Kang,W. Kang,X. Kang,A. Kappes,D. Kappesser,L. Kardum,T. Karg,M. Karl,A. Karle,A. Katil,U. Katz,M. Kauer,J. L. Kelley,M. Khanal,A. Khatee Zathul,A. Kheirandish,J. Kiryluk,S. R. Klein,A. Kochocki,R. Koirala,H. Kolanoski,T. Kontrimas,L. Köpke,C. Kopper,D. J. Koskinen,P. Koundal,M. Kovacevich,M. Kowalski,T. Kozynets,J. Krishnamoorthi,K. Kruiswijk,E. Krupczak,A. Kumar,E. Kun,N. Kurahashi,N. Lad,C. Lagunas Gualda,M. Lamoureux,M. J. Larson,S. Latseva,F. Lauber,J. P. Lazar,J. W. Lee,K. Leonard DeHolton,A. Leszczyńska,J. Liao,M. Lincetto,Y. T. Liu,M. Liubarska,E. Lohfink,C. Love,C. J. Lozano Mariscal,L. Lu,F. Lucarelli,W. Luszczak,Y. Lyu,J. Madsen,E. Magnus,K. B. M. Mahn,Y. Makino,E. Manao,S. Mancina,W. Marie Sainte,I. C. Mariş,S. Marka,Z. Marka,M. Marsee,I. Martinez-Soler,R. Maruyama,F. Mayhew,F. McNally,J. V. Mead,K. Meagher,S. Mechbal,A. Medina,M. Meier,Y. Merckx,L. Merten,J. Micallef,J. Mitchell,T. Montaruli,R. W. Moore,Y. Morii,R. Morse,M. Moulai,T. Mukherjee,R. Naab,R. Nagai,M. Nakos,U. Naumann,J. Necker,A. Negi,L. Neste,M. Neumann,H. Niederhausen,K. Noda,A. Noell,A. Novikov,A. Obertacke Pollmann,V. O'Dell,B. Oeyen,A. Olivas,R. Orsoe,J. Osborn,E. O'Sullivan,H. Pandya,N. Park,G. K. Parker,E. N. Paudel,L. Paul,C. Pérez de los Heros,T. Pernice,J. Peterson,S. Philippen,A. Pizzuto,M. Plum,A. Pontén,Y. Popovych,M. Prado Rodriguez,B. Pries,R. Procter-Murphy,G. T. Przybylski,C. Raab,J. Rack-Helleis,M. Ravn,K. Rawlins,Z. Rechav,A. Rehman,P. Reichherzer,E. Resconi,S. Reusch,W. Rhode,B. Riedel,A. Rifaie,E. J. Roberts,S. Robertson,S. Rodan,G. Roellinghoff,M. Rongen,A. Rosted,C. Rott,T. Ruhe,L. Ruohan,D. Ryckbosch,I. Safa,J. Saffer,P. Sampathkumar,A. Sandrock,M. Santander,S. Sarkar,S. Sarkar,J. Savelberg,P. Savina,P. Schaile,M. Schaufel,H. Schieler,S. Schindler,B. Schlüter,F. Schlüter,N. Schmeisser,T. Schmidt,J. Schneider,F. G. Schröder,L. Schumacher,S. Sclafani,D. Seckel,M. Seikh,M. Seo,S. Seunarine,P. Sevle Myhr,R. Shah,S. Shefali,N. Shimizu,M. Silva,B. Skrzypek,B. Smithers,R. Snihur,J. Soedingrekso,A. Søgaard,D. Soldin,P. Soldin,G. Sommani,C. Spannfellner,G. M. Spiczak,C. Spiering,M. Stamatikos,T. Stanev,T. Stezelberger,T. Stürwald,T. Stuttard,G. W. Sullivan,I. Taboada,S. Ter-Antonyan,A. Terliuk,M. Thiesmeyer,W. G. Thompson,J. Thwaites,S. Tilav,C. Tönnis,S. Toscano,D. Tosi,A. Trettin,R. Turcotte,J. P. Twagirayezu,M. A. Unland Elorrieta,A. K. Upadhyay,K. Upshaw,A. Vaidyanathan,N. Valtonen-Mattila,J. Vandenbroucke,N. van Eijndhoven,D. Vannerom,J. van Santen,J. Vara,J. Veitch-Michaelis,M. Venugopal,M. Vereecken,S. Verpoest,D. Veske,A. Vijai,C. Walck,A. Wang,C. Weaver,P. Weigel,A. Weindl,J. Weldert,A. Y. Wen,C. Wendt,J. Werthebach,M. Weyrauch,N. Whitehorn,C. H. Wiebusch,D. R. Williams,L. Witthaus,A. Wolf,M. Wolf,G. Wrede,X. W. Xu,J. P. Yanez,E. Yildizci,S. Yoshida,R. Young,S. Yu,T. Yuan,Z. Zhang,P. Zhelnin,P. Zilberman,M. Zimmerman
arxiv（2024）
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摘要
Galactic PeVatrons are sources that can accelerate cosmic rays to PeV
energies. The high-energy cosmic rays are expected to interact with the
surrounding ambient material or radiation, resulting in the production of gamma
rays and neutrinos. To optimize for the detection of such associated production
of gamma rays and neutrinos for a given source morphology and spectrum, a
multi-messenger analysis that combines gamma rays and neutrinos is required. In
this study, we use the Multi-Mission Maximum Likelihood framework (3ML) with
IceCube Maximum Likelihood Analysis software (i3mla) and HAWC Accelerated
Likelihood (HAL) to search for a correlation between 22 known gamma-ray sources
from the third HAWC gamma-ray catalog and 14 years of IceCube track-like data.
No significant neutrino emission from the direction of the HAWC sources was
found. We report the best-fit gamma-ray model and 90
from the 22 sources. From the neutrino flux limit, we conclude that the
gamma-ray emission from five of the sources can not be produced purely from
hadronic interactions. We report the limit for the fraction of gamma rays
produced by hadronic interactions for these five sources.
