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2025ApJ...982L..19C - Astrophys. J., 982, L19 (2025/March-3)

Constraining the Cosmic-Ray Energy Based on Observations of Nearby Galaxy Clusters by LHAASO.

CAO Z., AHARONIAN F., BAI Y.X., BAO Y.W., BASTIERI D., BI X.J., BI Y.J., BIAN W., BUKEVICH A.V., CAI C.M., CAO W.Y., CAO Z., CHANG J., CHANG J.F., CHEN A.M., CHEN E.S., CHEN H.X., CHEN L., CHEN L., CHEN M.J., CHEN M.L., CHEN Q.H., CHEN S., CHEN S.H., CHEN S.Z., CHEN T.L., CHEN X.B., CHEN X.J., CHEN Y., CHENG N., CHENG Y.D., CHU M.C., CUI M.Y., CUI S.W., CUI X.H., CUI Y.D., DAI B.Z., DAI H.L., DAI Z.G., DANZENGLUOBU, DIAO Y.X., DONG X.Q., DUAN K.K., FAN J.H., FAN Y.Z., FANG J., FANG J.H., FANG K., FENG C.F., FENG H., FENG L., FENG S.H., FENG X.T., FENG Y., FENG Y.L., GABICI S., GAO B., GAO C.D., GAO Q., GAO W., GAO W.K., GE M.M., GE T.T., GENG L.S., GIACINTI G., GONG G.H., GOU Q.B., GU M.H., GUO F.L., GUO J., GUO X.L., GUO Y.Q., GUO Y.Y., HAN Y.A., HANNUKSELA O.A., HASAN M., HE H.H., HE H.N., HE J.Y., HE X.Y., HE Y., HERNANDEZ-CADENA S., HOR Y.K., HOU B.W., HOU C., HOU X., HU H.B., HU S.C., HUANG C., HUANG D.H., HUANG J.J., HUANG T.Q., HUANG W.J., HUANG X.T., HUANG X.Y., HUANG Y., HUANG Y.Y., JI X.L., JIA H.Y., JIA K., JIANG H.B., JIANG K., JIANG X.W., JIANG Z.J., JIN M., KACI S., KANG M.M., KARPIKOV I., KHANGULYAN D., KULESHOV D., KURINOV K., LI B.B., LI C., LI C., LI D., LI F., LI H.B., LI H.C., LI J., LI J., LI K., LI L., LI R.L., LI S.D., LI T.Y., LI W.L., LI X.R., LI X., LI Y.Z., LI Z., LI Z., LIANG E.W., LIANG Y.F., LIN S.J., LIU B., LIU C., LIU D., LIU D.B., LIU H., LIU H.D., LIU J., LIU J.L., LIU J.R., LIU M.Y., LIU R.Y., LIU S.M., LIU W., LIU X., LIU Y., LIU Y., LIU Y.N., LOU Y.Q., LUO Q., LUO Y., LV H.K., MA B.Q., MA L.L., MA X.H., MAO J.R., MIN Z., MITTHUMSIRI W., MOU G.B., MU H.J., NAN Y.C., NERONOV A., NG K.C.Y., NI M.Y., NIE L., OU L.J., PATTARAKIJWANICH P., PEI Z.Y., QI J.C., QI M.Y., QIN J.J., RAZA A., REN C.Y., RUFFOLO D., SAIZ A., SAEED M., SEMIKOZ D., SHAO L., SHCHEGOLEV O., SHEN Y.Z., SHENG X.D., SHI Z.D., SHU F.W., SONG H.C., STENKIN Y.V., STEPANOV V., SU Y., SUN D.X., SUN H., SUN Q.N., SUN X.N., SUN Z.B., TABASAM N.H., TAKATA J., TAM P.H.T., TAN H.B., TANG Q.W., TANG R., TANG Z.B., TIAN W.W., TONG C.N., WAN L.H., WANG C., WANG G.W., WANG H.G., WANG H.H., WANG J.C., WANG K., WANG K., WANG K., WANG L.P., WANG L.Y., WANG L.Y., WANG R., WANG W., WANG X.G., WANG X.J., WANG X.Y., WANG Y., WANG Y.D., WANG Z.H., WANG Z.X., WANG Z., WEI D.M., WEI J.J., WEI Y.J., WEN T., WENG S.S., WU C.Y., WU H.R., WU Q.W., WU S., WU X.F., WU Y.S., XI S.Q., XIA J., XIA J.J., XIANG G.M., XIAO D.X., XIAO G., XIN Y.L., XING Y., XIONG D.R., XIONG Z., XU D.L., XU R.F., XU R.X., XU W.L., XUE L., YAN D.H., YAN J.Z., YAN T., YANG C.W., YANG C.Y., YANG F.F., YANG L.L., YANG M.J., YANG R.Z., YANG W.X., YAO Y.H., YAO Z.G., YE X.A., YIN L.Q., YIN N., YOU X.H., YOU Z.Y., YU Y.H., YUAN Q., YUE H., ZENG H.D., ZENG T.X., ZENG W., ZHA M., ZHANG B.B., ZHANG B.T., ZHANG F., ZHANG H., ZHANG H.M., ZHANG H.Y., ZHANG J.L., ZHANG L., ZHANG P.F., ZHANG P.P., ZHANG R., ZHANG S.R., ZHANG S.S., ZHANG W.Y., ZHANG X., ZHANG X.P., ZHANG Y., ZHANG Y., ZHANG Z.P., ZHAO J., ZHAO L., ZHAO L.Z., ZHAO S.P., ZHAO X.H., ZHAO Z.H., ZHENG F., ZHONG W.J., ZHOU B., ZHOU H., ZHOU J.N., ZHOU M., ZHOU P., ZHOU R., ZHOU X.X., ZHOU X.X., ZHU B.Y., ZHU C.G., ZHU F.R., ZHU H., ZHU K.J., ZOU Y.C. and ZUO X.

Abstract (from CDS):

Galaxy clusters act as reservoirs of high-energy cosmic rays (CRs). As CRs propagate through the intracluster medium, they generate diffuse γ-rays detectable by arrays such as LHAASO. These γ-rays result from proton-proton (pp) collisions of very high-energy cosmic rays or inverse Compton (IC) scattering of positron-electron pairs created by pγ interactions of ultra-high-energy cosmic rays (UHECRs). We analyzed diffuse γ-ray emission from the Coma, Perseus, and Virgo clusters using LHAASO data. Diffuse emission was modeled as a disk of radius R500 for each cluster while accounting for point sources. No significant diffuse emission was detected, yielding 95% confidence level (C.L.) upper limits on the γ-ray flux: for WCDA (1-25 TeV) and KM2A (>25 TeV), less than (49.4, 13.7, 54.0) and (1.34, 1.14, 0.40) × 10–14 ph cm–2 s–1 for Coma, Perseus, and Virgo, respectively. The γ-ray upper limits can be used to derive model-independent constraints on the integral energy of cosmic ray protons above 10 TeV (corresponding to the LHAASO observational range >1 TeV under the pp scenario) to be less than (1.96, 0.59, 0.08) × 1061 erg. The absence of detectable annuli/ring-like structures, indicative of cluster accretion or merging shocks, imposes further constraints on models in which the UHECRs are accelerated in the merging shocks of galaxy clusters.

Abstract Copyright: © 2025. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Galaxy clusters - Gamma-ray sources - Ultra-high-energy cosmic radiation - Perseus Cluster - Coma Cluster - Virgo Cluster

Simbad objects: 9

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