2024ApJ...975L..44C

Query : 2024ApJ...975L..44C

2024ApJ...975L..44C - Astrophys. J., 975, L44 (2024/November-2)

Detection of Very High-energy Gamma-Ray Emission from the Radio Galaxy M87 with LHAASO.

CAO Z., AHARONIAN F., AXIKEGU, BAI Y.X., BAO Y.W., BASTIERI D., BI X.J., BI Y.J., BIAN W., BUKEVICH A.V., CAO Q., CAO W.Y., CAO Z., CHANG J., CHANG J.F., CHEN A.M., CHEN E.S., CHEN H.X., CHEN L., 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 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, 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 Y., HOR Y.K., HOU B.W., HOU C., HOU X., HU H.B., HU Q., HU S.C., HUANG C., HUANG D.H., 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., KANG M.M., KARPIKOV I., KHANGULYAN D., KULESHOV D., KURINOV K., LI B.B., LI C.M., LI C., LI C., LI D., LI F., LI H.B., LI H.C., LI J., LI J., LI K., LI S.D., LI W.L., 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 M.Y., LIU R.Y., LIU S.M., LIU W., LIU Y., LIU Y.N., LUO Q., LUO Y., LV H.K., MA B.Q., MA L.L., MA X.H., MAO J.R., MIN Z., MITTHUMSIRI W., MU H.J., NAN Y.C., NERONOV A., NG K.C.Y., OU L.J., PATTARAKIJWANICH P., PEI Z.Y., QI J.C., QI M.Y., QIAO B.Q., QIN J.J., RAZA A., RUFFOLO D., SAIZ A., SAEED M., SEMIKOZ D., SHAO L., SHCHEGOLEV O., SHENG X.D., SHU F.W., SONG H.C., STENKIN Y.V., STEPANOV V., SU Y., SUN D.X., SUN Q.N., SUN X.N., SUN Z.B., TAKATA J., TAM P.H.T., TANG Q.W., TANG R., TANG Z.B., TIAN W.W., WAN L.H., WANG C., WANG C.B., WANG G.W., WANG H.G., WANG H.H., WANG J.C., WANG K., WANG K., WANG L.P., WANG L.Y., WANG P.H., WANG R., WANG W., WANG X.G., WANG X.Y., WANG Y., WANG Y.D., WANG Y.J., WANG Z.H., WANG Z.X., WANG Z., WANG Z., WEI D.M., WEI J.J., WEI Y.J., WEN T., WU C.Y., WU H.R., WU Q.W., WU S., WU X.F., WU Y.S., XI S.Q., XIA 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., YANG F.F., YANG L.L., YANG M.J., YANG R.Z., YANG W.X., YAO Y.H., YAO Z.G., 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 F., ZHANG H., ZHANG H.M., ZHANG H.Y., ZHANG J.L., ZHANG L., ZHANG P.F., ZHANG P.P., ZHANG R., ZHANG S.B., ZHANG S.R., ZHANG S.S., ZHANG X., ZHANG X.P., ZHANG Y.F., ZHANG Y., ZHANG Y., ZHAO B., ZHAO J., ZHAO L., ZHAO L.Z., ZHAO S.P., ZHAO X.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):

The nearby radio galaxy M87 is a very high-energy (VHE) gamma-ray emitter established by observations with ground-based gamma-ray detectors. Here we report the long-term monitoring of M87 from 2021 to 2024 with the Large High Altitude Air Shower Observatory (LHAASO). M87 has been detected by LHAASO with a statistical significance ∼ 9σ. The observed energy spectrum extends to 20 TeV, with a possible hardening at ∼20 TeV and then a clear softening at higher energies. Assuming that the intrinsic spectrum is described by a single power law up to 20 TeV, a tight upper bound on the extragalactic background light intensity is obtained. A strong VHE flare lasting 8 days, with a rise time of ${\tau }_{r}^{\mathrm{rise}}=1.05\pm 0.49$ days and decay time of ${\tau }_{d}^{\mathrm{decay}}=2.17\pm 0.58$ days, was found in early 2022. A possible GeV flare is seen also in Fermi Large Area Telescope data during the VHE flare period. The variability time as short as 1 day seen in the LHAASO data suggests a compact emission region with a size of ∼3 × 1015δ cm (δ being the Doppler factor of the emitting region), corresponding to a few Schwarzschild radii of the central supermassive black hole in M87. The continuous monitoring of the source reveals a duty cycle of ∼1% for VHE flares with a flux above 10–11 erg cm–2 s–1.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Active galactic nuclei - High energy astrophysics

Simbad objects: 4

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Number of rows : 4
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 4278 LIN 12 20 06.8242 +29 16 50.722 11.54 11.09 10.16     ~ 988 2
2 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
3 NAME Knot in M87 Jet PoG 12 30 49.355 +12 23 28.32           ~ 233 0
4 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3

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