Since the deployment of the CALorimetric Electron Telescope (CALET) on the exposure facility of the Japanese Experiment Module (JEM) `Kibo' of the International Space Station in 2015, CALET is accumulating cosmic ray data steadily without any serious faults up to now. Although CALET is basically a high-energy cosmic-ray detector, its composite and thick detector structure allow us to separate gamma rays from charged cosmic rays clearly up the TeV energy region. In this paper, analysis of gamma-ray events above 10 GeV obtained by the `high-energy' triggers, which is the basic trigger mode of CALET for cosmic-ray observations and is always effective regardless of the ISS position in orbit, are reported. Especially, good energy resolution (less than 3% at 10 GeV) of CALET enables us to search for spectral features in the gamma-ray energy spectrum such as lines possibly caused by annihilation of dark matter particles. Gamma-ray events above 10 GeV observed during five years of CALET operation have been analyzed to search for possible line signals in the energy spectra assuming various region-of-interests of the sky depending on the proposed Galactic density profile models. We found no hint of line signals and preliminary upper limits on parameters of the DM annihilation and decay models have been obtained.

High-energy gamma-ray observations above 10 GeV with CALET on the International Space Station / Mori M.;Adriani O.;Akaike Y.;Asano K.;Asaoka Y.;Berti E.;Bigongiari G.;Binns W. R.;Bongi M.;Brogi P.;Bruno A.;Buckley J. H.;Cannady N.;Castellini G.;Checchia C.;Cherry M. L.;Collazuol G.;Ebisawa K.;Ficklin A. W.;Fuke H.;Gonzi S.;Guzik T. G.;Hams T.;Hibino K.;Ichimura M.;Ioka K.;Ishizaki W.;Israel M. H.;Kasahara K.;Kataoka J.;Kataoka R.;Katayose Y.;Kato C.;Kawanaka N.;Kawakubo Y.;Kobayashi K.;Kohri K.;Krawczynski H. S.;Krizmanic J. F.;Maestro P.;Marrocchesi P. S.;Messineo A. M.;Mitchell J. W.;Miyake S.;Moiseev A. A.;Mori N.;Motz H. M.;Munakata K.;Nakahira S.;Nishimura J.;de Nolfo G. A.;Okuno S.;Ormes J. F.;Ospina N.;Ozawa S.;Pacini L.;Papini P.;Rauch B. F.;Ricciarini S. B.;Sakai K.;Sakamoto T.;Sasaki M.;Shimizu Y.;Shiomi A.;Spillantini P.;Stolzi F.;Sugita S.;Sulaj A.;Takita M.;Tamura T.;Terasawa T.;Torii S.;Tsunesada Y.;Uchihori Y.;Vannuccini E.;Wefel J. P.;Yamaoka K.;Yanagita S.;Yoshida A.;Yoshida K.;Zober W. V.. - In: POS PROCEEDINGS OF SCIENCE. - ISSN 1824-8039. - ELETTRONICO. - 395 - 37th International Cosmic Ray Conference (ICRC2021):(2022), pp. 619.0-619.0. [10.22323/1.395.0619]

High-energy gamma-ray observations above 10 GeV with CALET on the International Space Station

Adriani O.;Berti E.;Bongi M.;Gonzi S.;Pacini L.;Spillantini P.;
2022

Abstract

Since the deployment of the CALorimetric Electron Telescope (CALET) on the exposure facility of the Japanese Experiment Module (JEM) `Kibo' of the International Space Station in 2015, CALET is accumulating cosmic ray data steadily without any serious faults up to now. Although CALET is basically a high-energy cosmic-ray detector, its composite and thick detector structure allow us to separate gamma rays from charged cosmic rays clearly up the TeV energy region. In this paper, analysis of gamma-ray events above 10 GeV obtained by the `high-energy' triggers, which is the basic trigger mode of CALET for cosmic-ray observations and is always effective regardless of the ISS position in orbit, are reported. Especially, good energy resolution (less than 3% at 10 GeV) of CALET enables us to search for spectral features in the gamma-ray energy spectrum such as lines possibly caused by annihilation of dark matter particles. Gamma-ray events above 10 GeV observed during five years of CALET operation have been analyzed to search for possible line signals in the energy spectra assuming various region-of-interests of the sky depending on the proposed Galactic density profile models. We found no hint of line signals and preliminary upper limits on parameters of the DM annihilation and decay models have been obtained.
2022
395 - 37th International Cosmic Ray Conference (ICRC2021)
0
0
Mori M.;Adriani O.;Akaike Y.;Asano K.;Asaoka Y.;Berti E.;Bigongiari G.;Binns W. R.;Bongi M.;Brogi P.;Bruno A.;Buckley J. H.;Cannady N.;Castellini G.;Checchia C.;Cherry M. L.;Collazuol G.;Ebisawa K.;Ficklin A. W.;Fuke H.;Gonzi S.;Guzik T. G.;Hams T.;Hibino K.;Ichimura M.;Ioka K.;Ishizaki W.;Israel M. H.;Kasahara K.;Kataoka J.;Kataoka R.;Katayose Y.;Kato C.;Kawanaka N.;Kawakubo Y.;Kobayashi K.;Kohri K.;Krawczynski H. S.;Krizmanic J. F.;Maestro P.;Marrocchesi P. S.;Messineo A. M.;Mitchell J. W.;Miyake S.;Moiseev A. A.;Mori N.;Motz H. M.;Munakata K.;Nakahira S.;Nishimura J.;de Nolfo G. A.;Okuno S.;Ormes J. F.;Ospina N.;Ozawa S.;Pacini L.;Papini P.;Rauch B. F.;Ricciarini S. B.;Sakai K.;Sakamoto T.;Sasaki M.;Shimizu Y.;Shiomi A.;Spillantini P.;Stolzi F.;Sugita S.;Sulaj A.;Takita M.;Tamura T.;Terasawa T.;Torii S.;Tsunesada Y.;Uchihori Y.;Vannuccini E.;Wefel J. P.;Yamaoka K.;Yanagita S.;Yoshida A.;Yoshida K.;Zober W. V.
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Utilizza questo identificatore per citare o creare un link a questa risorsa: https://hdl.handle.net/2158/1349416
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