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2024ApJ...973..140A - Astrophys. J., 973, 140 (2024/October-1)

Combined Pre-supernova Alert System with KamLAND and Super-Kamiokande.

ABE S., EIZUKA M., FUTAGI S., GANDO A., GANDO Y., GOTO S., HACHIYA T., HATA K., ICHIMURA K., IEKI S., IKEDA H., INOUE K., ISHIDOSHIRO K., KAMEI Y., KAWADA N., KISHIMOTO Y., KOGA M., KURASAWA M., MITSUI T., MIYAKE H., MORITA D., NAKAHATA T., NAKAJIMA R., NAKAMURA K., NAKAMURA R., NAKAMURA R., NAKANE J., OZAKI H., SAITO K., SAKAI T., SHIMIZU I., SHIRAI J., SHIRAISHI K., SHOJI R., SUZUKI A., TAKEUCHI A., TAMAE K., WATANABE H., WATANABE K., YOSHIDA S., UMEHARA S., FUSHIMI K., KOTERA K., URANO Y., BERGER B.E., FUJIKAWA B.K., LEARNED J.G., MARICIC J., FU Z., SMOLSKY J., WINSLOW L.A., EFREMENKO Y., KARWOWSKI H.J., MARKOFF D.M., TORNOW W., DELL'ORO S., O'DONNELL T., DETWILER J.A., ENOMOTO S., DECOWSKI M.P., WEERMAN K.M., GRANT C., SONG H., LI A., AXANI S.N., GARCIA M. (The KamLAND Collaboration), ABE K., ABE S., BRONNER C., HAYATO Y., HIRAIDE K., HOSOKAWA K., IEKI K., IKEDA M., KAMEDA J., KANEMURA Y., KANESHIMA R., KASHIWAGI Y., KATAOKA Y., MIKI S., MINE S., MIURA M., MORIYAMA S., NAKAHATA M., NAKANO Y., NAKAYAMA S., NOGUCHI Y., SATO K., SEKIYA H., SHIBA H., SHIMIZU K., SHIOZAWA M., SONODA Y., SUZUKI Y., TAKEDA A., TAKEMOTO Y., TANAKA H., YANO T., HAN S., KAJITA T., OKUMURA K., TASHIRO T., TOMIYA T., WANG X., YOSHIDA S., FERNANDEZ P., LABARGA L., OSPINA N., ZALDIVAR B., POINTON B.W., KEARNS E., RAAF J.L., WAN L., WESTER T., BIAN J., GRISKEVICH N.J., SMY M.B., SOBEL H.W., TAKHISTOV V., YANKELEVICH A., HILL J., JANG M.C., LEE S.H., MOON D.H., PARK R.G., BODUR B., SCHOLBERG K., WALTER C.W., BEAUCHENE A., DRAPIER O., GIAMPAOLO A., MUELLER T.A., SANTOS A.D., PAGANINI P., QUILAIN B., ROGLY R., NAKAMURA T., JANG J.S., MACHADO L.N., LEARNED J.G., CHOI K., IOVINE N., CAO S., ANTHONY L.H.V., MARTIN D., PROUSE N.W., SCOTT M., UCHIDA Y., BERARDI V., CALABRIA N.F., CATANESI M.G., RADICIONI E., LANGELLA A., DE ROSA G., COLLAZUOL G., FELTRE M., IACOB F., MATTIAZZI M., LUDOVICI L., GONIN M., PERISSE L., PRONOST G., FUJISAWA C., HORIUCHI S., KOBAYASHI M., LIU Y.M., MAEKAWA Y., NISHIMURA Y., OKAZAKI R., AKUTSU R., FRIEND M., HASEGAWA T., ISHIDA T., KOBAYASHI T., JAKKAPU M., MATSUBARA T., NAKADAIRA T., NAKAMURA K., OYAMA Y., SAKASHITA K., SEKIGUCHI T., TSUKAMOTO T., PORTOCARRERO YREY A., BHUIYAN N., BURTON G.T., DI LODOVICO F., GAO J., GOLDSACK A., KATORI T., MIGENDA J., RAMSDEN R.M., XIE Z., ZSOLDOS S., SUZUKI A.T., TAKAGI Y., TAKEUCHI Y., ZHONG H., FENG J., FENG L., HU J.R., HU Z., KAWAUE M., KIKAWA T., MORI M., NAKAYA T., WENDELL R.A., YASUTOME K., JENKINS S.J., McCAULEY N., MEHTA P., TARRANT A., WILKING M.J., FUKUDA Y., ITOW Y., MENJO H., NINOMIYA K., YOSHIOKA Y., LAGODA J., MANDAL M., MIJAKOWSKI P., PRABHU Y.S., ZALIPSKA J., JIA M., JIANG J., SHI W., YANAGISAWA C., HARADA M., HINO Y., ISHINO H., KOSHIO Y., NAKANISHI F., SAKAI S., TADA T., TANO T., ISHIZUKA T., BARR G., BARROW D., COOK L., SAMANI S., WARK D., HOLIN A., NOVA F., JUNG S., YANG B.S., YANG J.Y., YOO J., FANNON J.E.P., KNEALE L., MALEK M., McELWEE J.M., THIESSE M.D., THOMPSON L.F., WILSON S.T., OKAZAWA H., LAKSHMI S.M., KIM S.B., KWON E., SEO J.W., YU I., ICHIKAWA A.K., NAKAMURA K.D., TAIRAFUNE S., NISHIJIMA K., EGUCHI A., NAKAGIRI K., NAKAJIMA Y., SHIMA S., TANIUCHI N., WATANABE E., YOKOYAMA M., DE PERIO P., FUJITA S., JESUS-VALLS C., MARTENS K., TSUI K.M., VAGINS M.R., XIA J., IZUMIYAMA S., KUZE M., MATSUMOTO R., TERADA K., ASAKA R., ISHITSUKA M., ITO H., OMMURA Y., SHIGETA N., SHINOKI M., YAMAUCHI K., YOSHIDA T., GAUR R., GOUSY-LEBLANC V., HARTZ M., KONAKA A., LI X., CHEN S., XU B.D., ZHANG A.Q., ZHANG B., POSIADALA-ZEZULA M., BOYD S.B., EDWARDS R., HADLEY D., NICHOLSON M., O'FLAHERTY M., RICHARDS B., ALI A., JAMIESON B., AMANAI S., MARTI L., MINAMINO A., SHIBAYAMA R., SUZUKI S. (The Super-Kamiokande Collaboration)

Abstract (from CDS):

Preceding a core-collapse supernova (CCSN), various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande (SK) via inverse beta decay interactions. Once these pre-supernova (pre-SN) neutrinos are observed, an early warning of the upcoming CCSN can be provided. In light of this, KamLAND and SK, both located in the Kamioka mine in Japan, have been monitoring pre-SN neutrinos since 2015 and 2021, respectively. Recently, we performed a joint study between KamLAND and SK on pre-SN neutrino detection. A pre-SN alert system combining the KamLAND detector and the SK detector was developed and put into operation, which can provide a supernova alert to the astrophysics community. Fully leveraging the complementary properties of these two detectors, the combined alert is expected to resolve a pre-SN neutrino signal from a 15 M⊙ star within 510 pc of the Earth at a significance level corresponding to a false alarm rate of no more than 1 per century. For a Betelgeuse-like model with optimistic parameters, it can provide early warnings up to 12 hr in advance.

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

Journal keyword(s): Particle astrophysics - Neutrino astronomy - Core-collapse supernovae

Simbad objects: 3

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