2019ApJ...885..133S

Query : 2019ApJ...885..133S

2019ApJ...885..133S - Astrophys. J., 885, 133-133 (2019/November-2)

Sensitivity of Super-Kamiokande with gadolinium to low energy antineutrinos from pre-supernova emission.

SIMPSON C., ABE K., BRONNER C., HAYATO Y., IKEDA M., ITO H., IYOGI K., KAMEDA J., KATAOKA Y., KATO Y., KISHIMOTO Y., MARTI L., MIURA M., MORIYAMA S., MOCHIZUKI T., NAKAHATA M., NAKAJIMA Y., NAKAYAMA S., OKADA T., OKAMOTO K., ORII A., PRONOST G., SEKIYA H., SHIOZAWA M., SONODA Y., TAKEDA A., TAKENAKA A., TANAKA H., YANO T., AKUTSU R., KAJITA T., OKUMURA K., WANG R., XIA J., BRAVO-BERGUNO D., LABARGA L., FERNANDEZ P., BLASZCZYK F.d.M., KACHULIS C., KEARNS E., RAAF J.L., STONE J.L., WAN L., WESTER T., SUSSMAN S., BERKMAN S., BIAN J., GRISKEVICH N.J., KROPP W.R., LOCKE S., MINE S., SMY M.B., SOBEL H.W., TAKHISTOV V., WEATHERLY P., GANEZER K.S., HILL J., KIM J.Y., LIM I.T., PARK R.G., BODUR B., SCHOLBERG K., WALTER C.W., COFFANI A., DRAPIER O., GONIN M., IMBER J., MUELLER T.A., PAGANINI P., ISHIZUKA T., NAKAMURA T., JANG J.S., CHOI K., LEARNED J.G., MATSUNO S., LITCHFIELD R.P., SZTUC A.A., UCHIDA Y., WASCKO M.O., BERARDI V., CALABRIA N.F., CATANESI M.G., INTONTI R.A., RADICIONI E., DE ROSA G., COLLAZUOL G., IACOB F., LUDOVICI L., NISHIMURA Y., CAO S., FRIEND M., HASEGAWA T., ISHIDA T., KOBAYASHI T., NAKADAIRA T., NAKAMURA K., OYAMA Y., SAKASHITA K., SEKIGUCHI T., TSUKAMOTO T., ABE K., HASEGAWA M., ISOBE Y., MIYABE H., NAKANO Y., SHIOZAWA T., SUGIMOTO T., SUZUKI A.T., TAKEUCHI Y., ALI A., ASHIDA Y., HAYASHINO T., HIROTA S., JIANG M., KIKAWA T., MORI M., NAKAMURA KE., NAKAYA T., WENDELL R.A., ANTHONY L.H.V., McCAULEY N., PRITCHARD A., TSUI K.M., FUKUDA Y., ITOW Y., MURRASE M., NIWA T., TAANI M., TSUKADA M., MIJAKOWSKI P., FRANKIEWICZ K., JUNG C.K., LI X., PALOMINO J.L., SANTUCCI G., VILELA C., WILKING M.J., YANAGISAWA C., FUKUDA D., HARADA M., HAGIWARA K., HORAI T., ISHINO H., ITO S., KOSHIO Y., SAKUDA M., TAKAHIRA Y., XU C., KUNO Y., COOK L., WARK D., DI LODOVICO F., MOLINA SEDGWICK S., RICHARDS B., ZSOLDOS S., KIM S.B., TACIK R., THIESSE M., THOMPSON L., OKAZAWA H., CHOI Y., NISHIJIMA K., KOSHIBA M., YOKOYAMA M., GOLDSACK A., MARTENS K., MURDOCH M., QUILAIN B., SUZUKI Y., VAGINS M.R., KUZE M., OKAJIMA Y., TANAKA M., YOSHIDA T., ISHITSUKA M., MATSUMOTO R., OHTA K., MARTIN J.F., NANTAIS C.M., TANAKA H.A., TOWSTEGO T., HARTZ M., KONAKA A., DE PERIO P., CHEN S., JAMIESON B., WALKER J., MINAMINO A., OKAMOTO K., PINTAUDI G. (The Super-Kamiokande Collaboration)

Abstract (from CDS):

Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improve the ability of the detector to identify neutrons. A core-collapse supernova (CCSN) will be preceded by an increasing flux of neutrinos and antineutrinos, from thermal and weak nuclear processes in the star, over a timescale of hours; some of which may be detected at SK-Gd. This could provide an early warning of an imminent CCSN, hours earlier than the detection of the neutrinos from core collapse. Electron antineutrino detection will rely on inverse beta decay events below the usual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximizing detection efficiency. Assuming normal neutrino mass ordering, more than 200 events could be detected in the final 12 hr before core collapse for a 15-25 solar mass star at around 200 pc, which is representative of the nearest red supergiant to Earth, α-Ori (Betelgeuse). At a statistical false alarm rate of 1 per century, detection could be up to 10 hr before core collapse, and a pre-supernova star could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to the astrophysics community following gadolinium loading.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): Neutrino astronomy - Supernova neutrinos - Particle astrophysics - Silicon burning

Simbad objects: 6

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Number of rows : 6
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 QSO J0509+0541 BLL 05 09 25.9644373872 +05 41 35.333820420 15.32 14.95 14.78 15.12   ~ 453 2
2 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4937 2
3 * alf Ori s*r 05 55 10.30536 +07 24 25.4304 4.38 2.27 0.42 -1.17 -2.45 M1-M2Ia-Iab 1671 0
4 * gam02 Vel WR* 08 09 31.95013 -47 20 11.7108 0.64 1.58 1.83 1.85 2.00 WC8+O7.5III-V 906 0
5 * alf Sco s*r 16 29 24.45970 -26 25 55.2094 4.08 2.75 0.91 -0.64 -1.87 M1.5Iab+B2Vn 746 0
6 * eps Peg LP* 21 44 11.1561394 +09 52 30.031152 5.61 3.91 2.39 1.34 0.58 K2Ib-II 446 0

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