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001     407652
005     20230622114145.0
020 _ _ |9 978-3-945931-22-6
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024 7 _ |2 ISSN
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035 _ _ |a 52345
037 _ _ |a PUBDB-2018-02580
041 _ _ |a eng
088 _ _ |2 DESY
|a DESY-PROC-2018-03
088 1 _ |a DESY-PROC-2018-03
100 1 _ |0 P:(DE-H253)PIP1003168
|a Lindner, Axel
|b 0
|e Editor
111 2 _ |0 C18-06-18.7
|2 inspire
|a 14th "Patras" Workshop on Axions, WIMPs and WISPs
|c Hamburg
|d 2018-06-18 - 2018-06-22
|g PATRAS 2018
|w Germany
245 _ _ |a Axions, WIMPs and WISPs
|b proceedings, 14th Patras workshop, PATRAS 2018, Hamburg, Germany, June 18-22, 2018
|c Editors: Axel Lindner, Todd Kozlowski
260 _ _ |a Hamburg
|b Verlag Deutsches Elektronen-Synchrotron
|c 2018
300 _ _ |a viii, 103 pages : illustrations
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490 0 _ |a DESY-PROC
520 _ _ |a A Galactic supernova (SN) axion signal would be detected in a future neutrino Mton-class water Cherenkov detector, such as the proposed Hyper-Kamiokande in Japan. The main detection channel for axions is absorption on the oxygen nuclei in the water. The subsequent oxygen de-excitation leads to a potentially detectable gamma signal. In this contribution we present a calculation of the SN axion signal and discuss its detectability in Hyper-Kamiokande.
536 _ _ |0 G:(DE-HGF)POF3-6211
|a 6211 - Extreme States of Matter: From Cold Ions to Hot Plasmas (POF3-621)
|c POF3-621
|f POF III
|x 0
650 _ 7 |2 DE-H253
|a Weakly interacting slim particle
650 _ 7 |2 DE-H253
|a Weakly interacting slender particle
650 _ 7 |2 DE-H253
|a Weakly interacting sub-eV particle
650 _ 7 |2 DE-H253
|a PATRAS 2018
650 _ 7 |2 DE-H253
|a WIMPs
650 _ 7 |2 DE-H253
|a Axions
650 _ 7 |2 DE-H253
|a WISPs
650 _ 7 |2 DE-H253
|a Weakly interacting massive particles
650 _ 7 |2 DE-H253
|a Hamburg
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|e Any Light Particle Search
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700 1 _ |0 P:(DE-H253)PIP1080659
|a Kozlowski, Todd
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787 0 _ |0 PUBDB-2021-00114
|a Carenza, Pierluca et.al.
|d 2019
|i IsMemberOf
|r arXiv:1808.04101 ; DESY-PROC-2018-03
|t Axion emission and detection from a Galactic supernova
852 7 _ |2 DE-H253
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eMedia Proceedings Konf.  2018 Hamburg 
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