Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors

Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors

The yields and production rates of the radioisotopes \(^9\)Li and \(^8\)He created by cosmic muon spallation on \(^{12}\)C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to differ...

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Veröffentlicht in:arXiv.org 2018-10
Hauptverfasser: de Kerret, H, Abrahão, T, Almazan, H, dos Anjos, J C, Appel, S, Barriere, J C, Bekman, I, Bezerra, T J C, Bezrukov, L, Blucher, E, Brugière, T, Buck, C, Busenitz, J, Cabrera, A, Cerrada, M, Chauveau, E, Chimenti, P, Corpace, O, Dawson, J V, Djurcic, Z, Etenko, A, Franco, D, Furuta, H, Gil-Botella, I, Givaudan, A, Gomez, H, Gonzalez, L F G, Goodman, M C, Hara, T, Haser, J, Hellwig, D, Hourlier, A, Ishitsuka, M, Jochum, J, Jollet, C, Kale, K, Kaneda, M, Karakac, M, Kawasaki, T, Kemp, E, Kryn, D, Kuze, M, Lachenmaier, T, Lane, C E, Lasserre, T, Lastoria, C, Lhuillier, D, Lima, H P, Lindner, M, López-Castaño, J M, LoSecco, J M, Lubsandorzhiev, B, Maeda, J, Mariani, C, Maricic, J, Martino, J, Matsubara, T, Mention, G, Meregaglia, A, Miletic, T, Milincic, R, Navas-Nicolás, D, Novella, P, Nunokawa, H, Oberauer, L, Obolensky, M, Onillon, A, Oralbaev, A, Palomares, C, Pepe, I M, Pronost, G, Reichenbacher, J, Reinhold, B, Settimo, M, Schönert, S, Schoppmann, S, Scola, L, Sharankova, R, Sibille, V, Sinev, V, Skorokhvatov, M, Soldin, P, Stahl, A, Stancu, I, Stokes, L F F, Suekane, F, Sukhotin, S, Sumiyoshi, T, Sun, Y, Tonazzo, A, Veyssiere, C, Viaud, B, Vivier, M, Wagner, S, Wiebusch, C, Wurm, M, Yang, G, Yermia, F
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Detectors
Radioisotopes
Scintillation counters
Sensors
Spallation
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container_title arXiv.org
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creator de Kerret, H
Abrahão, T
Almazan, H
dos Anjos, J C
Appel, S
Barriere, J C
Bekman, I
Bezerra, T J C
Bezrukov, L
Blucher, E
Brugière, T
Buck, C
Busenitz, J
Cabrera, A
Cerrada, M
Chauveau, E
Chimenti, P
Corpace, O
Dawson, J V
Djurcic, Z
Etenko, A
Franco, D
Furuta, H
Gil-Botella, I
Givaudan, A
Gomez, H
Gonzalez, L F G
Goodman, M C
Hara, T
Haser, J
Hellwig, D
Hourlier, A
Ishitsuka, M
Jochum, J
Jollet, C
Kale, K
Kaneda, M
Karakac, M
Kawasaki, T
Kemp, E
Kryn, D
Kuze, M
Lachenmaier, T
Lane, C E
Lasserre, T
Lastoria, C
Lhuillier, D
Lima, H P
Lindner, M
López-Castaño, J M
LoSecco, J M
Lubsandorzhiev, B
Maeda, J
Mariani, C
Maricic, J
Martino, J
Matsubara, T
Mention, G
Meregaglia, A
Miletic, T
Milincic, R
Navas-Nicolás, D
Novella, P
Nunokawa, H
Oberauer, L
Obolensky, M
Onillon, A
Oralbaev, A
Palomares, C
Pepe, I M
Pronost, G
Reichenbacher, J
Reinhold, B
Settimo, M
Schönert, S
Schoppmann, S
Scola, L
Sharankova, R
Sibille, V
Sinev, V
Skorokhvatov, M
Soldin, P
Stahl, A
Stancu, I
Stokes, L F F
Suekane, F
Sukhotin, S
Sumiyoshi, T
Sun, Y
Tonazzo, A
Veyssiere, C
Viaud, B
Vivier, M
Wagner, S
Wiebusch, C
Wurm, M
Yang, G
Yermia, F
description The yields and production rates of the radioisotopes \(^9\)Li and \(^8\)He created by cosmic muon spallation on \(^{12}\)C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of \(\sim\)120 m.w.e. (\(\sim\)300 m.w.e.) corresponding to a mean muon energy of \(32.1\pm2.0\,\mathrm{GeV}\) (\(63.7\pm5.5\,\mathrm{GeV}\)). Comparing the data to a detailed simulation of the \(^9\)Li and \(^8\)He decays, the contribution of the \(^8\)He radioisotope at both detectors is found to be compatible with zero. The observed \(^9\)Li yields in the near and far detectors are \(5.51\pm0.51\) and \(7.90\pm0.51\), respectively, in units of \(10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2} }\). The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the \(^9\)Li yield and the mean muon energy according to the power law \(Y = Y_0( / 1\,\mathrm{GeV})^{\overline{\alpha}}\), giving \(\overline{\alpha}=0.72\pm0.06\) and \(Y_0=(0.43\pm0.11)\times 10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2}}\). This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic \(^9\)Li background rates.
doi_str_mv 10.48550/arxiv.1802.08048
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The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of \(\sim\)120 m.w.e. (\(\sim\)300 m.w.e.) corresponding to a mean muon energy of \(32.1\pm2.0\,\mathrm{GeV}\) (\(63.7\pm5.5\,\mathrm{GeV}\)). Comparing the data to a detailed simulation of the \(^9\)Li and \(^8\)He decays, the contribution of the \(^8\)He radioisotope at both detectors is found to be compatible with zero. The observed \(^9\)Li yields in the near and far detectors are \(5.51\pm0.51\) and \(7.90\pm0.51\), respectively, in units of \(10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2} }\). The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the \(^9\)Li yield and the mean muon energy according to the power law \(Y = Y_0( &lt;E_{\mu} &gt;/ 1\,\mathrm{GeV})^{\overline{\alpha}}\), giving \(\overline{\alpha}=0.72\pm0.06\) and \(Y_0=(0.43\pm0.11)\times 10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2}}\). This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic \(^9\)Li background rates.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1802.08048</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Detectors ; Radioisotopes ; Scintillation counters ; Sensors ; Spallation</subject><ispartof>arXiv.org, 2018-10</ispartof><rights>2018. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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K</creatorcontrib><creatorcontrib>Kaneda, M</creatorcontrib><creatorcontrib>Karakac, M</creatorcontrib><creatorcontrib>Kawasaki, T</creatorcontrib><creatorcontrib>Kemp, E</creatorcontrib><creatorcontrib>Kryn, D</creatorcontrib><creatorcontrib>Kuze, M</creatorcontrib><creatorcontrib>Lachenmaier, T</creatorcontrib><creatorcontrib>Lane, C E</creatorcontrib><creatorcontrib>Lasserre, T</creatorcontrib><creatorcontrib>Lastoria, C</creatorcontrib><creatorcontrib>Lhuillier, D</creatorcontrib><creatorcontrib>Lima, H P</creatorcontrib><creatorcontrib>Lindner, M</creatorcontrib><creatorcontrib>López-Castaño, J M</creatorcontrib><creatorcontrib>LoSecco, J M</creatorcontrib><creatorcontrib>Lubsandorzhiev, B</creatorcontrib><creatorcontrib>Maeda, J</creatorcontrib><creatorcontrib>Mariani, C</creatorcontrib><creatorcontrib>Maricic, J</creatorcontrib><creatorcontrib>Martino, J</creatorcontrib><creatorcontrib>Matsubara, T</creatorcontrib><creatorcontrib>Mention, G</creatorcontrib><creatorcontrib>Meregaglia, A</creatorcontrib><creatorcontrib>Miletic, T</creatorcontrib><creatorcontrib>Milincic, R</creatorcontrib><creatorcontrib>Navas-Nicolás, D</creatorcontrib><creatorcontrib>Novella, P</creatorcontrib><creatorcontrib>Nunokawa, H</creatorcontrib><creatorcontrib>Oberauer, L</creatorcontrib><creatorcontrib>Obolensky, M</creatorcontrib><creatorcontrib>Onillon, A</creatorcontrib><creatorcontrib>Oralbaev, A</creatorcontrib><creatorcontrib>Palomares, C</creatorcontrib><creatorcontrib>Pepe, I M</creatorcontrib><creatorcontrib>Pronost, G</creatorcontrib><creatorcontrib>Reichenbacher, J</creatorcontrib><creatorcontrib>Reinhold, B</creatorcontrib><creatorcontrib>Settimo, M</creatorcontrib><creatorcontrib>Schönert, S</creatorcontrib><creatorcontrib>Schoppmann, S</creatorcontrib><creatorcontrib>Scola, L</creatorcontrib><creatorcontrib>Sharankova, R</creatorcontrib><creatorcontrib>Sibille, V</creatorcontrib><creatorcontrib>Sinev, V</creatorcontrib><creatorcontrib>Skorokhvatov, M</creatorcontrib><creatorcontrib>Soldin, P</creatorcontrib><creatorcontrib>Stahl, A</creatorcontrib><creatorcontrib>Stancu, I</creatorcontrib><creatorcontrib>Stokes, L F F</creatorcontrib><creatorcontrib>Suekane, F</creatorcontrib><creatorcontrib>Sukhotin, S</creatorcontrib><creatorcontrib>Sumiyoshi, T</creatorcontrib><creatorcontrib>Sun, Y</creatorcontrib><creatorcontrib>Tonazzo, A</creatorcontrib><creatorcontrib>Veyssiere, C</creatorcontrib><creatorcontrib>Viaud, B</creatorcontrib><creatorcontrib>Vivier, M</creatorcontrib><creatorcontrib>Wagner, S</creatorcontrib><creatorcontrib>Wiebusch, C</creatorcontrib><creatorcontrib>Wurm, M</creatorcontrib><creatorcontrib>Yang, G</creatorcontrib><creatorcontrib>Yermia, F</creatorcontrib><title>Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors</title><title>arXiv.org</title><description>The yields and production rates of the radioisotopes \(^9\)Li and \(^8\)He created by cosmic muon spallation on \(^{12}\)C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of \(\sim\)120 m.w.e. (\(\sim\)300 m.w.e.) corresponding to a mean muon energy of \(32.1\pm2.0\,\mathrm{GeV}\) (\(63.7\pm5.5\,\mathrm{GeV}\)). Comparing the data to a detailed simulation of the \(^9\)Li and \(^8\)He decays, the contribution of the \(^8\)He radioisotope at both detectors is found to be compatible with zero. The observed \(^9\)Li yields in the near and far detectors are \(5.51\pm0.51\) and \(7.90\pm0.51\), respectively, in units of \(10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2} }\). The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the \(^9\)Li yield and the mean muon energy according to the power law \(Y = Y_0( &lt;E_{\mu} &gt;/ 1\,\mathrm{GeV})^{\overline{\alpha}}\), giving \(\overline{\alpha}=0.72\pm0.06\) and \(Y_0=(0.43\pm0.11)\times 10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2}}\). This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic \(^9\)Li background rates.</description><subject>Detectors</subject><subject>Radioisotopes</subject><subject>Scintillation counters</subject><subject>Sensors</subject><subject>Spallation</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNqNjs1Kw0AUhYeCYNE-QHcXurGLpvOTtNN1VbroshshWKaZGzMlnavzo-LTG4oP4OrjcL4Dh7Gp4EWpq4ovTfh2n4XQXBZc81KP2FgqJRa6lPKWTWI8c87lai2rSo1ZfnHY2wjGW3gPZHOTHHkIJmEEaqGheKE39K6B-uF1U8_37uoOQdfzHcIFTcwBLXy51EHqEB4pn3qEbUf0Ax5NuA7agRYTNolCvGc3rekjTv54x2bPT4ftbjFc-MgY0_FMOfihOkq-VnqjxUqo_1m_g89RCQ</recordid><startdate>20181010</startdate><enddate>20181010</enddate><creator>de Kerret, H</creator><creator>Abrahão, T</creator><creator>Almazan, H</creator><creator>dos Anjos, J C</creator><creator>Appel, S</creator><creator>Barriere, J C</creator><creator>Bekman, I</creator><creator>Bezerra, T J C</creator><creator>Bezrukov, L</creator><creator>Blucher, E</creator><creator>Brugière, T</creator><creator>Buck, C</creator><creator>Busenitz, J</creator><creator>Cabrera, A</creator><creator>Cerrada, M</creator><creator>Chauveau, E</creator><creator>Chimenti, P</creator><creator>Corpace, O</creator><creator>Dawson, J V</creator><creator>Djurcic, Z</creator><creator>Etenko, A</creator><creator>Franco, D</creator><creator>Furuta, H</creator><creator>Gil-Botella, I</creator><creator>Givaudan, A</creator><creator>Gomez, H</creator><creator>Gonzalez, L F G</creator><creator>Goodman, M C</creator><creator>Hara, T</creator><creator>Haser, J</creator><creator>Hellwig, D</creator><creator>Hourlier, A</creator><creator>Ishitsuka, M</creator><creator>Jochum, J</creator><creator>Jollet, C</creator><creator>Kale, K</creator><creator>Kaneda, M</creator><creator>Karakac, M</creator><creator>Kawasaki, T</creator><creator>Kemp, 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B</creator><creator>Settimo, M</creator><creator>Schönert, S</creator><creator>Schoppmann, S</creator><creator>Scola, L</creator><creator>Sharankova, R</creator><creator>Sibille, V</creator><creator>Sinev, V</creator><creator>Skorokhvatov, M</creator><creator>Soldin, P</creator><creator>Stahl, A</creator><creator>Stancu, I</creator><creator>Stokes, L F F</creator><creator>Suekane, F</creator><creator>Sukhotin, S</creator><creator>Sumiyoshi, T</creator><creator>Sun, Y</creator><creator>Tonazzo, A</creator><creator>Veyssiere, C</creator><creator>Viaud, B</creator><creator>Vivier, M</creator><creator>Wagner, S</creator><creator>Wiebusch, C</creator><creator>Wurm, M</creator><creator>Yang, G</creator><creator>Yermia, F</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20181010</creationdate><title>Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors</title><author>de Kerret, H ; Abrahão, T ; Almazan, H ; dos Anjos, J C ; Appel, S ; Barriere, J C ; Bekman, I ; Bezerra, T J C ; Bezrukov, L ; Blucher, E ; Brugière, T ; Buck, C ; Busenitz, J ; Cabrera, A ; Cerrada, M ; Chauveau, E ; Chimenti, P ; Corpace, O ; Dawson, J V ; Djurcic, Z ; Etenko, A ; Franco, D ; Furuta, H ; Gil-Botella, I ; Givaudan, A ; Gomez, H ; Gonzalez, L F G ; Goodman, M C ; Hara, T ; Haser, J ; Hellwig, D ; Hourlier, A ; Ishitsuka, M ; Jochum, J ; Jollet, C ; Kale, K ; Kaneda, M ; Karakac, M ; Kawasaki, T ; Kemp, E ; Kryn, D ; Kuze, M ; Lachenmaier, T ; Lane, C E ; Lasserre, T ; Lastoria, C ; Lhuillier, D ; Lima, H P ; Lindner, M ; López-Castaño, J M ; LoSecco, J M ; Lubsandorzhiev, B ; Maeda, J ; Mariani, C ; Maricic, J ; Martino, J ; Matsubara, T ; Mention, G ; Meregaglia, A ; Miletic, T ; Milincic, R ; Navas-Nicolás, D ; Novella, P ; Nunokawa, H ; Oberauer, L ; Obolensky, M ; Onillon, A ; Oralbaev, A ; Palomares, C ; Pepe, I M ; Pronost, G ; Reichenbacher, J ; Reinhold, B ; Settimo, M ; Schönert, S ; Schoppmann, S ; Scola, L ; Sharankova, R ; Sibille, V ; Sinev, V ; Skorokhvatov, M ; Soldin, P ; Stahl, A ; Stancu, I ; Stokes, L F F ; Suekane, F ; Sukhotin, S ; Sumiyoshi, T ; Sun, Y ; Tonazzo, A ; Veyssiere, C ; Viaud, B ; Vivier, M ; Wagner, S ; Wiebusch, C ; Wurm, M ; Yang, G ; Yermia, F</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-proquest_journals_20738981613</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Detectors</topic><topic>Radioisotopes</topic><topic>Scintillation counters</topic><topic>Sensors</topic><topic>Spallation</topic><toplevel>online_resources</toplevel><creatorcontrib>de Kerret, H</creatorcontrib><creatorcontrib>Abrahão, T</creatorcontrib><creatorcontrib>Almazan, H</creatorcontrib><creatorcontrib>dos Anjos, J C</creatorcontrib><creatorcontrib>Appel, S</creatorcontrib><creatorcontrib>Barriere, J C</creatorcontrib><creatorcontrib>Bekman, I</creatorcontrib><creatorcontrib>Bezerra, T J C</creatorcontrib><creatorcontrib>Bezrukov, L</creatorcontrib><creatorcontrib>Blucher, E</creatorcontrib><creatorcontrib>Brugière, T</creatorcontrib><creatorcontrib>Buck, C</creatorcontrib><creatorcontrib>Busenitz, J</creatorcontrib><creatorcontrib>Cabrera, 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M</creatorcontrib><creatorcontrib>Soldin, P</creatorcontrib><creatorcontrib>Stahl, A</creatorcontrib><creatorcontrib>Stancu, I</creatorcontrib><creatorcontrib>Stokes, L F F</creatorcontrib><creatorcontrib>Suekane, F</creatorcontrib><creatorcontrib>Sukhotin, S</creatorcontrib><creatorcontrib>Sumiyoshi, T</creatorcontrib><creatorcontrib>Sun, Y</creatorcontrib><creatorcontrib>Tonazzo, A</creatorcontrib><creatorcontrib>Veyssiere, C</creatorcontrib><creatorcontrib>Viaud, B</creatorcontrib><creatorcontrib>Vivier, M</creatorcontrib><creatorcontrib>Wagner, S</creatorcontrib><creatorcontrib>Wiebusch, C</creatorcontrib><creatorcontrib>Wurm, M</creatorcontrib><creatorcontrib>Yang, G</creatorcontrib><creatorcontrib>Yermia, F</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science &amp; Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>de Kerret, H</au><au>Abrahão, T</au><au>Almazan, H</au><au>dos Anjos, J C</au><au>Appel, S</au><au>Barriere, J C</au><au>Bekman, I</au><au>Bezerra, T J C</au><au>Bezrukov, L</au><au>Blucher, E</au><au>Brugière, T</au><au>Buck, C</au><au>Busenitz, J</au><au>Cabrera, A</au><au>Cerrada, M</au><au>Chauveau, E</au><au>Chimenti, P</au><au>Corpace, O</au><au>Dawson, J V</au><au>Djurcic, Z</au><au>Etenko, A</au><au>Franco, D</au><au>Furuta, H</au><au>Gil-Botella, I</au><au>Givaudan, A</au><au>Gomez, H</au><au>Gonzalez, L F G</au><au>Goodman, M C</au><au>Hara, T</au><au>Haser, J</au><au>Hellwig, D</au><au>Hourlier, A</au><au>Ishitsuka, M</au><au>Jochum, J</au><au>Jollet, C</au><au>Kale, K</au><au>Kaneda, M</au><au>Karakac, M</au><au>Kawasaki, T</au><au>Kemp, E</au><au>Kryn, D</au><au>Kuze, M</au><au>Lachenmaier, T</au><au>Lane, C E</au><au>Lasserre, T</au><au>Lastoria, C</au><au>Lhuillier, D</au><au>Lima, H P</au><au>Lindner, M</au><au>López-Castaño, J M</au><au>LoSecco, J M</au><au>Lubsandorzhiev, B</au><au>Maeda, J</au><au>Mariani, C</au><au>Maricic, J</au><au>Martino, J</au><au>Matsubara, T</au><au>Mention, G</au><au>Meregaglia, A</au><au>Miletic, T</au><au>Milincic, R</au><au>Navas-Nicolás, D</au><au>Novella, P</au><au>Nunokawa, H</au><au>Oberauer, L</au><au>Obolensky, M</au><au>Onillon, A</au><au>Oralbaev, A</au><au>Palomares, C</au><au>Pepe, I M</au><au>Pronost, G</au><au>Reichenbacher, J</au><au>Reinhold, B</au><au>Settimo, M</au><au>Schönert, S</au><au>Schoppmann, S</au><au>Scola, L</au><au>Sharankova, R</au><au>Sibille, V</au><au>Sinev, V</au><au>Skorokhvatov, M</au><au>Soldin, P</au><au>Stahl, A</au><au>Stancu, I</au><au>Stokes, L F F</au><au>Suekane, F</au><au>Sukhotin, S</au><au>Sumiyoshi, T</au><au>Sun, Y</au><au>Tonazzo, A</au><au>Veyssiere, C</au><au>Viaud, B</au><au>Vivier, M</au><au>Wagner, S</au><au>Wiebusch, C</au><au>Wurm, M</au><au>Yang, G</au><au>Yermia, F</au><format>book</format><genre>document</genre><ristype>GEN</ristype><atitle>Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors</atitle><jtitle>arXiv.org</jtitle><date>2018-10-10</date><risdate>2018</risdate><eissn>2331-8422</eissn><abstract>The yields and production rates of the radioisotopes \(^9\)Li and \(^8\)He created by cosmic muon spallation on \(^{12}\)C, have been measured by the two detectors of the Double Chooz experiment. The identical detectors are located at separate sites and depths, which means they are subject to different muon spectra. The near (far) detector has an overburden of \(\sim\)120 m.w.e. (\(\sim\)300 m.w.e.) corresponding to a mean muon energy of \(32.1\pm2.0\,\mathrm{GeV}\) (\(63.7\pm5.5\,\mathrm{GeV}\)). Comparing the data to a detailed simulation of the \(^9\)Li and \(^8\)He decays, the contribution of the \(^8\)He radioisotope at both detectors is found to be compatible with zero. The observed \(^9\)Li yields in the near and far detectors are \(5.51\pm0.51\) and \(7.90\pm0.51\), respectively, in units of \(10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2} }\). The shallow overburdens of the near and far detectors give a unique insight when combined with measurements by KamLAND and Borexino to give the first multi--experiment, data driven relationship between the \(^9\)Li yield and the mean muon energy according to the power law \(Y = Y_0( &lt;E_{\mu} &gt;/ 1\,\mathrm{GeV})^{\overline{\alpha}}\), giving \(\overline{\alpha}=0.72\pm0.06\) and \(Y_0=(0.43\pm0.11)\times 10^{-8}\mu ^{-1} \mathrm{g^{-1} cm^{2}}\). This relationship gives future liquid scintillator based experiments the ability to predict their cosmogenic \(^9\)Li background rates.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1802.08048</doi><oa>free_for_read</oa></addata></record>
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subjects Detectors
Radioisotopes
Scintillation counters
Sensors
Spallation
title Yields and production rates of cosmogenic \(^9\)Li and \(^8\)He measured with the Double Chooz near and far detectors
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