Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe
Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
F. Agostini [verfasserIn] S. E. M. Ahmed Maouloud [verfasserIn] L. Althueser [verfasserIn] F. Amaro [verfasserIn] B. Antunovic [verfasserIn] E. Aprile [verfasserIn] L. Baudis [verfasserIn] D. Baur [verfasserIn] Y. Biondi [verfasserIn] A. Bismark [verfasserIn] P. A. Breur [verfasserIn] A. Brown [verfasserIn] G. Bruno [verfasserIn] R. Budnik [verfasserIn] C. Capelli [verfasserIn] J. Cardoso [verfasserIn] D. Cichon [verfasserIn] M. Clark [verfasserIn] A. P. Colijn [verfasserIn] J. J. Cuenca-García [verfasserIn] J. P. Cussonneau [verfasserIn] M. P. Decowski [verfasserIn] A. Depoian [verfasserIn] J. Dierle [verfasserIn] P. Di Gangi [verfasserIn] A. Di Giovanni [verfasserIn] S. Diglio [verfasserIn] J. M. F. dos Santos [verfasserIn] G. Drexlin [verfasserIn] K. Eitel [verfasserIn] R. Engel [verfasserIn] A. D. Ferella [verfasserIn] H. Fischer [verfasserIn] M. Galloway [verfasserIn] F. Gao [verfasserIn] F. Girard [verfasserIn] F. Glück [verfasserIn] L. Grandi [verfasserIn] R. Größle [verfasserIn] R. Gumbsheimer [verfasserIn] S. Hansmann-Menzemer [verfasserIn] F. Jörg [verfasserIn] G. Khundzakishvili [verfasserIn] A. Kopec [verfasserIn] F. Kuger [verfasserIn] L. M. Krauss [verfasserIn] H. Landsman [verfasserIn] R. F. Lang [verfasserIn] S. Lindemann [verfasserIn] M. Lindner [verfasserIn] J. A. M. Lopes [verfasserIn] A. Loya Villalpando [verfasserIn] C. Macolino [verfasserIn] A. Manfredini [verfasserIn] T. Marrodán Undagoitia [verfasserIn] J. Masbou [verfasserIn] E. Masson [verfasserIn] P. Meinhardt [verfasserIn] S. Milutinovic [verfasserIn] A. Molinario [verfasserIn] C. M. B. Monteiro [verfasserIn] M. Murra [verfasserIn] U. G. Oberlack [verfasserIn] M. Pandurovic [verfasserIn] R. Peres [verfasserIn] J. Pienaar [verfasserIn] M. Pierre [verfasserIn] V. Pizzella [verfasserIn] J. Qin [verfasserIn] D. Ramírez García [verfasserIn] S. Reichard [verfasserIn] N. Rupp [verfasserIn] P. Sanchez-Lucas [verfasserIn] G. Sartorelli [verfasserIn] D. Schulte [verfasserIn] M. Schumann [verfasserIn] L. Scotto Lavina [verfasserIn] M. Selvi [verfasserIn] M. Silva [verfasserIn] H. Simgen [verfasserIn] M. Steidl [verfasserIn] A. Terliuk [verfasserIn] C. Therreau [verfasserIn] D. Thers [verfasserIn] K. Thieme [verfasserIn] R. Trotta [verfasserIn] C. D. Tunnell [verfasserIn] K. Valerius [verfasserIn] G. Volta [verfasserIn] D. Vorkapic [verfasserIn] C. Weinheimer [verfasserIn] C. Wittweg [verfasserIn] J. Wolf [verfasserIn] J. P. Zopounidis [verfasserIn] K. Zuber [verfasserIn] DARWIN Collaboration [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2020 |
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| Übergeordnetes Werk: |
In: European Physical Journal C: Particles and Fields - SpringerOpen, 2017, 80(2020), 9, Seite 11 |
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| Übergeordnetes Werk: |
volume:80 ; year:2020 ; number:9 ; pages:11 |
| Links: |
Link aufrufen |
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| DOI / URN: |
10.1140/epjc/s10052-020-8196-z |
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| Katalog-ID: |
DOAJ068070187 |
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| 245 | 1 | 0 | |a Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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| 520 | |a Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. | ||
| 653 | 0 | |a Astrophysics | |
| 653 | 0 | |a Nuclear and particle physics. Atomic energy. Radioactivity | |
| 700 | 0 | |a S. E. M. Ahmed Maouloud |e verfasserin |4 aut | |
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| 700 | 0 | |a B. Antunovic |e verfasserin |4 aut | |
| 700 | 0 | |a E. Aprile |e verfasserin |4 aut | |
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| 700 | 0 | |a Y. Biondi |e verfasserin |4 aut | |
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| 700 | 0 | |a R. Größle |e verfasserin |4 aut | |
| 700 | 0 | |a R. Gumbsheimer |e verfasserin |4 aut | |
| 700 | 0 | |a S. Hansmann-Menzemer |e verfasserin |4 aut | |
| 700 | 0 | |a F. Jörg |e verfasserin |4 aut | |
| 700 | 0 | |a G. Khundzakishvili |e verfasserin |4 aut | |
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10.1140/epjc/s10052-020-8196-z doi (DE-627)DOAJ068070187 (DE-599)DOAJ8578e145f1c346b2ac06e5a732969a72 DE-627 ger DE-627 rakwb eng QB460-466 QC770-798 F. Agostini verfasserin aut Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. Astrophysics Nuclear and particle physics. Atomic energy. Radioactivity S. E. M. Ahmed Maouloud verfasserin aut L. Althueser verfasserin aut F. Amaro verfasserin aut B. Antunovic verfasserin aut E. Aprile verfasserin aut L. Baudis verfasserin aut D. Baur verfasserin aut Y. Biondi verfasserin aut A. Bismark verfasserin aut P. A. Breur verfasserin aut A. Brown verfasserin aut G. Bruno verfasserin aut R. Budnik verfasserin aut C. Capelli verfasserin aut J. Cardoso verfasserin aut D. Cichon verfasserin aut M. Clark verfasserin aut A. P. Colijn verfasserin aut J. J. Cuenca-García verfasserin aut J. P. Cussonneau verfasserin aut M. P. Decowski verfasserin aut A. Depoian verfasserin aut J. Dierle verfasserin aut P. Di Gangi verfasserin aut A. Di Giovanni verfasserin aut S. Diglio verfasserin aut J. M. F. dos Santos verfasserin aut G. Drexlin verfasserin aut K. Eitel verfasserin aut R. Engel verfasserin aut A. D. Ferella verfasserin aut H. Fischer verfasserin aut M. Galloway verfasserin aut F. Gao verfasserin aut F. Girard verfasserin aut F. Glück verfasserin aut L. Grandi verfasserin aut R. Größle verfasserin aut R. Gumbsheimer verfasserin aut S. Hansmann-Menzemer verfasserin aut F. Jörg verfasserin aut G. Khundzakishvili verfasserin aut A. Kopec verfasserin aut F. Kuger verfasserin aut L. M. Krauss verfasserin aut H. Landsman verfasserin aut R. F. Lang verfasserin aut S. Lindemann verfasserin aut M. Lindner verfasserin aut J. A. M. Lopes verfasserin aut A. Loya Villalpando verfasserin aut C. Macolino verfasserin aut A. Manfredini verfasserin aut T. Marrodán Undagoitia verfasserin aut J. Masbou verfasserin aut E. Masson verfasserin aut P. Meinhardt verfasserin aut S. Milutinovic verfasserin aut A. Molinario verfasserin aut C. M. B. Monteiro verfasserin aut M. Murra verfasserin aut U. G. Oberlack verfasserin aut M. Pandurovic verfasserin aut R. Peres verfasserin aut J. Pienaar verfasserin aut M. Pierre verfasserin aut V. Pizzella verfasserin aut J. Qin verfasserin aut D. Ramírez García verfasserin aut S. Reichard verfasserin aut N. Rupp verfasserin aut P. Sanchez-Lucas verfasserin aut G. Sartorelli verfasserin aut D. Schulte verfasserin aut M. Schumann verfasserin aut L. Scotto Lavina verfasserin aut M. Selvi verfasserin aut M. Silva verfasserin aut H. Simgen verfasserin aut M. Steidl verfasserin aut A. Terliuk verfasserin aut C. Therreau verfasserin aut D. Thers verfasserin aut K. Thieme verfasserin aut R. Trotta verfasserin aut C. D. Tunnell verfasserin aut K. Valerius verfasserin aut G. Volta verfasserin aut D. Vorkapic verfasserin aut C. Weinheimer verfasserin aut C. Wittweg verfasserin aut J. Wolf verfasserin aut J. P. Zopounidis verfasserin aut K. Zuber verfasserin aut DARWIN Collaboration verfasserin aut In European Physical Journal C: Particles and Fields SpringerOpen, 2017 80(2020), 9, Seite 11 (DE-627)253722934 (DE-600)1459069-4 14346052 nnns volume:80 year:2020 number:9 pages:11 https://doi.org/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 kostenfrei http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/toc/1434-6044 Journal toc kostenfrei https://doaj.org/toc/1434-6052 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 80 2020 9 11 |
| spelling |
10.1140/epjc/s10052-020-8196-z doi (DE-627)DOAJ068070187 (DE-599)DOAJ8578e145f1c346b2ac06e5a732969a72 DE-627 ger DE-627 rakwb eng QB460-466 QC770-798 F. Agostini verfasserin aut Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. Astrophysics Nuclear and particle physics. Atomic energy. Radioactivity S. E. M. Ahmed Maouloud verfasserin aut L. Althueser verfasserin aut F. Amaro verfasserin aut B. Antunovic verfasserin aut E. Aprile verfasserin aut L. Baudis verfasserin aut D. Baur verfasserin aut Y. Biondi verfasserin aut A. Bismark verfasserin aut P. A. Breur verfasserin aut A. Brown verfasserin aut G. Bruno verfasserin aut R. Budnik verfasserin aut C. Capelli verfasserin aut J. Cardoso verfasserin aut D. Cichon verfasserin aut M. Clark verfasserin aut A. P. Colijn verfasserin aut J. J. Cuenca-García verfasserin aut J. P. Cussonneau verfasserin aut M. P. Decowski verfasserin aut A. Depoian verfasserin aut J. Dierle verfasserin aut P. Di Gangi verfasserin aut A. Di Giovanni verfasserin aut S. Diglio verfasserin aut J. M. F. dos Santos verfasserin aut G. Drexlin verfasserin aut K. Eitel verfasserin aut R. Engel verfasserin aut A. D. Ferella verfasserin aut H. Fischer verfasserin aut M. Galloway verfasserin aut F. Gao verfasserin aut F. Girard verfasserin aut F. Glück verfasserin aut L. Grandi verfasserin aut R. Größle verfasserin aut R. Gumbsheimer verfasserin aut S. Hansmann-Menzemer verfasserin aut F. Jörg verfasserin aut G. Khundzakishvili verfasserin aut A. Kopec verfasserin aut F. Kuger verfasserin aut L. M. Krauss verfasserin aut H. Landsman verfasserin aut R. F. Lang verfasserin aut S. Lindemann verfasserin aut M. Lindner verfasserin aut J. A. M. Lopes verfasserin aut A. Loya Villalpando verfasserin aut C. Macolino verfasserin aut A. Manfredini verfasserin aut T. Marrodán Undagoitia verfasserin aut J. Masbou verfasserin aut E. Masson verfasserin aut P. Meinhardt verfasserin aut S. Milutinovic verfasserin aut A. Molinario verfasserin aut C. M. B. Monteiro verfasserin aut M. Murra verfasserin aut U. G. Oberlack verfasserin aut M. Pandurovic verfasserin aut R. Peres verfasserin aut J. Pienaar verfasserin aut M. Pierre verfasserin aut V. Pizzella verfasserin aut J. Qin verfasserin aut D. Ramírez García verfasserin aut S. Reichard verfasserin aut N. Rupp verfasserin aut P. Sanchez-Lucas verfasserin aut G. Sartorelli verfasserin aut D. Schulte verfasserin aut M. Schumann verfasserin aut L. Scotto Lavina verfasserin aut M. Selvi verfasserin aut M. Silva verfasserin aut H. Simgen verfasserin aut M. Steidl verfasserin aut A. Terliuk verfasserin aut C. Therreau verfasserin aut D. Thers verfasserin aut K. Thieme verfasserin aut R. Trotta verfasserin aut C. D. Tunnell verfasserin aut K. Valerius verfasserin aut G. Volta verfasserin aut D. Vorkapic verfasserin aut C. Weinheimer verfasserin aut C. Wittweg verfasserin aut J. Wolf verfasserin aut J. P. Zopounidis verfasserin aut K. Zuber verfasserin aut DARWIN Collaboration verfasserin aut In European Physical Journal C: Particles and Fields SpringerOpen, 2017 80(2020), 9, Seite 11 (DE-627)253722934 (DE-600)1459069-4 14346052 nnns volume:80 year:2020 number:9 pages:11 https://doi.org/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 kostenfrei http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/toc/1434-6044 Journal toc kostenfrei https://doaj.org/toc/1434-6052 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 80 2020 9 11 |
| allfields_unstemmed |
10.1140/epjc/s10052-020-8196-z doi (DE-627)DOAJ068070187 (DE-599)DOAJ8578e145f1c346b2ac06e5a732969a72 DE-627 ger DE-627 rakwb eng QB460-466 QC770-798 F. Agostini verfasserin aut Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. Astrophysics Nuclear and particle physics. Atomic energy. Radioactivity S. E. M. Ahmed Maouloud verfasserin aut L. Althueser verfasserin aut F. Amaro verfasserin aut B. Antunovic verfasserin aut E. Aprile verfasserin aut L. Baudis verfasserin aut D. Baur verfasserin aut Y. Biondi verfasserin aut A. Bismark verfasserin aut P. A. Breur verfasserin aut A. Brown verfasserin aut G. Bruno verfasserin aut R. Budnik verfasserin aut C. Capelli verfasserin aut J. Cardoso verfasserin aut D. Cichon verfasserin aut M. Clark verfasserin aut A. P. Colijn verfasserin aut J. J. Cuenca-García verfasserin aut J. P. Cussonneau verfasserin aut M. P. Decowski verfasserin aut A. Depoian verfasserin aut J. Dierle verfasserin aut P. Di Gangi verfasserin aut A. Di Giovanni verfasserin aut S. Diglio verfasserin aut J. M. F. dos Santos verfasserin aut G. Drexlin verfasserin aut K. Eitel verfasserin aut R. Engel verfasserin aut A. D. Ferella verfasserin aut H. Fischer verfasserin aut M. Galloway verfasserin aut F. Gao verfasserin aut F. Girard verfasserin aut F. Glück verfasserin aut L. Grandi verfasserin aut R. Größle verfasserin aut R. Gumbsheimer verfasserin aut S. Hansmann-Menzemer verfasserin aut F. Jörg verfasserin aut G. Khundzakishvili verfasserin aut A. Kopec verfasserin aut F. Kuger verfasserin aut L. M. Krauss verfasserin aut H. Landsman verfasserin aut R. F. Lang verfasserin aut S. Lindemann verfasserin aut M. Lindner verfasserin aut J. A. M. Lopes verfasserin aut A. Loya Villalpando verfasserin aut C. Macolino verfasserin aut A. Manfredini verfasserin aut T. Marrodán Undagoitia verfasserin aut J. Masbou verfasserin aut E. Masson verfasserin aut P. Meinhardt verfasserin aut S. Milutinovic verfasserin aut A. Molinario verfasserin aut C. M. B. Monteiro verfasserin aut M. Murra verfasserin aut U. G. Oberlack verfasserin aut M. Pandurovic verfasserin aut R. Peres verfasserin aut J. Pienaar verfasserin aut M. Pierre verfasserin aut V. Pizzella verfasserin aut J. Qin verfasserin aut D. Ramírez García verfasserin aut S. Reichard verfasserin aut N. Rupp verfasserin aut P. Sanchez-Lucas verfasserin aut G. Sartorelli verfasserin aut D. Schulte verfasserin aut M. Schumann verfasserin aut L. Scotto Lavina verfasserin aut M. Selvi verfasserin aut M. Silva verfasserin aut H. Simgen verfasserin aut M. Steidl verfasserin aut A. Terliuk verfasserin aut C. Therreau verfasserin aut D. Thers verfasserin aut K. Thieme verfasserin aut R. Trotta verfasserin aut C. D. Tunnell verfasserin aut K. Valerius verfasserin aut G. Volta verfasserin aut D. Vorkapic verfasserin aut C. Weinheimer verfasserin aut C. Wittweg verfasserin aut J. Wolf verfasserin aut J. P. Zopounidis verfasserin aut K. Zuber verfasserin aut DARWIN Collaboration verfasserin aut In European Physical Journal C: Particles and Fields SpringerOpen, 2017 80(2020), 9, Seite 11 (DE-627)253722934 (DE-600)1459069-4 14346052 nnns volume:80 year:2020 number:9 pages:11 https://doi.org/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 kostenfrei http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/toc/1434-6044 Journal toc kostenfrei https://doaj.org/toc/1434-6052 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 80 2020 9 11 |
| allfieldsGer |
10.1140/epjc/s10052-020-8196-z doi (DE-627)DOAJ068070187 (DE-599)DOAJ8578e145f1c346b2ac06e5a732969a72 DE-627 ger DE-627 rakwb eng QB460-466 QC770-798 F. Agostini verfasserin aut Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. Astrophysics Nuclear and particle physics. Atomic energy. Radioactivity S. E. M. Ahmed Maouloud verfasserin aut L. Althueser verfasserin aut F. Amaro verfasserin aut B. Antunovic verfasserin aut E. Aprile verfasserin aut L. Baudis verfasserin aut D. Baur verfasserin aut Y. Biondi verfasserin aut A. Bismark verfasserin aut P. A. Breur verfasserin aut A. Brown verfasserin aut G. Bruno verfasserin aut R. Budnik verfasserin aut C. Capelli verfasserin aut J. Cardoso verfasserin aut D. Cichon verfasserin aut M. Clark verfasserin aut A. P. Colijn verfasserin aut J. J. Cuenca-García verfasserin aut J. P. Cussonneau verfasserin aut M. P. Decowski verfasserin aut A. Depoian verfasserin aut J. Dierle verfasserin aut P. Di Gangi verfasserin aut A. Di Giovanni verfasserin aut S. Diglio verfasserin aut J. M. F. dos Santos verfasserin aut G. Drexlin verfasserin aut K. Eitel verfasserin aut R. Engel verfasserin aut A. D. Ferella verfasserin aut H. Fischer verfasserin aut M. Galloway verfasserin aut F. Gao verfasserin aut F. Girard verfasserin aut F. Glück verfasserin aut L. Grandi verfasserin aut R. Größle verfasserin aut R. Gumbsheimer verfasserin aut S. Hansmann-Menzemer verfasserin aut F. Jörg verfasserin aut G. Khundzakishvili verfasserin aut A. Kopec verfasserin aut F. Kuger verfasserin aut L. M. Krauss verfasserin aut H. Landsman verfasserin aut R. F. Lang verfasserin aut S. Lindemann verfasserin aut M. Lindner verfasserin aut J. A. M. Lopes verfasserin aut A. Loya Villalpando verfasserin aut C. Macolino verfasserin aut A. Manfredini verfasserin aut T. Marrodán Undagoitia verfasserin aut J. Masbou verfasserin aut E. Masson verfasserin aut P. Meinhardt verfasserin aut S. Milutinovic verfasserin aut A. Molinario verfasserin aut C. M. B. Monteiro verfasserin aut M. Murra verfasserin aut U. G. Oberlack verfasserin aut M. Pandurovic verfasserin aut R. Peres verfasserin aut J. Pienaar verfasserin aut M. Pierre verfasserin aut V. Pizzella verfasserin aut J. Qin verfasserin aut D. Ramírez García verfasserin aut S. Reichard verfasserin aut N. Rupp verfasserin aut P. Sanchez-Lucas verfasserin aut G. Sartorelli verfasserin aut D. Schulte verfasserin aut M. Schumann verfasserin aut L. Scotto Lavina verfasserin aut M. Selvi verfasserin aut M. Silva verfasserin aut H. Simgen verfasserin aut M. Steidl verfasserin aut A. Terliuk verfasserin aut C. Therreau verfasserin aut D. Thers verfasserin aut K. Thieme verfasserin aut R. Trotta verfasserin aut C. D. Tunnell verfasserin aut K. Valerius verfasserin aut G. Volta verfasserin aut D. Vorkapic verfasserin aut C. Weinheimer verfasserin aut C. Wittweg verfasserin aut J. Wolf verfasserin aut J. P. Zopounidis verfasserin aut K. Zuber verfasserin aut DARWIN Collaboration verfasserin aut In European Physical Journal C: Particles and Fields SpringerOpen, 2017 80(2020), 9, Seite 11 (DE-627)253722934 (DE-600)1459069-4 14346052 nnns volume:80 year:2020 number:9 pages:11 https://doi.org/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 kostenfrei http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/toc/1434-6044 Journal toc kostenfrei https://doaj.org/toc/1434-6052 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 80 2020 9 11 |
| allfieldsSound |
10.1140/epjc/s10052-020-8196-z doi (DE-627)DOAJ068070187 (DE-599)DOAJ8578e145f1c346b2ac06e5a732969a72 DE-627 ger DE-627 rakwb eng QB460-466 QC770-798 F. Agostini verfasserin aut Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. Astrophysics Nuclear and particle physics. Atomic energy. Radioactivity S. E. M. Ahmed Maouloud verfasserin aut L. Althueser verfasserin aut F. Amaro verfasserin aut B. Antunovic verfasserin aut E. Aprile verfasserin aut L. Baudis verfasserin aut D. Baur verfasserin aut Y. Biondi verfasserin aut A. Bismark verfasserin aut P. A. Breur verfasserin aut A. Brown verfasserin aut G. Bruno verfasserin aut R. Budnik verfasserin aut C. Capelli verfasserin aut J. Cardoso verfasserin aut D. Cichon verfasserin aut M. Clark verfasserin aut A. P. Colijn verfasserin aut J. J. Cuenca-García verfasserin aut J. P. Cussonneau verfasserin aut M. P. Decowski verfasserin aut A. Depoian verfasserin aut J. Dierle verfasserin aut P. Di Gangi verfasserin aut A. Di Giovanni verfasserin aut S. Diglio verfasserin aut J. M. F. dos Santos verfasserin aut G. Drexlin verfasserin aut K. Eitel verfasserin aut R. Engel verfasserin aut A. D. Ferella verfasserin aut H. Fischer verfasserin aut M. Galloway verfasserin aut F. Gao verfasserin aut F. Girard verfasserin aut F. Glück verfasserin aut L. Grandi verfasserin aut R. Größle verfasserin aut R. Gumbsheimer verfasserin aut S. Hansmann-Menzemer verfasserin aut F. Jörg verfasserin aut G. Khundzakishvili verfasserin aut A. Kopec verfasserin aut F. Kuger verfasserin aut L. M. Krauss verfasserin aut H. Landsman verfasserin aut R. F. Lang verfasserin aut S. Lindemann verfasserin aut M. Lindner verfasserin aut J. A. M. Lopes verfasserin aut A. Loya Villalpando verfasserin aut C. Macolino verfasserin aut A. Manfredini verfasserin aut T. Marrodán Undagoitia verfasserin aut J. Masbou verfasserin aut E. Masson verfasserin aut P. Meinhardt verfasserin aut S. Milutinovic verfasserin aut A. Molinario verfasserin aut C. M. B. Monteiro verfasserin aut M. Murra verfasserin aut U. G. Oberlack verfasserin aut M. Pandurovic verfasserin aut R. Peres verfasserin aut J. Pienaar verfasserin aut M. Pierre verfasserin aut V. Pizzella verfasserin aut J. Qin verfasserin aut D. Ramírez García verfasserin aut S. Reichard verfasserin aut N. Rupp verfasserin aut P. Sanchez-Lucas verfasserin aut G. Sartorelli verfasserin aut D. Schulte verfasserin aut M. Schumann verfasserin aut L. Scotto Lavina verfasserin aut M. Selvi verfasserin aut M. Silva verfasserin aut H. Simgen verfasserin aut M. Steidl verfasserin aut A. Terliuk verfasserin aut C. Therreau verfasserin aut D. Thers verfasserin aut K. Thieme verfasserin aut R. Trotta verfasserin aut C. D. Tunnell verfasserin aut K. Valerius verfasserin aut G. Volta verfasserin aut D. Vorkapic verfasserin aut C. Weinheimer verfasserin aut C. Wittweg verfasserin aut J. Wolf verfasserin aut J. P. Zopounidis verfasserin aut K. Zuber verfasserin aut DARWIN Collaboration verfasserin aut In European Physical Journal C: Particles and Fields SpringerOpen, 2017 80(2020), 9, Seite 11 (DE-627)253722934 (DE-600)1459069-4 14346052 nnns volume:80 year:2020 number:9 pages:11 https://doi.org/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 kostenfrei http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z kostenfrei https://doaj.org/toc/1434-6044 Journal toc kostenfrei https://doaj.org/toc/1434-6052 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 80 2020 9 11 |
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F. Agostini @@aut@@ S. E. M. Ahmed Maouloud @@aut@@ L. Althueser @@aut@@ F. Amaro @@aut@@ B. Antunovic @@aut@@ E. Aprile @@aut@@ L. Baudis @@aut@@ D. Baur @@aut@@ Y. Biondi @@aut@@ A. Bismark @@aut@@ P. A. Breur @@aut@@ A. Brown @@aut@@ G. Bruno @@aut@@ R. Budnik @@aut@@ C. Capelli @@aut@@ J. Cardoso @@aut@@ D. Cichon @@aut@@ M. Clark @@aut@@ A. P. Colijn @@aut@@ J. J. Cuenca-García @@aut@@ J. P. Cussonneau @@aut@@ M. P. Decowski @@aut@@ A. Depoian @@aut@@ J. Dierle @@aut@@ P. Di Gangi @@aut@@ A. Di Giovanni @@aut@@ S. Diglio @@aut@@ J. M. F. dos Santos @@aut@@ G. Drexlin @@aut@@ K. Eitel @@aut@@ R. Engel @@aut@@ A. D. Ferella @@aut@@ H. Fischer @@aut@@ M. Galloway @@aut@@ F. Gao @@aut@@ F. Girard @@aut@@ F. Glück @@aut@@ L. Grandi @@aut@@ R. Größle @@aut@@ R. Gumbsheimer @@aut@@ S. Hansmann-Menzemer @@aut@@ F. Jörg @@aut@@ G. Khundzakishvili @@aut@@ A. Kopec @@aut@@ F. Kuger @@aut@@ L. M. Krauss @@aut@@ H. Landsman @@aut@@ R. F. Lang @@aut@@ S. Lindemann @@aut@@ M. Lindner @@aut@@ J. A. M. Lopes @@aut@@ A. Loya Villalpando @@aut@@ C. Macolino @@aut@@ A. Manfredini @@aut@@ T. Marrodán Undagoitia @@aut@@ J. Masbou @@aut@@ E. Masson @@aut@@ P. Meinhardt @@aut@@ S. Milutinovic @@aut@@ A. Molinario @@aut@@ C. M. B. Monteiro @@aut@@ M. Murra @@aut@@ U. G. Oberlack @@aut@@ M. Pandurovic @@aut@@ R. Peres @@aut@@ J. Pienaar @@aut@@ M. Pierre @@aut@@ V. Pizzella @@aut@@ J. Qin @@aut@@ D. Ramírez García @@aut@@ S. Reichard @@aut@@ N. Rupp @@aut@@ P. Sanchez-Lucas @@aut@@ G. Sartorelli @@aut@@ D. Schulte @@aut@@ M. Schumann @@aut@@ L. Scotto Lavina @@aut@@ M. Selvi @@aut@@ M. Silva @@aut@@ H. Simgen @@aut@@ M. Steidl @@aut@@ A. Terliuk @@aut@@ C. Therreau @@aut@@ D. Thers @@aut@@ K. Thieme @@aut@@ R. Trotta @@aut@@ C. D. Tunnell @@aut@@ K. Valerius @@aut@@ G. Volta @@aut@@ D. Vorkapic @@aut@@ C. Weinheimer @@aut@@ C. Wittweg @@aut@@ J. Wolf @@aut@@ J. P. Zopounidis @@aut@@ K. Zuber @@aut@@ DARWIN Collaboration @@aut@@ |
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F. Agostini |
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F. Agostini misc QB460-466 misc QC770-798 misc Astrophysics misc Nuclear and particle physics. Atomic energy. Radioactivity Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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QB460-466 QC770-798 Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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misc QB460-466 misc QC770-798 misc Astrophysics misc Nuclear and particle physics. Atomic energy. Radioactivity |
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Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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F. Agostini |
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European Physical Journal C: Particles and Fields |
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European Physical Journal C: Particles and Fields |
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F. Agostini S. E. M. Ahmed Maouloud L. Althueser F. Amaro B. Antunovic E. Aprile L. Baudis D. Baur Y. Biondi A. Bismark P. A. Breur A. Brown G. Bruno R. Budnik C. Capelli J. Cardoso D. Cichon M. Clark A. P. Colijn J. J. Cuenca-García J. P. Cussonneau M. P. Decowski A. Depoian J. Dierle P. Di Gangi A. Di Giovanni S. Diglio J. M. F. dos Santos G. Drexlin K. Eitel R. Engel A. D. Ferella H. Fischer M. Galloway F. Gao F. Girard F. Glück L. Grandi R. Größle R. Gumbsheimer S. Hansmann-Menzemer F. Jörg G. Khundzakishvili A. Kopec F. Kuger L. M. Krauss H. Landsman R. F. Lang S. Lindemann M. Lindner J. A. M. Lopes A. Loya Villalpando C. Macolino A. Manfredini T. Marrodán Undagoitia J. Masbou E. Masson P. Meinhardt S. Milutinovic A. Molinario C. M. B. Monteiro M. Murra U. G. Oberlack M. Pandurovic R. Peres J. Pienaar M. Pierre V. Pizzella J. Qin D. Ramírez García S. Reichard N. Rupp P. Sanchez-Lucas G. Sartorelli D. Schulte M. Schumann L. Scotto Lavina M. Selvi M. Silva H. Simgen M. Steidl A. Terliuk C. Therreau D. Thers K. Thieme R. Trotta C. D. Tunnell K. Valerius G. Volta D. Vorkapic C. Weinheimer C. Wittweg J. Wolf J. P. Zopounidis K. Zuber DARWIN Collaboration |
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QB460-466 QC770-798 |
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Elektronische Aufsätze |
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F. Agostini |
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10.1140/epjc/s10052-020-8196-z |
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verfasserin |
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sensitivity of the darwin observatory to the neutrinoless double beta decay of $$^{136}$$ 136 xe |
| callnumber |
QB460-466 |
| title_auth |
Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
| abstract |
Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. |
| abstractGer |
Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. |
| abstract_unstemmed |
Abstract The DARWIN observatory is a proposed next-generation experiment to search for particle dark matter and for the neutrinoless double beta decay of $$^{136}$$ 136 Xe. Out of its 50 t total natural xenon inventory, 40 t will be the active target of a time projection chamber which thus contains about 3.6 t of $$^{136}$$ 136 Xe. Here, we show that its projected half-life sensitivity is $$2.4\times {10}^{27}\,{\hbox {year}}$$ 2.4×1027year , using a fiducial volume of 5 t of natural xenon and 10 year of operation with a background rate of less than 0.2 events/(t $$\cdot $$ · year) in the energy region of interest. This sensitivity is based on a detailed Monte Carlo simulation study of the background and event topologies in the large, homogeneous target. DARWIN will be comparable in its science reach to dedicated double beta decay experiments using xenon enriched in $$^{136}$$ 136 Xe. |
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Sensitivity of the DARWIN observatory to the neutrinoless double beta decay of $$^{136}$$ 136 Xe |
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https://doi.org/10.1140/epjc/s10052-020-8196-z https://doaj.org/article/8578e145f1c346b2ac06e5a732969a72 http://link.springer.com/article/10.1140/epjc/s10052-020-8196-z https://doaj.org/toc/1434-6044 https://doaj.org/toc/1434-6052 |
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S. E. M. Ahmed Maouloud L. Althueser F. Amaro B. Antunovic E. Aprile L. Baudis D. Baur Y. Biondi A. Bismark P. A. Breur A. Brown G. Bruno R. Budnik C. Capelli J. Cardoso D. Cichon M. Clark A. P. Colijn J. J. Cuenca-García J. P. Cussonneau M. P. Decowski A. Depoian J. Dierle P. Di Gangi A. Di Giovanni S. Diglio J. M. F. dos Santos G. Drexlin K. Eitel R. Engel A. D. Ferella H. Fischer M. Galloway F. Gao F. Girard F. Glück L. Grandi R. Größle R. Gumbsheimer S. Hansmann-Menzemer F. Jörg G. Khundzakishvili A. Kopec F. Kuger L. M. Krauss H. Landsman R. F. Lang S. Lindemann M. Lindner J. A. M. Lopes A. Loya Villalpando C. Macolino A. Manfredini T. Marrodán Undagoitia J. Masbou E. Masson P. Meinhardt S. Milutinovic A. Molinario C. M. B. Monteiro M. Murra U. G. Oberlack M. Pandurovic R. Peres J. Pienaar M. Pierre V. Pizzella J. Qin D. Ramírez García S. Reichard N. Rupp P. Sanchez-Lucas G. Sartorelli D. Schulte M. Schumann L. Scotto Lavina M. Selvi M. Silva H. Simgen M. Steidl A. Terliuk C. Therreau D. Thers K. Thieme R. Trotta C. D. Tunnell K. Valerius G. Volta D. Vorkapic C. Weinheimer C. Wittweg J. Wolf J. P. Zopounidis K. Zuber DARWIN Collaboration |
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S. E. M. Ahmed Maouloud L. Althueser F. Amaro B. Antunovic E. Aprile L. Baudis D. Baur Y. Biondi A. Bismark P. A. Breur A. Brown G. Bruno R. Budnik C. Capelli J. Cardoso D. Cichon M. Clark A. P. Colijn J. J. Cuenca-García J. P. Cussonneau M. P. Decowski A. Depoian J. Dierle P. Di Gangi A. Di Giovanni S. Diglio J. M. F. dos Santos G. Drexlin K. Eitel R. Engel A. D. Ferella H. Fischer M. Galloway F. Gao F. Girard F. Glück L. Grandi R. Größle R. Gumbsheimer S. Hansmann-Menzemer F. Jörg G. Khundzakishvili A. Kopec F. Kuger L. M. Krauss H. Landsman R. F. Lang S. Lindemann M. Lindner J. A. M. Lopes A. Loya Villalpando C. Macolino A. Manfredini T. Marrodán Undagoitia J. Masbou E. Masson P. Meinhardt S. Milutinovic A. Molinario C. M. B. Monteiro M. Murra U. G. Oberlack M. Pandurovic R. Peres J. Pienaar M. Pierre V. Pizzella J. Qin D. Ramírez García S. Reichard N. Rupp P. Sanchez-Lucas G. Sartorelli D. Schulte M. Schumann L. Scotto Lavina M. Selvi M. Silva H. Simgen M. Steidl A. Terliuk C. Therreau D. Thers K. Thieme R. Trotta C. D. Tunnell K. Valerius G. Volta D. Vorkapic C. Weinheimer C. Wittweg J. Wolf J. P. Zopounidis K. Zuber DARWIN Collaboration |
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2024-07-03T15:42:48.114Z |
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