Author: "U Oberlack" / Search Limiters: Available in Library Collection - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"U Oberlack"' showing total 47 results

Start Over Author "U Oberlack" Search Limiters Available in Library Collection

47 results on '"U Oberlack"'

1. The XENONnT dark matter experiment

Author: XENON Collaboration, E. Aprile, J. Aalbers, K. Abe, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, M. Balata, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, G. Bruno, R. Budnik, T. K. Bui, C. Cai, J. M. R. Cardoso, F. Cassese, A. Chiarini, D. Cichon, A. P. Cimental Chavez, A. P. Colijn, J. Conrad, R. Corrieri, J. J. Cuenca-García, J. P. Cussonneau, O. Dadoun, V. D’Andrea, M. P. Decowski, B. De Fazio, P. Di Gangi, S. Diglio, J. M. Disdier, D. Douillet, K. Eitel, A. Elykov, S. Farrell, A. D. Ferella, C. Ferrari, H. Fischer, M. Flierman, S. Form, D. Front, W. Fulgione, C. Fuselli, P. Gaemers, R. Gaior, A. Gallo Rosso, M. Galloway, F. Gao, R. Gardner, N. Garroum, R. Glade-Beucke, L. Grandi, J. Grigat, H. Guan, M. Guerzoni, M. Guida, R. Hammann, A. Higuera, C. Hils, L. Hoetzsch, N. F. Hood, J. Howlett, C. Huhmann, M. Iacovacci, G. Iaquaniello, L. Iven, Y. Itow, J. Jakob, F. Joerg, A. Joy, M. Kara, P. Kavrigin, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, F. Kuger, H. Landsman, R. F. Lang, L. Levinson, I. Li, S. Li, S. Liang, S. Lindemann, M. Lindner, K. Liu, J. Loizeau, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, F. Marignetti, T. Marrodán Undagoitia, P. Martella, K. Martens, J. Masbou, D. Masson, E. Masson, S. Mastroianni, E. Mele, M. Messina, R. Michinelli, K. Miuchi, A. Molinario, S. Moriyama, K. Morå, Y. Mosbacher, M. Murra, J. Müller, K. Ni, S. Nisi, U. Oberlack, D. Orlandi, R. Othegraven, B. Paetsch, J. Palacio, S. Parlati, P. Paschos, Q. Pellegrini, R. Peres, C. Peters, J. Pienaar, M. Pierre, G. Plante, T. R. Pollmann, J. Qi, J. Qin, D. Ramírez García, M. Rynge, J. Shi, R. Singh, L. Sanchez, J. M. F. dos Santos, I. Sarnoff, G. Sartorelli, J. Schreiner, D. Schulte, P. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, S. Shi, E. Shockley, M. Silva, H. Simgen, J. Stephen, M. Stern, B. K. Stillwell, A. Takeda, P.-L. Tan, D. Tatananni, A. Terliuk, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, F. Tönnies, K. Valerius, G. Volta, C. Weinheimer, M. Weiss, D. Wenz, J. Westermann, C. Wittweg, T. Wolf, V. H. S. Wu, Y. Xing, D. Xu, Z. Xu, M. Yamashita, L. Yang, J. Ye, L. Yuan, G. Zavattini, M. Zhong, and T. Zhu
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The multi-staged XENON program at INFN Laboratori Nazionali del Gran Sasso aims to detect dark matter with two-phase liquid xenon time projection chambers of increasing size and sensitivity. The XENONnT experiment is the latest detector in the program, planned to be an upgrade of its predecessor XENON1T. It features an active target of 5.9 tonnes of cryogenic liquid xenon (8.5 tonnes total mass in cryostat). The experiment is expected to extend the sensitivity to WIMP dark matter by more than an order of magnitude compared to XENON1T, thanks to the larger active mass and the significantly reduced background, improved by novel systems such as a radon removal plant and a neutron veto. This article describes the XENONnT experiment and its sub-systems in detail and reports on the detector performance during the first science run.
Published: 2024
Full Text: View/download PDF

2. Low-energy calibration of XENON1T with an internal $$^{{\textbf {37}}}$$ 37 Ar source

Author: E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, R. Budnik, T. K. Bui, C. Cai, C. Capelli, J. M. R. Cardoso, D. Cichon, A. P. Colijn, J. Conrad, J. J. Cuenca-García, J. P. Cussonneau, V. D’Andrea, M. P. Decowski, P. Di Gangi, S. Di Pede, S. Diglio, K. Eitel, A. Elykov, S. Farrell, A. D. Ferella, C. Ferrari, H. Fischer, W. Fulgione, P. Gaemers, R. Gaior, A. Gallo Rosso, M. Galloway, F. Gao, R. Glade-Beucke, L. Grandi, J. Grigat, M. Guida, R. Hammann, A. Higuera, C. Hils, L. Hoetzsch, J. Howlett, M. Iacovacci, Y. Itow, J. Jakob, F. Joerg, A. Joy, N. Kato, M. Kara, P. Kavrigin, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, F. Kuger, H. Landsman, R. F. Lang, L. Levinson, I. Li, S. Li, S. Liang, S. Lindemann, M. Lindner, K. Liu, J. Loizeau, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, E. Masson, S. Mastroianni, M. Messina, K. Miuchi, K. Mizukoshi, A. Molinario, S. Moriyama, K. Morå, Y. Mosbacher, M. Murra, J. Müller, K. Ni, U. Oberlack, B. Paetsch, J. Palacio, R. Peres, C. Peters, J. Pienaar, M. Pierre, V. Pizzella, G. Plante, J. Qi, J. Qin, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, L. Sanchez, P. Sanchez-Lucas, J. M. F. dos Santos, I. Sarnoff, G. Sartorelli, J. Schreiner, D. Schulte, P. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, S. Shi, E. Shockley, M. Silva, H. Simgen, A. Takeda, P.-L. Tan, A. Terliuk, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, F. Tönnies, K. Valerius, G. Volta, C. Weinheimer, M. Weiss, D. Wenz, C. Wittweg, T. Wolf, D. Xu, Z. Xu, M. Yamashita, L. Yang, J. Ye, L. Yuan, G. Zavattini, S. Zerbo, M. Zhong, T. Zhu, C. Geppert, J. Riemer, and XENON Collaboration
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract A low-energy electronic recoil calibration of XENON1T, a dual-phase xenon time projection chamber, with an internal $${}^{37}$$ 37 Ar source was performed. This calibration source features a 35-day half-life and provides two mono-energetic lines at 2.82 keV and 0.27 keV. The photon yield and electron yield at 2.82 keV are measured to be ( $$32.3\,\pm \,0.3$$ 32.3 ± 0.3 ) photons/keV and ( $$40.6\,\pm \,0.5$$ 40.6 ± 0.5 ) electrons/keV, respectively, in agreement with other measurements and with NEST predictions. The electron yield at 0.27 keV is also measured and it is ( $$68.0^{+6.3}_{-3.7}$$ 68 . 0 - 3.7 + 6.3 ) electrons/keV. The $${}^{37}$$ 37 Ar calibration confirms that the detector is well-understood in the energy region close to the detection threshold, with the 2.82 keV line reconstructed at ( $$2.83\,\pm \,0.02$$ 2.83 ± 0.02 ) keV, which further validates the model used to interpret the low-energy electronic recoil excess previously reported by XENON1T. The ability to efficiently remove argon with cryogenic distillation after the calibration proves that $${}^{37}$$ 37 Ar can be considered as a regular calibration source for multi-tonne xenon detectors.
Published: 2023
Full Text: View/download PDF

3. An approximate likelihood for nuclear recoil searches with XENON1T data

Author: E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, B. Cimmino, M. Clark, A. P. Colijn, J. Conrad, J. J. Cuenca-García, J. P. Cussonneau, V. D’Andrea, M. P. Decowski, P. Di Gangi, S. Di Pede, A. Di Giovanni, R. Di Stefano, S. Diglio, A. Elykov, S. Farrell, A. D. Ferella, H. Fischer, W. Fulgione, P. Gaemers, R. Gaior, M. Galloway, F. Gao, R. Glade-Beucke, L. Grandi, J. Grigat, A. Higuera, C. Hils, L. Hoetzsch, J. Howlett, M. Iacovacci, Y. Itow, J. Jakob, F. Joerg, A. Joy, N. Kato, P. Kavrigin, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, I. Li, S. Li, S. Liang, S. Lindemann, M. Lindner, K. Liu, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, E. Masson, S. Mastroianni, M. Messina, K. Miuchi, K. Mizukoshi, A. Molinario, S. Moriyama, K. Morå, Y. Mosbacher, M. Murra, J. Müller, K. Ni, U. Oberlack, B. Paetsch, J. Palacio, R. Peres, J. Pienaar, M. Pierre, V. Pizzella, G. Plante, J. Qi, J. Qin, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, L. Sanchez, J. M. F. dos Santos, G. Sartorelli, J. Schreiner, D. Schulte, P. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, S. Shi, E. Shockley, M. Silva, H. Simgen, A. Takeda, P. L. Tan, A. Terliuk, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, F. Tönnies, K. Valerius, G. Volta, Y. Wei, C. Weinheimer, M. Weiss, D. Wenz, C. Wittweg, T. Wolf, Z. Xu, M. Yamashita, L. Yang, J. Ye, L. Yuan, G. Zavattini, Y. Zhang, M. Zhong, T. Zhu, and XENON Collaboration
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The XENON collaboration has published stringent limits on specific dark matter – nucleon recoil spectra from dark matter recoiling on the liquid xenon detector target. In this paper, we present an approximate likelihood for the XENON1T 1 t-year nuclear recoil search applicable to any nuclear recoil spectrum. Alongside this paper, we publish data and code to compute upper limits using the method we present. The approximate likelihood is constructed in bins of reconstructed energy, profiled along the signal expectation in each bin. This approach can be used to compute an approximate likelihood and therefore most statistical results for any nuclear recoil spectrum. Computing approximate results with this method is approximately three orders of magnitude faster than the likelihood used in the original publications of XENON1T, where limits were set for specific families of recoil spectra. Using this same method, we include toy Monte Carlo simulation-derived binwise likelihoods for the upcoming XENONnT experiment that can similarly be used to assess the sensitivity to arbitrary nuclear recoil signatures in its eventual 20 t-year exposure.
Published: 2022
Full Text: View/download PDF

4. Material radiopurity control in the XENONnT experiment

Author: E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, B. Cimmino, M. Clark, A. P. Colijn, J. Conrad, J. J. Cuenca-García, J. P. Cussonneau, V. D’Andrea, M. P. Decowski, P. Di Gangi, S. Di Pede, A. Di Giovanni, R. Di Stefano, S. Diglio, A. Elykov, S. Farrell, A. D. Ferella, H. Fischer, W. Fulgione, P. Gaemers, R. Gaior, M. Galloway, F. Gao, R. Glade-Beucke, L. Grandi, J. Grigat, A. Higuera, C. Hils, K. Hiraide, L. Hoetzsch, J. Howlett, M. Iacovacci, Y. Itow, J. Jakob, F. Joerg, N. Kato, P. Kavrigin, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, I. Li, S. Liang, S. Lindemann, M. Lindner, K. Liu, F. Lombardi, J. Long, J. A. M. Lopes, Y. Ma, C. Macolino, J. Mahlstedt, A. Mancuso, L. Manenti, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, E. Masson, S. Mastroianni, M. Messina, K. Miuchi, K. Mizukoshi, A. Molinario, S. Moriyama, K. Morå, Y. Mosbacher, M. Murra, K. Ni, U. Oberlack, J. Palacio, R. Peres, J. Pienaar, M. Pierre, V. Pizzella, G. Plante, J. Qi, J. Qin, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, L. Sanchez, J. M. F. dos Santos, G. Sartorelli, J. Schreiner, D. Schulte, H. Schulze Eißing, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, E. Shockley, M. Silva, H. Simgen, A. Takeda, P. L. Tan, A. Terliuk, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, F. Tönnies, K. Valerius, G. Volta, Y. Wei, C. Weinheimer, M. Weiss, D. Wenz, J. Westermann, C. Wittweg, T. Wolf, Z. Xu, M. Yamashita, L. Yang, J. Ye, L. Yuan, G. Zavattini, Y. Zhang, M. Zhong, T. Zhu, J. P. Zopounidis, XENON Collaboration, M. Laubenstein, and S. Nisi
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The selection of low-radioactive construction materials is of the utmost importance for rare-event searches and thus critical to the XENONnT experiment. Results of an extensive radioassay program are reported, in which material samples have been screened with gamma-ray spectroscopy, mass spectrometry, and $$^{222}$$ 222 Rn emanation measurements. Furthermore, the cleanliness procedures applied to remove or mitigate surface contamination of detector materials are described. Screening results, used as inputs for a XENONnT Monte Carlo simulation, predict a reduction of materials background ( $$\sim $$ ∼ 17%) with respect to its predecessor XENON1T. Through radon emanation measurements, the expected $$^{222}$$ 222 Rn activity concentration in XENONnT is determined to be 4.2 ( $$^{+0.5}_{-0.7}$$ - 0.7 + 0.5 ) $$\upmu $$ μ Bq/kg, a factor three lower with respect to XENON1T. This radon concentration will be further suppressed by means of the novel radon distillation system.
Published: 2022
Full Text: View/download PDF

5. $$^{222}$$ 222 Rn emanation measurements for the XENON1T experiment

Author: XENON Collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, B. Cimmino, M. Clark, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, A. Depoian, P. Di Gangi, A. Di Giovanni, R. Di Stefano, S. Diglio, A. Elykov, G. Eurin, A. D. Ferella, W. Fulgione, P. Gaemers, R. Gaior, A. Gallo Rosso, M. Galloway, F. Gao, L. Grandi, M. Garbini, C. Hasterok, C. Hils, K. Hiraide, L. Hoetzsch, E. Hogenbirk, J. Howlett, M. Iacovacci, Y. Itow, F. Joerg, N. Kato, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J. A. M. Lopes, E. López Fune, C. Macolino, J. Mahlstedt, L. Manenti, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, S. Mastroianni, M. Messina, K. Miuchi, A. Molinario, K. Morå, S. Moriyama, Y. Mosbacher, M. Murra, J. Naganoma, K. Ni, U. Oberlack, K. Odgers, J. Palacio, B. Pelssers, R. Peres, J. Pienaar, V. Pizzella, G. Plante, J. Qin, H. Qiu, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, J. M. F. dos Santos, G. Sartorelli, N. Šarčević, M. Scheibelhut, S. Schindler, J. Schreiner, D. Schulte, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, E. Shockley, M. Silva, H. Simgen, A. Takeda, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, M. Vargas, G. Volta, O. Wack, H. Wang, Y. Wei, C. Weinheimer, M. Weiss, D. Wenz, J. Westermann, C. Wittweg, J. Wulf, Z. Xu, M. Yamashita, J. Ye, G. Zavattini, Y. Zhang, T. Zhu, and J. P. Zopounidis
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The selection of low-radioactive construction materials is of utmost importance for the success of low-energy rare event search experiments. Besides radioactive contaminants in the bulk, the emanation of radioactive radon atoms from material surfaces attains increasing relevance in the effort to further reduce the background of such experiments. In this work, we present the $$^{222}$$ 222 Rn emanation measurements performed for the XENON1T dark matter experiment. Together with the bulk impurity screening campaign, the results enabled us to select the radio-purest construction materials, targeting a $$^{222}$$ 222 Rn activity concentration of $$10\,\mathrm{\,}\upmu \mathrm{Bq}/\mathrm{kg}$$ 10 μ Bq / kg in $$3.2\,\mathrm{t}$$ 3.2 t of xenon. The knowledge of the distribution of the $$^{222}$$ 222 Rn sources allowed us to selectively eliminate problematic components in the course of the experiment. The predictions from the emanation measurements were compared to data of the $$^{222}$$ 222 Rn activity concentration in XENON1T. The final $$^{222}$$ 222 Rn activity concentration of $$(4.5\pm 0.1)\,\mathrm{\,}\upmu \mathrm{Bq}/\mathrm{kg}$$ ( 4.5 ± 0.1 ) μ Bq / kg in the target of XENON1T is the lowest ever achieved in a xenon dark matter experiment.
Published: 2021
Full Text: View/download PDF

6. Energy resolution and linearity of XENON1T in the MeV energy range

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, B. Cimmino, M. Clark, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, A. Depoian, P. Di Gangi, A. Di Giovanni, R. Di Stefano, S. Diglio, A. Elykov, G. Eurin, A. D. Ferella, W. Fulgione, P. Gaemers, R. Gaior, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, L. Grandi, C. Hasterok, C. Hils, K. Hiraide, L. Hoetzsch, E. Hogenbirk, J. Howlett, M. Iacovacci, Y. Itow, F. Joerg, N. Kato, S. Kazama, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J. A. M. Lopes, E. López Fune, C. Macolino, J. Mahlstedt, L. Manenti, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, K. Martens, J. Masbou, D. Masson, S. Mastroianni, M. Messina, K. Miuchi, A. Molinario, K. Morå, S. Moriyama, Y. Mosbacher, M. Murra, J. Naganoma, K. Ni, U. Oberlack, K. Odgers, J. Palacio, B. Pelssers, R. Peres, J. Pienaar, V. Pizzella, G. Plante, J. Qin, H. Qiu, D. Ramírez García, S. Reichard, A. Rocchetti, N. Rupp, J. M. F. dos Santos, G. Sartorelli, N. Šarčević, M. Scheibelhut, S. Schindler, J. Schreiner, D. Schulte, M. Schumann, L. Scotto Lavina, M. Selvi, F. Semeria, P. Shagin, E. Shockley, M. Silva, H. Simgen, A. Takeda, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, M. Vargas, G. Volta, O. Wack, H. Wang, Y. Wei, C. Weinheimer, M. Weiss Xu, D. Wenz, C. Wittweg, J. Wulf, Z. Xu, M. Yamashita, J. Ye, G. Zavattini, Y. Zhang, T. Zhu, and J. P. Zopounidis
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract Xenon dual-phase time projection chambers designed to search for weakly interacting massive particles have so far shown a relative energy resolution which degrades with energy above $$\sim $$ ∼ 200 keV due to the saturation effects. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of $$^{136} \hbox {Xe}$$ 136Xe at its Q value, $$Q_{\beta \beta }\simeq 2.46\,\hbox {MeV}$$ Qββ≃2.46MeV . For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at $$1\,\sigma /\mu $$ 1σ/μ is as low as ($$0.80 \pm 0.02$$ 0.80±0.02 ) % in its one-ton fiducial mass, and for single-site interactions at $$Q_{\beta \beta }$$ Qββ . We also present a new signal correction method to rectify the saturation effects of the signal readout system, resulting in more accurate position reconstruction and indirectly improving the energy resolution. The very good result achieved in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events.
Published: 2020
Full Text: View/download PDF

7. Intrinsic backgrounds from Rn and Kr in the XENON100 experiment

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. Calvén, J. M. R. Cardoso, M. Cervantes, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, C. Geis, L. W. Goetzke, Z. Greene, C. Grignon, C. Hasterok, E. Hogenbirk, R. Itay, B. Kaminsky, S. Kazama, G. Kessler, A. Kish, H. Landsman, R. F. Lang, D. Lellouch, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J. A. M. Lopes, A. Manfredini, I. Maris, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, M. Messina, K. Micheneau, A. Molinario, K. Morå, M. Murra, J. Naganoma, K. Ni, U. Oberlack, P. Pakarha, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, M.-C. Piro, V. Pizzella, G. Plante, N. Priel, D. Ramírez García, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, N. Rupp, J. M. F. dos Santos, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, M. Silva, H. Simgen, M. Von Sivers, A. Stein, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, M. Vargas, H. Wang, Z. Wang, M. Weber, Y. Wei, C. Weinheimer, C. Wittweg, J. Wulf, J. Ye, Y. Zhang, and XENON Collaboration
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract In this paper, we describe the XENON100 data analyses used to assess the target-intrinsic background sources radon ( ), thoron ( ) and krypton ( ). We detail the event selections of high-energy alpha particles and decay-specific delayed coincidences. We derive distributions of the individual radionuclides inside the detector and quantify their abundances during the main three science runs of the experiment over a period of $$\sim 4\,\hbox {years}$$ ∼4years , from January 2010 to January 2014. We compare our results to external measurements of radon emanation and krypton concentrations where we find good agreement. We report an observed reduction in concentrations of radon daughters that we attribute to the plating-out of charged ions on the negatively biased cathode.
Published: 2018
Full Text: View/download PDF

8. Material radioassay and selection for the XENON1T dark matter experiment

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. Calvén, J. M. R. Cardoso, M. Cervantes, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, D. Franco, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, C. Geis, L. W. Goetzke, L. Grandi, Z. Greene, C. Grignon, C. Hasterok, E. Hogenbirk, R. Itay, B. Kaminsky, G. Kessler, A. Kish, H. Landsman, R. F. Lang, D. Lellouch, L. Levinson, M. Le Calloch, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lopes, A. Manfredini, I. Maris, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, M. Messina, K. Micheneau, B. Miguez, A. Molinario, M. Murra, J. Naganoma, K. Ni, U. Oberlack, P. Pakarha, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, M.-C. Piro, V. Pizzella, G. Plante, N. Priel, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, N. Rupp, R. Saldanha, J. M. F. dos Santos, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, M. v. Sivers, A. Stein, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, N. Upole, H. Wang, Y. Wei, C. Weinheimer, J. Wulf, J. Ye, Y. Zhang, M. Laubenstein, S. Nisi, and XENON Collaboration
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The XENON1T dark matter experiment aims to detect weakly interacting massive particles (WIMPs) through low-energy interactions with xenon atoms. To detect such a rare event necessitates the use of radiopure materials to minimize the number of background events within the expected WIMP signal region. In this paper we report the results of an extensive material radioassay campaign for the XENON1T experiment. Using gamma-ray spectroscopy and mass spectrometry techniques, systematic measurements of trace radioactive impurities in over one hundred samples within a wide range of materials were performed. The measured activities allowed for stringent selection and placement of materials during the detector construction phase and provided the input for XENON1T detection sensitivity estimates through Monte Carlo simulations.
Published: 2017
Full Text: View/download PDF

9. The XENON1T dark matter experiment

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, B. Antunes, F. Arneodo, M. Balata, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, A. Breskin, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. Calvén, J. M. R. Cardoso, M. Cervantes, A. Chiarini, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, R. Corrieri, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, J.-M. Disdier, M. Doets, E. Duchovni, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, D. Franco, D. Front, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, C. Geis, K.-L. Giboni, L. W. Goetzke, L. Grandi, Z. Greene, C. Grignon, C. Hasterok, E. Hogenbirk, C. Huhmann, R. Itay, A. James, B. Kaminsky, S. Kazama, G. Kessler, A. Kish, H. Landsman, R. F. Lang, D. Lellouch, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J. A. M. Lopes, R. Maier, A. Manfredini, I. Maris, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, M. Messina, K. Micheneau, A. Molinario, K. Morå, M. Murra, J. Naganoma, K. Ni, U. Oberlack, D. Orlandi, R. Othegraven, P. Pakarha, S. Parlati, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, V. Pizzella, M.-C. Piro, G. Plante, N. Priel, D. Ramírez García, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, N. Rupp, J. M. F. dos Santos, R. Saldanha, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, M. v. Sivers, M. Stern, A. Stein, D. Tatananni, L. Tatananni, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, N. Upole, M. Vargas, O. Wack, R. Walet, H. Wang, Z. Wang, Y. Wei, C. Weinheimer, C. Wittweg, J. Wulf, J. Ye, Y. Zhang, and XENON Collaboration
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The XENON1T experiment at the Laboratori Nazionali del Gran Sasso (LNGS) is the first WIMP dark matter detector operating with a liquid xenon target mass above the ton-scale. Out of its 3.2 t liquid xenon inventory, 2.0 t constitute the active target of the dual-phase time projection chamber. The scintillation and ionization signals from particle interactions are detected with low-background photomultipliers. This article describes the XENON1T instrument and its subsystems as well as strategies to achieve an unprecedented low background level. First results on the detector response and the performance of the subsystems are also presented.
Published: 2017
Full Text: View/download PDF

10. Online $$^{222}$$ 222 Rn removal by cryogenic distillation in the XENON100 experiment

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. Calvén, J. M. R. Cardoso, M. Cervantes, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, E. Duchovni, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, D. Franco, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, C. Geis, L. W. Goetzke, L. Grandi, Z. Greene, C. Grignon, C. Hasterok, E. Hogenbirk, R. Itay, B. Kaminsky, G. Kessler, A. Kish, H. Landsman, R. F. Lang, D. Lellouch, L. Levinson, M. Le Calloch, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lopes, A. Manfredini, I. Maris, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, Y. Meng, M. Messina, K. Micheneau, B. Miguez, A. Molinario, M. Murra, J. Naganoma, K. Ni, U. Oberlack, S. E. A. Orrigo, P. Pakarha, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, M.-C. Piro, V. Pizzella, G. Plante, N. Priel, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, N. Rupp, R. Saldanha, J. M. F. dos Santos, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, M. v. Sivers, A. Stein, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, N. Upole, H. Wang, Y. Wei, C. Weinheimer, J. Wulf, J. Ye, Y. Zhang, XENON Collaboration, and I. Cristescu
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We describe the purification of xenon from traces of the radioactive noble gas radon using a cryogenic distillation column. The distillation column was integrated into the gas purification loop of the XENON100 detector for online radon removal. This enabled us to significantly reduce the constant $$^{222}$$ 222 Rn background originating from radon emanation. After inserting an auxiliary $$^{222}$$ 222 Rn emanation source in the gas loop, we determined a radon reduction factor of $$R\,>\,27$$ R > 27 (95% C.L.) for the distillation column by monitoring the $$^{222}$$ 222 Rn activity concentration inside the XENON100 detector.
Published: 2017
Full Text: View/download PDF

11. Removing krypton from xenon by cryogenic distillation to the ppq level

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. Calvén, J. M. R. Cardoso, M. Cervantes, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, E. Duchovni, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, D. Franco, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, C. Geis, L. W. Goetzke, L. Grandi, Z. Greene, C. Grignon, C. Hasterok, E. Hogenbirk, C. Huhmann, R. Itay, B. Kaminsky, G. Kessler, A. Kish, H. Landsman, R. F. Lang, D. Lellouch, L. Levinson, M. Le Calloch, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lopes, A. Manfredini, I. Maris, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, Y. Meng, M. Messina, K. Micheneau, B. Miguez, A. Molinario, M. Murra, J. Naganoma, K. Ni, U. Oberlack, S. E. A. Orrigo, P. Pakarha, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, M.-C. Piro, V. Pizzella, G. Plante, N. Priel, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, N. Rupp, R. Saldanha, J. M. F. dos Santos, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, M. v. Sivers, A. Stein, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, N. Upole, H. Wang, Y. Wei, C. Weinheimer, J. Wulf, J. Ye, Y. Zhang, I. Cristescu, and XENON Collaboration
Subjects: Xenon, Krypton, Distillation Column, Weakly Interact Massive Particle, Liquid Xenon, Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The XENON1T experiment aims for the direct detection of dark matter in a detector filled with 3.3 tons of liquid xenon. In order to achieve the desired sensitivity, the background induced by radioactive decays inside the detector has to be sufficiently low. One major contributor is the $$\beta $$ β -emitter $$^{85}$$ 85 Kr which is present in the xenon. For XENON1T a concentration of natural krypton in xenon $$\mathrm {^{nat}\mathrm{Kr/Xe}\,
Published: 2017
Full Text: View/download PDF

12. All-Sky-ASTROGAM: a MeV Companion for Multimessenger Astrophysics

Author: Sandro Mereghetti, P. von Balmoos, A. Morselli, R. Walter, A. M. Bykov, G. Ambrosi, Vincent Tatischeff, Irfan Kuvvetli, Lorraine Hanlon, Valentina Fioretti, A. A. Zdziarski, D. Bastieri, M. Mallamaci, Gottfried Kanbach, M. Tavani, S. Brandt, I. A. Grenier, A. De Angelis, A. Argan, P. Laurent, R. Rando, J. Mc Enery, Andrea Bulgarelli, U. Oberlack, Elisa Bernardini, E. Prandini, R. M. Curado da Silva, Koji Nakazawa, M. Hernanz, Andreas Zoglauer, J. Rico, Mosè Mariotti, Mark Pearce, D. H. Hartmann, Mn Mazziotta, Xin Wu, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), All-Sky-ASTROGAM, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Physics, Scintillation, Range (particle radiation), COSMIC cancer database, Calorimeter (particle physics), 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Compton scattering, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Occultation, Sky, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], media_common
Abstract: International audience; In the era of multi-messenger astronomy it is of paramount importance to have in space a gamma-ray monitor capable of detecting energetic transients in the energy range from 0.1 MeV to a few hundred MeV, with good imaging capabilities. The All-Sky-ASTROGAM mission proposal aims to place into an L2 orbit a gamma-ray instrument ($\sim$ 100 kg) dedicated to fast detection, localization, and gamma-ray spectroscopy of flaring and merging activity of compact objects in the Universe, with unprecedented sensitivity and polarimetric capability in the MeV range. The instrument is based on the ASTROGAM concept, which combines three detection systems of space-proven technology: a silicon tracker in which the cosmic gamma rays undergo Compton scattering or a pair conversion, a scintillation calorimeter to absorb and measure the energy of the secondary particles, and an anticoincidence system to veto the prompt reaction background induced by charged particles. The gamma-ray imager and the platform will be connected through a boom and will have almost no occultation, making possible a continuous monitoring of every single gamma-ray source in the sky during the entire mission lifetime.
Published: 2019
Full Text: View/download PDF

13. The XENON1T Data Acquisition System

Author: E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F.D. Amaro, V.C. Antochi, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M.L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, C. Capelli, J.M.R. Cardoso, D. Cichon, D. Coderre, A.P. Colijn, J. Conrad, J.P. Cussonneau, M.P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, A. Elykov, G. Eurin, J. Fei, A.D. Ferella, A. Fieguth, W. Fulgione, P. Gaemers, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, L. Grandi, Z. Greene, C. Hasterok, E. Hogenbirk, J. Howlett, M. Iacovacci, R. Itay, F. Joerg, S. Kazama, A. Kish, M. Kobayashi, G. Koltman, A. Kopec, H. Landsman, R.F. Lang, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J.A.M. Lopes, E. López Fune, C. Macolino, J. Mahlstedt, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, J. Masbou, D. Masson, S. Mastroianni, M. Messina, K. Micheneau, K. Miller, A. Molinario, K. Morå, Y. Mosbacher, M. Murra, J. Naganoma, K. Ni, U. Oberlack, K. Odgers, B. Pelssers, R. Peres, F. Piastra, J. Pienaar, V. Pizzella, G. Plante, R. Podviianiuk, H. Qiu, D. Ramírez García, S. Reichard, B. Riedel, A. Rocchetti, N. Rupp, J.M.F. dos Santos, G. Sartorelli, N. Šarčević, M. Scheibelhut, S. Schindler, J. Schreiner, D. Schulte, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C.D. Tunnell, N. Upole, M. Vargas, G. Volta, O. Wack, H. Wang, Y. Wei, C. Weinheimer, D. Wenz, C. Wittweg, J. Wulf, J. Ye, Y. Zhang, T. Zhu, J.P. Zopounidis, for the XENON collaboration, M. Pieracci, C. Tintori, Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), XENON, Aprile E., Aalbers J., Agostini F., Alfonsi M., Althueser L., Amaro F.D., Antochi V.C., Arneodo F., Barge D., Baudis L., Bauermeister B., Bellagamba L., Benabderrahmane M.L., Berger T., Breur P.A., Brown A., Brown E., Bruenner S., Bruno G., Budnik R., Butikofer L., Capelli C., Cardoso J.M.R., Cichon D., Coderre D., Colijn A.P., Conrad J., Cussonneau J.P., Decowski M.P., De Perio P., Gangi P.D., Giovanni A.D., Diglio S., Elykov A., Eurin G., Fei J., Ferella A.D., Fieguth A., Fulgione W., Gaemers P., Rosso A.G., Galloway M., Gao F., Garbini M., Grandi L., Greene Z., Hasterok C., Hogenbirk E., Howlett J., Iacovacci M., Itay R., Joerg F., Kazama S., Kish A., Kobayashi M., Koltman G., Kopec A., Landsman H., Lang R.F., Levinson L., Lin Q., Lindemann S., Lindner M., Lombardi F., Lopes J.A.M., Fune E.L., MacOlino C., Mahlstedt J., Manfredini A., Marignetti F., Undagoitia T.M., Masbou J., Masson D., Mastroianni S., Messina M., Micheneau K., Miller K., Molinario A., Mora K., Mosbacher Y., Murra M., Naganoma J., Ni K., Oberlack U., Odgers K., Pelssers B., Peres R., Piastra F., Pienaar J., Pizzella V., Plante G., Podviianiuk R., Qiu H., Garcia D.R., Reichard S., Riedel B., Rocchetti A., Rupp N., Santos J.M.F.D., Sartorelli G., Sarcevic N., Scheibelhut M., Schindler S., Schreiner J., Schulte D., Schumann M., Lavina L.S., Selvi M., Shagin P., Shockley E., Silva M., Simgen H., Therreau C., Thers D., Toschi F., Trinchero G., Tunnell C.D., Upole N., Vargas M., Volta G., Wack O., Wang H., Wei Y., Weinheimer C., Wenz D., Wittweg C., Wulf J., Ye J., Zhang Y., Zhu T., Zopounidis J.P., Collaboration F.T.X., Pieracci M., Tintori C., XENON (IHEF, IoP, FNWI), IoP (FNWI), Université de Nantes - Faculté des Sciences et des Techniques, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F. D., Antochi, V. C., Arneodo, F., Barge, D., Baudis, L., Bauermeister, B., Bellagamba, L., Benabderrahmane, M. L., Berger, T., Breur, P. A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Butikofer, L., Capelli, C., Cardoso, J. M. R., Cichon, D., Coderre, D., Colijn, A. P., Conrad, J., Cussonneau, J. P., Decowski, M. P., De Perio, P., Gangi, P. D., Giovanni, A. D., Diglio, S., Elykov, A., Eurin, G., Fei, J., Ferella, A. D., Fieguth, A., Fulgione, W., Gaemers, P., Rosso, A. G., Galloway, M., Gao, F., Garbini, M., Grandi, L., Greene, Z., Hasterok, C., Hogenbirk, E., Howlett, J., Iacovacci, M., Itay, R., Joerg, F., Kazama, S., Kish, A., Kobayashi, M., Koltman, G., Kopec, A., Landsman, H., Lang, R. F., Levinson, L., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Lopes, J. A. M., Fune, E. L., Macolino, C., Mahlstedt, J., Manfredini, A., Marignetti, F., Undagoitia, T. M., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Micheneau, K., Miller, K., Molinario, A., Mora, K., Mosbacher, Y., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Odgers, K., Pelssers, B., Peres, R., Piastra, F., Pienaar, J., Pizzella, V., Plante, G., Podviianiuk, R., Qiu, H., Garcia, D. R., Reichard, S., Riedel, B., Rocchetti, A., Rupp, N., Santos, J. M. F. D., Sartorelli, G., Sarcevic, N., Scheibelhut, M., Schindler, S., Schreiner, J., Schulte, D., Schumann, M., Lavina, L. S., Selvi, M., Shagin, P., Shockley, E., Silva, M., Simgen, H., Therreau, C., Thers, D., Toschi, F., Trinchero, G., Tunnell, C. D., Upole, N., Vargas, M., Volta, G., Wack, O., Wang, H., Wei, Y., Weinheimer, C., Wenz, D., Wittweg, C., Wulf, J., Ye, J., Zhang, Y., Zhu, T., Zopounidis, J. P., Collaboration, F. T. X., Pieracci, M., and Tintori, C.
Subjects: Physics - Instrumentation and Detectors, Computer science, FOS: Physical sciences, 01 natural sciences, Signal, Data acquisition, Software, Front-end electronics for detector readout, 0103 physical sciences, Calibration, Data acquisition concept, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation, Mathematical Physics, Time projection chamber, 010308 nuclear & particles physics, business.industry, Control and monitor systems online, Detector, Bandwidth (signal processing), Data acquisition concepts, Instrumentation and Detectors (physics.ins-det), Trigger concepts and systems (hardware and software), business, Energy (signal processing), Computer hardware
Abstract: The XENON1T liquid xenon time projection chamber is the most sensitive detector built to date for the measurement of direct interactions of weakly interacting massive particles with normal matter. The data acquisition system (DAQ) is constructed from commercial, open source, and custom components to digitize signals from the detector and store them for later analysis. The system achieves an extremely low signal threshold below a tenth of a photoelectron using a parallelized readout with the global trigger deferred to a later, software stage. The event identification is based on MongoDB database queries and has over 97% efficiency at recognizing interactions at the analysis energy threshold. A readout bandwidth over 300 MB/s is reached in calibration modes and is further expandable via parallelization. This DAQ system was successfully used during three years of operation of XENON1T., 14 pages, 6 figures, submitted to JINST; Version 2 with minor updates to text
Published: 2019
Full Text: View/download PDF

14. Erratum: Low-mass dark matter search using ionization signals in XENON100 [Phys. Rev. D 94 , 092001 (2016)]

Author: Y. Meng, P. de Perio, D. Cichon, U. Oberlack, T. Berger, S. Rosendahl, T. Marrodán Undagoitia, J. Pienaar, K. Micheneau, Jelle Aalbers, D. Franco, P. A. Breur, B. Kaminsky, Elena Aprile, G. Sartorelli, Michelle Galloway, C. Grignon, April S. Brown, M. P. Decowski, A. Manfredini, R. Itay, B. Miguez, Manfred Lindner, Jochen Schreiner, P. Shagin, Hulin Wang, Laura Baudis, Matthew Anthony, M. Cervantes, D. Thers, M. L. Benabderrahmane, Ethan Brown, A. Tiseni, C. Hasterok, A. Kish, M. Weber, Yuehuan Wei, D. Mayani, F. D. Amaro, A. Buss, E. Hogenbirk, L. Scotto Lavina, F. Arneodo, M. Le Calloch, Hardy Simgen, Lorne Levinson, R. Persiani, Guillaume Plante, A. D. Ferella, G. Kessler, P. Barrow, C. Weinheimer, C. Reuter, Z. Greene, Giacomo Bruno, M. Selvi, A. Fieguth, D. Coderre, S. Schindler, Boris Bauermeister, R. Wall, Luke Goetzke, S. E. A. Orrigo, E. K. U. Gross, C. Geis, A. Rizzo, P. Di Gangi, L. Rauch, N. Rupp, M. Scheibelhut, João Cardoso, S. Bruenner, J. Wulf, H. Landsman, C. Tunnell, R. Budnik, J. Naganoma, Jean-Pierre Cussonneau, D. Masson, Lukas Bütikofer, Ehud Duchovni, Marc Schumann, A. J. Melgarejo Fernandez, A. Lyashenko, Julien Masbou, M. Alfonsi, A. Stein, Bart Pelssers, R. F. Lang, A. P. Colijn, G. C. Trinchero, J.M.F. dos Santos, F. Agostini, M. von Sivers, A. Di Giovanni, M. Garbini, Sebastian Lindemann, F. V. Massoli, M. Murra, Payam Pakarha, N. Priel, S. Reichard, A. Molinario, Y. Zhang, F. L. Linde, C. Levy, F. Piastra, M. Messina, J.A.M. Lopes, W. Fulgione, and Jan Conrad
Subjects: Physics, 010308 nuclear & particles physics, Yield (chemistry), Ionization, 0103 physical sciences, Dark matter, Charge (physics), Atomic physics, 010306 general physics, Low Mass, 01 natural sciences
Abstract: In Fig. 5 of our original article, we compared measurements and predictions of the charge yield Qy. In that figure, the LUX points were misrepresented, and therefore we present here in Fig. 1 the corrected points from Ref. [1].
Published: 2017
Full Text: View/download PDF

15. Erratum: First axion results from the XENON100 experiment [Phys. Rev. D 90 , 062009 (2014)]

Author: H. Landsman, Daniel Lellouch, F. Piastra, S. Schindler, B. Miguez, L. Scotto Lavina, M. Selvi, M. Auger, Hardy Simgen, A. D. Ferella, Hulin Wang, C. Levy, Kaixuan Ni, D. Mayani Paras, M. Messina, K. Arisaka, G. Kessler, P. Shagin, N. Priel, A. Kish, J. Naganoma, F. Arneodo, H. Contreras, J.A.M. Lopes, C. Balan, Marc Schumann, Y. Meng, Ethan Brown, S. Reichard, W. Fulgione, M. P. Decowski, U. Oberlack, Manfred Lindner, O. Vitells, C. Geis, A. Rizzo, C. Grignon, A. Tiseni, A. Molinario, Giacomo Bruno, S. Macmullin, Florian Kaether, T. Marrodán Undagoitia, S. Bruenner, Gabriella Sartorelli, R. F. Lang, C. Weinheimer, A. P. Colijn, D. Thers, M. Weber, Guillaume Plante, Boris Bauermeister, W. Hampel, M. Garbini, April S. Brown, R. Itay, Jochen Schreiner, F. V. Massoli, M. Le Calloch, C. Reuter, S. E. A. Orrigo, Elena Aprile, João Cardoso, F. Gao, S. Rosendahl, J.M.F. dos Santos, F. Agostini, Sebastian Lindemann, E. Pantic, R. Budnik, Luke Goetzke, S. Fattori, G. C. Trinchero, A. J. Melgarejo Fernandez, M. Murra, Jean-Pierre Cussonneau, M. Alfonsi, K. Lung, Laura Baudis, J. Pienaar, P. Beltrame, Ehud Duchovni, A. Behrens, A. Lyashenko, A. Teymourian, P. Barrow, K. Bokeloh, E. K. U. Gross, R. Persiani, Julien Masbou, Aprile, E., Agostini, F., Alfonsi, M., Arisaka, K., Arneodo, F., Auger, M., Balan, C., Barrow, P., Baudis, L., Bauermeister, B., Behrens, A., Beltrame, P., Bokeloh, K., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Cardoso, J. m. r., Colijn, A. p., Contreras, H., Cussonneau, J. p., Decowski, M. p., Duchovni, E., Fattori, S., Ferella, A. d., Fulgione, W., Gao, F., Garbini, M., Geis, C., Goetzke, L. w., Grignon, C., Gross, E., Hampel, W., Itay, R., Kaether, F., Kessler, G., Kish, A., Landsman, H., Lang, R. f., Le Calloch, M., Lellouch, D., Levy, C., Lindemann, S., Lindner, M., Lopes, J. a. m., Lung, K., Lyashenko, A., Macmullin, S., Marrodán Undagoitia, T., Masbou, J., Massoli, F. v., Mayani Paras, D., Melgarejo Fernandez, A. j., Meng, Y., Messina, M., Miguez, B., Molinario, A., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Orrigo, S. e. a., Pantic, E., Persiani, R., Piastra, F., Pienaar, J., Plante, G., Priel, N., Reichard, S., Reuter, C., Rizzo, A., Rosendahl, S., dos Santos, J. m. f., Sartorelli, G., Schindler, S., Schreiner, J., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Simgen, H., Teymourian, A., Thers, D., Tiseni, A., Trinchero, G., Vitells, O., Wang, H., Weber, M., and Weinheimer, C.
Subjects: Physics, Particle physics, XENON DARK MATTER AXION, 010308 nuclear & particles physics, 0103 physical sciences, Limit (mathematics), 010306 general physics, Coupling (probability), 01 natural sciences, Axion
Abstract: n our paper, we presented searches for solar axions and galactic axionlike particles (ALPs) in the data collected by the XENON100 experiment (with an exposure of 224.6 days). We recently found a bug in the code to calculate the exclusion limit for galactic ALPs. This resulted in an underestimation of the ALP expected rate, which in turn led to an overly conservative limit, compared to what it should really be. We corrected the code, and the result of the XENON100 90% C.L. exclusion limit on galactic ALPs (shown in Fig. 1) was reevaluated. The corrected limit is stronger than the one previously published by approximately a factor of 5 across all masses and sets the best published limit on the axion-electron coupling, $g_{Ae}$, in the (1–40) keV/$c^2$ mass range.
Published: 2017
Full Text: View/download PDF

16. Detection of the 67.9 and 78.4 [CLC]ke[/CLC]V Lines Associated with the Radioactive Decay of [TSUP]44[/TSUP]T[CLC]i[/CLC] in Cassiopeia A

Author: U. Oberlack, Johan A. M. Bleeker, Hans Bloemen, Jelle Kaastra, J. Martin Laming, and Jacco Vink
Subjects: Cassiopeia A, Physics, Space and Planetary Science, Flux, Astronomy and Astrophysics, Astrophysics, Continuum (set theory), Supernova remnant, Power law, Energy (signal processing), Radioactive decay, Line (formation)
Abstract: We report the detection of the Sc-44 nuclear decay lines at 67.9 keV and 78.4 keV associated with the nuclear decay of Ti-44 in Cassiopeia A. The line emission was observed by the PDS instrument on board BeppoSAX, which recently observed the supernova remnant for over 500 ks. The detection of the line emission with a flux of (2.1 +/-0.7) 10^{-5} ph/cm^2/s in each line (90% confidence) is at the 5 sigma significance level, if we can assume that the 12-300 keV continuum is adequately represented by a single power law. However, as the nature of the continuum is not clear we investigate various other possibilities. A more conservative estimate of the line flux is made by assuming that a power law continuum is at least a good approximation to the continuum emission for a narrower 30-100 keV energy range. With this limitation the measured line flux is (1.9 +/- 0.9) 10^{-5} ph/cm^2/s, with the detection still at the 3.4 sigma significance level. We suggest that together with the CGRO-COMPTEL measurement of the Ca-44 line at 1157 keV of (3.5 +/- 0.9) 10^{-5} ph/cm^2/s a flux for all three lines of (2.5 +/- 1.0) 10^{-5} ph/cm^2/s for Cas A can be adopted. This implies an initial Ti-44 mass of (0.8 - 2.5) 10^{-4} Msun.
Published: 2001
Full Text: View/download PDF

17. The COMPTEL instrumental line background

Author: G. Weidenspointner, U. Oberlack, James M. Ryan, Derek W. Morris, Roland Diehl, Helmut Steinle, S. C. Kappadath, S. Plueschke, Volker Schoenfelder, Mark L. McConnell, and M. Varendorff
Subjects: Physics, Orbital elements, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Interstellar medium, Supernova, Space and Planetary Science, Observatory, Event (particle physics), Line (formation)
Abstract: The instrumental line background of the Compton telescope COMPTEL onboard the Compton Gamma-Ray Observatory is due to the activation and/or decay of many isotopes. The major components of this background can be attributed to eight individual isotopes, namely 2D, 22Na, 24Na, 28Al, 40K, 52Mn, 57Ni, and 208Tl. The identification of instrumental lines with specific isotopes is based on the line energies as well as on the variation of the event rate with time, cosmic-ray intensity, and deposited radiation dose during passages through the South-Atlantic Anomaly. The characteristic variation of the event rate due to a specific isotope depends on its life-time, orbital parameters such as the altitude of the satellite above Earth, and the solar cycle. A detailed understanding of the background contributions from instrumental lines is crucial at MeV energies for measuring the cosmic diffuse gamma-ray background and for observing gamma-ray line emission in the interstellar medium or from supernovae and their remnants. Procedures to determine the event rate from each background isotope are described, and their average activity in spacecraft materials over the first seven years of the mission is estimated., Comment: accepted for publication in A&A, 22 pages, 21 figures
Published: 2001
Full Text: View/download PDF

18. The first COMPTEL source catalogue

Author: V. Schönfelder, K. Bennett, J. J. Blom, H. Bloemen, W. Collmar, A. Connors, R. Diehl, W. Hermsen, A. Iyudin, R. M. Kippen, J. Knödlseder, L. Kuiper, G. G. Lichti, M. McConnell, D. Morris, R. Much, U. Oberlack, J. Ryan, G. Stacy, H. Steinle, A. Strong, R. Suleiman, R. van Dijk, M. Varendorff, C. Winkler, and O. R. Williams
Subjects: Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, Astrophysics (astro-ph), Interstellar cloud, Continuum (design consultancy), FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Supernova, Pulsar, Observatory, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: The imaging Compton telescope COMPTEL aboard NASA's Compton Gamma-Ray Observatory has opened the MeV gamma-ray band as a new window to astronomy. COMPTEL provided the first complete all-sky survey in the energy range 0.75 to 30 MeV. The catalogue, presented here, is largely restricted to published results. It contains firm as well as marginal detections of continuum and line emitting sources and presents upper limits for various types of objects. The numbers of the most significant detections are 32 for steady sources and 31 for gamma-ray bursters. Among the continuum sources, detected so far, are spin-down pulsars, stellar black-hole candidates, supernova remnants, interstellar clouds, nuclei of active galaxies, gamma-ray bursters, and the Sun during solar flares. Line detections have been made in the light of the 1.809 MeV 26Al line, the 1.157 MeV 44Ti line, the 847 and 1238 keV 56Co lines, and the neutron capture line at 2.223 MeV. For the identification of galactic sources, a modelling of the diffuse galactic emission is essential. Such a modelling at this time does not yet exist at the required degree of accuracy. Therefore, a second COMPTEL source catalogue will be produced after a detailed and accurate modelling of the diffuse interstellar emission has become possible., Comment: 50 pages including 4 figures; accepted for publication in A&A Supplements
Published: 2000
Full Text: View/download PDF

19. The Revised COMPTEL Orion Results

Author: Roland Diehl, Andrew W. Strong, V. Schönfelder, James M. Ryan, R. D. van der Meulen, K. Bennett, D. Morris, H. Bloemen, W. Hermsen, U. Oberlack, Jürgen Knödlseder, C. Winkler, G. G. Lichti, and C. de Vries
Subjects: Nuclear reaction, Physics, Space and Planetary Science, Nucleosynthesis, Flux, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Analysis method
Abstract: COMPTEL observations of the Orion/Monoceros region have shown distinct evidence for excessive 3-7 MeV emission that was attributed to nuclear de-excitation lines from accelerated 12C and 16O nuclei. Unfortunately, we must conclude now that this appears to be a spurious result. This conclusion follows from a better understanding of the instrumental background, from a better exposure of the region, and from an improved analysis method. We show here how the impact of each of these gradually reduces the signal to a less than 3 σ result. The prime underlying cause seems to be 24Na activation in and around the upper COMPTEL detectors. Combining all available data, we now set a 2 σ flux upper limit on the 3-7 MeV emission of Orion of 3 × 10-5 γ cm-2 s-1, to be compared with the previously derived flux of ~10-4 γ cm-2 s-1.
Published: 1999
Full Text: View/download PDF

20. 26 Al Radioactivity in the Galaxy

Author: R. Diehl, U. Oberlack, J. Knödlseder, K. Bennett, H. Bloemen, W. Hermsen, J. Ryan, V. Schönfelder, and P. von Ballmoos
Abstract: 26Al radioactivity is believed to originate predominantly from massive stars, ejected into interstellar medium in wind phases and/or supernova events. With its million-year decay time, penetrating γ-rays from 26Al decay measure the massive-star history averaged over a time scale of ≃million years, thus extending times cales accessible otherwise. The COMPTEL 1.809 MeV all-sky data from 5 years of observations show irregularities and features at intermediate latitudes, which may have a more local origin (≃ 1 kpc). We find that the large scale emission can be characterized by a Galactic scale height of ≃ 130 pc, and a Galactocentric scale radius of ≃ 5 kpc, with features from spiral structure. Catalogues from massive-star related objects do not significantly improve the description of COMPTEL data above this. Emission associated with nearby structures such as the Gould Belt, Loop I, or stellar aggregates, is indicated, yet cannot be clearly detected. Combined with our imaging results, this suggests that 26A1 yields from massive star ensembles depend on specifics of those stars and their history. Further 26A1 γ-ray studies are underway to help mapping of the massive star history in the solar vicinity.
Published: 1997
Full Text: View/download PDF

21. 26Al in the Local Interstellar Medium

Author: J. Knödlseder, K. Bennett, H. Bloemen, R. Diehl, W. Hermsen, U. Oberlack, J. Ryan, V. Schönfelder, and P. von Ballmoos
Abstract: We estimate the 1.8 MeV luminosity of the Sco-Cen association due to radioactive decay of 26A1 to (4 – 15) 10−5ph cm−2 s−1. We propose a low surface brightness, limb brightened bubble for the 1.8 MeV intensity distribution. The detectibility of this distribution with existing γ-ray telescopes is discussed.
Published: 1997
Full Text: View/download PDF

22. Exclusion of Leptophilic Dark Matter Models using XENON100 Electronic Recoil Data

Author: The XENON Collaboration, E. Aprile, F. Agostini, M. Alfonsi, L. Arazi, K. Arisaka, F. Arneodo, M. Auger, C. Balan, P. Barrow, L. Baudis, B. Bauermeister, A. Behrens, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, J. M. R. Cardoso, M. Cervantes, D. Coderre, A. P. Colijn, H. Contreras, J. P. Cussonneau, M. P. Decowski, A. Di Giovanni, E. Duchovni, S. Fattori, A. D. Ferella, A. Fieguth, W. Fulgione, F. Gao, M. Garbini, C. Geis, L. W. Goetzke, C. Grignon, E. Gross, W. Hampel, R. Itay, F. Kaether, B. Kaminsky, G. Kessler, A. Kish, H. Landsman, R. F. Lang, M. Le Calloch, D. Lellouch, L. Levinson, C. Levy, S. Lindemann, M. Lindner, J. A. M. Lopes, A. Lyashenko, S. Macmullin, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Mayani, A. J. Melgarejo Fernandez, Y. Meng, M. Messina, B. Miguez, A. Molinario, G. Morana, M. Murra, J. Naganoma, K. Ni, U. Oberlack, S. E. A. Orrigo, P. Pakarha, E. Pantic, R. Persiani, F. Piastra, J. Pienaar, G. Plante, N. Priel, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, J. M. F. dos Santos, G. Sartorelli, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Thers, A. Tiseni, G. Trinchero, C. Tunnell, O. Vitells, R. Wall, H. Wang, M. Weber, C. Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), XENON100, Astroparticle Physics (IHEF, IoP, FNWI), XENON Collaboration: […, Aprile E, Agostini F, Alfonsi M, Arazi L, Arisaka K, Arneodo F, Auger M, Balan C, Barrow P, Baudis L, Bauermeister B, Behrens A, Brown A, Brown E, Bruenner S, Bruno G, Budnik R, Bütikofer L, Cardoso JM, Cervantes M, Coderre D, Colijn AP, Contreras H, Cussonneau JP, Decowski MP, Di Giovanni A, Duchovni E, Fattori S, Ferella AD, Fieguth A, Fulgione W, Gao F, Garbini M, Geis C, Goetzke LW, Grignon C, Gross E, Hampel W, Itay R, Kaether F, Kaminsky B, Kessler G, Kish A, Landsman H, Lang RF, Le Calloch M, Lellouch D, Levinson L, Levy C, Lindemann S, Lindner M, Lopes JA, Lyashenko A, Macmullin S, Marrodán Undagoitia T, Masbou J, Massoli F V, Mayani D, Melgarejo Fernandez AJ, Meng Y, Messina M, Miguez B, Molinario A, Morana G, Murra M, Naganoma J, Ni K, Oberlack U, Orrigo SE, Pakarha P, Pantic E, Persiani R, Piastra F, Pienaar J, Plante G, Priel N, Rauch L, Reichard S, Reuter C, Rizzo A, Rosendahl S, dos Santos JM, Sartorelli G, Schindler S, Schreiner J, Schumann M, Scotto Lavina L, Selvi M, Shagin P, Simgen H, Teymourian A, Thers D, Tiseni A, Trinchero G, Tunnell C, Vitells O, Wall R, Wang H, Weber M, Weinheimer C, and …]
Subjects: Physics, Multidisciplinary, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, Scattering, Dark matter, Sigma, FOS: Physical sciences, Electron, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Physics - Experiment, Dark matter halo, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Experiment (hep-ex), Recoil, Dark Matter, Wimps, leptophilic dark matter models, Particle, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Laboratory experiments searching for galactic dark matter particles scattering off nuclei have so far not been able to establish a discovery. We use data from the XENON100 experiment to search for dark matter interacting with electrons. With no evidence for a signal above the low background of our experiment, we exclude a variety of representative dark matter models that would induce electronic recoils. For axial-vector couplings to electrons, we exclude cross-sections above 6x10^(-35) cm^2 for particle masses of m_chi = 2 GeV/c^2. Independent of the dark matter halo, we exclude leptophilic models as explanation for the long-standing DAMA/LIBRA signal, such as couplings to electrons through axial-vector interactions at a 4.4 sigma confidence level, mirror dark matter at 3.6 sigma, and luminous dark matter at 4.6 sigma., 4 pages, 4 figures, with supporting online material
Published: 2015
Full Text: View/download PDF

23. Activation in the COMPTEL double-scattering gamma-ray telescope

Author: James M. Ryan, G. Weidenspointner, D. J. Morris, H. de Boer, V. Schönfelder, K. Bennett, M. Varendorff, Mark L. McConnell, U. Oberlack, and Roland Diehl
Subjects: Physics, Photomultiplier, Photon, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Field of view, Astrophysics, Gamma-ray astronomy, law.invention, Telescope, Observatory, law, Scintillation counter, Astrophysics::Earth and Planetary Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: The COMPTEL gamma-ray telescope has been operating in low Earth orbit for six years, since the launch of the Compton Gamma-Ray Observatory in April 1991. Comparisons of data for different orbits and epochs show evidence of activation on time scales from minutes (/sup 27/Mg, /spl tau//sub 1/2/=9.5 min) to years (/sup 22/Na, /spl tau//sub 1/2/=2.58 yr). The activation is correlated with both the orbital altitude and solar cosmic-ray modulation. Because it requires coincident measurements in two different detectors, COMPTEL is most susceptible to instrumental background events in which two or more photons are produced simultaneously.
Published: 2002
Full Text: View/download PDF

24. Radioactivities in Population Studies: 26Al and 60Fe from OB Associations

Author: U. Oberlack, Dieter H. Hartmann, S. Plüschke, K. Kretschmer, and R. Diehl
Subjects: Physics, education.field_of_study, Astrophysics::High Energy Astrophysical Phenomena, Stellar rotation, Population, Observable, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kinetic energy, law.invention, Interstellar medium, Telescope, Stars, law, Stellar physics, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics::Galaxy Astrophysics
Abstract: The observation of the interstellar 1.809 MeV decay-line of radioactive 26 Al by the imaging gamma-ray telescope COMPTEL have let to the conclusion, that massive stars and their subsequent core-collapse su pernovae are the dominant sources of the interstellar 26 Al abundance. Massive stars are known to affect the surrounding interstellar medium by their energetic stellar winds and by the emission of ionising radia tion. We present a population synthesis model allowing the correlated investigation of the gamma-ray emission characteristics with integrated matter, kinetic energy and extreme ultra-violet radiation emission of as sociations of massive stars. We study the time evolution of the various observables. In addition, we discuss systematic as well as statistical un certainties affecting the model. Beside uncertainties in the input stellar physics such as stellar rotation, mass loss rates or internal mixing mod ifications due to a unknown binary component may lead to significant uncertainties.
Published: 2001
Full Text: View/download PDF

25. Gamma-Ray Line Emission from Superbubbles in the Interstellar Medium: The Cygnus Region

Author: S. Plueschke, U. Oberlack, Dieter H. Hartmann, Roland Diehl, and K. Kretschmer
Subjects: Physics, Spiral galaxy, Star formation, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Scale height, Superbubble, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Interstellar medium, Stars, Supernova, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The star forming process in the Milky Way is non-uniform in time and space. The scale of star forming regions ranges from groups within a few pc to large segments of spiral arms with linear dimension of order kpc. When many stars form in a relatively small volume over a short duration, a localized starburst ensues. The energetic impact of such a burst of star formation can severely affect the dynamic structure of the gaseous disk. Stellar winds and supernova explosions drive an expanding superbubble, whose size eventually exceeds the scale height of the disk and thus drives a disk-wind blowing metal enriched gas into the halo. We discuss the basic scenario of superbubble evolution, emphasizing the associated gamma-ray line signatures. In particular, we discuss nuclear line emission from 26Al and 60Fe in the Cygnus region., Comment: 5 pages, 3 figures, to appear in Proc. of Gamma-Ray Astrophysics 2001, to be published in AIP Conf. Proc. Series
Published: 2001
Full Text: View/download PDF

26. Summary of the first COMPTEL source catalogue

Author: O. R. Williams, U. Oberlack, Andrew W. Strong, Jürgen Knödlseder, K. Bennett, G. Stacy, R. Much, Helmut Steinle, H. Bloemen, C. Winkler, Mark L. McConnell, A. F. Iyudin, W. Hermsen, Werner Collmar, L. Kuiper, Derek W. Morris, Roland Diehl, J. J. Blom, Raid Suleiman, James M. Ryan, G. G. Lichti, R. M. Kippen, V. Schönfelder, R. van Dijk, A. Connors, and M. Varendorff
Subjects: Physics, Active galactic nucleus, Pulsar, High-energy astronomy, Gamma ray, Astronomy, Astrophysics, Gamma-ray astronomy, Sensitivity (control systems), Gamma ray detection
Published: 2000
Full Text: View/download PDF

27. Spectroscopy and Imaging Performance of the Liquid Xenon Gamma-Ray Imaging Telescope (LXeGRIT)

Author: U. Oberlack, Kyoko Takizawa, V. Egorov, K. L. Giboni, Edward L. Chupp, Elena Aprile, A. Curioni, Tadayoshi Doke, Sandro Ventura, P. P. Dunphy, and Jun Kikuchi
Subjects: Physics, Scintillation, Time projection chamber, Physics::Instrumentation and Detectors, Compton telescope, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, chemistry.chemical_element, FOS: Physical sciences, Astrophysics, Nuclear physics, Xenon, chemistry, Ionization, Angular resolution, Spectroscopy, Nuclear Experiment
Abstract: LXeGRIT is a balloon-borne Compton telescope based on a liquid xenon time projection chamber (LXeTPC) for imaging cosmic \g-rays in the energy band of 0.2-20 MeV. The detector, with 400 cm$^2$ area and 7 cm drift gap, is filled with high purity LXe. Both ionization and scintillation light signals are detected to measure the energy deposits and the three spatial coordinates of individual \g -ray interactions within the sensitive volume. The TPC has been characterized with repeated measurements of its spectral and Compton imaging response to \g -rays from radioactive sources such as \na, \cs, \yt and Am-Be. The detector shows a linear response to \g -rays in the energy range 511 keV -4.4 MeV, with an energy resolution (FWHM) of $ \Delta E/E=8.8% \: \sqrt{1\MeV /E}$. Compton imaging of \yt \g -ray events with two detected interactions is consistent with an angular resolution of $\sim$ 3 degrees (RMS) at 1.8 MeV., Comment: To appear in: Hard X-Ray, Gamma-Ray and Neutron Detector Physics XI, 2000; Proc. SPIE, vol. 4140; K.A. Flanagan & O.H. Siegmund, eds
Published: 2000
Full Text: View/download PDF

28. The COMPTEL instrumental-line background

Author: James M. Ryan, U. Oberlack, V. Schönfelder, G. Weidenspointner, Derek W. Morris, M. Varendorff, Mark L. McConnell, Roland Diehl, S. C. Kappadath, and S. Plüschke
Subjects: Physics, Orbital elements, Supernova, Isotope, Observatory, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Gamma-ray astronomy, Astrophysics, Line (formation)
Abstract: The instrumental-line background of the Compton telescope COMPTEL onboard the Compton Gamma-Ray Observatory is due to the activation and/or decay of a number of different isotopes. The major components of the COMPTEL instrumental-line background can be attributed to eight individual isotopes, namely 2D, 22Na, 24Na, 28Al, 40K, 52Mn, 57Ni, and 208Tl. In addition, evidence for the presence of 27Mg has been obtained in the search for gamma-ray lines from supernovae. The identification of the instrumental lines with specific isotopes is based on the line energies as well as on the variation of the activity with time, cosmic-ray intensity and deposited radiation dose during passages through the South-Atlantic Anomaly. The characteristic variation of the activity due to an individual isotope depends on its life-time, orbital parameters, and the solar cycle.
Published: 2000
Full Text: View/download PDF

29. COMPTEL 1.8 MeV all sky survey: The Cygnus region

Author: U. Oberlack, W. Hermsen, G. Weidenspointner, Mark L. McConnell, V. Schönfelder, H. Bloemen, Roland Diehl, S. Plüschke, James M. Ryan, K. Bennett, and Jürgen Knödlseder
Subjects: Physics, Stellar population, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Galactic ridge, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma-ray astronomy, Astrophysics, Vela, Galaxy, Interstellar medium, Stars, Astrophysics::Galaxy Astrophysics
Abstract: We present an updated version of COMPTEL’s 1.809 MeV sky survey. Based on eight years of observations we compare results from different imaging techniques using background from adjacent energy bands. We confirm the previously reported characteristics of the galactic 1.809 MeV emission, specifically an extended galactic ridge emission, mainly concentrated towards the inner galaxy, a peculiar emission feature in the Cygnus region, and a low-intensity ridge extending towards Carina and Vela. Because this gamma ray line is due to the decay of radioactive 26Al, predominantly synthesized in massive stars, one anticipates flux enhancements aligned with regions of recent star formation. This is born out by the observations. In particular the Cygnus feature, first presented in 1996 based on three years of COMPTEL data, is confirmed. Based on the stellar population we distinguish three prominent areas in this region, for which we separately derive fluxes, and discuss interpretations.
Published: 2000
Full Text: View/download PDF

30. 26Al in the local interstellar medium

Author: James M. Ryan, H. Bloemen, U. Oberlack, W. Hermsen, K. Bennett, J. Knoedlseder, Roland Diehl, Volker Schoenfelder, and P. von Ballmoos
Subjects: Physics, Interstellar medium, Astrophysics::High Energy Astrophysical Phenomena, Bubble, Astrophysics::Solar and Stellar Astrophysics, High Energy Physics::Experiment, Surface brightness, Astrophysics, Nuclear Experiment, Astrophysics::Galaxy Astrophysics, Intensity (heat transfer), Radioactive decay, Luminosity
Abstract: We estimate the 1.8 MeV luminosity of the Sco-Cen association due to radioactive decay of 26Al to (4-15) 10e-5 ph cm**-2 s**-1. We propose a low surface brightness, limb brightened bubble for the 1.8 MeV intensity distribution. The detectibility of this distribution with existing gamma-ray telescopes is discussed.
Published: 1998
Full Text: View/download PDF

31. Implications of Al-26 emission at 1.8 MeV from the VELA region

Author: U. Oberlack, Roland Diehl, T. Montmerle, Nikos Prantzos, and P. von Ballmoos
Subjects: Physics, Nuclear reaction, Wolf–Rayet star, Space and Planetary Science, Nucleosynthesis, Gum Nebula, Nuclear fusion, Astronomy, Astronomy and Astrophysics, Astrophysics, Gamma-ray astronomy, Near-Earth supernova, Vela
Published: 1994
Full Text: View/download PDF

32. Untersuchungen der Wellenabsorption im Bereich der unteren Hybridresonanz an einem Plasma hoher Ionenmasse / Investigations of Wave Absorption Near the Lower Hybrid Resonance in a Plasma of High Ion Mass

Author: B. Lammers, O. Vogel, U. Oberlack, and H. Schlüter
Subjects: Materials science, Electromagnetic absorption, Particle mass, General Physics and Astronomy, Resonance, Plasma, Physical and Theoretical Chemistry, Atomic physics, Wave equation, Mathematical Physics, Plasma resonance, Wave absorption, Ion
Abstract: The propagation and absorption of waves in the vicinity of the lower hybrid resonance are investigated under linear conditions in a cesium plasma generated by a Q-machine. The results of the measurements are compared with linear theories based on the fluid model. It is shown that in the case of high ion mass plasma only a theory including a finite k||-spectrum yields an appropriate description of wave absorption near the lower hybrid resonance.
Published: 1976
Full Text: View/download PDF

33. Resonanzverschiebungen in HF-Entladungen bei axialem Magnetfeld/Resonance Shifts in High Frequency Discharges in Axial Magnetic Field Configurations

Author: U. Oberlack, H. Schlüter, and B. Lammers
Subjects: Nuclear magnetic resonance, Absorption spectroscopy, Chemistry, Plasma composition, General Physics and Astronomy, Resonance, Plasma diagnostics, Plasma, Physical and Theoretical Chemistry, Mass spectrometry, Mathematical Physics, Plasma resonance, Magnetic field
Abstract: The pressure dependence of the lower hybrid resonance is investigated in a hydrogen plasma generated by a high frequency discharge. Appreciable shifts of the absorption peak with the neutral gas pressure are observed only in a mirror like magnetic field configuration. The measurements show that this shift cannot be explained by a change of the ion composition of the plasma, but must be attributed to two other mechanisms: The composition of the spectrum of the kn-components is influenced by the axial electron density profile so that at low pressure the higher modes of the spectrum are dominant.With higher pressure the formation of radial modes is favoured which leads to an additional apparent shift of the resonance.
Published: 1976
Full Text: View/download PDF

34. Absolutmessung der Leistungseinkopplung in ein Deuterium-Plasma bei der unteren Hybrid-Resonanz / Absolute Measurement of Power Transfer to a Deuterium Plasma Near the Lower Hybrid Resonance

Author: B. Lammers, U. Oberlack, and H. Schlüter
Subjects: Materials science, Absolute measurement, Dielectric heating, General Physics and Astronomy, Resonance, Maximum power transfer theorem, Plasma diagnostics, Plasma, Physical and Theoretical Chemistry, Atomic physics, Deuterium plasma, Mathematical Physics, Plasma control
Abstract: Absolute Measurement of Power Transfer to a Deuterium Plasma Near the Lower Hybrid Resonance The power transfer to a deuterium plasma generated by a high frequency discharge near the lower hybrid resonance is investigated in the range of several hundred watts. The results are compared with linear theories. Reasonable agreement is found between measurements and the linear theory of a bounded plasma as far as the wings of the resonance are concerned. But the dominant radial modes predicted by theory are not observed. Introduction of an empirical effective collision frequency ν* = 0.2 ωpe, however, results in good agreement between measurements and theory in the domain of these radial modes.
Published: 1975
Full Text: View/download PDF

35. Observation of two-neutrino double electron capture in 124Xe with XENON1T

Author: Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F. D., Anthony, M., Antochi, V. C., Arneodo, F., Baudis, L., Bauermeister, B., Benabderrahmane, M. L., Berger, T., Breur, P. A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Capelli, C., Cardoso, J. M. R., Cichon, D., Coderre, D., Colijn, A. P., Conrad, J., Cussonneau, J. P., Decowski, M. P., de Perio, P., di Gangi, P., di Giovanni, A., Diglio, S., Elykov, A., Eurin, G., Fei, J., Ferella, A. D., Fieguth, A., FULGIONE, VALTER, Gallo Rosso, A., Galloway, M., Gao, F., Garbini, M., Grandi, L., Greene, Z., Hasterok, C., Hogenbirk, E., Howlett, J., Iacovacci, M., Itay, R., Joerg, F., Kaminsky, B., Kazama, S., Kish, A., Koltman, G., Kopec, A., Landsman, H., Lang, R. F., Levinson, L., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Lopes, J. A. M., López Fune, E., Macolino, C., Mahlstedt, J., Manfredini, A., Marignetti, F., Marrodán Undagoitia, T., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Micheneau, K., Miller, K., Molinario, A., Morå, K., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Odgers, K., Pelssers, B., Peres, R., Piastra, F., Pienaar, J., Pizzella, V., Plante, G., Podviianiuk, R., Priel, N., Qiu, H., Ramírez García, D., Reichard, S., Riedel, B., Rizzo, A., Rocchetti, A., Rupp, N., Dos Santos, J. M. F., Sartorelli, G., Šarčević, N., Scheibelhut, M., Schindler, S., Schreiner, J., Schulte, D., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Shockley, E., Silva, M., Simgen, H., Therreau, C., Thers, D., Toschi, F., TRINCHERO, GIAN CARLO, Tunnell, C., Upole, N., Vargas, M., Wack, O., Wang, H., Wang, Z., Wei, Y., Weinheimer, C., Wenz, D., Wittweg, C., Wulf, J., Ye, J., Zhang, Y., Zhu, T., Zopounidis, J. P., XENON (IHEF, IoP, FNWI), Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F. D., Anthony, M., Antochi, V. C., Arneodo, F., Baudis, L., Bauermeister2, B., Benabderrahmane, M. L., Berger, T., Breur, P. A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Capelli, C., Cardoso, J. M. R., Cichon, D., Coderre, D., Colijn, A. P., Conrad, J., Cussonneau, J. P., Decowski, M. P., de Perio, P., Di Gangi, P., Di Giovanni, A., Diglio, S., Elykov, A., Eurin, G., Fei, J., Ferella, A. D., Fieguth, A., Fulgione, W., Gallo Rosso, A., Galloway, M., Gao, F., Garbini, M., Grandi, L., Greene, Z., Hasterok, C., Hogenbirk, E., Howlett, J., Iacovacci, M., Itay, R., Joerg, F., Kaminsky, B., Kazama, S., Kish, A., Koltman, G., Kopec, A., Landsman, H., Lang, R. F., Levinson, L., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Lopes, J. A. M., López Fune, E., Macolino, C., Mahlstedt, J., Manfredini, A., Marignetti, F., Marrodán Undagoitia, T., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Micheneau, K., Miller, K., Molinario, A., Morå, K., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Odgers, K., Pelssers, B., Peres, R., Piastra, F., Pienaar, J., Pizzella, V., Plante, G., Podviianiuk, R., Priel, N., Qiu, H., Ramírez García, D., Reichard, S., Riedel, B., Rizzo, A., Rocchetti, A., Rupp, N., dos Santos, J. M. F., Sartorelli, G., Šarčević, N., Scheibelhut, M., Schindler, S., Schreiner, J., Schulte, D., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Shockley, E., Silva, M., Simgen, H., Therreau, C., Thers, D., Toschi, F., Trinchero, G., Tunnell, C., Upole, N., Vargas, M., Wack, O., Wang, H., Wang, Z., Wei, Y., Weinheimer, C., Wenz, D., Wittweg, C., Wulf, J., Ye, J., Zhang, Y., Zhu &amp, T., Zopounidis, J. P., E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, M. Anthony, V. C. Antochi, F. Arneodo, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, S. Diglio, A. Elykov, G. Eurin, J. Fei, A. D. Ferella, A. Fieguth, W. Fulgione, A. Gallo Rosso, M. Galloway, F. Gao, M. Garbini, L. Grandi, Z. Greene, C. Hasterok, E. Hogenbirk, J. Howlett, M. Iacovacci, R. Itay, F. Joerg, B. Kaminsky, S. Kazama, A. Kish, G. Koltman, A. Kopec, H. Landsman, R. F. Lang, L. Levinson, Q. Lin, S. Lindemann, M. Lindner, F. Lombardi, J. A. M. Lopes, E. López Fune, C. Macolino, J. Mahlstedt, A. Manfredini, F. Marignetti, T. Marrodán Undagoitia, J. Masbou, D. Masson, S. Mastroianni, M. Messina, K. Micheneau, K. Miller, A. Molinario, K. Morå, M. Murra, J. Naganoma, K. Ni, U. Oberlack, K. Odgers, B. Pelssers, R. Peres, F. Piastra, J. Pienaar, V. Pizzella, G. Plante, R. Podviianiuk, N. Priel, H. Qiu, D. Ramírez García, S. Reichard, B. Riedel, A. Rizzo, A. Rocchetti, N. Rupp, J. M. F. dos Santos, G. Sartorelli, N. Šarčević, M. Scheibelhut, S. Schindler, J. Schreiner, D. Schulte, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, E. Shockley, M. Silva, H. Simgen, C. Therreau, D. Thers, F. Toschi, G. Trinchero, C. Tunnell, N. Upole, M. Vargas, O. Wack, H. Wang, Z. Wang, Y. Wei, C. Weinheimer, D. Wenz, C. Wittweg, J. Wulf, J. Ye, Y. Zhang, T. Zhu & J. P. Zopounidis, Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), XENON, Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique)
Subjects: electron, Particle physics, Xenon, half-life, Age of the universe, Electron capture, Dark matter, background: model, chemistry.chemical_element, FOS: Physical sciences, electron: capture, n: thermal, 7. Clean energy, 01 natural sciences, weak process, background: low, Neutrino, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, S076H2N, Physics, xenon: liquid, Multidisciplinary, Isotope, 010308 nuclear & particles physics, iodine, neutrino: Majorana: mass, higher-order: 2, Nuclear structure, double-beta decay, dark matter: detector, energy: calibration, Neutrino, Xenon, half-life, electron, double electron capture, weak process, double electron capture, Orders of magnitude (time), chemistry, Dark Matter detector Electron Capture Low Background Double Beta Decay, xenon: nuclide, target: mass, numerical calculations: Monte Carlo, energy spectrum: measured, statistical, acceptance
Abstract: International audience; Two-neutrino double electron capture (2νECEC) is a second-order weak-interaction process with a predicted half-life that surpasses the age of the Universe by many orders of magnitude1. Until now, indications of 2νECEC decays have only been seen for two isotopes2,3,4,5, 78Kr and 130Ba, and instruments with very low background levels are needed to detect them directly with high statistical significance6,7. The 2νECEC half-life is an important observable for nuclear structure models8,9,10,11,12,13,14 and its measurement represents a meaningful step in the search for neutrinoless double electron capture—the detection of which would establish the Majorana nature of the neutrino and would give access to the absolute neutrino mass15,16,17. Here we report the direct observation of 2νECEC in 124Xe with the XENON1T dark-matter detector. The significance of the signal is 4.4 standard deviations and the corresponding half-life of 1.8 × 1022 years (statistical uncertainty, 0.5 × 1022 years; systematic uncertainty, 0.1 × 1022 years) is the longest measured directly so far. This study demonstrates that the low background and large target mass of xenon-based dark-matter detectors make them well suited for measuring rare processes and highlights the broad physics reach of larger next-generation experiments18,19,20.
Published: 2019
Full Text: View/download PDF

36. First Axion Results from the XENON100 Experiment

Author: Xenon, The Collaboration, Aprile, E., Agostini, F., Alfonsi, M., Arisaka, K., Arneodo, F., Auger, M., Balan, C., Barrow, P., Baudis, L., Bauermeister, B., Behrens, A., Beltrame, P., Bokeloh, K., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Cardoso, J. M. R., Colijn, A. P., Contreras, H., Cussonneau, J. P., Decowski, M. P., Duchovni, E., Fattori, S., Ferella, A. D., Fulgione, W., Gao, F., Garbini, M., Geis, C., Goetzke, L. W., Grignon, C., Gross, E., Hampel, W., Itay, R., Kaether, F., Kessler, G., Kish, A., Landsman, H., Lang, R. F., Le Calloch, M., Lellouch, D., Levy, C., Lindemann, S., Lindner, M., Lopes, J. A. M., Lung, K., Lyashenko, A., Macmullin, S., Marrodan Undagoitia, T., Masbou, J., Massoli, F. V., Mayani Paras, D., Melgarejo Fernandez, A. J., Meng, Y., Messina, M., Miguez, B., Molinario, A., Murra, M., Naganoma, J., Oberlack, U., Orrigo, S. E. A., Pantic, E., Persiani, R., Piastra, F., Pienaar, J., Plante, G., Priel, N., Reichard, S., Reuter, C., Rizzo, A., Rosendahl, S., Dos Santos, J. M. F., Sartorelli, G., Schindler, S., Schreiner, J., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Simgen, H., Teymourian, A., Thers, D., Tiseni, A., Gian Carlo Trinchero, Vitells, O., Wang, H., Weber, M., Weinheimer, C., Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, Astroparticle Physics (IHEF, IoP, FNWI), E. Aprile, F. Agostini, M. Alfonsi, K. Arisaka, F. Arneodo, M. Auger, C. Balan, P. Barrow, L. Baudi, B. Bauermeister, A. Behren, P. Beltrame, K. Bokeloh, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, J. M. R. Cardoso, A. P. Colijn, H. Contrera, J. P. Cussonneau, M. P. Decowski, E. Duchovni, S. Fattori, A. D. Ferella, W. Fulgione, F. Gao, M. Garbini, C. Gei, L. W. Goetzke, C. Grignon, E. Gro, W. Hampel, R. Itay, F. Kaether, G. Kessler, A. Kish, H. Landsman, R. F. Lang, M. Le Calloch, D. Lellouch, C. Levy, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, A. Lyashenko, S. MacMullin, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Mayani Para, A. J. Melgarejo Fernandez, Y. Meng, M. Messina, B. Miguez, A. Molinario, M. Murra, J. Naganoma, K. Ni, U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, F. Piastra, J. Pienaar, G. Plante, N. Priel, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, J. M. F. dos Santo, G. Sartorelli, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, A. Tiseni, G. Trinchero, O. Vitell, H. Wang, M. Weber, C. Weinheimer, and The XENON100 Collaboration
Subjects: Nuclear and High Energy Physics, Particle physics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Dark matter, chemistry.chemical_element, FOS: Physical sciences, Astrophysics, 01 natural sciences, Cosmology, dark matter, Xenon, High Energy Physics - Phenomenology (hep-ph), Assioni, 0103 physical sciences, 010306 general physics, Axion, Liquid Xenon, Coupling, Coupling constant, Quantum chromodynamics, Physics, 010308 nuclear & particles physics, hep-ph, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, chemistry, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first results of searches for axions and axion-like-particles with the XENON100 experiment. The axion-electron coupling constant, $g_{Ae}$, has been tested by exploiting the axio-electric effect in liquid xenon. A profile likelihood analysis of 224.6 live days $\times$ 34 kg exposure has shown no evidence for a signal. By rejecting $g_{Ae}$, larger than $7.7 \times 10^{-12}$ (90% CL) in the solar axion search, we set the best limit to date on this coupling. In the frame of the DFSZ and KSVZ models, we exclude QCD axions heavier than 0.3 eV/c$^2$ and 80 eV/c$^2$, respectively. For axion-like-particles, under the assumption that they constitute the whole abundance of dark matter in our galaxy, we constrain $g_{Ae}$, to be lower than $1 \times 10^{-12}$ (90% CL) for masses between 5 and 10 keV/c$^2$. We present the first results of searches for axions and axionlike particles with the XENON100 experiment. The axion-electron coupling constant, gAe, has been probed by exploiting the axioelectric effect in liquid xenon. A profile likelihood analysis of 224.6 live days × 34-kg exposure has shown no evidence for a signal. By rejecting gAe larger than 7.7×10-12 (90% C.L.) in the solar axion search, we set the best limit to date on this coupling. In the frame of the DFSZ and KSVZ models, we exclude QCD axions heavier than 0.3 and 80 eV/c2, respectively. For axionlike particles, under the assumption that they constitute the whole abundance of dark matter in our galaxy, we constrain gAe to be lower than 1×10-12 (90% C.L.) for masses between 5 and 10 keV/c2. We present the first results of searches for axions and axion-like-particles with the XENON100 experiment. The axion-electron coupling constant, $g_{Ae}$, has been probed by exploiting the axio-electric effect in liquid xenon. A profile likelihood analysis of 224.6 live days $\times$ 34 kg exposure has shown no evidence for a signal. By rejecting $g_{Ae}$, larger than $7.7 \times 10^{-12}$ (90\% CL) in the solar axion search, we set the best limit to date on this coupling. In the frame of the DFSZ and KSVZ models, we exclude QCD axions heavier than 0.3 eV/c$^2$ and 80 eV/c$^2$, respectively. For axion-like-particles, under the assumption that they constitute the whole abundance of dark matter in our galaxy, we constrain $g_{Ae}$, to be lower than $1 \times 10^{-12}$ (90\% CL) for mass range from 1 to 40 keV/c$^2$, and set the best limit to date as well.
Published: 2014
Full Text: View/download PDF

37. Response of the XENON100 dark matter detector to nuclear recoils

Author: Aprile, E., Alfonsi, M., Arisaka, K., Arneodo, F., Balan, C., Baudis, L., Bauermeister, B., Behrens, A., Beltrame, P., Bokeloh, K., Brown, A., Brown, E., Brünner, S., Bruno, G., Budnik, R., Cardoso, J., Chen, W., Choi, B., Colijn, A., Contreras, H., Cussonneau, J., Decowski, M., Duchovni, E., Fattori, S., Ferella, A., Fulgione, W., Gao, F., Garbini, M., Geis, C., Ghag, C., Giboni, K., Goetzke, L., Grignon, C., Gross, E., Hampel, W., Itay, R., Kaether, F., Kessler, G., Kish, A., Lamblin, J., Landsman, H., Lang, R., Calloch, M., Levy, C., Lim, K., Lin, Q., Lindemann, S., Lindner, M., Lopes, J., Lung, K., Marrodan Undagoitia, T., Undagoitia, T., Fernandez, A., Meng, Y., Messina, M., Molinario, A., Ni, K., Oberlack, U., Orrigo, S., Pantic, E., Persiani, R., Plante, G., Priel, N., Rizzo, A., Rosendahl, S., Santos, J., Sartorelli, G., Schreiner, J., Schumann, M., Lavina, L., Scovell, P., Selvi, M., Shagin, P., Simgen, H., Teymourian, A., Thers, D., Vitells, O., Wang, H., Weber, M., Weinheimer, C., Schuhmacher, H., Wiegel, B., Astroparticle Physics (IHEF, IoP, FNWI), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudi, B. Bauermeister, A. Behren, P. Beltrame, K. Bokeloh, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, A. P. Colijn, H. Contrera, J. P. Cussonneau, M. P. Decowski, E. Duchovni, S. Fattori, A. D. Ferella, W. Fulgione, F. Gao, M. Garbini, C. Gei, C. Ghag, K.-L. Giboni, L. W. Goetzke, C. Grignon, E. Gro, W. Hampel, R. Itay, F. Kaether, G. Kessler, A. Kish, H. Landsman, R. F. Lang, M. Le Calloch, C. Levy, K. E. Lim, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, T. Marrodán Undagoitia, F. V. Massoli, A. J. Melgarejo Fernandez, Y. Meng, M. Messina, A. Molinario, K. Ni, U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, G. Plante, N. Priel, A. Rizzo, S. Rosendahl, J. M. F. dos Santo, G. Sartorelli, J. Schreiner, M. Schumann, L. Scotto Lavina, P. R. Scovell, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, O. Vitell, H. Wang, M. Weber, C. Weinheimer, H. Schuhmacher, B. Wiegel, and XENON Collaboration
Subjects: Nuclear and High Energy Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Monte Carlo method, Dark matter, FOS: Physical sciences, 01 natural sciences, dark matter, Particle detector, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Recoil, Ionization, 0103 physical sciences, 010306 general physics, Nuclear Experiment, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Scintillation, 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron source, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Results from the nuclear recoil calibration of the XENON100 dark matter detector installed underground at the Laboratori Nazionali del Gran Sasso (LNGS), Italy are presented. Data from measurements with an external 241AmBe neutron source are compared with a detailed Monte Carlo simulation which is used to extract the energy dependent charge-yield Qy and relative scintillation efficiency Leff. A very good level of absolute spectral matching is achieved in both observable signal channels - scintillation S1 and ionization S2 - along with agreement in the 2-dimensional particle discrimination space. The results confirm the validity of the derived signal acceptance in earlier reported dark matter searches of the XENON100 experiment., Comment: 10 pages, 10 figures. Matches version accepted by PRD. Contains revised representation of expected WIMP event signature. Conclusions remain unaffected
Published: 2013
Full Text: View/download PDF

38. Limits on spin-dependent WIMP-nucleon cross sections from 225 live days of XENON100 data

Author: Marc Schumann, P. Shagin, A. Behrens, Ehud Duchovni, E. Pantic, M. Messina, J. A. M. Lopes, A. Kish, M. Garbini, K. Arisaka, Jean-Pierre Cussonneau, Hardy Simgen, A. D. Ferella, D. Thers, Boris Bauermeister, R. F. Lang, João Cardoso, K. Lung, A. P. Colijn, T. Marrodán Undagoitia, Ch. Weinheimer, Laura Baudis, Hui Wang, F. Gao, M. P. Decowski, Manfred Lindner, C. Ghag, C. Levy, M. Selvi, W. T. Chen, J. Lamblin, H. Landsman, Daniel Lellouch, P. R. Scovell, H. Contreras, P. Beltrame, Florian Kaether, Kaixuan Ni, Ran Budnik, F. V. Massoli, A. Molinario, Qing Lin, B. Choi, J.M.F. dos Santos, L. Scotto Lavina, Sebastian Lindemann, S. Rosendahl, S. Fattori, A. Teymourian, N. Priel, C. Balan, W. Hampel, Karl Giboni, W. Fulgione, Ethan Brown, Elena Aprile, F. Arneodo, April S. Brown, Uwe Oberlack, K. E. Lim, Jochen Schreiner, C. Grignon, A. J. Melgarejo Fernandez, M. Le Calloch, M. Alfonsi, O. Vitells, A. Rizzo, S. E. A. Orrigo, Y. Meng, Giacomo Bruno, G. Sartorelli, M. Weber, G. Plante, Luke Goetzke, K. Bokeloh, E. K. U. Gross, R. Persiani, Astroparticle Physics (IHEF, IoP, FNWI), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudi, B. Bauermeister, A. Behren, P. Beltrame, K. Bokeloh, A. Brown, E. Brown, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, A. P. Colijn, H. Contrera, J. P. Cussonneau, M. P. Decowski, E. Duchovni, S. Fattori, A. D. Ferella, W. Fulgione, F. Gao, M. Garbini, C. Ghag, K.-L. Giboni, L. W. Goetzke, C. Grignon, E. Gro, W. Hampel, F. Kaether, A. Kish, J. Lamblin, H. Landsman, R. F. Lang, M. Le Calloch, D. Lellouch, C. Levy, K. E. Lim, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, T. Marrodán Undagoitia, F. V. Massoli, A. J. Melgarejo Fernandez, Y. Meng, M. Messina, A. Molinario, K. Ni, U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, G. Plante, N. Priel, A. Rizzo, S. Rosendahl, J. M. F. dos Santo, G. Sartorelli, J. Schreiner, M. Schumann, L. Scotto Lavina, P. R. Scovell, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, O. Vitell, H. Wang, M. Weber, C. Weinheimer, and XENON100 collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Dark matter, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, dark matter, Particle detector, High Energy Physics - Experiment, Nuclear physics, Cross section (physics), High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010306 general physics, Pseudovector, Instrumentation and Methods for Astrophysics (astro-ph.IM), Spin-½, Physics, 010308 nuclear & particles physics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Nucleon, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new experimental constraints on the elastic, spin-dependent WIMP-nucleon cross section using recent data from the XENON100 experiment, operated in the Laboratori Nazionali del Gran Sasso in Italy. An analysis of 224.6 live days x 34 kg of exposure acquired during 2011 and 2012 revealed no excess signal due to axial-vector WIMP interactions with 129-Xe and 131-Xe nuclei. This leads to the most stringent upper limits on WIMP-neutron cross sections for WIMP masses above 6 GeV, with a minimum cross section of 3.5 x 10^{-40} cm^2 at a WIMP mass of 45 GeV, at 90% confidence level., Comment: 5 pages, 3 figures; corrected caption of figure 3
Published: 2013
Full Text: View/download PDF

39. The distributed Slow Control System of the XENON100 experiment

Author: Y. Mei, E. Pantic, Jean-Pierre Cussonneau, F. V. Massoli, Qing Lin, A. Manzur, K. E. Lim, O. Vitells, A. C. C. Ribeiro, Giacomo Bruno, W. Fulgione, A. Rizzo, B. Choi, J. A. M. Lopes, L. Scotto Lavina, A. Kish, Ethan Brown, Gabriella Sartorelli, E. Duchovni, Laura Baudis, W. Hampel, A. D. Ferella, M. Weber, S. E. A. Orrigo, João Cardoso, M. Selvi, F. Gao, G. Plante, T. Marrodán Undagoitia, Kaixuan Ni, Ch. Weinheimer, P. Beltrame, R. Persiani, Hui Wang, W. T. Chen, S. Rosendahl, Marc Schumann, P. Shagin, A. Molinario, A. Teymourian, K. Arisaka, H. Simgen, Uwe Oberlack, P. R. Scovell, S. Fattori, Daniel McKinsey, H. Contreras, F. Arneodo, M. Garbini, Eilam Gross, Luke Goetzke, A. Behrens, K. Bokeloh, Y. Meng, Elena Aprile, E. Nativ, Ran Budnik, A. J. Melgarejo Fernandez, K. Lung, C. Levy, M. Alfonsi, J.M.F. dos Santos, R. F. Lang, M. Le Calloch, Stefan Lindemann, J. Lamblin, J. Schreiner, M. P. Decowski, Manfred Lindner, C. Balan, N. Priel, D. Thers, C. Grignon, K. L. Giboni, J. V. Patricio, E Aprile, M Alfonsi, K Arisaka, F Arneodo, C Balan, L Baudi, A Behren, P Beltrame, K Bokeloh, E Brown, G M Bruno, R Budnik, M Le Calloch, J M Cardoso, W -T Chen, B Choi, H Contrera, J -P Cussonneau, M P Decowski, E Duchovni, S Fattori, A D Ferella, W Fulgione, F Gao, M Garbini, K -L Giboni, L W Goetzke, C Grignon, E Gro, W Hampel, D N McKinsey, A Kish, J Lamblin, R F Lang, C Levy, K E Lim, Q Lin, S Lindemann, M Lindner, J A M Lope, K Lung, A Manzur, T Marrodán Undagoitia, F V Massoli, Y Mei, A J Melgarejo Fernandez, Y Meng, A Molinario, E Nativ, K Ni, U Oberlack, S E A Orrigo, E Pantic, J V Patricio, R Persiani, G Plante, N Priel, A C C Ribeiro, A Rizzo, S Rosendahl, J M F dos Santo, G Sartorelli, J Schreiner, M Schumann, L Scotto Lavina, P R Scovell, M Selvi, P Shagin, H Simgen, A Teymourian, D Ther, O Vitell, H Wang, M Weber, C Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, IoP (FNWI), Gravitation and Astroparticle Physics Amsterdam, GRAPPA (ITFA, IoP, FNWI), Faculty of Science, and Other Research IHEF (IoP, FNWI)
Subjects: Physics - Instrumentation and Detectors, architecture, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Java, Computer science, Real-time computing, FOS: Physical sciences, chemistry.chemical_element, Control and monitor systems online, Control systems, Detector control systems (detector and experiment monitoring and slow-control systems, architecture, hardware, algorithms, databases), algorithms, 01 natural sciences, Xenon, 0103 physical sciences, hardware, DETECTOR CONTROL SYSTEMS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], CONTROL SYSTEMS, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation, Mathematical Physics, computer.programming_language, Time projection chamber, 010308 nuclear & particles physics, business.industry, Detector control systems (detector and experiment monitoring and slow-control systems, Emphasis (telecommunications), Volume (computing), Instrumentation and Detectors (physics.ins-det), Modular design, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], chemistry, Control system, Astrophysics - Instrumentation and Methods for Astrophysics, databases), business, computer, System software
Abstract: The XENON100 experiment, in operation at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, was designed to search for evidence of dark matter interactions inside a volume of liquid xenon using a dual-phase time projection chamber. This paper describes the Slow Control System (SCS) of the experiment with emphasis on the distributed architecture as well as on its modular and expandable nature. The system software was designed according to the rules of Object-Oriented Programming and coded in Java, thus promoting code reusability and maximum flexibility during commissioning of the experiment. The SCS has been continuously monitoring the XENON100 detector since mid 2008, remotely recording hundreds of parameters on a few dozen instruments in real time, and setting emergency alarms for the most important variables., Comment: 12 pages, 4 figures
Published: 2012
Full Text: View/download PDF

40. Dark Matter Results from 100 Live Days of XENON100 Data

Author: K. Arisaka, Marc Schumann, P. Shagin, F. Arneodo, J. A. M. Lopes, A. Kish, G. Sartorelli, K. E. Lim, R. Santorelli, Manfred Lindner, C. W. Lam, K. Bokeloh, S. Fattori, A. Behrens, M. Selvi, J. Lamblin, Eilam Gross, Elena Aprile, David B. Cline, D. Thers, Y. Mei, E. Pantic, R. F. Lang, A. Teymourian, R. Persiani, Ethan Brown, T. Bruch, K. L. Giboni, Hardy Simgen, A. D. Ferella, Hongwei Wang, M. Weber, T. Marrodán Undagoitia, C. Levy, Ch. Weinheimer, B. Choi, G. Plante, K. Lung, Laura Baudis, J.M.F. dos Santos, Sebastian Lindemann, Kaixuan Ni, A. J. Melgarejo Fernandez, S. E. A. Orrigo, A. C. C. Ribeiro, Giacomo Bruno, O. Vitells, Uwe Oberlack, Qing Lin, Ehud Duchovni, A. Askin, João Cardoso, F. Gao, W. T. Chen, E. Aprile, K. Arisaka, F. Arneodo, A. Askin, L. Baudi, A. Behren, K. Bokeloh, E. Brown, T. Bruch, G. Bruno, J. M. R. Cardoso, W.-T. Chen, B. Choi, D. Cline, E. Duchovni, S. Fattori, A. D. Ferella, F. Gao, K.-L. Giboni, E. Gro, A. Kish, C. W. Lam, J. Lamblin, R. F. Lang, C. Levy, K. E. Lim, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, T. Marrodan Undagoitia, Y. Mei, A. J. Melgarejo Fernandez, K. Ni| U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, G. Plante, A. C. C. Ribeiro, R. Santorelli, J. M. F. dos Santo, G. Sartorelli, M. Schumann, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, O. Vitell, H. Wang, M. Weber, C. Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and XENON100
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large Underground Xenon experiment, 010308 nuclear & particles physics, DARK MATTER, Dark matter, Hadron, FOS: Physical sciences, General Physics and Astronomy, Elementary particle, Fermion, 01 natural sciences, Particle detector, High Energy Physics - Experiment, WIMPS, Nuclear physics, High Energy Physics - Experiment (hep-ex), XENON, WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], TPC, 010306 general physics, Nucleon, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results from the direct search for dark matter with the XENON100 detector, installed underground at the Laboratori Nazionali del Gran Sasso of INFN, Italy. XENON100 is a two-phase time projection chamber with a 62 kg liquid xenon target. Interaction vertex reconstruction in three dimensions with millimeter precision allows to select only the innermost 48 kg as ultra-low background fiducial target. In 100.9 live days of data, acquired between January and June 2010, no evidence for dark matter is found. Three candidate events were observed in a pre-defined signal region with an expected background of 1.8 +/- 0.6 events. This leads to the most stringent limit on dark matter interactions today, excluding spin-independent elastic WIMP-nucleon scattering cross-sections above 7.0x10^-45 cm^2 for a WIMP mass of 50 GeV/c^2 at 90% confidence level., 5 pages, 5 figures; matches accepted version
Published: 2011
Full Text: View/download PDF

41. Implications on inelastic dark matter from 100 live days of XENON100 data

Author: E. Pantic, Ethan Brown, M. Selvi, David B. Cline, Y. Mei, J.M.F. dos Santos, Hui Wang, T. Marrodán Undagoitia, Manfred Lindner, Ch. Weinheimer, B. Choi, A. Behrens, Sebastian Lindemann, Karl Giboni, K. Arisaka, R. Santorelli, F. Arneodo, M. Weber, G. Plante, Hardy Simgen, A. D. Ferella, S. Fattori, J. A. M. Lopes, K. Lung, A. Kish, Laura Baudis, A. Teymourian, C. W. Lam, D. Thers, R. F. Lang, A. C. C. Ribeiro, Giacomo Bruno, Elena Aprile, C. Levy, T. Bruch, Kaixuan Ni, K. E. Lim, S. E. A. Orrigo, J. Lamblin, Uwe Oberlack, O. Vitells, Ehud Duchovni, A. J. Melgarejo Fernandez, Qing Lin, A. Askin, João Cardoso, F. Gao, W. T. Chen, Marc Schumann, P. Shagin, G. Sartorelli, R. Persiani, K. Bokeloh, E. K. U. Gross, E. Aprile, K. Arisaka, F. Arneodo, A. Askin, L. Baudi, A. Behren, K. Bokeloh, E. Brown, T. Bruch, G. Bruno, J. M. R. Cardoso, W.-T. Chen, B. Choi, D. Cline, E. Duchovni, S. Fattori, A. D. Ferella, F. Gao, K.-L. Giboni, E. Gro, A. Kish, C. W. Lam, J. Lamblin, R. F. Lang, C. Levy, K. E. Lim, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, T. Marrodán Undagoitia, Y. Mei, A. J. Melgarejo Fernandez, K. Ni, U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, G. Plante, A. C. C. Ribeiro, R. Santorelli, J. M. F. dos Santo, G Sartorelli, M. Schumann, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, O. Vitell, H. Wang, M. Weber, C. Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and XENON100
Subjects: Physics, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Scattering, DARK MATTER, Signal region, Dark matter, FOS: Physical sciences, 01 natural sciences, WIMPS, Nuclear physics, XENON, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], TPC, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The XENON100 experiment has recently completed a dark matter run with 100.9 live-days of data, taken from January to June 2010. Events in a 48kg fiducial volume in the energy range between 8.4 and 44.6 keVnr have been analyzed. A total of three events have been found in the predefined signal region, compatible with the background prediction of (1.8 \pm 0.6) events. Based on this analysis we present limits on the WIMP-nucleon cross section for inelastic dark matter. With the present data we are able to rule out the explanation for the observed DAMA/LIBRA modulation as being due to inelastic dark matter scattering off iodine at a 90% confidence level., Comment: 3 pages, 3 figures
Published: 2011
Full Text: View/download PDF

42. Observation and applications of single-electron charge signals in the XENON100 experiment

Author: F. V. Massoli, Qing Lin, W. Fulgione, Y. Meng, H. Landsman, Uwe Oberlack, M. Garbini, João Cardoso, B. Choi, F. Gao, W. T. Chen, S. E. A. Orrigo, M. Messina, K. Arisaka, A. Behrens, M. Weber, Auke-Pieter Colijn, K. E. Lim, F. Piastra, S. Fattori, Abbe Brown, G. Kessler, G. Plante, W. Hampel, O. Vitells, R. Persiani, R. Itay, J. Naganoma, F. Arneodo, M. Selvi, A. J. Melgarejo Fernandez, Kaixuan Ni, Hui Wang, E. Pantic, H. Simgen, M. Le Calloch, M. Alfonsi, C. Grignon, K. L. Giboni, Florian Kaether, Boris Bauermeister, C. Balan, J. A. M. Lopes, A. Kish, Elena Aprile, Eilam Gross, Giacomo Bruno, T. Marrodán Undagoitia, Luke Goetzke, S. Bruenner, Ch. Weinheimer, C. Ghag, K. Bokeloh, C. Levy, J. Schreiner, M. P. Decowski, H. Contreras, Manfred Lindner, R. F. Lang, A. Molinario, N. Priel, Jean-Pierre Cussonneau, P. Beltrame, S. Rosendahl, A. Teymourian, A. Rizzo, Ethan Brown, Marc Schumann, P. Shagin, J. Lamblin, D. Thers, E. Duchovni, Laura Baudis, Ran Budnik, Gabriella Sartorelli, L. Scotto Lavina, K. Lung, A. D. Ferella, J.M.F. dos Santos, Sebastian Lindemann, E Aprile, M Alfonsi, K Arisaka, F Arneodo, C Balan, L Baudi, B Bauermeister, A Behren, P Beltrame, K Bokeloh, A Brown, E Brown, S Bruenner, G Bruno, R Budnik, J M R Cardoso, W-T Chen, B Choi, A P Colijn, H Contrera, J P Cussonneau, M P Decowski, E Duchovni, S Fattori, A D Ferella, W Fulgione, F Gao, M Garbini, C Ghag, K-L Giboni, L W Goetzke, C Grignon, E Gro, W Hampel, R Itay, F Kaether, G Kessler, A Kish, J Lamblin, H Landsman, R F Lang, M Le Calloch, C Levy, K E Lim, Q Lin, S Lindemann, M Lindner, J A M Lope, K Lung, T Marrodán Undagoitia, F V Massoli, A J Melgarejo Fernandez, Y Meng, M Messina, A Molinario, J Naganoma, K Ni, U Oberlack, S E A Orrigo, E Pantic, R Persiani, F Piastra, G Plante, N Priel, A Rizzo, S Rosendahl, J M F dos Santo, G Sartorelli, J Schreiner, M Schumann, L Scotto Lavina, M Selvi, P Shagin, H Simgen, A Teymourian, D Ther, O Vitell, H Wang, M Weber, C Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, Astroparticle Physics (IHEF, IoP, FNWI), and The XENON100 collaboration
Subjects: Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Drift velocity, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Instrumentation and Detectors, Dark matter, chemistry.chemical_element, FOS: Physical sciences, double phase TPC, 01 natural sciences, dark matter, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Xenon, WIMP, photoionization, single electron, xenon, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Time projection chamber, 010308 nuclear & particles physics, Scattering, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), 3. Good health, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], chemistry, Weakly interacting massive particles, Atomic physics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The XENON100 dark matter experiment uses liquid xenon in a time projection chamber (TPC) to measure xenon nuclear recoils resulting from the scattering of dark matter Weakly Interacting Massive Particles (WIMPs). In this paper, we report the observation of single-electron charge signals which are not related to WIMP interactions. These signals, which show the excellent sensitivity of the detector to small charge signals, are explained as being due to the photoionization of impurities in the liquid xenon and of the metal components inside the TPC. They are used as a unique calibration source to characterize the detector. We explain how we can infer crucial parameters for the XENON100 experiment: the secondary-scintillation gain, the extraction yield from the liquid to the gas phase and the electron drift velocity., Comment: 16 pages, 8 figures. Accepted for publication in Journal of Physics G: Nuclear and Particle Physics
Published: 2014
Full Text: View/download PDF

43. Conceptual design and simulation of a water Cherenkov muon veto for the XENON1T experiment

Author: Y. Meng, M. Murra, N. Priel, Jean-Pierre Cussonneau, M. Messina, Florian Kaether, M. Selvi, K. Arisaka, Gian Carlo Trinchero, Eilam Gross, A. Rizzo, A. Behrens, C. Reuter, S. Schindler, Luke Goetzke, S. E. A. Orrigo, J. A. M. Lopes, J. Naganoma, Auke-Pieter Colijn, A. Kish, D. Mayani Paras, Gabriella Sartorelli, A. Lyashenko, R. Persiani, S. Reichard, A. Molinario, L. Levinson, B. Miguez, F. Arneodo, P. Barrow, Giacomo Bruno, F. V. Massoli, A. Teymourian, S. Fattori, W. Hampel, Amos Breskin, Boris Bauermeister, R. F. Lang, E. Pantic, K. Bokeloh, D. Lellouch, Ethan Brown, João Cardoso, L. Scotto Lavina, W. Fulgione, J. Schreiner, M. Weber, S. MacMullin, M. P. Decowski, Manfred Lindner, Ran Budnik, A. D. Ferella, G. Kessler, K. Lung, D. Thers, G. Plante, A. Tiseni, Hongwei Wang, C. Grignon, F. Piastra, J.M.F. dos Santos, Marc Schumann, P. Shagin, Julien Masbou, H. Simgen, J. Pienaar, F. Agostini, A. J. Melgarejo Fernandez, M. Auger, M. Alfonsi, P. Beltrame, S. Rosendahl, Sebastian Lindemann, C. Balan, G. Morana, Elena Aprile, T. Marrodán Undagoitia, Ch. Weinheimer, Uwe Oberlack, April S. Brown, R. Itay, M. Garbini, E. Duchovni, Laura Baudis, M. Le Calloch, S. Bruenner, C. Levy, O. Vitells, C. Geis, H. Contreras, H. Landsman, E. Aprile, F. Agostini, M. Alfonsi, K. Arisaka, F. Arneodo, M. Auger, C. Balan, P. Barrow, L. Baudi, B. Bauermeister, A. Behren, P. Beltrame, K. Bokeloh, A. Breskin, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, J.M.R. Cardoso, A.P. Colijn, H. Contrera, J.P. Cussonneau, M.P. Decowski, E. Duchovni, S. Fattori, A.D. Ferella, W. Fulgione, M. Garbini, C. Gei, L.W. Goetzke, C. Grignon, E. Gro, W. Hampel, R. Itay, F. Kaether, G. Kessler, A. Kish, H. Landsman, R.F. Lang, M. Le Calloch, D. Lellouch, L. Levinson, C. Levy, S. Lindemann, M. Lindner, J.A.M. Lope, K. Lung, A. Lyashenko, S. MacMullin, T. Marrodán Undagoitia, J. Masbou, F.V. Massoli, D. Mayani Para, A.J. Melgarejo Fernandez, Y. Meng, M. Messina, B. Miguez, A. Molinario, G. Morana, M. Murra, J. Naganoma, U. Oberlack, S.E.A. Orrigo, E. Pantic, R. Persiani, F. Piastra, J. Pienaar, G. Plante, N. Priel, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, J.M.F. dos Santo, G. Sartorelli, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, A. Tiseni, G. Trinchero, O. Vitell, H. Wang, M. Weber, C. Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), XENON100, Gravitation and Astroparticle Physics Amsterdam, IHEF (IoP, FNWI), IoP (FNWI), Faculty of Science, Other Research IHEF (IoP, FNWI), GRAPPA (ITFA, IoP, FNWI), and The XENON100 Collabration
Subjects: axions, Physics - Instrumentation and Detectors, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cherenkov and transition radiation, Cherenkov detector, Physics::Instrumentation and Detectors, Dark matter, Detector modelling and simulations I (interaction of radiation with matter, chemistry.chemical_element, FOS: Physical sciences, 01 natural sciences, law.invention, Nuclear physics, Xenon, WIMP, law, Cherenkov and transition radiation, Detector modelling and simulations, Cherenkov detectors, Dark Matter detectors, etc.), 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Dark Matter detectors (WIMPs, Mathematical Physics, Cherenkov radiation, etc), Physics, Muon, Time projection chamber, 010308 nuclear & particles physics, Cherenkov detectors, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, interaction of photons with matter, Instrumentation and Detectors (physics.ins-det), Dark Matter detectors (WIMPs, axions, etc.), interaction of hadrons with matter, etc), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], interaction of hadrons with matter, chemistry, High Energy Physics::Experiment, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: XENON is a direct detection dark matter project, consisting of a time projection chamber (TPC) that uses xenon in double phase as a sensitive detection medium. XENON100, located at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, is one of the most sensitive experiments of its field. During the operation of XENON100, the design and construction of the next generation detector (of ton-scale mass) of the XENON project, XENON1T, is taking place. XENON1T is being installed at LNGS as well. It has the goal to reduce the background by two orders of magnitude compared to XENON100, aiming at a sensitivity of $2 \cdot 10^{-47} \mathrm{cm}^{\mathrm{2}}$ for a WIMP mass of 50 GeV/c$^{2}$. With this goal, an active system that is able to tag muons and their induced backgrounds is crucial. This active system will consist of a water Cherenkov detector realized with a water volume $\sim$10 m high and $\sim$10 m in diameter, equipped with photomultipliers of 8 inches diameter and a reflective foil. In this paper we present the design and optimization study for this muon veto water Cherenkov detector, which has been carried out with a series of Monte Carlo simulations, based on the GEANT4 toolkit. This study showed the possibility to reach very high detection efficiencies in tagging the passage of both the muon and the shower of secondary particles coming from the interaction of the muon in the rock: >99.5% for the former type of events (which represent $\sim$ 1/3 of all the cases) and >70% for the latter type of events (which represent $\sim$ 2/3 of all the cases). In view of the upgrade of XENON1T, that will aim to an improvement in sensitivity of one order of magnitude with a rather easy doubling of the xenon mass, the results of this study have been verified in the upgraded geometry, obtaining the same conclusions.
Published: 2014
Full Text: View/download PDF

44. Dark matter results from 225 live days of XENON100 data

Author: W. Hampel, M. Garbini, J.M.F. dos Santos, J. Lamblin, K. Bokeloh, Jean-Pierre Cussonneau, S. Rosendahl, Ethan Brown, M. Selvi, Sebastian Lindemann, Eilam Gross, Boris Bauermeister, P. Beltrame, Jochen Schreiner, Luke Goetzke, Hardy Simgen, A. D. Ferella, G. Sartorelli, A. Teymourian, F. Arneodo, Laura Baudis, H. Landsman, M. Le Calloch, J. A. M. Lopes, S. Fattori, Y. Meng, O. Vitells, A. Rizzo, David B. Cline, S. E. A. Orrigo, A. Kish, João Cardoso, K. Arisaka, R. Persiani, L. Scotto Lavina, C. Grignon, K. L. Giboni, H. Contreras, F. Gao, A. Behrens, E. Pantic, C. Balan, D. Thers, Ehud Duchovni, W. T. Chen, K. E. Lim, M. Weber, Auke-Pieter Colijn, R. F. Lang, Uwe Oberlack, Elena Aprile, Kaixuan Ni, E. Nativ, T. Marrodán Undagoitia, G. Plante, B. Choi, Ch. Weinheimer, A. J. Melgarejo Fernandez, P. R. Scovell, C. Ghag, F. V. Massoli, Qing Lin, M. Alfonsi, K. Lung, A. Molinario, W. Fulgione, Giacomo Bruno, C. Levy, N. Priel, Hui Wang, Florian Kaether, M. P. Decowski, Manfred Lindner, Marc Schumann, P. Shagin, Ran Budnik, Astroparticle Physics (IHEF, IoP, FNWI), E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudi, B. Bauermeister, A. Behren, P. Beltrame, K. Bokeloh, E. Brown, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, D. Cline, A. P. Colijn, H. Contrera, J. P. Cussonneau, M. P. Decowski, E. Duchovni, S. Fattori, A. D. Ferella, W. Fulgione, F. Gao, M. Garbini, C. Ghag, K.-L. Giboni, L. W. Goetzke, C. Grignon, E. Gro, W. Hampel, F. Kaether, A. Kish, J. Lamblin, H. Landsman, R. F. Lang, M. Le Calloch, C. Levy, K. E. Lim, Q. Lin, S. Lindemann, M. Lindner, J. A. M. Lope, K. Lung, T. Marrodán Undagoitia, F. V. Massoli, A. J. Melgarejo Fernandez, Y. Meng, A. Molinario, E. Nativ, K. Ni, U. Oberlack, S. E. A. Orrigo, E. Pantic, R. Persiani, G. Plante, N. Priel, A. Rizzo, S. Rosendahl, J. M. F. dos Santo, G. Sartorelli, J. Schreiner, M. Schumann, L. Scotto Lavina, P. R. Scovell, M. Selvi, P. Shagin, H. Simgen, A. Teymourian, D. Ther, O. Vitell, H. Wang, M. Weber, C. Weinheimer, Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), and XENON100
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics - Instrumentation and Detectors, Large Underground Xenon experiment, Dark matter, FOS: Physical sciences, General Physics and Astronomy, WIMP Argon Programme, 01 natural sciences, 7. Clean energy, Particle detector, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Liquid Xenon, Physics, Range (particle radiation), 010308 nuclear & particles physics, DARK MATTER, Instrumentation and Detectors (physics.ins-det), High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], DAMA/NaI, TPC, PandaX, Direct search for Dark Matter, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on a search for particle dark matter with the XENON100 experiment, operated at the Laboratori Nazionali del Gran Sasso (LNGS) for 13 months during 2011 and 2012. XENON100 features an ultra-low electromagnetic background of (5.3 \pm 0.6) \times 10^-3 events (kg day keVee)^-1 in the energy region of interest. A blind analysis of 224.6 live days \times 34 kg exposure has yielded no evidence for dark matter interactions. The two candidate events observed in the pre-defined nuclear recoil energy range of 6.6-30.5 keVnr are consistent with the background expectation of (1.0 \pm 0.2) events. A Profile Likelihood analysis using a 6.6-43.3 keVnr energy range sets the most stringent limit on the spin-independent elastic WIMP-nucleon scattering cross section for WIMP masses above 8 GeV/c^2, with a minimum of 2 \times 10^-45 cm^2 at 55 GeV/c^2 and 90% confidence level., 6 pages, 5 figures. Matches version accepted by PRL. Includes limits up to 10 TeV/c^2, published as supplementary material: http://prl.aps.org/supplemental/PRL/v109/i18/e181301 Please cite high mass limits as "Phys. Rev. Lett. 109, 181301 (2012), online supplementary material."
Published: 2012
Full Text: View/download PDF

45. The XENONnT dark matter experiment.

Author: Aprile E, Aalbers J, Abe K, Ahmed Maouloud S, Althueser L, Andrieu B, Angelino E, Angevaare JR, Antochi VC, Antón Martin D, Arneodo F, Balata M, Baudis L, Baxter AL, Bazyk M, Bellagamba L, Biondi R, Bismark A, Brookes EJ, Brown A, Bruenner S, Bruno G, Budnik R, Bui TK, Cai C, Cardoso JMR, Cassese F, Chiarini A, Cichon D, Cimental Chavez AP, Colijn AP, Conrad J, Corrieri R, Cuenca-García JJ, Cussonneau JP, Dadoun O, D'Andrea V, Decowski MP, De Fazio B, Gangi PD, Diglio S, Disdier JM, Douillet D, Eitel K, Elykov A, Farrell S, Ferella AD, Ferrari C, Fischer H, Flierman M, Form S, Front D, Fulgione W, Fuselli C, Gaemers P, Gaior R, Rosso AG, Galloway M, Gao F, Gardner R, Garroum N, Glade-Beucke R, Grandi L, Grigat J, Guan H, Guerzoni M, Guida M, Hammann R, Higuera A, Hils C, Hoetzsch L, Hood NF, Howlett J, Huhmann C, Iacovacci M, Iaquaniello G, Iven L, Itow Y, Jakob J, Joerg F, Joy A, Kara M, Kavrigin P, Kazama S, Kobayashi M, Koltman G, Kopec A, Kuger F, Landsman H, Lang RF, Levinson L, Li I, Li S, Liang S, Lindemann S, Lindner M, Liu K, Loizeau J, Lombardi F, Long J, Lopes JAM, Ma Y, Macolino C, Mahlstedt J, Mancuso A, Manenti L, Marignetti F, Marrodán Undagoitia T, Martella P, Martens K, Masbou J, Masson D, Masson E, Mastroianni S, Mele E, Messina M, Michinelli R, Miuchi K, Molinario A, Moriyama S, Morå K, Mosbacher Y, Murra M, Müller J, Ni K, Nisi S, Oberlack U, Orlandi D, Othegraven R, Paetsch B, Palacio J, Parlati S, Paschos P, Pellegrini Q, Peres R, Peters C, Pienaar J, Pierre M, Plante G, Pollmann TR, Qi J, Qin J, García DR, Rynge M, Shi J, Singh R, Sanchez L, Santos JMFD, Sarnoff I, Sartorelli G, Schreiner J, Schulte D, Schulte P, Schulze Eißing H, Schumann M, Scotto Lavina L, Selvi M, Semeria F, Shagin P, Shi S, Shockley E, Silva M, Simgen H, Stephen J, Stern M, Stillwell BK, Takeda A, Tan PL, Tatananni D, Terliuk A, Thers D, Toschi F, Trinchero G, Tunnell C, Tönnies F, Valerius K, Volta G, Weinheimer C, Weiss M, Wenz D, Westermann J, Wittweg C, Wolf T, Wu VHS, Xing Y, Xu D, Xu Z, Yamashita M, Yang L, Ye J, Yuan L, Zavattini G, Zhong M, and Zhu T
Abstract: The multi-staged XENON program at INFN Laboratori Nazionali del Gran Sasso aims to detect dark matter with two-phase liquid xenon time projection chambers of increasing size and sensitivity. The XENONnT experiment is the latest detector in the program, planned to be an upgrade of its predecessor XENON1T. It features an active target of 5.9 tonnes of cryogenic liquid xenon (8.5 tonnes total mass in cryostat). The experiment is expected to extend the sensitivity to WIMP dark matter by more than an order of magnitude compared to XENON1T, thanks to the larger active mass and the significantly reduced background, improved by novel systems such as a radon removal plant and a neutron veto. This article describes the XENONnT experiment and its sub-systems in detail and reports on the detector performance during the first science run., (© The Author(s) 2024.)
Published: 2024
Full Text: View/download PDF

46. Material radiopurity control in the XENONnT experiment.

Author: Aprile E, Abe K, Agostini F, Ahmed Maouloud S, Alfonsi M, Althueser L, Angelino E, Angevaare JR, Antochi VC, Antón Martin D, Arneodo F, Baudis L, Baxter AL, Bellagamba L, Biondi R, Bismark A, Brown A, Bruenner S, Bruno G, Budnik R, Capelli C, Cardoso JMR, Cichon D, Cimmino B, Clark M, Colijn AP, Conrad J, Cuenca-García JJ, Cussonneau JP, D'Andrea V, Decowski MP, Gangi PD, Pede SD, Giovanni AD, Stefano RD, Diglio S, Elykov A, Farrell S, Ferella AD, Fischer H, Fulgione W, Gaemers P, Gaior R, Galloway M, Gao F, Glade-Beucke R, Grandi L, Grigat J, Higuera A, Hils C, Hiraide K, Hoetzsch L, Howlett J, Iacovacci M, Itow Y, Jakob J, Joerg F, Kato N, Kavrigin P, Kazama S, Kobayashi M, Koltman G, Kopec A, Landsman H, Lang RF, Levinson L, Li I, Liang S, Lindemann S, Lindner M, Liu K, Lombardi F, Long J, Lopes JAM, Ma Y, Macolino C, Mahlstedt J, Mancuso A, Manenti L, Manfredini A, Marignetti F, Marrodán Undagoitia T, Martens K, Masbou J, Masson D, Masson E, Mastroianni S, Messina M, Miuchi K, Mizukoshi K, Molinario A, Moriyama S, Morå K, Mosbacher Y, Murra M, Ni K, Oberlack U, Palacio J, Peres R, Pienaar J, Pierre M, Pizzella V, Plante G, Qi J, Qin J, Ramírez García D, Reichard S, Rocchetti A, Rupp N, Sanchez L, Dos Santos JMF, Sartorelli G, Schreiner J, Schulte D, Schulze Eißing H, Schumann M, Lavina LS, Selvi M, Semeria F, Shagin P, Shockley E, Silva M, Simgen H, Takeda A, Tan PL, Terliuk A, Therreau C, Thers D, Toschi F, Trinchero G, Tunnell C, Tönnies F, Valerius K, Volta G, Wei Y, Weinheimer C, Weiss M, Wenz D, Westermann J, Wittweg C, Wolf T, Xu Z, Yamashita M, Yang L, Ye J, Yuan L, Zavattini G, Zhang Y, Zhong M, Zhu T, Zopounidis JP, Laubenstein M, and Nisi S
Abstract: The selection of low-radioactive construction materials is of the utmost importance for rare-event searches and thus critical to the XENONnT experiment. Results of an extensive radioassay program are reported, in which material samples have been screened with gamma-ray spectroscopy, mass spectrometry, and 222 Rn emanation measurements. Furthermore, the cleanliness procedures applied to remove or mitigate surface contamination of detector materials are described. Screening results, used as inputs for a XENONnT Monte Carlo simulation, predict a reduction of materials background ( ∼ 17%) with respect to its predecessor XENON1T. Through radon emanation measurements, the expected 222 Rn activity concentration in XENONnT is determined to be 4.2 ( - 0.7 + 0.5 ) μ Bq/kg, a factor three lower with respect to XENON1T. This radon concentration will be further suppressed by means of the novel radon distillation system., (© The Author(s) 2022.)
Published: 2022
Full Text: View/download PDF

47. 222 Rn emanation measurements for the XENON1T experiment.

Author: Aprile E, Aalbers J, Agostini F, Alfonsi M, Althueser L, Amaro FD, Antochi VC, Angelino E, Angevaare JR, Arneodo F, Barge D, Baudis L, Bauermeister B, Bellagamba L, Benabderrahmane ML, Berger T, Breur PA, Brown A, Brown E, Bruenner S, Bruno G, Budnik R, Capelli C, Cardoso JMR, Cichon D, Cimmino B, Clark M, Coderre D, Colijn AP, Conrad J, Cussonneau JP, Decowski MP, Depoian A, Di Gangi P, Di Giovanni A, Di Stefano R, Diglio S, Elykov A, Eurin G, Ferella AD, Fulgione W, Gaemers P, Gaior R, Rosso AG, Galloway M, Gao F, Grandi L, Garbini M, Hasterok C, Hils C, Hiraide K, Hoetzsch L, Hogenbirk E, Howlett J, Iacovacci M, Itow Y, Joerg F, Kato N, Kazama S, Kobayashi M, Koltman G, Kopec A, Landsman H, Lang RF, Levinson L, Lin Q, Lindemann S, Lindner M, Lombardi F, Lopes JAM, López Fune E, Macolino C, Mahlstedt J, Manenti L, Manfredini A, Marignetti F, Undagoitia TM, Martens K, Masbou J, Masson D, Mastroianni S, Messina M, Miuchi K, Molinario A, Morå K, Moriyama S, Mosbacher Y, Murra M, Naganoma J, Ni K, Oberlack U, Odgers K, Palacio J, Pelssers B, Peres R, Pienaar J, Pizzella V, Plante G, Qin J, Qiu H, García DR, Reichard S, Rocchetti A, Rupp N, Santos JMFD, Sartorelli G, Šarčević N, Scheibelhut M, Schindler S, Schreiner J, Schulte D, Schumann M, Lavina LS, Selvi M, Semeria F, Shagin P, Shockley E, Silva M, Simgen H, Takeda A, Therreau C, Thers D, Toschi F, Trinchero G, Tunnell C, Vargas M, Volta G, Wack O, Wang H, Wei Y, Weinheimer C, Weiss M, Wenz D, Westermann J, Wittweg C, Wulf J, Xu Z, Yamashita M, Ye J, Zavattini G, Zhang Y, Zhu T, and Zopounidis JP
Abstract: The selection of low-radioactive construction materials is of utmost importance for the success of low-energy rare event search experiments. Besides radioactive contaminants in the bulk, the emanation of radioactive radon atoms from material surfaces attains increasing relevance in the effort to further reduce the background of such experiments. In this work, we present the 222 Rn emanation measurements performed for the XENON1T dark matter experiment. Together with the bulk impurity screening campaign, the results enabled us to select the radio-purest construction materials, targeting a 222 Rn activity concentration of 10 μ Bq / kg in 3.2 t of xenon. The knowledge of the distribution of the 222 Rn sources allowed us to selectively eliminate problematic components in the course of the experiment. The predictions from the emanation measurements were compared to data of the 222 Rn activity concentration in XENON1T. The final 222 Rn activity concentration of ( 4.5 ± 0.1 ) μ Bq / kg in the target of XENON1T is the lowest ever achieved in a xenon dark matter experiment., (© The Author(s) 2021.)
Published: 2021
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

47 results on '"U Oberlack"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources