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1. Analysis of the XENON100 dark matter search data

Author

S. E. A. Orrigo, Marc Schumann, P. Shagin, J. A. M. Lopes, A. Kish, Luke Goetzke, Jean-Pierre Cussonneau, K. E. Lim, Elena Aprile, E. Nativ, W. Hampel, M. Selvi, Ehud Duchovni, K. Bokeloh, E. K. U. Gross, João Cardoso, Hui Wang, Uwe Oberlack, Jochen Schreiner, M. Weber, F. Gao, A. Behrens, T. Marrodán Undagoitia, F. V. Massoli, Qing Lin, M. Le Calloch, J.M.F. dos Santos, O. Vitells, Ch. Weinheimer, A. Rizzo, P. Beltrame, W. Fulgione, N. Priel, C. Grignon, A. J. Melgarejo Fernandez, A. Teymourian, M. Garbini, K. Arisaka, S. Rosendahl, Sebastian Lindemann, M. Alfonsi, F. Arneodo, W. T. Chen, Ran Budnik, Kaixuan Ni, R. Persiani, Karl Giboni, David B. Cline, G. Sartorelli, Laura Baudis, C. Balan, Giacomo Bruno, Hardy Simgen, A. D. Ferella, H. Contreras, E. Pantic, K. Lung, Ethan Brown, M. P. Decowski, Manfred Lindner, Y. Mei, P. R. Scovell, Guillaume Plante, Y. Meng, A. Molinario, S. Fattori, C. Levy, B. Choi, D. Thers, R. F. Lang, J. Lamblin, H. Landsman, L. Scotto Lavina, The XENON100 Collaboration, Astroparticle Physics (IHEF, IoP, FNWI), Aprile, E., Alfonsi, M., Arisaka, K., Arneodo, F., Balan, C., Baudis, L., Behrens, A., Beltrame, P., Bokeloh, K., Brown, E., Bruno, G., Budnik, R., Cardoso, J.M.R., Chen, W.-T., Choi, B., Cline, D.B., Contreras, H., Cussonneau, J.P., Decowski, M.P., Duchovni, E., Fattori, S., Ferella, A.D., Fulgione, W., Gao, F., Garbini, M., Giboni, K.-L., Goetzke, L.W., Grignon, C., Gross, E., Hampel, W., Kish, A., Lamblin, J., Landsman, H., Lang, R.F., Le Calloch, M., Levy, C., Lim, K.E., Lin, Q., Lindemann, S., Lindner, M., Lopes, J.A.M., Lung, K., Marrodán Undagoitia, T., Massoli, F.V., Mei, Y., Melgarejo Fernandez, A.J., Meng, Y., Molinario, A., Nativ, E., Ni, K., Oberlack, U., Orrigo, S.E.A., Pantic, E., Persiani, R., Plante, G., Priel, N., Rizzo, A., Rosendahl, S., Dos Santos, J.M.F., Sartorelli, G., Schreiner, J., Schumann, M., Scotto Lavina, L., Scovell, P.R., Selvi, M., Shagin, P., Simgen, H., Teymourian, A., Thers, D., Vitells, O., Wang, H., Weber, M., and Weinheimer, C.

Subjects
Large Underground Xenon experiment, Physics - Instrumentation and Detectors, Xenon, WIMP, Physics::Instrumentation and Detectors, Direct detection, Dark matter, chemistry.chemical_element, FOS: Physical sciences, DarkSide, WIMP Argon Programme, Nuclear physics, Statistical analysis, Nuclear Experiment, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Time projection chamber, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), WIMPs, chemistry, Weakly interacting massive particles, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The XENON100 experiment, situated in the Laboratori Nazionali del Gran Sasso, aims at the direct detection of dark matter in the form of weakly interacting massive particles (WIMPs), based on their interactions with xenon nuclei in an ultra low background dual-phase time projection chamber. This paper describes the general methods developed for the analysis of the XENON100 data. These methods have been used in the 100.9 and 224.6 live days science runs from which results on spin-independent elastic, spin-dependent elastic and inelastic WIMP-nucleon cross-sections have already been reported., Comment: 18 pages, 17 figures, information for the 224.6 live days run included

Published
2014
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2. 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
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3. 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
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