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arxiv: 1709.02222 · v1 · pith:7ECNZHZHnew · submitted 2017-09-07 · 🌌 astro-ph.CO · hep-ex· hep-ph

Search for Bosonic Super-WIMP Interactions with the XENON100 Experiment

XENON Collaboration: E. Aprile , J. Aalbers , F. Agostini , M. Alfonsi , L. Althueser , F. D. Amaro , M. Anthony , F. Arneodo
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P. Barrow L. Baudis B. Bauermeister M. L. Benabderrahmane T. Berger P. A. Breur A. Brown E. Brown S. Bruenner G. Bruno R. Budnik B\"utikofer J. Calven 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 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 J. Howlett 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. Marrod\'an Undagoitia J. Masbou F. V. Massoli D. Masson D. Mayani M. Messina K. Micheneau A. Molinario K. Mor{\aa} M. Murra J. Naganoma K. Ni U. Oberlack P. Pakarha B. Pelssers R. Persiani F. Piastra J. Pienaar V. Pizzella M.-C. Piro G. Plante N. Priel D. Ram\'irez Garc\'ia 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. v. Sivers A. Stein D. Thers A. Tiseni G. Trinchero C. Tunnell M. Vargas H. Wang Z. Wang Y. Wei C. Weinheimer C. Wittweg J. Wulf J. Ye Y. Zhang T. Zhu
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classification 🌌 astro-ph.CO hep-exhep-ph
keywords super-wimpsxenon100alphabosonicdarkexperimentlimitsmatter
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We present results of searches for vector and pseudo-scalar bosonic super-WIMPs, which are dark matter candidates with masses at the keV-scale, with the XENON100 experiment. XENON100 is a dual-phase xenon time projection chamber operated at the Laboratori Nazionali del Gran Sasso. A profile likelihood analysis of data with an exposure of 224.6 live days $\times$ 34\,kg showed no evidence for a signal above the expected background. We thus obtain new and stringent upper limits in the $(8-125)$\,keV/c$^2$ mass range, excluding couplings to electrons with coupling constants of $g_{ae} > 3\times10^{-13}$ for pseudo-scalar and $\alpha'/\alpha > 2\times10^{-28}$ for vector super-WIMPs, respectively. These limits are derived under the assumption that super-WIMPs constitute all of the dark matter in our galaxy.

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