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arxiv 1404.1455 v3 pith:REMBRDBR submitted 2014-04-05 astro-ph.CO astro-ph.GAhep-ph

First Axion Results from the XENON100 Experiment

The XENON100 Collaboration: E. Aprile , F. Agostini , M. Alfonsi , K. Arisaka , F. Arneodo , M. Auger , C. Balan , P. Barrow
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L. Baudis B. Bauermeister A. Behrens P. Beltrame K. Bokeloh A. Brown E. Brown S. Bruenner G. Bruno R. Budnik J. M. R. Cardoso A. P. Colijn H. Contreras J. P. Cussonneau M. P. Decowski E. Duchovni S. Fattori A. D. Ferella W. Fulgione F. Gao M. Garbini C. Geis L. W. Goetzke C. Grignon E. Gross 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. Lopes K. Lung A. Lyashenko S. Macmullin T. Marrodan Undagoitia J. Masbou F. V. Massoli D. Mayani Paras A. J. Melgarejo Fernandez Y. Meng M. Messina B. Miguez A. Molinario 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 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 O. Vitells H. Wang M. Weber C. Weinheimer
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classification astro-ph.CO astro-ph.GAhep-ph
keywords timesaxionaxion-like-particlesaxionsbestcouplingdateexperiment
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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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.

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