The Xenon1T Dark Matter Search Experiment

  • Elena AprileEmail author
Conference paper
Part of the Springer Proceedings in Physics book series (SPPHY, volume 148)


The worldwide race towards direct dark matter detection in the form of Weakly Interacting Massive Particles (WIMPs) has been dramatically accelerated by the remarkable progress and evolution of liquid xenon time projection chambers (LXeTPCs). With a realistic discovery potential, Xenon100 has already reached a sensitivity of 7 × 10−45 cm2, and continues to accrue data at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy towards its ultimate sensitivity reach at the σ SI ∼ 2 × 10−45 cm2 level for the spin-independent WIMP-nucleon cross-section. To fully explore the favoured parameter space for WIMP dark matter in search of a first robust and statistically significant discovery, or to confirm any hint of a signal from Xenon100, the next phase of the Xenon program will be a detector at the ton scale – Xenon1T. The Xenon1T detector, based on 2.2 ton of LXe viewed by low radioactivity photomultiplier tubes and housed in a water Cherenkov muon veto at LNGS, is presented. With an experimental aim of probing WIMP interaction cross-sections above of order σ SI ∼ 2 × 10−47 cm2 within 2 years of operation, Xenon1T will provide the sensitivity to probe a particularly favourable region of electroweak physics on a timescale compatible with complementary ground and satellite based indirect searches and with accelerator dark matter searches at the LHC. Indeed, for a σ SI ∼ 10−45 cm2 and 100 GeV/c2 WIMP mass, Xenon1T could detect of order 100 events in this exposure, providing statistics for placing significant constraints on the WIMP mass.


Dark Matter Time Projection Chamber Direct Dark Matter Detection Wimp Mass Drift Volume 
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  1. 1.
    Angle, J., et al. (XENON10 Coll.): Phys. Rev. Lett. 100 (2008) 021303 [arXiv:0706.0039]Google Scholar
  2. 2.
    Aprile, E., et al. (XENON100 Coll.): arXiv:1107.2155Google Scholar
  3. 3.
    Aprile, E., et al. (XENON100 Coll.): Phys. Rev. Lett. 107 (2011) 131302 [arXiv:1104.2549]Google Scholar
  4. 4.
    Aprile, E., et al. (XENON100 Coll.): Phys. Rev. D 83 (2011) 082001 [arXiv:1107.2155]Google Scholar
  5. 5.
    Aprile, E., et al. (XENON100 Coll.): Astropart. Phys. 35, 43 (2011)Google Scholar
  6. 6.
    Neder, H., et al.: Appl. Rad. Isot. 53, 191 (2000)CrossRefGoogle Scholar
  7. 7.
    Abe, K., et al. (XMASS Coll.): Astropart. Phys. 31, 290 (2009)Google Scholar
  8. 8.
    Liu, J., et al. (XMASS Coll.): TAUP2011
  9. 9.
    Leonard, D.S., et al. (EXO Coll.): Nucl. Instrum. Meth. A 591 (2008) 490 [arXiv:0709.4524]Google Scholar
  10. 10.
    Trotta, R., et al.: J. High Energy Phys. 12, 024 (2008)MathSciNetADSCrossRefGoogle Scholar
  11. 11.
    Buchmueller, O., et al.: arXiv:1102.4585Google Scholar

Copyright information

© Springer Science+Business Media Dordrecht 2013

Authors and Affiliations

  1. 1.Columbia UniversityNew YorkUSA
  2. 2.XENON collaborationNewYorkUSA

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