Constraining the spin-dependent WIMP-nucleon cross sections with XENON1T. (arXiv:1902.03234v1 [astro-ph.CO])

Constraining the spin-dependent WIMP-nucleon cross sections with XENON1T. (arXiv:1902.03234v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Aprile_E/0/1/0/all/0/1">E. Aprile</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aalbers_J/0/1/0/all/0/1">J. Aalbers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agostini_F/0/1/0/all/0/1">F. Agostini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfonsi_M/0/1/0/all/0/1">M. Alfonsi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Althueser_L/0/1/0/all/0/1">L. Althueser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaro_F/0/1/0/all/0/1">F. D. Amaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anthony_M/0/1/0/all/0/1">M. Anthony</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antochi_V/0/1/0/all/0/1">V. C. Antochi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arneodo_F/0/1/0/all/0/1">F. Arneodo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baudis_L/0/1/0/all/0/1">L. Baudis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bauermeister_B/0/1/0/all/0/1">B. Bauermeister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benabderrahmane_M/0/1/0/all/0/1">M. L. Benabderrahmane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_T/0/1/0/all/0/1">T. Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breur_P/0/1/0/all/0/1">P. A. Breur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">A. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">A. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_E/0/1/0/all/0/1">E. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruenner_S/0/1/0/all/0/1">S. Bruenner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruno_G/0/1/0/all/0/1">G. Bruno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budnik_R/0/1/0/all/0/1">R. Budnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capelli_C/0/1/0/all/0/1">C. Capelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cardoso_J/0/1/0/all/0/1">J. M. R. Cardoso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cichon_D/0/1/0/all/0/1">D. Cichon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coderre_D/0/1/0/all/0/1">D. Coderre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colijn_A/0/1/0/all/0/1">A. P. Colijn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conrad_J/0/1/0/all/0/1">J. Conrad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cussonneau_J/0/1/0/all/0/1">J. P. Cussonneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decowski_M/0/1/0/all/0/1">M. P. Decowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perio_P/0/1/0/all/0/1">P. de Perio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gangi_P/0/1/0/all/0/1">P. Di Gangi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giovanni_A/0/1/0/all/0/1">A. Di Giovanni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diglio_S/0/1/0/all/0/1">S. Diglio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elykov_A/0/1/0/all/0/1">A. Elykov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eurin_G/0/1/0/all/0/1">G. Eurin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fei_J/0/1/0/all/0/1">J. Fei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferella_A/0/1/0/all/0/1">A. D. Ferella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fieguth_A/0/1/0/all/0/1">A. Fieguth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fulgione_W/0/1/0/all/0/1">W. Fulgione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosso_A/0/1/0/all/0/1">A. Gallo Rosso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galloway_M/0/1/0/all/0/1">M. Galloway</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_F/0/1/0/all/0/1">F. Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garbini_M/0/1/0/all/0/1">M. Garbini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grandi_L/0/1/0/all/0/1">L. Grandi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greene_Z/0/1/0/all/0/1">Z. Greene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasterok_C/0/1/0/all/0/1">C. Hasterok</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hogenbirk_E/0/1/0/all/0/1">E. Hogenbirk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howlett_J/0/1/0/all/0/1">J. Howlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iacovacci_M/0/1/0/all/0/1">M. Iacovacci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Itay_R/0/1/0/all/0/1">R. Itay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joerg_F/0/1/0/all/0/1">F. Joerg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazama_S/0/1/0/all/0/1">S. Kazama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kish_A/0/1/0/all/0/1">A. Kish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koltman_G/0/1/0/all/0/1">G. Koltman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kopec_A/0/1/0/all/0/1">A. Kopec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landsman_H/0/1/0/all/0/1">H. Landsman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lang_R/0/1/0/all/0/1">R. F. Lang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levinson_L/0/1/0/all/0/1">L. Levinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Q/0/1/0/all/0/1">Q. Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lindemann_S/0/1/0/all/0/1">S. Lindemann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lindner_M/0/1/0/all/0/1">M. Lindner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lombardi_F/0/1/0/all/0/1">F. Lombardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopes_J/0/1/0/all/0/1">J. A. M. Lopes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fune_E/0/1/0/all/0/1">E. López Fune</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macolino_C/0/1/0/all/0/1">C. Macolino</a>, et al. (66 additional authors not shown)

We report the first experimental results on spin-dependent elastic
WIMP-nucleon scattering from the XENON1T dark matter search experiment. The
analysis uses the full tonne-year exposure of XENON1T to constrain the
spin-dependent proton-only and neutron-only cases. No significant signal excess
is observed, and a profile likelihood ratio analysis is used to set exclusion
limits on the WIMP-nucleon interactions. This includes the most stringent
constraint to date on the WIMP-neutron cross section, with a minimum of
$6.3times10^{-42}$ cm$^2$ at 30 GeV/c${}^2$ and 90% confidence level. The
results are compared with those from collider searches and used to exclude new
parameter space in an isoscalar theory with an axial-vector mediator.

http://arxiv.org/icons/sfx.gif