Search for inelastic scattering of WIMP dark matter in XENON1T. (arXiv:2011.10431v2 [hep-ex] UPDATED)

Search for inelastic scattering of WIMP dark matter in XENON1T. (arXiv:2011.10431v2 [hep-ex] UPDATED)
<a href="http://arxiv.org/find/hep-ex/1/au:+Collaboration_XENON/0/1/0/all/0/1">XENON Collaboration</a>: <a href="http://arxiv.org/find/hep-ex/1/au:+Aprile_E/0/1/0/all/0/1">E. Aprile</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Aalbers_J/0/1/0/all/0/1">J. Aalbers</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Agostini_F/0/1/0/all/0/1">F. Agostini</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Alfonsi_M/0/1/0/all/0/1">M. Alfonsi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Althueser_L/0/1/0/all/0/1">L. Althueser</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Amaro_F/0/1/0/all/0/1">F. D. Amaro</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Andaloro_S/0/1/0/all/0/1">S. Andaloro</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Angelino_E/0/1/0/all/0/1">E. Angelino</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Angevaare_J/0/1/0/all/0/1">J. R. Angevaare</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Antochi_V/0/1/0/all/0/1">V. C. Antochi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Arneodo_F/0/1/0/all/0/1">F. Arneodo</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Baudis_L/0/1/0/all/0/1">L. Baudis</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bauermeister_B/0/1/0/all/0/1">B. Bauermeister</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bellagamba_L/0/1/0/all/0/1">L. Bellagamba</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Benabderrahmane_M/0/1/0/all/0/1">M. L. Benabderrahmane</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brown_A/0/1/0/all/0/1">A. Brown</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brown_E/0/1/0/all/0/1">E. Brown</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bruenner_S/0/1/0/all/0/1">S. Bruenner</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bruno_G/0/1/0/all/0/1">G. Bruno</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Budnik_R/0/1/0/all/0/1">R. Budnik</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Capelli_C/0/1/0/all/0/1">C. Capelli</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cardoso_J/0/1/0/all/0/1">J. M. R. Cardoso</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cichon_D/0/1/0/all/0/1">D. Cichon</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cimmino_B/0/1/0/all/0/1">B. Cimmino</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Clark_M/0/1/0/all/0/1">M. Clark</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Coderre_D/0/1/0/all/0/1">D. Coderre</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Colijn_A/0/1/0/all/0/1">A. P. Colijn</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Conrad_J/0/1/0/all/0/1">J. Conrad</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cuenca_J/0/1/0/all/0/1">J. Cuenca</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cussonneau_J/0/1/0/all/0/1">J. P. Cussonneau</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Decowski_M/0/1/0/all/0/1">M. P. Decowski</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Depoian_A/0/1/0/all/0/1">A. Depoian</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Gangi_P/0/1/0/all/0/1">P. Di Gangi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Giovanni_A/0/1/0/all/0/1">A. Di Giovanni</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Stefano_R/0/1/0/all/0/1">R. Di Stefano</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Diglio_S/0/1/0/all/0/1">S. Diglio</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Elykov_A/0/1/0/all/0/1">A. Elykov</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Ferella_A/0/1/0/all/0/1">A. D. Ferella</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Fulgione_W/0/1/0/all/0/1">W. Fulgione</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Gaemers_P/0/1/0/all/0/1">P. Gaemers</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Gaior_R/0/1/0/all/0/1">R. Gaior</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Galloway_M/0/1/0/all/0/1">M. Galloway</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Gao_F/0/1/0/all/0/1">F. Gao</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Grandi_L/0/1/0/all/0/1">L. Grandi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hils_C/0/1/0/all/0/1">C. Hils</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hiraide_K/0/1/0/all/0/1">K. Hiraide</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hoetzsch_L/0/1/0/all/0/1">L. Hoetzsch</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Howlett_J/0/1/0/all/0/1">J. Howlett</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Iacovacci_M/0/1/0/all/0/1">M. Iacovacci</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Itow_Y/0/1/0/all/0/1">Y. Itow</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Joerg_F/0/1/0/all/0/1">F. Joerg</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kato_N/0/1/0/all/0/1">N. Kato</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kazama_S/0/1/0/all/0/1">S. Kazama</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kobayashi_M/0/1/0/all/0/1">M. Kobayashi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Koltman_G/0/1/0/all/0/1">G. Koltman</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kopec_A/0/1/0/all/0/1">A. Kopec</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Landsman_H/0/1/0/all/0/1">H. Landsman</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lang_R/0/1/0/all/0/1">R. F. Lang</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Levinson_L/0/1/0/all/0/1">L. Levinson</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Liang_S/0/1/0/all/0/1">S. Liang</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lin_Q/0/1/0/all/0/1">Q. Lin</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lindemann_S/0/1/0/all/0/1">S. Lindemann</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lindner_M/0/1/0/all/0/1">M. Lindner</a>, et al. (77 additional authors not shown)

We report the results of a search for the inelastic scattering of weakly
interacting massive particles (WIMPs) in the XENON1T dark matter experiment.
Scattering off $^{129}$Xe is the most sensitive probe of inelastic WIMP
interactions, with a signature of a 39.6 keV de-excitation photon detected
simultaneously with the nuclear recoil. Using an exposure of 0.89 tonne-years,
we find no evidence of inelastic WIMP scattering with a significance of more
than 2$sigma$. A profile-likelihood ratio analysis is used to set upper limits
on the cross-section of WIMP-nucleus interactions. We exclude new parameter
space for WIMPs heavier than 100 GeV/c${}^2$, with the strongest upper limit of
$3.3 times 10^{-39}$ cm${}^2$ for 130 GeV/c${}^2$ WIMPs at 90% confidence
level.

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