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First Dark Matter Search Results from the XENON1T Experiment

Authors :
Aprile, E.
Aalbers, J.
Agostini, F.
Alfonsi, M.
Amaro, F. D.
Anthony, M.
Arneodo, F.
Barrow, P.
Baudis, L.
Bauermeister, B.
Benabderrahmane, M. L.
Berger, T.
Breur, P. A.
Brown, A.
Brown, E.
Bruenner, S.
Bruno, G.
Budnik, R.
Bütikofer, L.
Calvén, J.
Cardoso, J. M. R.
Cervantes, M.
Cichon, D.
Coderre, D.
Colijn, A. P.
Conrad, J.
Cussonneau, J. P.
Decowski, M. P.
de Perio, P.
Di Gangi, P.
Di Giovanni, A.
Diglio, S.
Eurin, G.
Fei, J.
Ferella, A. D.
Fieguth, A.
Fulgione, W.
Rosso, A. Gallo
Galloway, M.
Gao, F.
Garbini, M.
Gardner, R.
Geis, C.
Goetzke, L. W.
Grandi, L.
Greene, Z.
Grignon, C.
Hasterok, C.
Hogenbirk, E.
Howlett, J.
Itay, R.
Kaminsky, B.
Kazama, S.
Kessler, G.
Kish, A.
Landsman, H.
Lang, R. F.
Lellouch, D.
Levinson, L.
Lin, Q.
Lindemann, S.
Lindner, M.
Lombardi, F.
Lopes, J. A. M.
Manfredini, A.
Mariş, I.
Undagoitia, T. Marrodán
Masbou, J.
Massoli, F. V.
Masson, D.
Mayani, D.
Messina, M.
Micheneau, K.
Molinario, A.
Morå, K.
Murra, M.
Naganoma, J.
Ni, K.
Oberlack, U.
Pakarha, P.
Pelssers, B.
Persiani, R.
Piastra, F.
Pienaar, J.
Pizzella, V.
Piro, M. -C.
Plante, G.
Priel, N.
Rauch, L.
Reichard, S.
Reuter, C.
Riedel, B.
Rizzo, A.
Rosendahl, S.
Rupp, N.
Saldanha, R.
Santos, J. M. F. dos
Sartorelli, G.
Scheibelhut, M.
Schindler, S.
Schreiner, J.
Schumann, M.
Lavina, L. Scotto
Selvi, M.
Shagin, P.
Shockley, E.
Silva, M.
Simgen, H.
Sivers, M. v.
Stein, A.
Thapa, S.
Thers, D.
Tiseni, A.
Trinchero, G.
Tunnell, C.
Vargas, M.
Upole, N.
Wang, H.
Wang, Z.
Wei, Y.
Weinheimer, C.
Wulf, J.
Ye, J.
Zhang, Y.
Zhu, T.
Aprile, E.
Aalbers, J.
Agostini, F.
Alfonsi, M.
Amaro, F. D.
Anthony, M.
Arneodo, F.
Barrow, P.
Baudis, L.
Bauermeister, B.
Benabderrahmane, M. L.
Berger, T.
Breur, P. A.
Brown, A.
Brown, E.
Bruenner, S.
Bruno, G.
Budnik, R.
Bütikofer, L.
Calvén, J.
Cardoso, J. M. R.
Cervantes, M.
Cichon, D.
Coderre, D.
Colijn, A. P.
Conrad, J.
Cussonneau, J. P.
Decowski, M. P.
de Perio, P.
Di Gangi, P.
Di Giovanni, A.
Diglio, S.
Eurin, G.
Fei, J.
Ferella, A. D.
Fieguth, A.
Fulgione, W.
Rosso, A. Gallo
Galloway, M.
Gao, F.
Garbini, M.
Gardner, R.
Geis, C.
Goetzke, L. W.
Grandi, L.
Greene, Z.
Grignon, C.
Hasterok, C.
Hogenbirk, E.
Howlett, J.
Itay, R.
Kaminsky, B.
Kazama, S.
Kessler, G.
Kish, A.
Landsman, H.
Lang, R. F.
Lellouch, D.
Levinson, L.
Lin, Q.
Lindemann, S.
Lindner, M.
Lombardi, F.
Lopes, J. A. M.
Manfredini, A.
Mariş, I.
Undagoitia, T. Marrodán
Masbou, J.
Massoli, F. V.
Masson, D.
Mayani, D.
Messina, M.
Micheneau, K.
Molinario, A.
Morå, K.
Murra, M.
Naganoma, J.
Ni, K.
Oberlack, U.
Pakarha, P.
Pelssers, B.
Persiani, R.
Piastra, F.
Pienaar, J.
Pizzella, V.
Piro, M. -C.
Plante, G.
Priel, N.
Rauch, L.
Reichard, S.
Reuter, C.
Riedel, B.
Rizzo, A.
Rosendahl, S.
Rupp, N.
Saldanha, R.
Santos, J. M. F. dos
Sartorelli, G.
Scheibelhut, M.
Schindler, S.
Schreiner, J.
Schumann, M.
Lavina, L. Scotto
Selvi, M.
Shagin, P.
Shockley, E.
Silva, M.
Simgen, H.
Sivers, M. v.
Stein, A.
Thapa, S.
Thers, D.
Tiseni, A.
Trinchero, G.
Tunnell, C.
Vargas, M.
Upole, N.
Wang, H.
Wang, Z.
Wei, Y.
Weinheimer, C.
Wulf, J.
Ye, J.
Zhang, Y.
Zhu, T.
Publication Year :
2017

Abstract

We report the first dark matter search results from XENON1T, a $\sim$2000-kg-target-mass dual-phase (liquid-gas) xenon time projection chamber in operation at the Laboratori Nazionali del Gran Sasso in Italy and the first ton-scale detector of this kind. The blinded search used 34.2 live days of data acquired between November 2016 and January 2017. Inside the (1042$\pm$12) kg fiducial mass and in the [5, 40] $\mathrm{keV}_{\mathrm{nr}}$ energy range of interest for WIMP dark matter searches, the electronic recoil background was $(1.93 \pm 0.25) \times 10^{-4}$ events/(kg $\times$ day $\times \mathrm{keV}_{\mathrm{ee}}$), the lowest ever achieved in a dark matter detector. A profile likelihood analysis shows that the data is consistent with the background-only hypothesis. We derive the most stringent exclusion limits on the spin-independent WIMP-nucleon interaction cross section for WIMP masses above 10 GeV/c${}^2$, with a minimum of 7.7 $\times 10^{-47}$ cm${}^2$ for 35-GeV/c${}^2$ WIMPs at 90% confidence level.<br />Comment: 6 pages, 4 figures, v2 data upload Fig 2/4, v3 as accepted by PRL with textual clarifications, v4 data upload Fig 1

Details

Database :
OAIster
Publication Type :
Electronic Resource
Accession number :
edsoai.on1138911662
Document Type :
Electronic Resource
Full Text :
https://doi.org/10.1103.PhysRevLett.119.181301