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Design and performance of the field cage for the XENONnT experiment
E. Aprile, K. Abe, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, G. Bruno, et al (144)
Sep 22 2023 hep-ex physics.ins-det arXiv:2309.11996v1

@misc{2309.11996, author = {E.~Aprile and K.~Abe and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and M.~Bazyk and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Cimental Chávez and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~DÁndrea and M.~P.~Decowski and P.~Di Gangi and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and H.~Guan and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and Q.~Pellegrini and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and G.~Plante and T.~R.~Pollmann and J.~Qi and J.~Qin and D.~Ramírez García and N.~Šarčević and J.~Shi and R.~Singh and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and V.~H.~S.~Wu and Y.~Xing and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{D}esign and performance of the field cage for the {XENON}n{T} experiment}, year = {2023}, eprint = {2309.11996}, note = {arXiv:2309.11996v1} }
PDF
The precision in reconstructing events detected in a dual-phase time projection chamber depends on an homogeneous and well understood electric field within the liquid target. In the XENONnT TPC the field homogeneity is achieved through a double-array field cage, consisting of two nested arrays of field shaping rings connected by an easily accessible resistor chain. Rather than being connected to the gate electrode, the topmost field shaping ring is independently biased, adding a degree of freedom to tune the electric field during operation. Two-dimensional finite element simulations were used to optimize the field cage, as well as its operation. Simulation results were compared to ${}^{83m}\mathrm{Kr}$ calibration data. This comparison indicates an accumulation of charge on the panels of the TPC which is constant over time, as no evolution of the reconstructed position distribution of events is observed. The simulated electric field was then used to correct the charge signal for the field dependence of the charge yield. This correction resolves the inconsistent measurement of the drift electron lifetime when using different calibrations sources and different field cage tuning voltages.
Search for events in XENON1T associated with Gravitational Waves
XENON Collaboration, E. Aprile, K. Abe, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antoń Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, et al (143)
Jun 22 2023 hep-ex physics.ins-det arXiv:2306.11871v2

@misc{2306.11871, author = {XENON Collaboration and E.~Aprile and K.~Abe and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antoń Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and M.~Bazyk and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and A.~P.~Cimental Chavez and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and H.~Guan and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and D.~G.~Layos Carlos and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and Q.~Pellegrini and R.~Peres and C Peters and J.~Pienaar and M.~Pierre and G.~Plante and T.~R.~Pollmann and J.~Qi and J.~Qin and D.~Ramírez García and J.~Shi and R.~Singh and L.Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and V.~H.~S.~Wu and Y.~Xing and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{S}earch for events in {XENON}1{T} associated with {G}ravitational {W}aves}, year = {2023}, eprint = {2306.11871}, note = {arXiv:2306.11871v2} }
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We perform a blind search for particle signals in the XENON1T dark matter detector that occur close in time to gravitational wave signals in the LIGO and Virgo observatories. No particle signal is observed in the nuclear recoil, electronic recoil, CE$\nu$NS, and S2-only channels within $\pm$ 500 seconds of observations of the gravitational wave signals GW170104, GW170729, GW170817, GW170818, and GW170823. We use this null result to constrain mono-energetic neutrinos and Beyond Standard Model particles emitted in the closest coalescence GW170817, a binary neutron star merger. We set new upper limits on the fluence (time-integrated flux) of coincident neutrinos down to 17 keV at 90% confidence level. Furthermore, we constrain the product of coincident fluence and cross section of Beyond Standard Model particles to be less than $10^{-29}$ cm$^2$/cm$^2$ in the [5.5-210] keV energy range at 90% confidence level.
Searching for Heavy Dark Matter near the Planck Mass with XENON1T
E. Aprile, K. Abe, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, G. Bruno, et al (147)
Apr 24 2023 hep-ex physics.ins-det arXiv:2304.10931v1

@misc{2304.10931, author = {E.~Aprile and K.~Abe and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and M.~Bazyk and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Cimental Chavez and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and H.~Guan and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and Q.~Pellegrini and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and T.~R.~Pollmann and J.~Qi and J.~Qin and D.~Ramírez García and R.~Singh and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and V.~H.~S.~Wu and Y.~Xing and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{S}earching for {H}eavy {D}ark {M}atter near the {P}lanck {M}ass with {XENON}1{T}}, year = {2023}, eprint = {2304.10931}, note = {arXiv:2304.10931v1} }
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Multiple viable theoretical models predict heavy dark matter particles with a mass close to the Planck mass, a range relatively unexplored by current experimental measurements. We use 219.4 days of data collected with the XENON1T experiment to conduct a blind search for signals from Multiply-Interacting Massive Particles (MIMPs). Their unique track signature allows a targeted analysis with only 0.05 expected background events from muons. Following unblinding, we observe no signal candidate events. This work places strong constraints on spin-independent interactions of dark matter particles with a mass between 1$\times$10$^{12}\,$GeV/c$^2$ and 2$\times$10$^{17}\,$GeV/c$^2$. In addition, we present the first exclusion limits on spin-dependent MIMP-neutron and MIMP-proton cross-sections for dark matter particles with masses close to the Planck scale.
Detector signal characterization with a Bayesian network in XENONnT
XENON Collaboration, E. Aprile, K. Abe, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, et al (147)
Apr 13 2023 hep-ex arXiv:2304.05428v2

@misc{2304.05428, author = {XENON Collaboration and E.~Aprile and K.~Abe and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and M.~Bazyk and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Cimental Chavez and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and H.~Guan and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and Q.~Pellegrini and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and T.~R.~Pollmann and J.~Qi and J.~Qin and D.~Ramírez García and R.~Singh and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and V.~H.~S.~Wu and Y.~Xing and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{D}etector signal characterization with a {B}ayesian network in {XENON}n{T}}, year = {2023}, eprint = {2304.05428}, howpublished = {Phys. Rev. D 108, 012016 (2023)}, doi = {10.1103/PhysRevD.108.012016}, note = {arXiv:2304.05428v2} }
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We developed a detector signal characterization model based on a Bayesian network trained on the waveform attributes generated by a dual-phase xenon time projection chamber. By performing inference on the model, we produced a quantitative metric of signal characterization and demonstrate that this metric can be used to determine whether a detector signal is sourced from a scintillation or an ionization process. We describe the method and its performance on electronic-recoil (ER) data taken during the first science run of the XENONnT dark matter experiment. We demonstrate the first use of a Bayesian network in a waveform-based analysis of detector signals. This method resulted in a 3% increase in ER event-selection efficiency with a simultaneously effective rejection of events outside of the region of interest. The findings of this analysis are consistent with the previous analysis from XENONnT, namely a background-only fit of the ER data.
First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment
XENON Collaboration, E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, M. Bazyk, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, et al (146)
Mar 28 2023 hep-ex astro-ph.CO astro-ph.IM hep-ph physics.ins-det arXiv:2303.14729v2

@misc{2303.14729, author = {XENON Collaboration and E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and M.~Bazyk and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Cimental Chavez and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and H.~Guan and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and R.~Singh and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and V.~H.~S.~Wu and Y.~Xing and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{F}irst {D}ark {M}atter {S}earch with {N}uclear {R}ecoils from the {XENON}n{T} {E}xperiment}, year = {2023}, eprint = {2303.14729}, howpublished = {Phys. Rev. Lett. 131, 041003 (2023)}, doi = {10.1103/PhysRevLett.131.041003}, note = {arXiv:2303.14729v2} }
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We report on the first search for nuclear recoils from dark matter in the form of weakly interacting massive particles (WIMPs) with the XENONnT experiment which is based on a two-phase time projection chamber with a sensitive liquid xenon mass of $5.9$ t. During the approximately 1.1 tonne-year exposure used for this search, the intrinsic $^{85}$Kr and $^{222}$Rn concentrations in the liquid target were reduced to unprecedentedly low levels, giving an electronic recoil background rate of $(15.8\pm1.3)~\mathrm{events}/(\mathrm{t\cdot y \cdot keV})$ in the region of interest. A blind analysis of nuclear recoil events with energies between $3.3$ keV and $60.5$ keV finds no significant excess. This leads to a minimum upper limit on the spin-independent WIMP-nucleon cross section of $2.58\times 10^{-47}~\mathrm{cm}^2$ for a WIMP mass of $28~\mathrm{GeV}/c^2$ at $90\%$ confidence level. Limits for spin-dependent interactions are also provided. Both the limit and the sensitivity for the full range of WIMP masses analyzed here improve on previous results obtained with the XENON1T experiment for the same exposure.
The Triggerless Data Acquisition System of the XENONnT Experiment
E. Aprile, J. Aalbers, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, E. J. Brookes, A. Brown, S. Bruenner, et al (145)
Dec 22 2022 physics.ins-det hep-ex arXiv:2212.11032v1

@misc{2212.11032, author = {E.~Aprile and J.~Aalbers and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and E.~J.~Brookes and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Cimental Chavez and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and M.~Flierman and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and N.~F.~Hood and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and A.~Rocchetti and L.~Sanchez and P.~Sanchez-Lucas and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and S.~Zerbo and M.~Zhong and T.~Zhu}, title = {{T}he {T}riggerless {D}ata {A}cquisition {S}ystem of the {XENON}n{T} {E}xperiment}, year = {2022}, eprint = {2212.11032}, note = {arXiv:2212.11032v1} }
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The XENONnT detector uses the latest and largest liquid xenon-based time projection chamber (TPC) operated by the XENON Collaboration, aimed at detecting Weakly Interacting Massive Particles and conducting other rare event searches. The XENONnT data acquisition (DAQ) system constitutes an upgraded and expanded version of the XENON1T DAQ system. For its operation, it relies predominantly on commercially available hardware accompanied by open-source and custom-developed software. The three constituent subsystems of the XENONnT detector, the TPC (main detector), muon veto, and the newly introduced neutron veto, are integrated into a single DAQ, and can be operated both independently and as a unified system. In total, the DAQ digitizes the signals of 698 photomultiplier tubes (PMTs), of which 253 from the top PMT array of the TPC are digitized twice, at $\times10$ and $\times0.5$ gain. The DAQ for the most part is a triggerless system, reading out and storing every signal that exceeds the digitization thresholds. Custom-developed software is used to process the acquired data, making it available within $\mathcal{O}\left(10\text{ s}\right)$ for live data quality monitoring and online analyses. The entire system with all the three subsystems was successfully commissioned and has been operating continuously, comfortably withstanding readout rates that exceed $\sim500$ MB/s during calibration. Livetime during normal operation exceeds $99\%$ and is $\sim90\%$ during most high-rate calibrations. The combined DAQ system has collected more than 2 PB of both calibration and science data during the commissioning of XENONnT and the first science run.
Low-energy Calibration of XENON1T with an Internal $^{37}$Ar Source
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, et al (144)
Nov 28 2022 physics.ins-det hep-ex arXiv:2211.14191v3

@misc{2211.14191, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and P.~Sanchez-Lucas and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and S.~Zerbo and M.~Zhong and T.~Zhu and C.~Geppert and J.~Riemer}, title = {{L}ow-energy {C}alibration of {XENON}1{T} with an {I}nternal $^{37}${A}r {S}ource}, year = {2022}, eprint = {2211.14191}, note = {arXiv:2211.14191v3} }
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A low-energy electronic recoil calibration of XENON1T, a dual-phase xenon time projection chamber, with an internal $^{37}$Ar source was performed. This calibration source features a 35-day half-life and provides two mono-energetic lines at 2.82 keV and 0.27 keV. The photon yield and electron yield at 2.82 keV are measured to be (32.3$\pm$0.3) photons/keV and (40.6$\pm$0.5) electrons/keV, respectively, in agreement with other measurements and with NEST predictions. The electron yield at 0.27 keV is also measured and it is (68.0$^{+6.3}_{-3.7}$) electrons/keV. The $^{37}$Ar calibration confirms that the detector is well-understood in the energy region close to the detection threshold, with the 2.82 keV line reconstructed at (2.83$\pm$0.02) keV, which further validates the model used to interpret the low-energy electronic recoil excess previously reported by XENON1T. The ability to efficiently remove argon with cryogenic distillation after the calibration proves that $^{37}$Ar can be considered as a regular calibration source for multi-tonne xenon detectors.
Effective Field Theory and Inelastic Dark Matter Results from XENON1T
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, R. Budnik, et al (140)
Oct 17 2022 hep-ex hep-ph arXiv:2210.07591v2

@misc{2210.07591, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Cai and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.~L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{E}ffective {F}ield {T}heory and {I}nelastic {D}ark {M}atter {R}esults from {XENON}1{T}}, year = {2022}, eprint = {2210.07591}, note = {arXiv:2210.07591v2} }
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In this work, we expand on the XENON1T nuclear recoil searches to study the individual signals of dark matter interactions from operators up to dimension-eight in a Chiral Effective Field Theory (ChEFT) and a model of inelastic dark matter (iDM). We analyze data from two science runs of the XENON1T detector totaling 1\u2009tonne$\times$year exposure. For these analyses, we extended the region of interest from [4.9, 40.9]$\,$keV$_{\text{NR}}$ to [4.9, 54.4]$\,$keV$_{\text{NR}}$ to enhance our sensitivity for signals that peak at nonzero energies. We show that the data is consistent with the background-only hypothesis, with a small background over-fluctuation observed peaking between 20 and 50$\,$keV$_{\text{NR}}$, resulting in a maximum local discovery significance of 1.7\,$\sigma$ for the Vector$\otimes$Vector$_{\text{strange}}$ ($VV_s$) ChEFT channel for a dark matter particle of 70$\,$GeV/c$^2$, and $1.8\,\sigma$ for an iDM particle of 50$\,$GeV/c$^2$ with a mass splitting of 100$\,$keV/c$^2$. For each model, we report 90\,\% confidence level (CL) upper limits. We also report upper limits on three benchmark models of dark matter interaction using ChEFT where we investigate the effect of isospin-breaking interactions. We observe rate-driven cancellations in regions of the isospin-breaking couplings, leading to up to 6 orders of magnitude weaker upper limits with respect to the isospin-conserving case.
An approximate likelihood for nuclear recoil searches with XENON1T data
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A.L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, et al (134)
Oct 14 2022 hep-ex physics.ins-det arXiv:2210.07231v1

@misc{2210.07231, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and S.~Farrell and A.~D.~Ferella and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and Y.~Zhang and M.~Zhong and T.~Zhu}, title = {{A}n approximate likelihood for nuclear recoil searches with {XENON}1{T} data}, year = {2022}, eprint = {2210.07231}, note = {arXiv:2210.07231v1} }
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The XENON collaboration has published stringent limits on specific dark matter -nucleon recoil spectra from dark matter recoiling on the liquid xenon detector target. In this paper, we present an approximate likelihood for the XENON1T 1 tonne-year nuclear recoil search applicable to any nuclear recoil spectrum. Alongside this paper, we publish data and code to compute upper limits using the method we present. The approximate likelihood is constructed in bins of reconstructed energy, profiled along the signal expectation in each bin. This approach can be used to compute an approximate likelihood and therefore most statistical results for any nuclear recoil spectrum. Computing approximate results with this method is approximately three orders of magnitude faster than the likelihood used in the original publications of XENON1T, where limits were set for specific families of recoil spectra. Using this same method, we include toy Monte Carlo simulation-derived binwise likelihoods for the upcoming XENONnT experiment that can similarly be used to assess the sensitivity to arbitrary nuclear recoil signatures in its eventual 20 tonne-year exposure.
Search for New Physics in Electronic Recoil Data from XENONnT
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, R. Budnik, et al (146)
Jul 26 2022 hep-ex arXiv:2207.11330v2

@misc{2207.11330, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.~K.~Bui and C.~Cai and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and C.~Ferrari and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Gardner and R.~Glade-Beucke and L.~Grandi and J.~Grigat and M.~Guida and R.~Hammann and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and F.~Kuger and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and P.~Paschos and R.~Peres and C.~Peters and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and J.~Stephen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and D.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and M.~Zhong and T.~Zhu}, title = {{S}earch for {N}ew {P}hysics in {E}lectronic {R}ecoil {D}ata from {XENON}n{T}}, year = {2022}, eprint = {2207.11330}, howpublished = {Phys. Rev. Lett. 129, 161805 (2022)}, doi = {10.1103/PhysRevLett.129.161805}, note = {arXiv:2207.11330v2} }
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We report on a blinded analysis of low-energy electronic-recoil data from the first science run of the XENONnT dark matter experiment. Novel subsystems and the increased 5.9 tonne liquid xenon target reduced the background in the (1, 30) keV search region to $(15.8 \pm 1.3)$ events/(tonne$\times$year$\times$keV), the lowest ever achieved in a dark matter detector and $\sim$5 times lower than in XENON1T. With an exposure of 1.16 tonne-years, we observe no excess above background and set stringent new limits on solar axions, an enhanced neutrino magnetic moment, and bosonic dark matter.
Double-Weak Decays of $^{124}$Xe and $^{136}$Xe in the XENON1T and XENONnT Experiments
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, B. Andrieu, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, et al (140)
May 10 2022 hep-ex nucl-ex arXiv:2205.04158v3

@misc{2205.04158, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and B.~Andrieu and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Cai and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and K.~Eitel and A.~Elykov and S.~Farrell and A.~D.~Ferella and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and M.~Guida and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and P.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shi and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and S.~Zerbo and M.~Zhong and T.~Zhu}, title = {{D}ouble-{W}eak {D}ecays of $^{124}${X}e and $^{136}${X}e in the {XENON}1{T} and {XENON}n{T} {E}xperiments}, year = {2022}, eprint = {2205.04158}, howpublished = {Phys. Rev. C 106, 024328 (2022)}, doi = {10.1103/PhysRevC.106.024328}, note = {arXiv:2205.04158v3} }
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We present results on the search for double-electron capture ($2\nu\text{ECEC}$) of $^{124}$Xe and neutrinoless double-$\beta$ decay ($0\nu\beta\beta$) of $^{136}$Xe in XENON1T. We consider captures from the K- up to the N-shell in the $2\nu\text{ECEC}$ signal model and measure a total half-life of $T_{1/2}^{2\nu\text{ECEC}}=(1.1\pm0.2_\text{stat}\pm0.1_\text{sys})\times 10^{22}\;\text{yr}$ with a $0.87\;\text{kg}\times\text{yr}$ isotope exposure. The statistical significance of the signal is $7.0\,\sigma$. We use XENON1T data with $36.16\;\text{kg}\times\text{yr}$ of $^{136}$Xe exposure to search for $0\nu\beta\beta$. We find no evidence of a signal and set a lower limit on the half-life of $T_{1/2}^{0\nu\beta\beta} > 1.2 \times 10^{24}\;\text{yr}\; \text{at}\; 90\,\%\;\text{CL}$. This is the best result from a dark matter detector without an enriched target to date. We also report projections on the sensitivity of XENONnT to $0\nu\beta\beta$. Assuming a $275\;\text{kg}\times\text{yr}$ $^{136}$Xe exposure, the expected sensitivity is $T_{1/2}^{0\nu\beta\beta} > 2.1 \times 10^{25}\;\text{yr}\; \text{at}\; 90\,\%\;\text{CL}$, corresponding to an effective Majorana mass range of $\langle m_{\beta\beta} \rangle < (0.19 - 0.59)\;\text{eV/c}^2$.
A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics
J. Aalbers, K. Abe, V. Aerne, F. Agostini, S. Ahmed Maouloud, D.S. Akerib, D.Yu. Akimov, J. Akshat, A.K. Al Musalhi, F. Alder, S.K. Alsum, L. Althueser, C.S. Amarasinghe, F.D. Amaro, A. Ames, T.J. Anderson, B. Andrieu, N. Angelides, E. Angelino, J. Angevaare, et al (577)
Mar 07 2022 physics.ins-det astro-ph.CO hep-ex nucl-ex arXiv:2203.02309v1

@misc{2203.02309, author = {J.~Aalbers and K.~Abe and V.~Aerne and F.~Agostini and S.~Ahmed Maouloud and D.S.~Akerib and D.Yu.~Akimov and J.~Akshat and A.K.~Al Musalhi and F.~Alder and S.K.~Alsum and L.~Althueser and C.S.~Amarasinghe and F.D.~Amaro and A.~Ames and T.J.~Anderson and B.~Andrieu and N.~Angelides and E.~Angelino and J.~Angevaare and V.C.~Antochi and D.~Antón Martin and B.~Antunovic and E.~Aprile and H.M.~Araújo and J.E.~Armstrong and F.~Arneodo and M.~Arthurs and P.~Asadi and S.~Baek and X.~Bai and D.~Bajpai and A.~Baker and J.~Balajthy and S.~Balashov and M.~Balzer and A.~Bandyopadhyay and J.~Bang and E.~Barberio and J.W.~Bargemann and L.~Baudis and D.~Bauer and D.~Baur and A.~Baxter and A.L.~Baxter and M.~Bazyk and K.~Beattie and J.~Behrens and N.F.~Bell and L.~Bellagamba and P.~Beltrame and M.~Benabderrahmane and E.P.~Bernard and G.F.~Bertone and P.~Bhattacharjee and A.~Bhatti and A.~Biekert and T.P.~Biesiadzinski and A.R.~Binau and R.~Biondi and Y.~Biondi and H.J.~Birch and F.~Bishara and A.~Bismark and C.~Blanco and G.M.~Blockinger and E.~Bodnia and C.~Boehm and A.I.~Bolozdynya and P.D.~Bolton and S.~Bottaro and C.~Bourgeois and B.~Boxer and P.~Brás and A.~Breskin and P.A.~Breur and C.A.J.~Brew and J.~Brod and E.~Brookes and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and T.K.~Bui and S.~Burdin and S.~Buse and J.K.~Busenitz and D.~Buttazzo and M.~Buuck and A.~Buzulutskov and R.~Cabrita and C.~Cai and D.~Cai and C.~Capelli and J.M.R.~Cardoso and M.C.~Carmona-Benitez and M.~Cascella and R.~Catena and S.~Chakraborty and C.~Chan and S.~Chang and A.~Chauvin and A.~Chawla and H.~Chen and V.~Chepel and N.I.~Chott and D.~Cichon and A.~Cimental Chavez and B.~Cimmino and M.~Clark and R.T.~Co and A.P.~Colijn and J.~Conrad and M.V.~Converse and M.~Costa and A.~Cottle and G.~Cox and O.~Creaner and J.J.~Cuenca Garcia and J.P.~Cussonneau and J.E.~Cutter and C.E.~Dahl and V.~D'Andrea and A.~David and M.P.~Decowski and J.B.~Dent and F.F.~Deppisch and L.~de Viveiros and P.~Di Gangi and A.~Di Giovanni and S.~Di Pede and J.~Dierle and S.~Diglio and J.E.Y.~Dobson and M.~Doerenkamp and D.~Douillet and G.~Drexlin and E.~Druszkiewicz and D.~Dunsky and K.~Eitel and A.~Elykov and T.~Emken and R.~Engel and S.R.~Eriksen and M.~Fairbairn and A.~Fan and J.J.~Fan and S.J.~Farrell and S.~Fayer and N.M.~Fearon and A.~Ferella and C.~Ferrari and A.~Fieguth and A.~Fieguth and S.~Fiorucci and H.~Fischer and H.~Flaecher and M.~Flierman and T.~Florek and R.~Foot and P.J.~Fox and R.~Franceschini and E.D.~Fraser and C.S.~Frenk and S.~Frohlich and T.~Fruth and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and R.J.~Gaitskell and M.~Galloway and F.~Gao and I.~Garcia Garcia and J.~Genovesi and C.~Ghag and S.~Ghosh and E.~Gibson and W.~Gil and D.~Giovagnoli and F.~Girard and R.~Glade-Beucke and F.~Glück and S.~Gokhale and A.de Gouvêa and L.~Gráf and L.~Grandi and J.~Grigat and B.~Grinstein and M.G.D.van der Grinten and R.~Grössle and H.~Guan and M.~Guida and R.~Gumbsheimer and C.B.~Gwilliam and C.R.~Hall and L.J.~Hall and R.~Hammann and K.~Han and V.~Hannen and S.~Hansmann-Menzemer and R.~Harata and S.P.~Hardin and E.~Hardy and C.A.~Hardy and K.~Harigaya and R.~Harnik and S.J.~Haselschwardt and M.~Hernandez and S.A.~Hertel and A.~Higuera and C.~Hils and S.~Hochrein and L.~Hoetzsch and M.~Hoferichter and N.~Hood and D.~Hooper and M.~Horn and J.~Howlett and D.Q.~Huang and Y.~Huang and D.~Hunt and M.~Iacovacci and G.~Iaquaniello and R.~Ide and C.M.~Ignarra and G.~Iloglu and Y.~Itow and E.~Jacquet and O.~Jahangir and J.~Jakob and R.S.~James and A.~Jansen and W.~Ji and X.~Ji and F.~Joerg and J.~Johnson and A.~Joy and A.C.~Kaboth and A.C.~Kamaha and K.~Kanezaki and K.~Kar and M.~Kara and N.~Kato and P.~Kavrigin and S.~Kazama and A.W.~Keaveney and J.~Kellerer and D.~Khaitan and A.~Khazov and G.~Khundzakishvili and I.~Khurana and B.~Kilminster and M.~Kleifges and P.~Ko and M.~Kobayashi and M.~Kobayashi and D.~Kodroff and G.~Koltmann and A.~Kopec and A.~Kopmann and J.~Kopp and L.~Korley and V.N.~Kornoukhov and E.V.~Korolkova and H.~Kraus and L.M.~Krauss and S.~Kravitz and L.~Kreczko and V.A.~Kudryavtsev and F.~Kuger and J.~Kumar and B.~López Paredes and L.~LaCascio and Q.~Laine and H.~Landsman and R.F.~Lang and E.A.~Leason and J.~Lee and D.S.~Leonard and K.T.~Lesko and L.~Levinson and C.~Levy and I.~Li and S.C.~Li and T.~Li and S.~Liang and C.S.~Liebenthal and J.~Lin and Q.~Lin and S.~Lindemann and M.~Lindner and A.~Lindote and R.~Linehan and W.H.~Lippincott and X.~Liu and K.~Liu and J.~Liu and J.~Loizeau and F.~Lombardi and J.~Long and M.I.~Lopes and E.~Lopez Asamar and W.~Lorenzon and C.~Lu and S.~Luitz and Y.~Ma and P.A.N.~Machado and C.~Macolino and T.~Maeda and J.~Mahlstedt and P.A.~Majewski and A.~Manalaysay and A.~Mancuso and L.~Manenti and A.~Manfredini and R.L.~Mannino and N.~Marangou and J.~March-Russell and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and R.~Martin and I.~Martinez-Soler and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Mastronardi and J.A.~Matias-Lopes and M.E.~McCarthy and N.~McFadden and E.~McGinness and D.N.~McKinsey and J.~McLaughlin and K.~McMichael and P.~Meinhardt and J.~Menéndez and Y.~Meng and M.~Messina and R.~Midha and D.~Milisavljevic and E.H.~Miller and B.~Milosevic and S.~Milutinovic and S.A.~Mitra and K.~Miuchi and E.~Mizrachi and K.~Mizukoshi and A.~Molinario and A.~Monte and C.M.B.~Monteiro and M.E.~Monzani and J.S.~Moore and K.~Morå and J.A.~Morad and J.D.~Morales Mendoza and S.~Moriyama and E.~Morrison and E.~Morteau and Y.~Mosbacher and B.J.~Mount and J.~Mueller and A.St.J.~Murphy and M.~Murra and D.~Naim and S.~Nakamura and E.~Nash and N.~Navaieelavasani and A.~Naylor and C.~Nedlik and H.N.~Nelson and F.~Neves and J.L.~Newstead and K.~Ni and J.A.~Nikoleyczik and V.~Niro and U.G.~Oberlack and M.~Obradovic and K.~Odgers and C.A.J.~O'Hare and P.~Oikonomou and I.~Olcina and K.~Oliver-Mallory and A.~Oranday and J.~Orpwood and I.~Ostrovskiy and K.~Ozaki and B.~Paetsch and S.~Pal and J.~Palacio and K.J.~Palladino and J.~Palmer and P.~Panci and M.~Pandurovic and A.~Parlati and N.~Parveen and S.J.~Patton and V.~Pěč and Q.~Pellegrini and B.~Penning and G.~Pereira and R.~Peres and Y.~Perez-Gonzalez and E.~Perry and T.~Pershing and R.~Petrossian-Byrne and J.~Pienaar and A.~Piepke and G.~Pieramico and M.~Pierre and M.~Piotter and V.~Pizella and G.~Plante and T.~Pollmann and D.~Porzio and J.~Qi and Y.~Qie and J.~Qin and N.~Raj and M.~Rajado Silva and K.~Ramanathan and D.~Ramírez García and J.~Ravanis and L.~Redard-Jacot and D.~Redigolo and S.~Reichard and J.~Reichenbacher and C.A.~Rhyne and A.~Richards and Q.~Riffard and G.R.C.~Rischbieter and A.~Rocchetti and S.L.~Rosenfeld and R.~Rosero and N.~Rupp and T.~Rushton and S.~Saha and L.~Sanchez and P.~Sanchez-Lucas and D.~Santone and J.M.F.~dos Santos and I.~Sarnoff and G.~Sartorelli and A.B.M.R.~Sazzad and M.~Scheibelhut and R.W.~Schnee and M.~Schrank and J.~Schreiner and P.~Schulte and D.~Schulte and H.~Schulze Eissing and M.~Schumann and T.~Schwemberger and A.~Schwenk and T.~Schwetz and L.~Scotto Lavina and P.R.~Scovell and H.~Sekiya and M.~Selvi and E.~Semenov and F.~Semeria and P.~Shagin and S.~Shaw and S.~Shi and E.~Shockley and T.A.~Shutt and R.~Si-Ahmed and J.J.~Silk and C.~Silva and M.C.~Silva and H.~Simgen and F.~Šimkovic and G.~Sinev and R.~Singh and W.~Skulski and J.~Smirnov and R.~Smith and M.~Solmaz and V.N.~Solovov and P.~Sorensen and J.~Soria and T.J.~Sparmann and I.~Stancu and M.~Steidl and A.~Stevens and K.~Stifter and L.E.~Strigari and D.~Subotic and B.~Suerfu and A.M.~Suliga and T.J.~Sumner and P.~Szabo and M.~Szydagis and A.~Takeda and Y.~Takeuchi and P.-L.~Tan and C.~Taricco and W.C.~Taylor and D.J.~Temples and A.~Terliuk and P.A.~Terman and D.~Thers and K.~Thieme and Th.~Thümmler and D.R.~Tiedt and M.~Timalsina and W.H.~To and F.~Toennies and Z.~Tong and F.~Toschi and D.R.~Tovey and J.~Tranter and M.~Trask and G.C.~Trinchero and M.~Tripathi and D.R.~Tronstad and R.~Trotta and Y.D.~Tsai and C.D.~Tunnell and W.G.~Turner and R.~Ueno and P.~Urquijo and U.~Utku and A.~Vaitkus and K.~Valerius and E.~Vassilev and S.~Vecchi and V.~Velan and S.~Vetter and A.C.~Vincent and L.~Vittorio and G.~Volta and B.~von Krosigk and M.~von Piechowski and D.~Vorkapic and C.E.M.~Wagner and A.M.~Wang and B.~Wang and Y.~Wang and W.~Wang and J.J.~Wang and L.-T.~Wang and M.~Wang and Y.~Wang and J.R.~Watson and Y.~Wei and C.~Weinheimer and E.~Weisman and M.~Weiss and D.~Wenz and S.M.~West and T.J.~Whitis and M.~Williams and M.J.~Wilson and D.~Winkler and C.~Wittweg and J.~Wolf and T.~Wolf and F.L.H.~Wolfs and S.~Woodford and D.~Woodward and C.J.~Wright and V.H.S.~Wu and P.~Wu and S.~Wüstling and M.~Wurm and Q.~Xia and X.~Xiang and Y.~Xing and J.~Xu and Z.~Xu and D.~Xu and M.~Yamashita and R.~Yamazaki and H.~Yan and L.~Yang and Y.~Yang and J.~Ye and M.~Yeh and I.~Young and H.B.~Yu and T.T.~Yu and L.~Yuan and G.~Zavattini and S.~Zerbo and Y.~Zhang and M.~Zhong and N.~Zhou and X.~Zhou and T.~Zhu and Y.~Zhu and Y.~Zhuang and J.P.~Zopounidis and K.~Zuber and J.~Zupan}, title = {{A} {N}ext-{G}eneration {L}iquid {X}enon {O}bservatory for {D}ark {M}atter and {N}eutrino {P}hysics}, year = {2022}, eprint = {2203.02309}, note = {arXiv:2203.02309v1} }
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The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector.
Application and modeling of an online distillation method to reduce krypton and argon in XENON1T
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, A. Bernard, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, et al (134)
Dec 24 2021 physics.ins-det hep-ex arXiv:2112.12231v2

@misc{2112.12231, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and A.~Bernard and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and S.~Farrell and A.~D.~Ferella and H.~Fischer and S.~Form and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and A.~Higuera and C.~Hils and K.~Hiraide and L.~Hoetzsch and J.~Howlett and C.~Huhmann and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and N.~Kato and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and K.~Ni and U.~Oberlack and J.~Palacio and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and D.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and J.~Westermann and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and Y.~Zhang and M.~Zhong and T.~Zhu and J.~P.~Zopounidis}, title = {{A}pplication and modeling of an online distillation method to reduce krypton and argon in {XENON}1{T}}, year = {2021}, eprint = {2112.12231}, howpublished = {Progress of Theoretical and Experimental Physics, Volume 2022, Issue 5, May 2022, 053H01}, doi = {10.1093/ptep/ptac074}, note = {arXiv:2112.12231v2} }
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A novel online distillation technique was developed for the XENON1T dark matter experiment to reduce intrinsic background components more volatile than xenon, such as krypton or argon, while the detector was operating. The method is based on a continuous purification of the gaseous volume of the detector system using the XENON1T cryogenic distillation column. A krypton-in-xenon concentration of $(360 \pm 60)$ ppq was achieved. It is the lowest concentration measured in the fiducial volume of an operating dark matter detector to date. A model was developed and fit to the data to describe the krypton evolution in the liquid and gas volumes of the detector system for several operation modes over the time span of 550 days, including the commissioning and science runs of XENON1T. The online distillation was also successfully applied to remove Ar-37 after its injection for a low energy calibration in XENON1T. This makes the usage of Ar-37 as a regular calibration source possible in the future. The online distillation can be applied to next-generation experiments to remove krypton prior to, or during, any science run. The model developed here allows further optimization of the distillation strategy for future large scale detectors.
Emission of Single and Few Electrons in XENON1T and Limits on Light Dark Matter
E. Aprile, K. Abe, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, E. Angelino, J. R. Angevaare, V. C. Antochi, D. Antón Martin, F. Arneodo, L. Baudis, A. L. Baxter, L. Bellagamba, A. Bernard, R. Biondi, A. Bismark, A. Brown, S. Bruenner, G. Bruno, et al (135)
Dec 23 2021 hep-ex physics.ins-det arXiv:2112.12116v3

@misc{2112.12116, author = {E.~Aprile and K.~Abe and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and D.~Antón Martin and F.~Arneodo and L.~Baudis and A.~L.~Baxter and L.~Bellagamba and A.~Bernard and R.~Biondi and A.~Bismark and A.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and V.~D'Andrea and M.~P.~Decowski and P.~Di Gangi and S.~Di Pede and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and S.~Farrell and A.~D.~Ferella and H.~Fischer and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and R.~Glade-Beucke and L.~Grandi and J.~Grigat and A.~Higuera and C.~Hils and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and J.~Jakob and F.~Joerg and A.~Joy and N.~Kato and P.~Kavrigin and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and I.~Li and S.~Li and S.~Liang and S.~Lindemann and M.~Lindner and K.~Liu and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and E.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and S.~Moriyama and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Müller and K.~Ni and U.~Oberlack and B.~Paetsch and J.~Palacio and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and L.~Sanchez and J.~M.~F.~dos Santos and I.~Sarnoff and G.~Sartorelli and J.~Schreiner and D.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Shenyang and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and P.-L.~Tan and A.~Terliuk and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and F.~Tönnies and K.~Valerius and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and L.~Yuan and G.~Zavattini and Y.~Zhang and M.~Zhong and T.~Zhu and J.~P.~Zopounidis}, title = {{E}mission of {S}ingle and {F}ew {E}lectrons in {XENON}1{T} and {L}imits on {L}ight {D}ark {M}atter}, year = {2021}, eprint = {2112.12116}, howpublished = {Phys. Rev. D 106, 022001 (2022)}, doi = {10.1103/PhysRevD.106.022001}, note = {arXiv:2112.12116v3} }
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Delayed single- and few-electron emissions plague dual-phase time projection chambers, limiting their potential to search for light-mass dark matter. This paper examines the origins of these events in the XENON1T experiment. Characterization of the intensity of delayed electron backgrounds shows that the resulting emissions are correlated, in time and position, with high-energy events and can effectively be vetoed. In this work we extend previous S2-only analyses down to a single electron. From this analysis, after removing the correlated backgrounds, we observe rates < 30 events/(electron*kg*day) in the region of interest spanning 1 to 5 electrons. We derive 90% confidence upper limits for dark matter-electron scattering, first direct limits on the electric dipole, magnetic dipole, and anapole interactions, and bosonic dark matter models, where we exclude new parameter space for dark photons and solar dark photons.
Improved quality tests of R11410-21 photomultiplier tubes for the XENONnT experiment
V. C. Antochi, L. Baudis, J. Bollig, A. Brown, R. Budnik, D. Cichon, J. Conrad, A. D. Ferella, M. Galloway, L. Hoetzsch, S. Kazama, G. Koltman, H. Landsman, M. Lindner, J. Mahlstedt, T. Marrodán Undagoitia, B. Pelssers, G. Volta, O. Wack, J. Wulf
May 03 2021 physics.ins-det astro-ph.IM hep-ex arXiv:2104.15051v1

@misc{2104.15051, author = {V.~C.~Antochi and L.~Baudis and J.~Bollig and A.~Brown and R.~Budnik and D.~Cichon and J.~Conrad and A.~D.~Ferella and M.~Galloway and L.~Hoetzsch and S.~Kazama and G.~Koltman and H.~Landsman and M.~Lindner and J.~Mahlstedt and T.~Marrodán Undagoitia and B.~Pelssers and G.~Volta and O.~Wack and J.~Wulf}, title = {{I}mproved quality tests of {R}11410-21 photomultiplier tubes for the {XENON}n{T} experiment}, year = {2021}, eprint = {2104.15051}, note = {arXiv:2104.15051v1} }
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Photomultiplier tubes (PMTs) are often used in low-background particle physics experiments, which rely on an excellent response to single-photon signals and stable long-term operation. In particular, the Hamamatsu R11410 model is the light sensor of choice for liquid xenon dark matter experiments, including XENONnT. The same PMT model was also used for the predecessor, XENON1T, where issues affecting its long-term operation were observed. Here, we report on an improved PMT testing procedure which ensures optimal performance in XENONnT. Using both new and upgraded facilities, we tested 368 new PMTs in a cryogenic xenon environment. We developed new tests targeted at the detection of light emission and the degradation of the PMT vacuum through small leaks, which can lead to spurious signals known as afterpulses, both of which were observed in XENON1T. We exclude the use of 26 of the 368 tested PMTs and categorise the remainder according to their performance. Given that we have improved the testing procedure, yet we rejected fewer PMTs, we expect significantly better PMT performance in XENONnT.
Search for Coherent Elastic Scattering of Solar $^8$B Neutrinos in the XENON1T Dark Matter Experiment
E. Aprile, J. Aalbers, F. Agostini, S. Ahmed Maouloud, M. Alfonsi, L. Althueser, F. D. Amaro, S. Andaloro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (118)
Dec 08 2020 hep-ex arXiv:2012.02846v2

@misc{2012.02846, author = {E.~Aprile and J.~Aalbers and F.~Agostini and S.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and S.~Andaloro and V.~C.~Antochi and E.~Angelino and J.~R.~Angevaare and F.~Arneodo and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~Cuenca and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and L.~Grandi and C.~Hils and K.~Hiraide and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and S.~Liang and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and M.~Pierre and J.~Pienaar and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and D.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and K.~Valerius and M.~Vargas and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{S}earch for {C}oherent {E}lastic {S}cattering of {S}olar $^8${B} {N}eutrinos in the {XENON}1{T} {D}ark {M}atter {E}xperiment}, year = {2020}, eprint = {2012.02846}, howpublished = {Phys. Rev. Lett. 126, 091301 (2021)}, doi = {10.1103/PhysRevLett.126.091301}, note = {arXiv:2012.02846v2} }
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We report on a search for nuclear recoil signals from solar $^8$B neutrinos elastically scattering off xenon nuclei in XENON1T data, lowering the energy threshold from 2.6 keV to 1.6 keV. We develop a variety of novel techniques to limit the resulting increase in backgrounds near the threshold. No significant $^8$B neutrino-like excess is found in an exposure of 0.6 t $\times$ y. For the first time, we use the non-detection of solar neutrinos to constrain the light yield from 1-2 keV nuclear recoils in liquid xenon, as well as non-standard neutrino-quark interactions. Finally, we improve upon world-leading constraints on dark matter-nucleus interactions for dark matter masses between 3 GeV/c$^2$ and 11 GeV/c$^2$ by as much as an order of magnitude.
Search for inelastic scattering of WIMP dark matter in XENON1T
XENON Collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, S. Andaloro, E. Angelino, J. R. Angevaare, V. C. Antochi, F. Arneodo, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (121)
Nov 23 2020 hep-ex astro-ph.CO arXiv:2011.10431v2

@misc{2011.10431, author = {XENON Collaboration and E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and S.~Andaloro and E.~Angelino and J.~R.~Angevaare and V.~C.~Antochi and F.~Arneodo and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~Cuenca and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and L.~Grandi and C.~Hils and K.~Hiraide and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and S.~Liang and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and J.~Schreiner and D.~Schulte and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and K.~Valerius and M.~Vargas and G.~Volta and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and T.~Wolf and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{S}earch for inelastic scattering of {WIMP} dark matter in {XENON}1{T}}, year = {2020}, eprint = {2011.10431}, note = {arXiv:2011.10431v2} }
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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.
$^{222}$Rn emanation measurements for the XENON1T experiment
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, et al (123)
Sep 30 2020 physics.ins-det hep-ex arXiv:2009.13981v3

@misc{2009.13981, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and J.~R.~Angevaare and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and G.~Eurin and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and L.~Grandi and M.~Garbini and C.~Hasterok and C.~Hils and K.~Hiraide and L.~Hoetzsch and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante and J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and M.~Vargas and G.~Volta and O.~Wack and H.~Wang and Y.~Wei and C.~Weinheimer and M.Weiss and D.~Wenz and J.~Westermann and C.~Wittweg and J.~Wulf and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {$^{222}${R}n emanation measurements for the {XENON}1{T} experiment}, year = {2020}, eprint = {2009.13981}, note = {arXiv:2009.13981v3} }
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The selection of low-radioactive construction materials is of utmost importance for the success of low-energy rare event search experiments. Besides radioactive contaminants in the bulk, the emanation of radioactive radon atoms from material surfaces attains increasing relevance in the effort to further reduce the background of such experiments. In this work, we present the $^{222}$Rn emanation measurements performed for the XENON1T dark matter experiment. Together with the bulk impurity screening campaign, the results enabled us to select the radio-purest construction materials, targeting a $^{222}$Rn activity concentration of 10 $\mu$Bq/kg in 3.2 t of xenon. The knowledge of the distribution of the $^{222}$Rn sources allowed us to selectively eliminate critical components in the course of the experiment. The predictions from the emanation measurements were compared to data of the $^{222}$Rn activity concentration in XENON1T. The final $^{222}$Rn activity concentration of (4.5 $\pm$ 0.1) $\mu$Bq/kg in the target of XENON1T is the lowest ever achieved in a xenon dark matter experiment.
Projected WIMP Sensitivity of the XENONnT Dark Matter Experiment
XENON collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, A. Brown, E. Brown, S. Bruenner, et al (120)
Jul 20 2020 physics.ins-det astro-ph.CO hep-ex arXiv:2007.08796v2

@misc{2007.08796, author = {XENON collaboration and E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and J.~R.~Angevaare and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and G.~Eurin and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and L.~Grandi and C.~Hasterok and C.~Hils and K.~Hiraide and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante and J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and K.~Valerius and M.~Vargas and G.~Volta and H.~Wang and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{P}rojected {WIMP} {S}ensitivity of the {XENON}n{T} {D}ark {M}atter {E}xperiment}, year = {2020}, eprint = {2007.08796}, howpublished = {JCAP11(2020)031}, doi = {10.1088/1475-7516/2020/11/031}, note = {arXiv:2007.08796v2} }
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XENONnT is a dark matter direct detection experiment, utilizing 5.9 t of instrumented liquid xenon, located at the INFN Laboratori Nazionali del Gran Sasso. In this work, we predict the experimental background and project the sensitivity of XENONnT to the detection of weakly interacting massive particles (WIMPs). The expected average differential background rate in the energy region of interest, corresponding to (1, 13) keV and (4, 50) keV for electronic and nuclear recoils, amounts to $12.3 \pm 0.6$ (keV t y)$^{-1}$ and $(2.2\pm 0.5)\times 10^{-3}$ (keV t y)$^{-1}$, respectively, in a 4 t fiducial mass. We compute unified confidence intervals using the profile construction method, in order to ensure proper coverage. With the exposure goal of 20 t$\,$y, the expected sensitivity to spin-independent WIMP-nucleon interactions reaches a cross-section of $1.4\times10^{-48}$ cm$^2$ for a 50 GeV/c$^2$ mass WIMP at 90% confidence level, more than one order of magnitude beyond the current best limit, set by XENON1T. In addition, we show that for a 50 GeV/c$^2$ WIMP with cross-sections above $2.6\times10^{-48}$ cm$^2$ ($5.0\times10^{-48}$ cm$^2$) the median XENONnT discovery significance exceeds 3$\sigma$ (5$\sigma$). The expected sensitivity to the spin-dependent WIMP coupling to neutrons (protons) reaches $2.2\times10^{-43}$ cm$^2$ ($6.0\times10^{-42}$ cm$^2$).
Excess Electronic Recoil Events in XENON1T
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. R. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (119)
Jun 19 2020 hep-ex astro-ph.CO hep-ph arXiv:2006.09721v3

@misc{2006.09721, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and J.~R.~Angevaare and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and R.~Di Stefano and S.~Diglio and A.~Elykov and G.~Eurin and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and M.~Galloway and F.~Gao and L.~Grandi and C.~Hasterok and C.~Hils and K.~Hiraide and L.~Hoetzsch and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~Long and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Mancuso and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and K.~Mizukoshi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante and J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and M.~Vargas and G.~Volta and H.~Wang and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis and X.~Mougeot}, title = {{E}xcess {E}lectronic {R}ecoil {E}vents in {XENON}1{T}}, year = {2020}, eprint = {2006.09721}, howpublished = {Phys. Rev. D 102, 072004 (2020)}, doi = {10.1103/PhysRevD.102.072004}, note = {arXiv:2006.09721v3} }
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We report results from searches for new physics with low-energy electronic recoil data recorded with the XENON1T detector. With an exposure of 0.65 t-y and an unprecedentedly low background rate of $76\pm2$ events/(t y keV) between 1 and 30 keV, the data enables sensitive searches for solar axions, an enhanced neutrino magnetic moment, and bosonic dark matter. An excess over known backgrounds is observed at low energies and most prominent between 2 and 3 keV. The solar axion model has a 3.4$\sigma$ significance, and a 3D 90% confidence surface is reported for axion couplings to electrons, photons, and nucleons. This surface is inscribed in the cuboid defined by $g_{ae}<3.8 \times 10^{-12}$, $g_{ae}g_{an}^{eff}<4.8\times 10^{-18}$, and $g_{ae}g_{a\gamma}<7.7\times10^{-22} GeV^{-1}$, and excludes either $g_{ae}=0$ or $g_{ae}g_{a\gamma}=g_{ae}g_{an}^{eff}=0$. The neutrino magnetic moment signal is similarly favored over background at 3.2$\sigma$ and a confidence interval of $\mu_{\nu} \in (1.4,2.9)\times10^{-11}\mu_B$ (90% C.L.) is reported. Both results are in strong tension with stellar constraints. The excess can also be explained by $\beta$ decays of tritium at 3.2$\sigma$ with a trace amount that can neither be confirmed nor excluded with current knowledge of its production and reduction mechanisms. The significances of the solar axion and neutrino magnetic moment hypotheses are reduced to 2.0$\sigma$ and 0.9$\sigma$, respectively, if an unconstrained tritium component is included in the fitting. With respect to bosonic dark matter, the excess favors a monoenergetic peak at ($2.3\pm0.2$) keV (68% C.L.) with a 3.0$\sigma$ global (4.0$\sigma$ local) significance. We also consider the possibility that $^{37}$Ar may be present in the detector and yield a 2.82 keV peak. Contrary to tritium, the $^{37}$Ar concentration can be tightly constrained and is found to be negligible.
Solar Neutrino Detection Sensitivity in DARWIN via Electron Scattering
J. Aalbers, F. Agostini, S. E. M. Ahmed Maouloud, M. Alfonsi, L. Althueser, F. Amaro, J. Angevaare, V. C. Antochi, B. Antunovic, E. Aprile, L. Arazi, F. Arneodo, M. Balzer, L. Baudis, D. Baur, M. L. Benabderrahmane, Y. Biondi, A. Bismark, C. Bourgeois, A. Breskin, et al (146)
Jun 08 2020 physics.ins-det astro-ph.SR hep-ex hep-ph arXiv:2006.03114v2

@misc{2006.03114, author = {J.~Aalbers and F.~Agostini and S.~E.~M.~Ahmed Maouloud and M.~Alfonsi and L.~Althueser and F.~Amaro and J.~Angevaare and V.~C.~Antochi and B.~Antunovic and E.~Aprile and L.~Arazi and F.~Arneodo and M.~Balzer and L.~Baudis and D.~Baur and M.~L.~Benabderrahmane and Y.~Biondi and A.~Bismark and C.~Bourgeois and A.~Breskin and P.~A.~Breur and A.~Brown and E.~Brown and S.~Brünner and G.~Bruno and R.~Budnik and C.~Capelli and J.~Cardoso and D.~Cichon and M.~Clark and A.~P.~Colijn and J.~Conrad and J.~J.~Cuenca-García and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian and J.~Dierle and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and D.~Douillet and G.~Drexlin and K.~Eitel and R.~Engel and E.~Erdal and A.~D.~Ferella and H.~Fischer and P.~Fischer and W.~Fulgione and P.~Gaemers and M.~Galloway and F.~Gao and D.~Giovagnoli and F.~Girard and R.~Glade-Beucke and F.~Glück and L.~Grandi and S.~Grohmann and R.~Größle and R.~Gumbsheimer and V.~Hannen and S.~Hansmann-Menzemer and C.~Hils and B.~Holzapfel and J.~Howlett and G.~Iaquaniello and F.~Jörg and M.~Keller and J.~Kellerer and G.~Khundzakishvili and B.~Kilminster and M.~Kleifges and T.~K.~Kleiner and G.~Koltmann and A.~Kopec and A.~Kopmann and L.~M.~Krauss and F.~Kuger and L.~LaCascio and H.~Landsman and R.~F.~Lang and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and A.~Loya Villalpando and Y.~Ma and C.~Macolino and J.~Mahlstedt and A.~Manfredini and T.~Marrodán Undagoitia and J.~Masbou and D.~Masson and E.~Masson and N.~McFadden and P.~Meinhardt and R.~Meyer and B.~Milosevic and S.~Milutinovic and A.~Molinario and C.~M.~B.~Monteiro and K.Morå and E.~Morteau and Y.~Mosbacher and M.~Murra and J.~L.~Newstead and K.~Ni and U.~G.~Oberlack and M.~Obradovic and K.~Odgers and I.~Ostrovskiy and J.~Palacio and M.~Pandurovic and B.~Pelssers and R.~Peres and J.~Pienaar and M.~Pierre and V.~Pizzella and G.~Plante and J.~Qi and J.~Qin and D.~Ramírez García and S.~E.~Reichard and N.~Rupp and P.~Sanchez-Lucas and J.~Santos and G.~Sartorelli and D.~Schulte and H.-C.~Schultz-Coulon and H.~Schulze Eißing and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and S.~Sharma and W.~Shen and M.~Silva and H.~Simgen and M.~Steidl and S.~Stern and D.~Subotic and P.~Szabo and A.~Terliuk and C.~Therreau and D.~Thers and K.~Thieme and F.~Toennies and R.~Trotta and C.~D.~Tunnell and K.~Valerius and G.~Volta and D.~Vorkapic and M.~Weber and Y.~Wei and C.~Weinheimer and M.~Weiss and D.~Wenz and C.~Wittweg and J.~Wolf and S.~Wuestling and M.~Wurm and Y.~Xing and T.~Zhu and Y.~Zhu and J.~P.~Zopounidis and K.~Zuber}, title = {{S}olar {N}eutrino {D}etection {S}ensitivity in {DARWIN} via {E}lectron {S}cattering}, year = {2020}, eprint = {2006.03114}, note = {arXiv:2006.03114v2} }
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We detail the sensitivity of the liquid xenon (LXe) DARWIN observatory to solar neutrinos via elastic electron scattering. We find that DARWIN will have the potential to measure the fluxes of five solar neutrino components: $pp$, $^7$Be, $^{13}$N, $^{15}$O and $pep$. The precision of the $^{13}$N, $^{15}$O and $pep$ components is hindered by the double-beta decay of $^{136}$Xe and, thus, would benefit from a depleted target. A high-statistics observation of $pp$ neutrinos would allow us to infer the values of the weak mixing angle, $\sin^2\theta_w$, and the electron-type neutrino survival probability, $P_e$, in the electron recoil energy region from a few keV up to 200 keV for the first time, with relative precision of 5% and 4%, respectively, at an exposure of 300 ty. An observation of $pp$ and $^7$Be neutrinos would constrain the neutrino-inferred solar luminosity down to 0.2%. A combination of all flux measurements would distinguish between the high (GS98) and low metallicity (AGS09) solar models with 2.1-2.5$\sigma$ significance, independent of external measurements from other experiments or a measurement of $^8$B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, we demonstrate that with a depleted target DARWIN may be sensitive to the neutrino capture process of $^{131}$Xe.
Finding Dark Matter Faster with Explicit Profile Likelihoods
J. Aalbers, B. Pelssers, V. C. Antochi, P. L. Tan, J. Conrad
Mar 30 2020 physics.ins-det astro-ph.CO astro-ph.IM hep-ex arXiv:2003.12483v2

@misc{2003.12483, author = {J.~Aalbers and B.~Pelssers and V.~C.~Antochi and P.~L.~Tan and J.~Conrad}, title = {{F}inding {D}ark {M}atter {F}aster with {E}xplicit {P}rofile {L}ikelihoods}, year = {2020}, eprint = {2003.12483}, howpublished = {Phys. Rev. D 102, 072010 (2020)}, doi = {10.1103/PhysRevD.102.072010}, note = {arXiv:2003.12483v2} }
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Liquid xenon time-projection chambers are the world's most sensitive detectors for a wide range of dark matter candidates. We show that the statistical analysis of their data can be improved by replacing detector response Monte Carlo simulations with an equivalent deterministic calculation. This allows the use of high-dimensional undiscretized models, yielding up to $\sim\! 2$ times better discrimination of the dominant backgrounds. In turn, this could significantly extend the physics reach of upcoming experiments such as XENONnT and LZ, and bring forward a potential $5 \sigma$ dark matter discovery by over a year.
Energy resolution and linearity of XENON1T in the MeV energy range
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, J. Angevaare, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, et al (118)
Mar 10 2020 physics.ins-det astro-ph.IM hep-ex nucl-ex arXiv:2003.03825v2

@misc{2003.03825, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and J.~Angevaare and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and B.~Cimmino and M.~Clark and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and A.~Depoian P.~Di Gangi A.~Di Giovanni R.~Di Stefano and S.~Diglio and A.~Elykov and G.~Eurin and A.~D.~Ferella and W.~Fulgione and P.~Gaemers and R.~Gaior and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and C.~Hasterok and C.~Hils and K.~Hiraide and L.~Hoetzsch and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and Y.~Itow and F.~Joerg and N.~Kato and S.~Kazama and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Miuchi and A.~Molinario and K.~Morå and S.~Moriyama and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and A.~Takeda and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and M.~Vargas and G.~Volta and O.~Wack and H.~Wang and Y.~Wei and C.~Weinheimer and M.~Weiss Xu and D.~Wenz and C.~Wittweg and J.~Wulf and Z.~Xu and M.~Yamashita and J.~Ye and G.~Zavattini and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{E}nergy resolution and linearity of {XENON}1{T} in the {M}e{V} energy range}, year = {2020}, eprint = {2003.03825}, howpublished = {Eur. Phys. J. C 80, 785 (2020)}, doi = {10.1140/epjc/s10052-020-8284-0}, note = {arXiv:2003.03825v2} }
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Xenon dual-phase time projection chambers designed to search for Weakly Interacting Massive Particles have so far shown a relative energy resolution which degrades with energy above $\sim$200 keV due to the saturation effects. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of $^{136}$Xe at its $Q$-value, $Q_{\beta\beta}\simeq$ 2.46 MeV. For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at 1 $\sigma/\mu$ is as low as (0.80$\pm$0.02) % in its one-ton fiducial mass, and for single-site interactions at $Q_{\beta\beta}$. We also present a new signal correction method to rectify the saturation effects of the signal readout system, resulting in more accurate position reconstruction and indirectly improving the energy resolution. The very good result achieved in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events.
Search for Light Dark Matter Interactions Enhanced by the Migdal effect or Bremsstrahlung in XENON1T
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (114)
Jul 31 2019 hep-ex astro-ph.CO physics.ins-det arXiv:1907.12771v4

@misc{1907.12771, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and P.~de Perio and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and A.~Elykov and G.~Eurin and J.~Fei and A.~D.~Ferella and A.~Fieguth and W.~Fulgione and P.~Gaemers and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and Z.~Greene and C.~Hasterok and C.~Hils and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and R.~Itay and F.~Joerg and S.~Kazama and A.~Kish and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and L.~Manenti and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and J.~Masbou and S.~Mastroianni and M.~Messina and K.~Micheneau and K.~Miller and A.~Molinario and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and B.~Riedel and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and N.~Upole and M.~Vargas and G.~Volta and O.~Wack and H.~Wang and Y.~Wei and C.~Weinheimer and D.~Wenz and C.~Wittweg and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{S}earch for {L}ight {D}ark {M}atter {I}nteractions {E}nhanced by the {M}igdal effect or {B}remsstrahlung in {XENON}1{T}}, year = {2019}, eprint = {1907.12771}, howpublished = {Phys. Rev. Lett. 123, 241803 (2019)}, doi = {10.1103/PhysRevLett.123.241803}, note = {arXiv:1907.12771v4} }
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Direct dark matter detection experiments based on a liquid xenon target are leading the search for dark matter particles with masses above $\sim$ 5 GeV/c$^2$, but have limited sensitivity to lighter masses because of the small momentum transfer in dark matter-nucleus elastic scattering. However, there is an irreducible contribution from inelastic processes accompanying the elastic scattering, which leads to the excitation and ionization of the recoiling atom (the Migdal effect) or the emission of a Bremsstrahlung photon. In this letter, we report on a probe of low-mass dark matter with masses down to about 85 MeV/c$^2$ by looking for electronic recoils induced by the Migdal effect and Bremsstrahlung, using data from the XENON1T experiment. Besides the approach of detecting both scintillation and ionization signals, we exploit an approach that uses ionization signals only, which allows for a lower detection threshold. This analysis significantly enhances the sensitivity of XENON1T to light dark matter previously beyond its reach.
Light Dark Matter Search with Ionization Signals in XENON1T
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, E. Angelino, F. Arneodo, D. Barge, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (113)
Jul 29 2019 hep-ex astro-ph.CO arXiv:1907.11485v2

@misc{1907.11485, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and E.~Angelino and F.~Arneodo and D.~Barge and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and P.~de Perio and A.~Depoian and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and A.~Elykov and G.~Eurin and J.~Fei and A.~D.~Ferella and A.~Fieguth and W.~Fulgione and P.~Gaemers and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and Z.~Greene and C.~Hasterok and C.~Hils and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and R.~Itay and F.~Joerg and S.~Kazama and A.~Kish and M.~Kobayashi and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and J.~Masbou and S.~Mastroianni and M.~Messina and K.~Micheneau and K.~Miller and A.~Molinario and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and J.~Palacio and B.~Pelssers and R.~Peres and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and J.~Qin and H.~Qiu and D.~Ramírez García and S.~Reichard and B.~Riedel and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and N.~Upole and M.~Vargas and G.~Volta and O.~Wack and H.~Wang and Y.~Wei and C.~Weinheimer and D.~Wenz and C.~Wittweg and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{L}ight {D}ark {M}atter {S}earch with {I}onization {S}ignals in {XENON}1{T}}, year = {2019}, eprint = {1907.11485}, howpublished = {Phys. Rev. Lett. 123, 251801 (2019)}, doi = {10.1103/PhysRevLett.123.251801}, note = {arXiv:1907.11485v2} }
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We report constraints on light dark matter (DM) models using ionization signals in the XENON1T experiment. We mitigate backgrounds with strong event selections, rather than requiring a scintillation signal, leaving an effective exposure of $(22 \pm 3)$ tonne-days. Above $\sim\!0.4\,\mathrm{keV}_\mathrm{ee}$, we observe $<1 \, \text{event}/(\text{tonne} \times \text{day} \times \text{keV}_\text{ee})$, which is more than one thousand times lower than in similar searches with other detectors. Despite observing a higher rate at lower energies, no DM or CEvNS detection may be claimed because we cannot model all of our backgrounds. We thus exclude new regions in the parameter spaces for DM-nucleus scattering for DM masses $m_\chi$ within $3-6\,\mathrm{GeV}/\mathrm{c}^2$, DM-electron scattering for $m_\chi > 30\,\mathrm{MeV}/\mathrm{c}^2$, and absorption of dark photons and axion-like particles for $m_\chi$ within $0.186 - 1 \, \mathrm{keV}/\mathrm{c}^2$.
XENON1T Dark Matter Data Analysis: Signal Reconstruction, Calibration and Event Selection
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, F. Arneodo, L. Baudis, B. Bauermeister, L. Bellagamba, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, et al (108)
Jun 12 2019 physics.ins-det hep-ex arXiv:1906.04717v2

@misc{1906.04717, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and F.~Arneodo and L.~Baudis and B.~Bauermeister and L.~Bellagamba and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and P.~de Perio and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and A.~Elykov and G.~Eurin and J.~Fei and A.~D.~Ferella and A.~Fieguth and W.~Fulgione and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and Z.~Greene and C.~Hasterok and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and R.~Itay and F.~Joerg and S.~Kazama and A.~Kish and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Micheneau and K.~Miller and A.~Molinario and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and B.~Pelssers and R.~Peres and F.~Piastra and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and H.~Qiu and D.~Ramírez García and S.~Reichard and B.~Riedel and A.~Rizzo and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and N.~Upole and M.~Vargas and O.~Wack and H.~Wang and Z.~Wang and Y.~Wei and C.~Weinheimer and D.~Wenz and C.~Wittweg and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{XENON}1{T} {D}ark {M}atter {D}ata {A}nalysis: {S}ignal {R}econstruction, {C}alibration and {E}vent {S}election}, year = {2019}, eprint = {1906.04717}, howpublished = {Phys. Rev. D 100, 052014 (2019)}, doi = {10.1103/PhysRevD.100.052014}, note = {arXiv:1906.04717v2} }
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The XENON1T experiment at the Laboratori Nazionali del Gran Sasso is the most sensitive direct detection experiment for dark matter in the form of weakly interacting particles (WIMPs) with masses above $6\,$GeV/$c^2$ scattering off nuclei. The detector employs a dual-phase time projection chamber with 2.0 metric tons of liquid xenon in the target. A one metric $\mathrm{ton}\times\mathrm{year}$ exposure of science data was collected between October 2016 and February 2018. This article reports on the performance of the detector during this period and describes details of the data analysis that led to the most stringent exclusion limits on various WIMP-nucleon interaction models to date. In particular, signal reconstruction, event selection and calibration of the detector response to nuclear and electronic recoils in XENON1T are discussed.
XENON1T Dark Matter Data Analysis: Signal & Background Models, and Statistical Inference
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, V. C. Antochi, F. Arneodo, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, C. Capelli, J. M. R. Cardoso, et al (106)
Mar 01 2019 physics.ins-det hep-ex arXiv:1902.11297v2

@misc{1902.11297, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and V.~C.~Antochi and F.~Arneodo and L.~Baudis and B.~Bauermeister and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and P.~de Perio and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and A.~Elykov and G.~Eurin and J.~Fei and A.~D.~Ferella and A.~Fieguth and W.~Fulgione and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and Z.~Greene and C.~Hasterok and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and R.~Itay and F.~Joerg and S.~Kazama and A.~Kish and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Micheneau and K.~Miller and A.~Molinario and K.~Morå and Y.~Mosbacher and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and B.~Pelssers and F.~Piastra and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and H.~Qiu and D.~Ramírez García and S.~Reichard and B.~Riedel and A.~Rizzo and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and N.~Upole and M.~Vargas and O.~Wack and H.~Wang and Z.~Wang and Y.~Wei and C.~Weinheimer and D.~Wenz and C.~Wittweg and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{XENON}1{T} {D}ark {M}atter {D}ata {A}nalysis: {S}ignal & {B}ackground {M}odels, and {S}tatistical {I}nference}, year = {2019}, eprint = {1902.11297}, note = {arXiv:1902.11297v2} }
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The XENON1T experiment searches for dark matter particles through their scattering off xenon atoms in a 2 tonne liquid xenon target. The detector is a dual-phase time projection chamber, which measures simultaneously the scintillation and ionization signals produced by interactions in target volume, to reconstruct energy and position, as well as the type of the interaction. The background rate in the central volume of XENON1T detector is the lowest achieved so far with a liquid xenon-based direct detection experiment. In this work we describe the response model of the detector, the background and signal models, and the statistical inference procedures used in the dark matter searches with a 1 tonne$\times$year exposure of XENON1T data, that leaded to the best limit to date on WIMP-nucleon spin-independent elastic scatter cross-section for WIMP masses above 6 GeV/c$^2$.
First results on the scalar WIMP-pion coupling, using the XENON1T experiment
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, M. Anthony, V. C. Antochi, F. Arneodo, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, et al (112)
Dec 03 2018 hep-ph astro-ph.CO hep-ex nucl-th arXiv:1811.12482v2

@misc{1811.12482, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and M.~Anthony and V.~C.~Antochi and F.~Arneodo and L.~Baudis and B.~Bauermeister and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and C.~Capelli and J.~M.~R.~Cardoso and D.~Cichon and D.~Coderre and A.~P.~Colijn and J.~Conrad and J.~P.~Cussonneau and M.~P.~Decowski and P.~de Perio and P.~Di Gangi and A.~Di Giovanni and S.~Diglio and A.~Elykov and G.~Eurin and J.~Fei and A.~D.~Ferella and A.~Fieguth and W.~Fulgione and A.~Gallo Rosso and M.~Galloway and F.~Gao and M.~Garbini and L.~Grandi and Z.~Greene and C.~Hasterok and E.~Hogenbirk and J.~Howlett and M.~Iacovacci and R.~Itay and F.~Joerg and B.~Kaminsky and S.~Kazama and A.~Kish and G.~Koltman and A.~Kopec and H.~Landsman and R.~F.~Lang and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and E.~López Fune and C.~Macolino and J.~Mahlstedt and A.~Manfredini and F.~Marignetti and T.~Marrodán Undagoitia and J.~Masbou and D.~Masson and S.~Mastroianni and M.~Messina and K.~Micheneau and K.~Miller and A.~Molinario and K.~Morå and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and K.~Odgers and B.~Pelssers and F.~Piastra and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and N.~Priel and H.~Qiu and D.~Ramírez García and S.~Reichard and B.~Riedel and A.~Rizzo and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and N.~Šarčević and M.~Scheibelhut and S.~Schindler and J.~Schreiner and D.~Schulte and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and C.~Therreau and D.~Thers and F.~Toschi and G.~Trinchero and C.~Tunnell and N.~Upole and M.~Vargas and O.~Wack and H.~Wang and Z.~Wang and Y.~Wei and C.~Weinheimer and C.~Wittweg and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis and M.~Hoferichter and P.~Klos and J.~Menéndez and A.~Schwenk}, title = {{F}irst results on the scalar {WIMP}-pion coupling, using the {XENON}1{T} experiment}, year = {2018}, eprint = {1811.12482}, howpublished = {Phys. Rev. Lett. 122, 071301 (2019)}, doi = {10.1103/PhysRevLett.122.071301}, note = {arXiv:1811.12482v2} }
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We present first results on the scalar WIMP-pion coupling from 1 t$\times$yr of exposure with the XENON1T experiment. This interaction is generated when the WIMP couples to a virtual pion exchanged between the nucleons in a nucleus. In contrast to most non-relativistic operators, these pion-exchange currents can be coherently enhanced by the total number of nucleons, and therefore may dominate in scenarios where spin-independent WIMP-nucleon interactions are suppressed. Moreover, for natural values of the couplings, they dominate over the spin-dependent channel due to their coherence in the nucleus. Using the signal model of this new WIMP-pion channel, no significant excess is found, leading to an upper limit cross section of $6.4\times10^{-46}$ cm$^2$ (90 % confidence level) at 30 GeV/c$^2$ WIMP mass.
Combined readout of a triple-GEM detector
Vasile C. Antochi, Elisabetta Baracchini, Gianluca Cavoto, Emanuele Di Marco, Michela Marafini, Giovanni Mazzitelli, Davide Pinci, Francesco Renga, Sandro Tomassini, Cecilia Voena
Mar 20 2018 physics.ins-det hep-ex arXiv:1803.06860v1

@misc{1803.06860, author = {Vasile C.~Antochi and Elisabetta Baracchini and Gianluca Cavoto and Emanuele Di Marco and Michela Marafini and Giovanni Mazzitelli and Davide Pinci and Francesco Renga and Sandro Tomassini and Cecilia Voena}, title = {{C}ombined readout of a triple-{GEM} detector}, year = {2018}, eprint = {1803.06860}, note = {arXiv:1803.06860v1} }
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Optical readout of GEM based devices by means of high granularity and low noise CMOS sensors allows to obtain very interesting tracking performance. Space resolution of the order of tens of $\mu$m were measured on the GEM plane along with an energy resolution of 20%$\div$30%. The main limitation of CMOS sensors is represented by their poor information about time structure of the event. In this paper, the use of a concurrent light readout by means of a suitable photomultiplier and the acquisition of the electric signal induced on the GEM electrode are exploited to provide the necessary timing informations. The analysis of the PMT waveform allows a 3D reconstruction of each single clusters with a resolution on z of 100 $\mu$m. Moreover, from the PMT signals it is possible to obtain a fast reconstruction of the energy released within the detector with a resolution of the order of 25% even in the tens of keV range useful, for example, for triggering purpose.
US Cosmic Visions: New Ideas in Dark Matter 2017: Community Report
Marco Battaglieri, Alberto Belloni, Aaron Chou, Priscilla Cushman, Bertrand Echenard, Rouven Essig, Juan Estrada, Jonathan L. Feng, Brenna Flaugher, Patrick J. Fox, Peter Graham, Carter Hall, Roni Harnik, JoAnne Hewett, Joseph Incandela, Eder Izaguirre, Daniel McKinsey, Matthew Pyle, Natalie Roe, Gray Rybka, et al (231)
Jul 18 2017 hep-ph astro-ph.CO hep-ex arXiv:1707.04591v1

@misc{1707.04591, author = {Marco Battaglieri and Alberto Belloni and Aaron Chou and Priscilla Cushman and Bertrand Echenard and Rouven Essig and Juan Estrada and Jonathan L.~Feng and Brenna Flaugher and Patrick J.~Fox and Peter Graham and Carter Hall and Roni Harnik and JoAnne Hewett and Joseph Incandela and Eder Izaguirre and Daniel McKinsey and Matthew Pyle and Natalie Roe and Gray Rybka and Pierre Sikivie and Tim M.~P.~Tait and Natalia Toro and Richard Van De Water and Neal Weiner and Kathryn Zurek and Eric Adelberger and Andrei Afanasev and Derbin Alexander and James Alexander and Vasile Cristian Antochi and David Mark Asner and Howard Baer and Dipanwita Banerjee and Elisabetta Baracchini and Phillip Barbeau and Joshua Barrow and Noemie Bastidon and James Battat and Stephen Benson and Asher Berlin and Mark Bird and Nikita Blinov and Kimberly K.~Boddy and Mariangela Bondi and Walter M.~Bonivento and Mark Boulay and James Boyce and Maxime Brodeur and Leah Broussard and Ranny Budnik and Philip Bunting and Marc Caffee and Sabato Stefano Caiazza and Sheldon Campbell and Tongtong Cao and Gianpaolo Carosi and Massimo Carpinelli and Gianluca Cavoto and Andrea Celentano and Jae Hyeok Chang and Swapan Chattopadhyay and Alvaro Chavarria and Chien-Yi Chen and Kenneth Clark and John Clarke and Owen Colegrove and Jonathon Coleman and David Cooke and Robert Cooper and Michael Crisler and Paolo Crivelli and Francesco D'Eramo and Domenico D'Urso and Eric Dahl and William Dawson and Marzio De Napoli and Raffaella De Vita and Patrick DeNiverville and Stephen Derenzo and Antonia Di Crescenzo and Emanuele Di Marco and Keith R.~Dienes and Milind Diwan and Dongwi Handiipondola Dongwi and Alex Drlica-Wagner and Sebastian Ellis and Anthony Chigbo Ezeribe and Glennys Farrar and Francesc Ferrer and Enectali Figueroa-Feliciano and Alessandra Filippi and Giuliana Fiorillo and Bartosz Fornal and Arne Freyberger and Claudia Frugiuele and Cristian Galbiati and Iftah Galon and Susan Gardner and Andrew Geraci and Gilles Gerbier and Mathew Graham and Edda Gschwendtner and Christopher Hearty and Jaret Heise and Reyco Henning and Richard J.~Hill and David Hitlin and Yonit Hochberg and Jason Hogan and Maurik Holtrop and Ziqing Hong and Todd Hossbach and T.~B.~Humensky and Philip Ilten and Kent Irwin and John Jaros and Robert Johnson and Matthew Jones and Yonatan Kahn and Narbe Kalantarians and Manoj Kaplinghat and Rakshya Khatiwada and Simon Knapen and Michael Kohl and Chris Kouvaris and Jonathan Kozaczuk and Gordan Krnjaic and Valery Kubarovsky and Eric Kuflik and Alexander Kusenko and Rafael Lang and Kyle Leach and Tongyan Lin and Mariangela Lisanti and Jing Liu and Kun Liu and Ming Liu and Dinesh Loomba and Joseph Lykken and Katherine Mack and Jeremiah Mans and Humphrey Maris and Thomas Markiewicz and Luca Marsicano and C.~J.~Martoff and Giovanni Mazzitelli and Christopher McCabe and Samuel D.~McDermott and Art McDonald and Bryan McKinnon and Dongming Mei and Tom Melia and Gerald A.~Miller and Kentaro Miuchi and Sahara Mohammed Prem Nazeer and Omar Moreno and Vasiliy Morozov and Frederic Mouton and Holger Mueller and Alexander Murphy and Russell Neilson and Tim Nelson and Christopher Neu and Yuri Nosochkov and Ciaran O'Hare and Noah Oblath and John Orrell and Jonathan Ouellet and Saori Pastore and Sebouh Paul and Maxim Perelstein and Annika Peter and Nguyen Phan and Nan Phinney and Michael Pivovaroff and Andrea Pocar and Maxim Pospelov and Josef Pradler and Paolo Privitera and Stefano Profumo and Mauro Raggi and Surjeet Rajendran and Nunzio Randazzo and Tor Raubenheimer and Christian Regenfus and Andrew Renshaw and Adam Ritz and Thomas Rizzo and Leslie Rosenberg and Andre Rubbia and Ben Rybolt and Tarek Saab and Benjamin R.~Safdi and Elena Santopinto and Andrew Scarff and Michael Schneider and Philip Schuster and George Seidel and Hiroyuki Sekiya and Ilsoo Seong and Gabriele Simi and Valeria Sipala and Tracy Slatyer and Oren Slone and Peter F Smith and Jordan Smolinsky and Daniel Snowden-Ifft and Matthew Solt and Andrew Sonnenschein and Peter Sorensen and Neil Spooner and Brijesh Srivastava and Ion Stancu and Louis Strigari and Jan Strube and Alexander O.~Sushkov and Matthew Szydagis and Philip Tanedo and David Tanner and Rex Tayloe and William Terrano and Jesse Thaler and Brooks Thomas and Brianna Thorpe and Thomas Thorpe and Javier Tiffenberg and Nhan Tran and Marco Trovato and Christopher Tully and Tony Tyson and Tanmay Vachaspati and Sven Vahsen and Karl van Bibber and Justin Vandenbroucke and Anthony Villano and Tomer Volansky and Guojian Wang and Thomas Ward and William Wester and Andrew Whitbeck and David A.~Williams and Matthew Wing and Lindley Winslow and Bogdan Wojtsekhowski and Hai-Bo Yu and Shin-Shan Yu and Tien-Tien Yu and Xilin Zhang and Yue Zhao and Yi-Ming Zhong}, title = {{US} {C}osmic {V}isions: {N}ew {I}deas in {D}ark {M}atter 2017: {C}ommunity {R}eport}, year = {2017}, eprint = {1707.04591}, note = {arXiv:1707.04591v1} }
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This white paper summarizes the workshop "U.S. Cosmic Visions: New Ideas in Dark Matter" held at University of Maryland on March 23-25, 2017.
Carbon nanotubes as target for directional detection of light WIMP
V.C. Antochi, E. Baracchini, G. Cavoto, E. Di Marco, G. Mazzitelli, D. Pinci, A.D. Polosa, F. Renga, C. Voena
Jul 11 2017 physics.ins-det hep-ex arXiv:1707.02549v1

@misc{1707.02549, author = {V.C.~Antochi and E.~Baracchini and G.~Cavoto and E.~Di Marco and G.~Mazzitelli and D.~Pinci and A.D.~Polosa and F.~Renga and C.~Voena}, title = {{C}arbon nanotubes as target for directional detection of light {WIMP}}, year = {2017}, eprint = {1707.02549}, note = {arXiv:1707.02549v1} }
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In this paper I will briefly introduce the idea of using Carbon Nanotubes (CNT) as target for the detection of low mass WIMPs with the additional information of directionality. I will also present the experimental efforts of developing a Time Projection Chamber with a CNT target inside and the results of a test beam at the Beam Test Facility of INFN-LNF.