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T. J. Sumner

Bio: T. J. Sumner is an academic researcher from Imperial College London. The author has contributed to research in topics: Dark matter & Xenon. The author has an hindex of 62, co-authored 329 publications receiving 16405 citations. Previous affiliations of T. J. Sumner include University of Rochester & University of Florida.
Topics: Dark matter, Xenon, WIMP, Scintillation, Pathfinder


Papers
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Journal ArticleDOI
D. S. Akerib1, Henrique Araujo2, X. Bai3, A. J. Bailey2, J. Balajthy4, S. Bedikian5, Ethan Bernard5, A. Bernstein6, Alexander Bolozdynya1, A. W. Bradley1, D. Byram7, Sidney Cahn5, M. C. Carmona-Benitez8, C. Chan9, J.J. Chapman9, A. A. Chiller7, C. Chiller7, K. Clark1, T. Coffey1, A. Currie2, A. Curioni5, Steven Dazeley6, L. de Viveiros10, A. Dobi4, J. E. Y. Dobson11, E. M. Dragowsky1, E. Druszkiewicz12, B. N. Edwards5, C. H. Faham13, S. Fiorucci9, C. E. Flores14, R. J. Gaitskell9, V. M. Gehman13, C. Ghag15, K.R. Gibson1, Murdock Gilchriese13, C. R. Hall4, M. Hanhardt3, S. A. Hertel5, M. Horn5, D. Q. Huang9, M. Ihm16, R. G. Jacobsen16, L. Kastens5, K. Kazkaz6, R. Knoche4, S. Kyre8, R. L. Lander14, N. A. Larsen5, C. Lee1, David Leonard4, K. T. Lesko13, A. Lindote10, M.I. Lopes10, A. Lyashenko5, D.C. Malling9, R. L. Mannino17, Daniel McKinsey5, Dongming Mei7, J. Mock14, M. Moongweluwan12, J. A. Morad14, M. Morii18, A. St. J. Murphy11, C. Nehrkorn8, H. N. Nelson8, F. Neves10, James Nikkel5, R. A. Ott14, M. Pangilinan9, P. D. Parker5, E. K. Pease5, K. Pech1, P. Phelps1, L. Reichhart15, T. A. Shutt1, C. Silva10, W. Skulski12, C. Sofka17, V. N. Solovov10, P. Sorensen6, T.M. Stiegler17, K. O'Sullivan5, T. J. Sumner2, Robert Svoboda14, M. Sweany14, Matthew Szydagis14, D. J. Taylor, B. P. Tennyson5, D. R. Tiedt3, Mani Tripathi14, S. Uvarov14, J.R. Verbus9, N. Walsh14, R. C. Webb17, J. T. White17, D. White8, M. S. Witherell8, M. Wlasenko18, F.L.H. Wolfs12, M. Woods14, Chao Zhang7 
TL;DR: The first WIMP search data set is reported, taken during the period from April to August 2013, presenting the analysis of 85.3 live days of data, finding that the LUX data are in disagreement with low-mass W IMP signal interpretations of the results from several recent direct detection experiments.
Abstract: The Large Underground Xenon (LUX) experiment is a dual-phase xenon time-projection chamber operating at the Sanford Underground Research Facility (Lead, South Dakota). The LUX cryostat was filled for the first time in the underground laboratory in February 2013. We report results of the first WIMP search data set, taken during the period from April to August 2013, presenting the analysis of 85.3 live days of data with a fiducial volume of 118 kg. A profile-likelihood analysis technique shows our data to be consistent with the background-only hypothesis, allowing 90% confidence limits to be set on spin-independent WIMP-nucleon elastic scattering with a minimum upper limit on the cross section of 7.6 × 10(-46) cm(2) at a WIMP mass of 33 GeV/c(2). We find that the LUX data are in disagreement with low-mass WIMP signal interpretations of the results from several recent direct detection experiments.

1,962 citations

Journal ArticleDOI
D. S. Akerib1, S. Alsum2, Henrique Araujo3, X. Bai4, A. J. Bailey3, J. Balajthy5, P. Beltrame, Ethan Bernard6, A. Bernstein7, T. P. Biesiadzinski1, E. M. Boulton6, R. Bramante1, P. Brás8, D. Byram9, Sidney Cahn10, M. C. Carmona-Benitez11, C. Chan12, A.A. Chiller9, C. Chiller9, A. Currie3, J. E. Cutter13, T. J. R. Davison, A. Dobi14, J. E. Y. Dobson15, E. Druszkiewicz16, B. N. Edwards10, C. H. Faham14, S. Fiorucci12, R. J. Gaitskell12, V. M. Gehman14, C. Ghag15, K.R. Gibson1, M. G. D. Gilchriese14, C. R. Hall5, M. Hanhardt4, S. J. Haselschwardt11, S. A. Hertel6, D. P. Hogan6, M. Horn6, D. Q. Huang12, C. M. Ignarra17, M. Ihm6, R.G. Jacobsen6, W. Ji1, K. Kamdin6, K. Kazkaz7, D. Khaitan16, R. Knoche5, N.A. Larsen10, C. Lee1, B. G. Lenardo7, K. T. Lesko14, A. Lindote8, M.I. Lopes8, A. Manalaysay13, R. L. Mannino18, M. F. Marzioni, Daniel McKinsey6, D. M. Mei9, J. Mock19, M. Moongweluwan16, J. A. Morad13, A. St. J. Murphy20, C. Nehrkorn11, H. N. Nelson11, F. Neves8, K. O’Sullivan6, K. C. Oliver-Mallory6, K. J. Palladino17, E. K. Pease6, P. Phelps1, L. Reichhart15, C. Rhyne12, S. Shaw15, T. A. Shutt1, C. Silva8, M. Solmaz11, V. N. Solovov8, P. Sorensen14, S. Stephenson13, T. J. Sumner3, Matthew Szydagis19, D. J. Taylor, W. C. Taylor12, B. P. Tennyson10, P. A. Terman18, D. R. Tiedt4, W. H. To1, Mani Tripathi13, L. Tvrznikova6, S. Uvarov13, J.R. Verbus12, R. C. Webb18, J. T. White18, T. J. Whitis1, M. S. Witherell14, F.L.H. Wolfs16, Jilei Xu7, K. Yazdani3, Sarah Young19, Chao Zhang9 
TL;DR: This search yields no evidence of WIMP nuclear recoils and constraints on spin-independent weakly interacting massive particle (WIMP)-nucleon scattering using a 3.35×10^{4} kg day exposure of the Large Underground Xenon experiment are reported.
Abstract: We report constraints on spin-independent weakly interacting massive particle (WIMP)-nucleon scattering using a 3.35×10^{4} kg day exposure of the Large Underground Xenon (LUX) experiment. A dual-phase xenon time projection chamber with 250 kg of active mass is operated at the Sanford Underground Research Facility under Lead, South Dakota (USA). With roughly fourfold improvement in sensitivity for high WIMP masses relative to our previous results, this search yields no evidence of WIMP nuclear recoils. At a WIMP mass of 50 GeV c^{-2}, WIMP-nucleon spin-independent cross sections above 2.2×10^{-46} cm^{2} are excluded at the 90% confidence level. When combined with the previously reported LUX exposure, this exclusion strengthens to 1.1×10^{-46} cm^{2} at 50 GeV c^{-2}.

1,844 citations

02 Feb 2017
TL;DR: The LISA Consortium as mentioned in this paper proposed a 4-year mission in response to ESA's call for missions for L3, which is an all-sky monitor and will offer a wide view of a dynamic cosmos using Gravitational Waves as new and unique messengers to unveil The Gravitational Universe.
Abstract: Following the selection of The Gravitational Universe by ESA, and the successful flight of LISA Pathfinder, the LISA Consortium now proposes a 4 year mission in response to ESA's call for missions for L3. The observatory will be based on three arms with six active laser links, between three identical spacecraft in a triangular formation separated by 2.5 million km. LISA is an all-sky monitor and will offer a wide view of a dynamic cosmos using Gravitational Waves as new and unique messengers to unveil The Gravitational Universe. It provides the closest ever view of the infant Universe at TeV energy scales, has known sources in the form of verification binaries in the Milky Way, and can probe the entire Universe, from its smallest scales near the horizons of black holes, all the way to cosmological scales. The LISA mission will scan the entire sky as it follows behind the Earth in its orbit, obtaining both polarisations of the Gravitational Waves simultaneously, and will measure source parameters with astrophysically relevant sensitivity in a band from below $10^{-4}\,$Hz to above $10^{-1}\,$Hz.

935 citations

Journal ArticleDOI
Michele Armano1, Heather Audley2, G. Auger3, J. Baird4, Massimo Bassan5, Pierre Binétruy3, M. Born2, Daniele Bortoluzzi6, N. Brandt7, M. Caleno1, L. Carbone6, Antonella Cavalleri8, A. Cesarini6, Giacomo Ciani6, G. Congedo6, A. M. Cruise9, Karsten Danzmann2, M. de Deus Silva1, R. De Rosa, M. Diaz-Aguilo10, L. Di Fiore, Ingo Diepholz2, G. Dixon9, Rita Dolesi6, N. Dunbar7, Luigi Ferraioli11, Valerio Ferroni6, Walter Fichter, E. D. Fitzsimons12, R. Flatscher7, M. Freschi1, A. F. García Marín2, C. García Marirrodriga1, R. Gerndt7, Lluis Gesa10, Ferran Gibert6, Domenico Giardini11, R. Giusteri6, F. Guzmán2, Aniello Grado13, Catia Grimani14, A. Grynagier, J. Grzymisch1, I. Harrison15, Gerhard Heinzel2, M. Hewitson2, Daniel Hollington4, D. Hoyland9, Mauro Hueller6, Henri Inchauspe3, Oliver Jennrich1, Ph. Jetzer16, Ulrich Johann7, B. Johlander1, Nikolaos Karnesis2, B. Kaune2, N. Korsakova2, Christian J. Killow17, J. A. Lobo10, Ivan Lloro10, L. Liu6, J. P. López-Zaragoza10, R. Maarschalkerweerd15, Davor Mance11, V. Martín10, L. Martin-Polo1, J. Martino3, F. Martin-Porqueras1, S. Madden1, Ignacio Mateos10, Paul McNamara1, José F. F. Mendes15, L. Mendes1, A. Monsky2, Daniele Nicolodi6, Miquel Nofrarías10, S. Paczkowski2, Michael Perreur-Lloyd17, Antoine Petiteau3, P. Pivato6, Eric Plagnol3, P. Prat3, U. Ragnit1, B. Rais3, Juan Ramos-Castro18, J. Reiche2, D. I. Robertson17, H. Rozemeijer1, F. Rivas10, G. Russano6, J Sanjuán10, P. Sarra, A. Schleicher7, D. Shaul4, Jacob Slutsky19, Carlos F. Sopuerta10, Ruggero Stanga20, F. Steier2, T. J. Sumner4, D. Texier1, James Ira Thorpe19, C. Trenkel7, Michael Tröbs2, H. B. Tu6, Daniele Vetrugno6, Stefano Vitale6, V Wand2, Gudrun Wanner2, H. Ward17, C. Warren7, Peter Wass4, D. Wealthy7, W. J. Weber6, L. Wissel2, A. Wittchen2, A. Zambotti6, C. Zanoni6, Tobias Ziegler7, Peter Zweifel11 
TL;DR: The first results of the LISA Pathfinder in-flight experiment demonstrate that two free-falling reference test masses, such as those needed for a space-based gravitational wave observatory like LISA, can be put in free fall with a relative acceleration noise with a square root of the power spectral density.
Abstract: We report the first results of the LISA Pathfinder in-flight experiment. The results demonstrate that two free-falling reference test masses, such as those needed for a space-based gravitational wave observatory like LISA, can be put in free fall with a relative acceleration noise with a square root of the power spectral density of 5.2 +/- 0.1 fm s(exp -2)/square root of Hz, or (0.54 +/- 0.01) x 10(exp -15) g/square root of Hz, with g the standard gravity, for frequencies between 0.7 and 20 mHz. This value is lower than the LISA Pathfinder requirement by more than a factor 5 and within a factor 1.25 of the requirement for the LISA mission, and is compatible with Brownian noise from viscous damping due to the residual gas surrounding the test masses. Above 60 mHz the acceleration noise is dominated by interferometer displacement readout noise at a level of (34.8 +/- 0.3) fm square root of Hz, about 2 orders of magnitude better than requirements. At f less than or equal to 0.5 mHz we observe a low-frequency tail that stays below 12 fm s(exp -2)/square root of Hz down to 0.1 mHz. This performance would allow for a space-based gravitational wave observatory with a sensitivity close to what was originally foreseen for LISA.

523 citations

Journal ArticleDOI
TL;DR: The New Gravitational-Wave Observatory (NGO) as discussed by the authors, a mission under study by the European Space Agency for launch in the early 2020s, will survey the low-frequency gravitational wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers, the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultra-compact binaries, both detached and mass transferring, in
Abstract: We review the expected science performance of the New Gravitational-Wave Observatory (NGO, a.k.a. eLISA), a mission under study by the European Space Agency for launch in the early 2020s. eLISA will survey the low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers; the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultra-compact binaries, both detached and mass transferring, in the Galaxy; and possibly unforeseen sources such as the relic gravitational-wave radiation from the early Universe. eLISA's high signal-to-noise measurements will provide new insight into the structure and history of the Universe, and they will test general relativity in its strong-field dynamical regime.

462 citations


Cited by
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[...]

08 Dec 2001-BMJ
TL;DR: There is, I think, something ethereal about i —the square root of minus one, which seems an odd beast at that time—an intruder hovering on the edge of reality.
Abstract: There is, I think, something ethereal about i —the square root of minus one. I remember first hearing about it at school. It seemed an odd beast at that time—an intruder hovering on the edge of reality. Usually familiarity dulls this sense of the bizarre, but in the case of i it was the reverse: over the years the sense of its surreal nature intensified. It seemed that it was impossible to write mathematics that described the real world in …

33,785 citations

Journal ArticleDOI
01 Apr 1988-Nature
TL;DR: In this paper, a sedimentological core and petrographic characterisation of samples from eleven boreholes from the Lower Carboniferous of Bowland Basin (Northwest England) is presented.
Abstract: Deposits of clastic carbonate-dominated (calciclastic) sedimentary slope systems in the rock record have been identified mostly as linearly-consistent carbonate apron deposits, even though most ancient clastic carbonate slope deposits fit the submarine fan systems better. Calciclastic submarine fans are consequently rarely described and are poorly understood. Subsequently, very little is known especially in mud-dominated calciclastic submarine fan systems. Presented in this study are a sedimentological core and petrographic characterisation of samples from eleven boreholes from the Lower Carboniferous of Bowland Basin (Northwest England) that reveals a >250 m thick calciturbidite complex deposited in a calciclastic submarine fan setting. Seven facies are recognised from core and thin section characterisation and are grouped into three carbonate turbidite sequences. They include: 1) Calciturbidites, comprising mostly of highto low-density, wavy-laminated bioclast-rich facies; 2) low-density densite mudstones which are characterised by planar laminated and unlaminated muddominated facies; and 3) Calcidebrites which are muddy or hyper-concentrated debrisflow deposits occurring as poorly-sorted, chaotic, mud-supported floatstones. These

9,929 citations

Journal ArticleDOI
TL;DR: The current status of particle dark matter, including experimental evidence and theoretical motivations, including direct and indirect detection techniques, is discussed in this paper. But the authors focus on neutralinos in models of supersymmetry and Kaluza-Klein dark matter in universal extra dimensions.

4,614 citations

Journal Article
TL;DR: The first direct detection of gravitational waves and the first observation of a binary black hole merger were reported in this paper, with a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ.
Abstract: On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160) Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

4,375 citations