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The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics
XLZD Collaboration, J. Aalbers, K. Abe, M. Adrover, S. Ahmed Maouloud, D. S. Akerib, A. K. Al Musalhi, F. Alder, L. Althueser, D. W. P. Amaral, C. S. Amarasinghe, A. Ames, B. Andrieu, N. Angelides, E. Angelino, B. Antunovic, E. Aprile, H. M. Araújo, J. E. Armstrong, M. Arthurs, et al (424)
Oct 23 2024 hep-ex hep-ph physics.ins-det arXiv:2410.17137v1

@misc{2410.17137, author = {XLZD Collaboration and J.~Aalbers and K.~Abe and M.~Adrover and S.~Ahmed Maouloud and D.~S.~Akerib and A.~K.~Al Musalhi and F.~Alder and L.~Althueser and D.~W.~P.~Amaral and C.~S.~Amarasinghe and A.~Ames and B.~Andrieu and N.~Angelides and E.~Angelino and B.~Antunovic and E.~Aprile and H.~M.~Araújo and J.~E.~Armstrong and M.~Arthurs and M.~Babicz and D.~Bajpai and A.~Baker and M.~Balzer and J.~Bang and E.~Barberio and J.~W.~Bargemann and E.~Barillier and A.~Basharina-Freshville and L.~Baudis and D.~Bauer and M.~Bazyk and K.~Beattie and N.~Beaupere and N.~F.~Bell and L.~Bellagamba and T.~Benson and A.~Bhatti and T.~P.~Biesiadzinski and R.~Biondi and Y.~Biondi and H.~J.~Birch and E.~Bishop and A.~Bismark and C.~Boehm and K.~Boese and A.~Bolotnikov and P.~Brás and R.~Braun and A.~Breskin and C.~A.~J.~Brew and S.~Brommer and A.~Brown and G.~Bruni and R.~Budnik and S.~Burdin and C.~Cai and C.~Capelli and G.~Carini and M.~C.~Carmona-Benitez and M.~Carter and A.~Chauvin and A.~Chawla and H.~Chen and J.~J.~Cherwinka and Y.~T.~Chin and N.~I.~Chott and A.~P.~Cimental Chavez and K.~Clark and A.~P.~Colijn and D.~J.~Colling and J.~Conrad and M.~V.~Converse and R.~Coronel and D.~Costanzo and A.~Cottle and G.~Cox and J.~J.~Cuenca-García and D.~Curran and D.~Cussans and V.~D'Andrea and L.~C.~Daniel Garcia and I.~Darlington and S.~Dave and A.~David and G.~J.~Davies and M.~P.~Decowski and A.~Deisting and J.~Delgaudio and S.~Dey and C.~Di Donato and L.~Di Felice and P.~Di Gangi and S.~Diglio and C.~Ding and J.~E.~Y.~Dobson and M.~Doerenkamp and G.~Drexlin and E.~Druszkiewicz and C.~L.~Dunbar and K.~Eitel and A.~Elykov and R.~Engel and S.~R.~Eriksen and S.~Fayer and N.~M.~Fearon and A.~D.~Ferella and C.~Ferrari and N.~Fieldhouse and H.~Fischer and H.~Flaecher and T.~Flehmke and M.~Flierman and E.~D.~Fraser and T.~M.~A.~Fruth and K.~Fujikawa and W.~Fulgione and C.~Fuselli and P.~Gaemers and R.~Gaior and R.~J.~Gaitskell and N.~Gallice and M.~Galloway and F.~Gao and N.~Garroum and A.~Geffre and J.~Genovesi and C.~Ghag and S.~Ghosh and R.~Giacomobono and R.~Gibbons and F.~Girard and R.~Glade-Beucke and F.~Glück and S.~Gokhale and L.~Grandi and J.~Green and J.~Grigat and M.~G.~D.~van der Grinten and R.~Größle and H.~Guan and M.~Guida and P.~Gyorgy and J.~J.~Haiston and C.~R.~Hall and T.~Hall and R.~Hammann and V.~Hannen and S.~Hansmann-Menzemer and N.~Hargittai and E.~Hartigan-O'Connor and S.~J.~Haselschwardt and M.~Hernandez and S.~A.~Hertel and A.~Higuera and C.~Hils and K.~Hiraoka and L.~Hoetzsch and M.~Hoferichter and G.~J.~Homenides and N.~F.~Hood and M.~Horn and D.~Q.~Huang and S.~Hughes and D.~Hunt and M.~Iacovacci and Y.~Itow and E.~Jacquet and J.~Jakob and R.~S.~James and F.~Joerg and S.~Jones and A.~C.~Kaboth and F.~Kahlert and A.~C.~Kamaha and Y.~Kaminaga and M.~Kara and P.~Kavrigin and S.~Kazama and M.~Keller and P.~Kemp-Russell and D.~Khaitan and P.~Kharbanda and B.~Kilminster and J.~Kim and R.~Kirk and M.~Kleifges and M.~Klute and M.~Kobayashi and D.~Kodroff and D.~Koke and A.~Kopec and E.~V.~Korolkova and H.~Kraus and S.~Kravitz and L.~Kreczko and B.~von Krosigk and V.~A.~Kudryavtsev and F.~Kuger and N.~Kurita and H.~Landsman and R.~F.~Lang and C.~Lawes and J.~Lee and B.~Lehnert and D.~S.~Leonard and K.~T.~Lesko and L.~Levinson and A.~Li and I.~Li and S.~Li and S.~Liang and Z.~Liang and J.~Lin and Y.~-T.~Lin and S.~Lindemann and S.~Linden and M.~Lindner and A.~Lindote and W.~H.~Lippincott and K.~Liu and J.~Loizeau and F.~Lombardi and J.~A.~M.~Lopes and M.~I.~Lopes and W.~Lorenzon and M.~Loutit and C.~Lu and G.~M.~Lucchetti and T.~Luce and S.~Luitz and Y.~Ma and C.~Macolino and J.~Mahlstedt and B.~Maier and P.~A.~Majewski and A.~Manalaysay and A.~Mancuso and L.~Manenti and R.~L.~Mannino and F.~Marignetti and T.~Marley and T.~Marrodán Undagoitia and K.~Martens and J.~Masbou and E.~Masson and S.~Mastroianni and C.~Maupin and C.~McCabe and M.~E.~McCarthy and D.~N.~McKinsey and J.~B.~McLaughlin and A.~Melchiorre and J.~Menéndez and M.~Messina and E.~H.~Miller and B.~Milosovic and S.~Milutinovic and K.~Miuchi and R.~Miyata and E.~Mizrachi and A.~Molinario and C.~M.~B.~Monteiro and M.~E.~Monzani and K.~Morå and S.~Moriyama and E.~Morrison and E.~Morteau and Y.~Mosbacher and B.~J.~Mount and J.~Müller and M.~Murdy and A.~St.~J.~Murphy and M.~Murra and A.~Naylor and H.~N.~Nelson and F.~Neves and J.~L.~Newstead and A.~Nguyen and K.~Ni and C.~O'Hare and U.~Oberlack and M.~Obradovic and I.~Olcina and K.~C.~Oliver-Mallory and G.~D.~Orebi Gann and J.~Orpwood and I.~Ostrowskiy and S.~Ouahada and K.~Oyulmaz and B.~Paetsch and K.~J.~Palladino and J.~Palmer and Y.~Pan and M.~Pandurovic and N.~J.~Pannifer and S.~Paramesvaran and S.~J.~Patton and Q.~Pellegrini and B.~Penning and G.~Pereira and R.~Peres and E.~Perry and T.~Pershing and F.~Piastra and J.~Pienaar and A.~Piepke and M.~Pierre and G.~Plante and T.~R.~Pollmann and L.~Principe and J.~Qi and K.~Qiao and Y.~Qie and J.~Qin and S.~Radeka and V.~Radeka and M.~Rajado and D.~Ramírez García and A.~Ravindran and A.~Razeto and J.~Reichenbacher and C.~A.~Rhyne and A.~Richards and G.~R.~C.~Rischbieter and H.~S.~Riyat and R.~Rosero and A.~Roy and T.~Rushton and D.~Rynders and R.~Saakyan and L.~Sanchez and P.~Sanchez-Lucas and D.~Santone and J.~M.~F.~dos Santos and G.~Sartorelli and A.~B.~M.~R.~Sazzad and A.~Scaffidi and R.~W.~Schnee and J.~Schreiner and P.~Schulte and H.~Schulze and Eißing and M.~Schumann and A.~Schwenck and A.~Schwenk and L.~Scotto Lavina and M.~Selvi and F.~Semeria and P.~Shagin and S.~Sharma and S.~Shaw and W.~Shen and L.~Sherman and S.~Shi and S.~Y.~Shi and T.~Shimada and T.~Shutt and J.~J.~Silk and C.~Silva and H.~Simgen and G.~Sinev and R.~Singh and J.~Siniscalco and M.~Solmaz and V.~N.~Solovov and Z.~Song and P.~Sorensen and J.~Soria and O.~Stanley and M.~Steidl and T.~Stenhouse and A.~Stevens and K.~Stifter and T.~J.~Sumner and A.~Takeda and P.-L.~Tan and D.~J.~Taylor and W.~C.~Taylor and D.~Thers and T.~Thümmler and D.~R.~Tiedt and F.~Tönnies and Z.~Tong and F.~Toschi and D.~R.~Tovey and J.~Tranter and M.~Trask and G.~Trinchero and M.~Tripathi and D.~R.~Tronstad and R.~Trotta and C.~D.~Tunnell and P.~Urquijo and A.~Usón and M.~Utoyama and A.~C.~Vaitkus and O.~Valentino and K.~Valerius and S.~Vecchi and V.~Velan and S.~Vetter and L.~de Viveiros and G.~Volta and D.~Vorkapic and A.~Wang and J.~J.~Wang and W.~Wang and Y.~Wang and D.~Waters and K.~M.~Weerman and C.~Weinheimer and M.~Weiss and D.~Wenz and T.~J.~Whitis and K.~Wild and M.~Williams and M.~Wilson and S.~T.~Wilson and C.~Wittweg and J.~Wolf and F.~L.~H.~Wolfs and S.~Woodford and D.~Woodward and M.~Worcester and C.~J.~Wright and V.~H.~S.~Wu and S.~W üstling and M.~Wurm and Q.~Xia and Y.~Xing and D.~Xu and J.~Xu and Y.~Xu and Z.~Xu and M.~Yamashita and L.~Yang and J.~Ye and M.~Yeh and B.~Yu and G.~Zavattini and W.~Zha and M.~Zhong and K.~Zuber}, title = {{T}he {XLZD} {D}esign {B}ook: {T}owards the {N}ext-{G}eneration {L}iquid {X}enon {O}bservatory for {D}ark {M}atter and {N}eutrino {P}hysics}, year = {2024}, eprint = {2410.17137}, note = {arXiv:2410.17137v1} }
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This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60-80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3$\sigma$ evidence potential for the spin-independent WIMP-nucleon cross sections as low as $3\times10^{-49}\rm cm^2$ (at 40 GeV/c$^2$ WIMP mass). The observatory is also projected to have a 3$\sigma$ observation potential of neutrinoless double-beta decay of $^{136}$Xe at a half-life of up to $5.7\times 10^{27}$ years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae.
Ultralight vector dark matter search using data from the KAGRA O3GK run
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, A. G. Abac, R. Abbott, H. Abe, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, N. Adhikari, R. X. Adhikari, V. K. Adkins, V. B. Adya, C. Affeldt, D. Agarwal, M. Agathos, O. D. Aguiar, I. Aguilar, et al (1783)
Mar 06 2024 astro-ph.CO gr-qc hep-ph arXiv:2403.03004v1

@misc{2403.03004, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and A.~G.~Abac and R.~Abbott and H.~Abe and I.~Abouelfettouh and F.~Acernese and K.~Ackley and C.~Adamcewicz and S.~Adhicary and N.~Adhikari and R.~X.~Adhikari and V.~K.~Adkins and V.~B.~Adya and C.~Affeldt and D.~Agarwal and M.~Agathos and O.~D.~Aguiar and I.~Aguilar and L.~Aiello and A.~Ain and P.~Ajith and T.~Akutsu and S.~Albanesi and R.~A.~Alfaidi and A.~Al-Jodah and C.~Alléné and A.~Allocca and S.~Al-Shammari and P.~A.~Altin and S.~Alvarez-Lopez and A.~Amato and L.~Amez-Droz and A.~Amorosi and C.~Amra and S.~Anand and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Andia and M.~Ando and T.~Andrade and N.~Andres and M.~Andrés-Carcasona and T.~Andrić and J.~Anglin and S.~Ansoldi and J.~M.~Antelis and S.~Antier and M.~Aoumi and E.~Z.~Appavuravther and S.~Appert and S.~K.~Apple and K.~Arai and A.~Araya and M.~C.~Araya and J.~S.~Areeda and N.~Aritomi and F.~Armato and N.~Arnaud and M.~Arogeti and S.~M.~Aronson and K.~G.~Arun and G.~Ashton and Y.~Aso and M.~Assiduo and S.~Assis de Souza Melo and S.~M.~Aston and P.~Astone and F.~Aubin and K.~AultONeal and G.~Avallone and S.~Babak and F.~Badaracco and C.~Badger and S.~Bae and S.~Bagnasco and E.~Bagui and Y.~Bai and J.~G.~Baier and R.~Bajpai and T.~Baka and M.~Ball and G.~Ballardin and S.~W.~Ballmer and S.~Banagiri and B.~Banerjee and D.~Bankar and P.~Baral and J.~C.~Barayoga and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and S.~D.~Barthelmy and M.~A.~Barton and I.~Bartos and S.~Basak and A.~Basalaev and R.~Bassiri and A.~Basti and M.~Bawaj and P.~Baxi and J.~C.~Bayley and A.~C.~Baylor and M.~Bazzan and B.~Bécsy and V.~M.~Bedakihale and F.~Beirnaert and M.~Bejger and D.~Belardinelli and A.~S.~Bell and V.~Benedetto and D.~Beniwal and W.~Benoit and J.~D.~Bentley and M.~Ben Yaala and S.~Bera and M.~Berbel and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and M.~Beroiz and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and N.~Bevins and R.~Bhandare and U.~Bhardwaj and R.~Bhatt and D.~Bhattacharjee and S.~Bhaumik and S.~Bhowmick and A.~Bianchi and I.~A.~Bilenko and G.~Billingsley and A.~Binetti and S.~Bini and O.~Birnholtz and S.~Biscoveanu and A.~Bisht and M.~Bitossi and M.-A.~Bizouard and J.~K.~Blackburn and C.~D.~Blair and D.~G.~Blair and F.~Bobba and N.~Bode and G.~Bogaert and G.~Boileau and M.~Boldrini and G.~N.~Bolingbroke and A.~Bolliand and L.~D.~Bonavena and R.~Bondarescu and F.~Bondu and E.~Bonilla and M.~S.~Bonilla and A.~Bonino and R.~Bonnand and P.~Booker and A.~Borchers and V.~Boschi and S.~Bose and V.~Bossilkov and V.~Boudart and A.~Boumerdassi and A.~Bozzi and C.~Bradaschia and P.~R.~Brady and M.~Braglia and A.~Branch and M.~Branchesi and M.~Breschi and T.~Briant and A.~Brillet and M.~Brinkmann and P.~Brockill and E.~Brockmueller and A.~F.~Brooks and D.~D.~Brown and M.~L.~Brozzetti and S.~Brunett and G.~Bruno and R.~Bruntz and J.~Bryant and F.~Bucci and J.~Buchanan and O.~Bulashenko and T.~Bulik and H.~J.~Bulten and A.~Buonanno and K.~Burtnyk and R.~Buscicchio and D.~Buskulic and C.~Buy and R.~L.~Byer and G.~S.~Cabourn Davies and G.~Cabras and R.~Cabrita and L.~Cadonati and G.~Cagnoli and C.~Cahillane and J.~Calderón Bustillo and J.~D.~Callaghan and T.~A.~Callister and E.~Calloni and J.~B.~Camp and G.~Caneva Santoro and M.~Cannavacciuolo and K.~C.~Cannon and H.~Cao and Z.~Cao and L.~A.~Capistran and E.~Capocasa and E.~Capote and G.~Carapella and F.~Carbognani and M.~Carlassara and J.~B.~Carlin and M.~Carpinelli and G.~Carrillo and J.~J.~Carter and G.~Carullo and J.~Casanueva Diaz and C.~Casentini and G.~Castaldi and S.~Y.~Castro-Lucas and S.~Caudill and M.~Cavaglià and R.~Cavalieri and G.~Cella and P.~Cerdá-Durán and E.~Cesarini and W.~Chaibi and P.~Chakraborty and S.~Chalathadka Subrahmanya and C.~Chan and J.~C.~L.~Chan and K.~H.~M.~Chan and M.~Chan and W.~L.~Chan and K.~Chandra and R.-J.~Chang and P.~Chanial and S.~Chao and C.~Chapman-Bird and E.~L.~Charlton and P.~Charlton and E.~Chassande-Mottin and C.~Chatterjee and Debarati Chatterjee and Deep Chatterjee and M.~Chaturvedi and S.~Chaty and K.~Chatziioannou and A.~Chen and A.~H.-Y.~Chen and D.~Chen and H.~Chen and H.~Y.~Chen and K.~H.~Chen and X.~Chen and Yi-Ru Chen and Yanbei Chen and Yitian Chen and H.~P.~Cheng and P.~Chessa and H.~T.~Cheung and H.~Y.~Chia and F.~Chiadini and C.~Chiang and G.~Chiarini and A.~Chiba and R.~Chiba and R.~Chierici and A.~Chincarini and M.~L.~Chiofalo and A.~Chiummo and C.~Chou and S.~Choudhary and N.~Christensen and S.~S.~Y.~Chua and K.~W.~Chung and G.~Ciani and P.~Ciecielag and M.~Cieślar and M.~Cifaldi and A.~A.~Ciobanu and R.~Ciolfi and F.~Clara and J.~A.~Clark and T.~A.~Clarke and P.~Clearwater and S.~Clesse and F.~Cleva and E.~Coccia and E.~Codazzo and P.-F.~Cohadon and M.~Colleoni and C.~G.~Collette and J.~Collins and S.~Colloms and A.~Colombo and M.~Colpi and C.~M.~Compton and L.~Conti and S.~J.~Cooper and T.~R.~Corbitt and I.~Cordero-Carrión and S.~Corezzi and N.~J.~Cornish and A.~Corsi and S.~Cortese and C.~A.~Costa and R.~Cottingham and M.~W.~Coughlin and A.~Couineaux and J.-P.~Coulon and S.~T.~Countryman and J.-F.~Coupechoux and B.~Cousins and P.~Couvares and D.~M.~Coward and M.~J.~Cowart and D.~C.~Coyne and R.~Coyne and K.~Craig and R.~Creed and J.~D.~E.~Creighton and T.~D.~Creighton and P.~Cremonese and A.~W.~Criswell and J.~C.~G.~Crockett-Gray and M.~Croquette and R.~Crouch and S.~G.~Crowder and J.~R.~Cudell and T.~J.~Cullen and A.~Cumming and E.~Cuoco and M.~Cusinato and P.~Dabadie and T.~Dal Canton and S.~Dall'Osso and G.~Dálya and B.~D'Angelo and S.~Danilishin and S.~D'Antonio and K.~Danzmann and K.~E.~Darroch and L.~P.~Dartez and A.~Dasgupta and S.~Datta and V.~Dattilo and A.~Daumas and N.~Davari and I.~Dave and A.~Davenport and M.~Davier and T.~F.~Davies and D.~Davis and L.~Davis and M.~C.~Davis and E.~J.~Daw and M.~Dax and J.~De Bolle and M.~Deenadayalan and J.~Degallaix and M.~De Laurentis and S.~Deléglise and V.~Del Favero and F.~De Lillo and D.~Dell'Aquila and W.~Del Pozzo and F.~De Marco and F.~De Matteis and V.~D'Emilio and N.~Demos and T.~Dent and A.~Depasse and N.~DePergola and R.~De Pietri and R.~De Rosa and C.~De Rossi and R.~De Simone and A.~Dhani and S.~Dhurandhar and R.~Diab and M.~C.~Díaz and M.~Di Cesare and G.~Dideron and N.~A.~Didio and T.~Dietrich and L.~Di Fiore and C.~Di Fronzo and F.~Di Giovanni and M.~Di Giovanni and T.~Di Girolamo and D.~Diksha and A.~Di Michele and J.~Ding and S.~Di Pace and I.~Di Palma and F.~Di Renzo and Divyajyoti and A.~Dmitriev and Z.~Doctor and E.~Dohmen and P.~P.~Doleva and L.~Donahue and L.~D'Onofrio and F.~Donovan and K.~L.~Dooley and T.~Dooney and S.~Doravari and O.~Dorosh and M.~Drago and J.~C.~Driggers and Y.~Drori and J.-G.~Ducoin and L.~Dunn and U.~Dupletsa and D.~D'Urso and H.~Duval and P.-A.~Duverne and S.~E.~Dwyer and C.~Eassa and M.~Ebersold and T.~Eckhardt and G.~Eddolls and B.~Edelman and T.~B.~Edo and O.~Edy and A.~Effler and J.~Eichholz and H.~Einsle and M.~Eisenmann and R.~A.~Eisenstein and A.~Ejlli and M.~Emma and E.~Engelby and A.~J.~Engl and L.~Errico and R.~C.~Essick and H.~Estellés and D.~Estevez and T.~Etzel and M.~Evans and T.~Evstafyeva and B.~E.~Ewing and J.~M.~Ezquiaga and F.~Fabrizi and F.~Faedi and V.~Fafone and S.~Fairhurst and P.~C.~Fan and A.~M.~Farah and B.~Farr and W.~M.~Farr and G.~Favaro and M.~Favata and M.~Fays and M.~Fazio and J.~Feicht and M.~M.~Fejer and E.~Fenyvesi and D.~L.~Ferguson and I.~Ferrante and T.~A.~Ferreira and F.~Fidecaro and A.~Fiori and I.~Fiori and M.~Fishbach and R.~P.~Fisher and R.~Fittipaldi and V.~Fiumara and R.~Flaminio and S.~M.~Fleischer and L.~S.~Fleming and E.~Floden and E.~M.~Foley and H.~Fong and J.~A.~Font and B.~Fornal and P.~W.~F.~Forsyth and K.~Franceschetti and N.~Franchini and S.~Frasca and F.~Frasconi and A.~Frattale Mascioli and Z.~Frei and A.~Freise and O.~Freitas and R.~Frey and W.~Frischhertz and V.~V.~Frolov and G.~G.~Fronzé and M.~Fuentes-Garcia and S.~Fujii and I.~Fukunaga and P.~Fulda and M.~Fyffe and W.~E.~Gabella and B.~Gadre and J.~R.~Gair and S.~Galaudage and S.~Gallardo and B.~Gallego and R.~Gamba and A.~Gamboa and D.~Ganapathy and A.~Ganguly and S.~G.~Gaonkar and B.~Garaventa and J.~Garcia-Bellido and C.~García-Núñez and C.~García-Quirós and J.~W.~Gardner and K.~A.~Gardner and J.~Gargiulo and A.~Garron and F.~Garufi and C.~Gasbarra and B.~Gateley and V.~Gayathri and G.~Gemme and A.~Gennai and J.~George and R.~George and O.~Gerberding and L.~Gergely and N.~Ghadiri and Archisman Ghosh and Shaon Ghosh and Shrobana Ghosh and Suprovo Ghosh and Tathagata Ghosh and L.~Giacoppo and J.~A.~Giaime and K.~D.~Giardina and D.~R.~Gibson and D.~T.~Gibson and C.~Gier and P.~Giri and F.~Gissi and S.~Gkaitatzis and J.~Glanzer and A.~E.~Gleckl and F.~Glotin and J.~Godfrey and P.~Godwin and N.~L.~Goebbels and E.~Goetz and J.~Golomb and S.~Gomez Lopez and B.~Goncharov and G.~González and P.~Goodarzi and A.~W.~Goodwin-Jones and M.~Gosselin and A.~S.~Göttel and R.~Gouaty and D.~W.~Gould and S.~Goyal and B.~Grace and A.~Grado and V.~Graham and A.~E.~Granados and M.~Granata and V.~Granata and L.~Granda Argianas and S.~Gras and P.~Grassia and C.~Gray and R.~Gray and G.~Greco and A.~C.~Green and S.~M.~Green and S.~R.~Green and A.~M.~Gretarsson and E.~M.~Gretarsson and D.~Griffith and W.~L.~Griffiths and H.~L.~Griggs and G.~Grignani and A.~Grimaldi and C.~Grimaud and H.~Grote and A.~S.~Gruson and D.~Guerra and D.~Guetta and G.~M.~Guidi and A.~R.~Guimaraes and H.~K.~Gulati and F.~Gulminelli and A.~M.~Gunny and H.~Guo and W.~Guo and Y.~Guo and Anchal Gupta and Anuradha Gupta and Ish Gupta and N.~C.~Gupta and P.~Gupta and S.~K.~Gupta and T.~Gupta and N.~Gupte and R.~Gurav and J.~Gurs and N.~Gutierrez and F.~Guzman and D.~Haba and M.~Haberland and L.~Haegel and G.~Hain and S.~Haino and E.~D.~Hall and E.~Z.~Hamilton and G.~Hammond and W.-B.~Han and M.~Haney and J.~Hanks and C.~Hanna and M.~D.~Hannam and O.~A.~Hannuksela and A.~G.~Hanselman and H.~Hansen and J.~Hanson and R.~Harada and T.~Harder and K.~Haris and T.~Harmark and J.~Harms and G.~M.~Harry and I.~W.~Harry and B.~Haskell and C.-J.~Haster and J.~S.~Hathaway and K.~Haughian and H.~Hayakawa and K.~Hayama and J.~Healy and A.~Heffernan and A.~Heidmann and M.~C.~Heintze and J.~Heinze and J.~Heinzel and H.~Heitmann and F.~Hellman and P.~Hello and A.~F.~Helmling-Cornell and G.~Hemming and M.~Hendry and I.~S.~Heng and E.~Hennes and J.-S.~Hennig and M.~Hennig and C.~Henshaw and A.~Hernandez and T.~Hertog and M.~Heurs and A.~L.~Hewitt and S.~Higginbotham and S.~Hild and P.~Hill and S.~Hill and Y.~Himemoto and A.~S.~Hines and N.~Hirata and C.~Hirose and J.~Ho and S.~Hoang and S.~Hochheim and D.~Hofman and N.~A.~Holland and K.~Holley-Bockelmann and I.~J.~Hollows and Z.~J.~Holmes and D.~E.~Holz and C.~Hong and J.~Hornung and S.~Hoshino and S.~Hourihane and E.~J.~Howell and C.~G.~Hoy and D.~Hoyland and C.~A.~Hrishikesh and H.-F.~Hsieh and C.~Hsiung and H.~C.~Hsu and S.-C.~Hsu and W.-F.~Hsu and P.~Hu and Q.~Hu and H.~Y.~Huang and Y.-J.~Huang and Y.~Huang and Y.~T.~Huang and A.~D.~Huddart and B.~Hughey and D.~C.~Y.~Hui and V.~Hui and R.~Hur and S.~Husa and R.~Huxford and T.~Huynh-Dinh and A.~Iakovlev and G.~A.~Iandolo and A.~Iess and K.~Inayoshi and Y.~Inoue and G.~Iorio and J.~Irwin and M.~Isi and M.~A.~Ismail and Y.~Itoh and M.~Iwaya and B.~R.~Iyer and V.~JaberianHamedan and P.-E.~Jacquet and S.~J.~Jadhav and S.~P.~Jadhav and T.~Jain and A.~L.~James and P.~A.~James and R.~Jamshidi and A.~Z.~Jan and K.~Jani and L.~Janiurek and J.~Janquart and K.~Janssens and N.~N.~Janthalur and S.~Jaraba and P.~Jaranowski and P.~Jasal and R.~Jaume and W.~Javed and A.~Jennings and W.~Jia and J.~Jiang and H.-B.~Jin and K.~Johansmeyer and G.~R.~Johns and N.~A.~Johnson and R.~Johnston and N.~Johny and D.~H.~Jones and D.~I.~Jones and R.~Jones and S.~Jose and P.~Joshi and L.~Ju and K.~Jung and J.~Junker and V.~Juste and T.~Kajita and C.~Kalaghatgi and V.~Kalogera and M.~Kamiizumi and N.~Kanda and S.~Kandhasamy and G.~Kang and J.~B.~Kanner and S.~J.~Kapadia and D.~P.~Kapasi and S.~Karat and C.~Karathanasis and S.~Karki and R.~Kashyap and M.~Kasprzack and W.~Kastaun and J.~Kato and T.~Kato and S.~Katsanevas and E.~Katsavounidis and W.~Katzman and T.~Kaur and R.~Kaushik and K.~Kawabe and D.~Keitel and J.~Kelley-Derzon and J.~Kennington and R.~Kesharwani and J.~S.~Key and S.~Khadka and F.~Y.~Khalili and F.~Khan and I.~Khan and T.~Khanam and E.~A.~Khazanov and M.~Khursheed and W.~Kiendrebeogo and N.~Kijbunchoo and C.~Kim and J.~C.~Kim and K.~Kim and M.~H.~Kim and S.~Kim and W.~S.~Kim and Y.-M.~Kim and C.~Kimball and N.~Kimura and M.~Kinley-Hanlon and M.~Kinnear and J.~S.~Kissel and T.~Kiyota and S.~Klimenko and T.~Klinger and A.~M.~Knee and N.~Knust and P.~Koch and S.~M.~Koehlenbeck and G.~Koekoek and K.~Kohri and K.~Kokeyama and S.~Koley and P.~Kolitsidou and M.~Kolstein and K.~Komori and A.~K.~H.~Kong and A.~Kontos and M.~Korobko and R.~V.~Kossak and X.~Kou and A.~Koushik and N.~Kouvatsos and M.~Kovalam and N.~Koyama and D.~B.~Kozak and S.~L.~Kranzhoff and V.~Kringel and N.~V.~Krishnendu and A.~Królak and G.~Kuehn and P.~Kuijer and S.~Kulkarni and A.~Kulur Ramamohan and A.~Kumar and Praveen Kumar and Prayush Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and S.~Kuroyanagi and S.~Kuwahara and K.~Kwak and K.~Kwan and G.~Lacaille and P.~Lagabbe and D.~Laghi and S.~Lai and A.~H.~Laity and M.~H.~Lakkis and E.~Lalande and M.~Lalleman and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and A.~La Rana and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and J.~Lawrence and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and S.~LeBohec and Y.~K.~Lecoeuche and H.~M.~Lee and H.~W.~Lee and K.~Lee and R.-K.~Lee and R.~Lee and S.~Lee and Y.~Lee and I.~N.~Legred and J.~Lehmann and L.~Lehner and A.~Lemaître and M.~Lenti and M.~Leonardi and E.~Leonova and M.~Lequime and N.~Leroy and M.~Lesovsky and N.~Letendre and M.~Lethuillier and C.~Levesque and Y.~Levin and K.~Leyde and A.~K.~Y.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and Chien-Yu Lin and Chun-Yu Lin and E.~T.~Lin and F.~Lin and H.~Lin and L.~C.-C.~Lin and F.~Linde and S.~D.~Linker and T.~B.~Littenberg and A.~Liu and G.~C.~Liu and Jian Liu and F.~Llamas and J.~Llobera-Querol and R.~K.~L.~Lo and J.-P.~Locquet and L.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott IV and J.~D.~Lough and H.~A.~Loughlin and C.~O.~Lousto and M.~J.~Lowry and H.~Lück and D.~Lumaca and A.~P.~Lundgren and A.~W.~Lussier and L.-T.~Ma and S.~Ma and M.~Ma'arif and R.~Macas and M.~MacInnis and R.~R.~Maciy and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and D.~Macri and K.~Maeda and S.~Maenaut and I.~Magaña Hernandez and S.~S.~Magare and C.~Magazzù and R.~M.~Magee and E.~Maggio and R.~Maggiore and M.~Magnozzi and M.~Mahesh and S.~Mahesh and M.~Maini and S.~Majhi and E.~Majorana and C.~N.~Makarem and J.~A.~Malaquias-Reis and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and B.~Mannix and G.~L.~Mansell and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and D.~Marín Pina and F.~Marion and S.~Márka and Z.~Márka and C.~Markakis and A.~S.~Markosyan and A.~Markowitz and E.~Maros and A.~Marquina and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and B.~B.~Martinez and M.~Martinez and V.~Martinez and A.~Martini and K.~Martinovic and J.~C.~Martins and D.~V.~Martynov and E.~J.~Marx and L.~Massaro and A.~Masserot and M.~Masso-Reid and M.~Mastrodicasa and S.~Mastrogiovanni and M.~Mateu-Lucena and M.~Matiushechkina and M.~Matsuyama and N.~Mavalvala and N.~Maxwell and G.~McCarrol and R.~McCarthy and D.~E.~McClelland and S.~McCormick and L.~McCuller and G.~I.~McGhee and K.~B.~M.~McGowan and M.~Mchedlidze and C.~McIsaac and J.~McIver and K.~McKinney and A.~McLeod and T.~McRae and S.~T.~McWilliams and D.~Meacher and A.~K.~Mehta and Q.~Meijer and A.~Melatos and S.~Mellaerts and A.~Menendez-Vazquez and C.~S.~Menoni and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~R.~Mérou and J.~D.~Merritt and M.~Merzougui and C.~Messenger and C.~Messick and M.~Meyer-Conde and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and A.~L.~Miller and S.~Miller and M.~Millhouse and E.~Milotti and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and L.~Mirasola and M.~Miravet-Tenés and C.-A.~Miritescu and A.~K.~Mishra and A.~Mishra and C.~Mishra and T.~Mishra and A.~L.~Mitchell and J.~G.~Mitchell and S.~Mitra and V.~P.~Mitrofanov and G.~Mitselmakher and R.~Mittleman and O.~Miyakawa and S.~Miyamoto and S.~Miyoki and G.~Mo and L.~Mobilia and L.~M.~Modafferi and S.~R.~P.~Mohapatra and S.~R.~Mohite and M.~Molina-Ruiz and C.~Mondal and M.~Mondin and M.~Montani and C.~J.~Moore and M.~Morales and D.~Moraru and F.~Morawski and A.~More and S.~More and C.~Moreno and G.~Moreno and S.~Morisaki and Y.~Moriwaki and G.~Morras and A.~Moscatello and P.~Mourier and B.~Mours and C.~M.~Mow-Lowry and S.~Mozzon and F.~Muciaccia and D.~Mukherjee and Samanwaya Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and C.~L.~Mungioli and M.~Munn and W.~R.~Munn Oberg and M.~Murakoshi and P.~G.~Murray and S.~Muusse and S.~L.~Nadji and A.~Nagar and N.~Nagarajan and K.~N.~Nagler and K.~Nakamura and H.~Nakano and M.~Nakano and D.~Nandi and V.~Napolano and P.~Narayan and I.~Nardecchia and H.~Narola and L.~Naticchioni and R.~K.~Nayak and B.~F.~Neil and J.~Neilson and A.~Nelson and T.~J.~N.~Nelson and M.~Nery and A.~Neunzert and S.~Ng and C.~Nguyen and P.~Nguyen and L.~Nguyen Quynh and S.~A.~Nichols and A.~B.~Nielsen and G.~Nieradka and A.~Niko and Y.~Nishino and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and W.~Niu and F.~Nocera and M.~Norman and C.~North and J.~Novak and J.~F.~Nuño Siles and G.~Nurbek and L.~K.~Nuttall and K.~Obayashi and J.~Oberling and J.~O'Dell and M.~Oertel and A.~Offermans and G.~Oganesyan and J.~J.~Oh and K.~Oh and S.~H.~Oh and T.~O'Hanlon and M.~Ohashi and M.~Ohkawa and F.~Ohme and H.~Ohta and A.~S.~Oliveira and R.~Oliveri and V.~Oloworaran and B.~O'Neal and K.~Oohara and B.~O'Reilly and N.~D.~Ormsby and M.~Orselli and R.~O'Shaughnessy and Y.~Oshima and S.~Oshino and S.~Ossokine and C.~Osthelder and D.~J.~Ottaway and A.~Ouzriat and H.~Overmier and B.~J.~Owen and A.~E.~Pace and R.~Pagano and M.~A.~Page and A.~Pai and S.~A.~Pai and A.~Pal and S.~Pal and M.~A.~Palaia and O.~Palashov and M.~Pálfi and P.~P.~Palma and C.~Palomba and K.~C.~Pan and P.~K.~Panda and L.~Panebianco and P.~T.~H.~Pang and F.~Pannarale and B.~C.~Pant and F.~H.~Panther and C.~D.~Panzer and F.~Paoletti and A.~Paoli and A.~Paolone and E.~E.~Papalexakis and L.~Papalini and G.~Papigkiotis and A.~Parisi and J.~Park and W.~Parker and G.~Pascale and D.~Pascucci and A.~Pasqualetti and R.~Passaquieti and D.~Passuello and O.~Patane and M.~Patel and D.~Pathak and M.~Pathak and A.~Patra and B.~Patricelli and A.~S.~Patron and S.~Paul and E.~Payne and T.~Pearce and M.~Pedraza and R.~Pegna and A.~Pele and F.~E.~Peña Arellano and S.~Penn and M.~D.~Penuliar and A.~Perego and A.~Pereira and J.~J.~Perez and C.~Périgois and C.~C.~Perkins and G.~Perna and A.~Perreca and J.~Perret and S.~Perriès and J.~W.~Perry and D.~Pesios and C.~Petrillo and H.~P.~Pfeiffer and H.~Pham and K.~A.~Pham and K.~S.~Phukon and H.~Phurailatpam and O.~J.~Piccinni and M.~Pichot and M.~Piendibene and F.~Piergiovanni and L.~Pierini and G.~Pierra and V.~Pierro and M.~Pietrzak and M.~Pillas and F.~Pilo and L.~Pinard and C.~Pineda-Bosque and I.~M.~Pinto and M.~Pinto and B.~J.~Piotrzkowski and M.~Pirello and M.~D.~Pitkin and A.~Placidi and E.~Placidi and M.~L.~Planas and W.~Plastino and R.~Poggiani and E.~Polini and L.~Pompili and J.~Poon and E.~Porcelli and J.~Portell and E.~K.~Porter and C.~Posnansky and R.~Poulton and J.~Powell and M.~Pracchia and B.~K.~Pradhan and T.~Pradier and A.~K.~Prajapati and K.~Prasai and R.~Prasanna and P.~Prasia and G.~Pratten and M.~Principe and G.~A.~Prodi and L.~Prokhorov and P.~Prosposito and L.~Prudenzi and A.~Puecher and J.~Pullin and M.~Punturo and F.~Puosi and P.~Puppo and M.~Pürrer and H.~Qi and J.~Qin and G.~Quéméner and V.~Quetschke and C.~Quigley and P.~J.~Quinonez and R.~Quitzow-James and F.~J.~Raab and G.~Raaijmakers and N.~Radulesco and P.~Raffai and S.~X.~Rail and S.~Raja and C.~Rajan and B.~Rajbhandari and D.~S.~Ramirez and K.~E.~Ramirez and F.~A.~Ramis Vidal and A.~Ramos-Buades and D.~Rana and E.~Randel and S.~Ranjan and P.~Rapagnani and B.~Ratto and S.~Rawat and A.~Ray and V.~Raymond and M.~Razzano and J.~Read and M.~Recaman Payo and T.~Regimbau and L.~Rei and S.~Reid and S.~W.~Reid and D.~H.~Reitze and P.~Relton and A.~Renzini and P.~Rettegno and B.~Revenu and A.~Reza and M.~Rezac and A.~S.~Rezaei and F.~Ricci and M.~Ricci and D.~Richards and C.~J.~Richardson and J.~W.~Richardson and A.~Rijal and K.~Riles and H.~K.~Riley and S.~Rinaldi and J.~Rittmeyer and C.~Robertson and F.~Robinet and M.~Robinson and A.~Rocchi and L.~Rolland and J.~G.~Rollins and M.~Romanelli and A.~E.~Romano and R.~Romano and A.~Romero and I.~M.~Romero-Shaw and J.~H.~Romie and S.~Ronchini and T.~J.~Roocke and L.~Rosa and T.~J.~Rosauer and C.~A.~Rose and D.~Rosińska and M.~P.~Ross and M.~Rossello and S.~Rowan and S.~K.~Roy and S.~Roy and D.~Rozza and P.~Ruggi and E.~Ruiz Morales and K.~Ruiz-Rocha and S.~Sachdev and T.~Sadecki and J.~Sadiq and P.~Saffarieh and M.~R.~Sah and S.~S.~Saha and T.~Sainrat and S.~Sajith Menon and K.~Sakai and M.~Sakellariadou and T.~Sako and S.~Sakon and O.~S.~Salafia and F.~Salces-Carcoba and L.~Salconi and M.~Saleem and F.~Salemi and M.~Sallé and S.~Salvador and A.~Sanchez and E.~J.~Sanchez and J.~H.~Sanchez and L.~E.~Sanchez and N.~Sanchis-Gual and J.~R.~Sanders and E.~M.~Sänger and T.~R.~Saravanan and N.~Sarin and A.~Sasli and P.~Sassi and B.~Sassolas and H.~Satari and R.~Sato and S.~Sato and Y.~Sato and O.~Sauter and R.~L.~Savage and T.~Sawada and H.~L.~Sawant and S.~Sayah and D.~Schaetzl and M.~Scheel and J.~Scheuer and M.~G.~Schiworski and P.~Schmidt and S.~Schmidt and R.~Schnabel and M.~Schneewind and R.~M.~S.~Schofield and K.~Schouteden and H.~Schuler and B.~W.~Schulte and B.~F.~Schutz and E.~Schwartz and J.~Scott and S.~M.~Scott and T.~C.~Seetharamu and M.~Seglar-Arroyo and Y.~Sekiguchi and D.~Sellers and A.~S.~Sengupta and D.~Sentenac and E.~G.~Seo and J.~W.~Seo and V.~Sequino and A.~Sergeev and M.~Serra and G.~Servignat and Y.~Setyawati and T.~Shaffer and U.~S.~Shah and M.~S.~Shahriar and M.~A.~Shaikh and B.~Shams and L.~Shao and A.~K.~Sharma and P.~Sharma and S.~Sharma-Chaudhary and P.~Shawhan and N.~S.~Shcheblanov and B.~Shen and Y.~Shikano and M.~Shikauchi and K.~Shimode and H.~Shinkai and J.~Shiota and D.~H.~Shoemaker and D.~M.~Shoemaker and R.~W.~Short and S.~ShyamSundar and A.~Sider and H.~Siegel and M.~Sieniawska and D.~Sigg and L.~Silenzi and M.~Simmonds and L.~P.~Singer and A.~Singh and D.~Singh and M.~K.~Singh and A.~Singha and A.~M.~Sintes and V.~Sipala and V.~Skliris and B.~J.~J.~Slagmolen and T.~J.~Slaven-Blair and J.~Smetana and J.~R.~Smith and L.~Smith and R.~J.~E.~Smith and W.~J.~Smith and J.~Soldateschi and S.~N.~Somala and K.~Somiya and K.~Soni and S.~Soni and V.~Sordini and F.~Sorrentino and N.~Sorrentino and R.~Soulard and T.~Souradeep and A.~Southgate and E.~Sowell and V.~Spagnuolo and A.~P.~Spencer and M.~Spera and P.~Spinicelli and A.~K.~Srivastava and F.~Stachurski and D.~A.~Steer and J.~Steinlechner and S.~Steinlechner and N.~Stergioulas and P.~Stevens and M.~StPierre and L.~C.~Strang and G.~Stratta and M.~D.~Strong and A.~Strunk and R.~Sturani and A.~L.~Stuver and M.~Suchenek and S.~Sudhagar and N.~Sueltmann and A.~G.~Sullivan and K.~D.~Sullivan and L.~Sun and S.~Sunil and A.~Sur and J.~Suresh and P.~J.~Sutton and Takamasa Suzuki and Takanori Suzuki and B.~L.~Swinkels and A.~Syx and M.~J.~Szczepańczyk and P.~Szewczyk and M.~Tacca and H.~Tagoshi and S.~C.~Tait and H.~Takahashi and R.~Takahashi and A.~Takamori and K.~Takatani and H.~Takeda and M.~Takeda and C.~J.~Talbot and C.~Talbot and M.~Tamaki and N.~Tamanini and D.~Tanabe and K.~Tanaka and S.~J.~Tanaka and T.~Tanaka and A.~J.~Tanasijczuk and D.~Tang and S.~Tanioka and D.~B.~Tanner and L.~Tao and R.~D.~Tapia and E.~N.~Tapia San Martín and R.~Tarafder and C.~Taranto and A.~Taruya and J.~D.~Tasson and M.~Teloi and R.~Tenorio and H.~Themann and A.~Theodoropoulos and M.~P.~Thirugnanasambandam and L.~M.~Thomas and M.~Thomas and P.~Thomas and J.~E.~Thompson and S.~R.~Thondapu and K.~A.~Thorne and E.~Thrane and J.~Tissino and A.~Tiwari and Shubhanshu Tiwari and Srishti Tiwari and V.~Tiwari and M.~R.~Todd and A.~M.~Toivonen and K.~Toland and A.~E.~Tolley and T.~Tomaru and K.~Tomita and T.~Tomura and C.~Tong-Yu and A.~Toriyama and N.~Toropov and A.~Torres-Forné and C.~I.~Torrie and M.~Toscani and I.~Tosta e Melo and E.~Tournefier and A.~A.~Trani and A.~Trapananti and F.~Travasso and G.~Traylor and J.~Trenado and M.~Trevor and M.~C.~Tringali and A.~Tripathee and L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and T.~T.~L.~Tsang and R.~Tso and S.~Tsuchida and L.~Tsukada and T.~Tsutsui and K.~Turbang and M.~Turconi and C.~Turski and H.~Ubach and A.~S.~Ubhi and T.~Uchiyama and R.~P.~Udall and T.~Uehara and K.~Ueno and C.~S.~Unnikrishnan and T.~Ushiba and A.~Utina and M.~Vacatello and H.~Vahlbruch and N.~Vaidya and G.~Vajente and A.~Vajpeyi and G.~Valdes and J.~Valencia and M.~Valentini and S.~A.~Vallejo-Peña and S.~Vallero and V.~Valsan and N.~van Bakel and M.~van Beuzekom and M.~van Dael and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and M.~van der Sluys and A.~Van de Walle and J.~van Dongen and K.~Vandra and H.~van Haevermaet and J.~V.~van Heijningen and J.~Vanosky and M.~H.~P.~M.~van Putten and Z.~van Ranst and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and V.~Varma and M.~Vasúth and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and S.~Venikoudis and J.~Venneberg and P.~Verdier and D.~Verkindt and B.~Verma and P.~Verma and Y.~Verma and S.~M.~Vermeulen and D.~Veske and F.~Vetrano and A.~Veutro and A.~M.~Vibhute and A.~Viceré and S.~Vidyant and A.~D.~Viets and A.~Vijaykumar and A.~Vilkha and V.~Villa-Ortega and E.~T.~Vincent and J.-Y.~Vinet and S.~Viret and A.~Virtuoso and S.~Vitale and H.~Vocca and D.~Voigt and E.~R.~G.~von Reis and J.~S.~A.~von Wrangel and S.~P.~Vyatchanin and L.~E.~Wade and M.~Wade and K.~J.~Wagner and R.~C.~Walet and M.~Walker and G.~S.~Wallace and L.~Wallace and H.~Wang and J.~Z.~Wang and W.~H.~Wang and Z.~Wang and G.~Waratkar and R.~L.~Ward and J.~Warner and M.~Was and T.~Washimi and N.~Y.~Washington and D.~Watarai and K.~E.~Wayt and B.~Weaver and C.~R.~Weaving and S.~A.~Webster and M.~Weinert and A.~J.~Weinstein and R.~Weiss and C.~M.~Weller and R.~A.~Weller and F.~Wellmann and L.~Wen and P.~Weßels and K.~Wette and J.~T.~Whelan and D.~D.~White and B.~F.~Whiting and C.~Whittle and J.~B.~Wildberger and O.~S.~Wilk and D.~Wilken and K.~Willetts and D.~Williams and M.~J.~Williams and N.~S.~Williams and J.~L.~Willis and B.~Willke and M.~Wils and C.~C.~Wipf and G.~Woan and J.~Woehler and J.~K.~Wofford and N.~E.~Wolfe and D.~Wong and H.~T.~Wong and H.~W.~Y.~Wong and I.~C.~F.~Wong and J.~L.~Wright and M.~Wright and C.~Wu and D.~S.~Wu and H.~Wu and D.~M.~Wysocki and L.~Xiao and V.~A.~Xu and Y.~Xu and N.~Yadav and H.~Yamamoto and K.~Yamamoto and M.~Yamamoto and T.~S.~Yamamoto and T.~Yamamoto and S.~Yamamura and R.~Yamazaki and S.~Yan and T.~Yan and F.~W.~Yang and F.~Yang and K.~Z.~Yang and L.-C.~Yang and Y.~Yang and Z.~Yarbrough and S.-W.~Yeh and A.~B.~Yelikar and S.~M.~C.~Yeung and X.~Yin and J.~Yokoyama and T.~Yokozawa and J.~Yoo and H.~Yu and H.~Yuzurihara and A.~Zadrożny and A.~J.~Zannelli and M.~Zanolin and M.~Zeeshan and T.~Zelenova and J.-P.~Zendri and M.~Zeoli and M.~Zerrad and M.~Zevin and A.~C.~Zhang and J.~Zhang and L.~Zhang and R.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and Yue Zhao and Yuhang Zhao and Y.~Zheng and H.~Zhong and S.~Zhong and R.~Zhou and Z.-H.~Zhu and M.~E.~Zucker and J.~Zweizig and T.~Fujimori and H.~Fujimoto and T.~Fujita and Y.~Manita and I.~Obata and H.~Takidera}, title = {{U}ltralight vector dark matter search using data from the {KAGRA} {O}3{GK} run}, year = {2024}, eprint = {2403.03004}, note = {arXiv:2403.03004v1} }
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Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for $U(1)_{B-L}$ gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the $U(1)_{B-L}$ gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM.
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.
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.
Report of the Topical Group on Particle Dark Matter for Snowmass 2021
Jodi Cooley, Tongyan Lin, W. Hugh Lippincott, Tracy R. Slatyer, Tien-Tien Yu, Daniel S. Akerib, Tsuguo Aramaki, Daniel Baxter, Torsten Bringmann, Ray Bunker, Daniel Carney, Susana Cebrián, Thomas Y. Chen, Priscilla Cushman, C.E. Dahl, Rouven Essig, Alden Fan, Richard Gaitskell, Cristano Galbiati, Graciela B. Gelmini, et al (54)
Sep 16 2022 hep-ph astro-ph.CO astro-ph.HE hep-ex arXiv:2209.07426v1

@misc{2209.07426, author = {Jodi Cooley and Tongyan Lin and W.~Hugh Lippincott and Tracy R.~Slatyer and Tien-Tien Yu and Daniel S.~Akerib and Tsuguo Aramaki and Daniel Baxter and Torsten Bringmann and Ray Bunker and Daniel Carney and Susana Cebrián and Thomas Y.~Chen and Priscilla Cushman and C.E.~Dahl and Rouven Essig and Alden Fan and Richard Gaitskell and Cristano Galbiati and Graciela B.~Gelmini and Graham K.~Giovanetti and Guillaume Giroux and Luca Grandi and J.~Patrick Harding and Scott Haselschwardt and Lauren Hsu and Shunsaku Horiuchi and Yonatan Kahn and Doojin Kim and Geon-Bo Kim and Scott Kravitz and V.~A.~Kudryavtsev and Noah Kurinsky and Rafael F.~Lang and Rebecca K.~Leane and Benjamin V.~Lehmann and Cecilia Levy and Shengchao Li and Ben Loer and Aaron Manalaysay and C.~J Martoff and Gopolang Mohlabeng and M.E.~Monzani and Alexander St J.~Murphy and Russell Neilson and Harry N.~Nelson and Ciaran A.~J.~O'Hare and K.J.~Palladino and Aditya Parikh and Jong-Chul Park and Kerstin Perez and Stefano Profumo and Nirmal Raj and Brandon M.~Roach and Tarek Saab and Maria Luísa Sarsa and Richard Schnee and Sally Shaw and Seodong Shin and Kuver Sinha and Kelly Stifter and Aritoki Suzuki and M.~Szydagis and Tim M.P.~Tait and Volodymyr Takhistov and Yu-Dai Tsai and S.~E.~Vahsen and Edoardo Vitagliano and Philip von Doetinchem and Gensheng Wang and Shawn Westerdale and David A.~Williams and Xin Xiang and Liang Yang}, title = {{R}eport of the {T}opical {G}roup on {P}article {D}ark {M}atter for {S}nowmass 2021}, year = {2022}, eprint = {2209.07426}, note = {arXiv:2209.07426v1} }
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This report summarizes the findings of the CF1 Topical Subgroup to Snowmass 2021, which was focused on particle dark matter. One of the most important scientific goals of the next decade is to reveal the nature of dark matter (DM). To accomplish this goal, we must delve deep, to cover high priority targets including weakly-interacting massive particles (WIMPs), and search wide, to explore as much motivated DM parameter space as possible. A diverse, continuous portfolio of experiments at large, medium, and small scales that includes both direct and indirect detection techniques maximizes the probability of discovering particle DM. Detailed calibrations and modeling of signal and background processes are required to make a convincing discovery. In the event that a candidate particle is found through different means, for example at a particle collider, the program described in this report is also essential to show that it is consistent with the actual cosmological DM. The US has a leading role in both direct and indirect detection dark matter experiments -- to maintain this leading role, it is imperative to continue funding major experiments and support a robust R\&D program.
Snowmass2021 Cosmic Frontier White Paper: Puzzling Excesses in Dark Matter Searches and How to Resolve Them
Rebecca K. Leane, Seodong Shin, Liang Yang, Govinda Adhikari, Haider Alhazmi, Tsuguo Aramaki, Daniel Baxter, Francesca Calore, Regina Caputo, Ilias Cholis, Tansu Daylan, Mattia Di Mauro, Philip von Doetinchem, Ke Han, Dan Hooper, Shunsaku Horiuchi, Doojin Kim, Kyoungchul Kong, Rafael F. Lang, Qing Lin, et al (19)
Mar 15 2022 hep-ph astro-ph.HE hep-ex arXiv:2203.06859v1

@misc{2203.06859, author = {Rebecca K.~Leane and Seodong Shin and Liang Yang and Govinda Adhikari and Haider Alhazmi and Tsuguo Aramaki and Daniel Baxter and Francesca Calore and Regina Caputo and Ilias Cholis and Tansu Daylan and Mattia Di Mauro and Philip von Doetinchem and Ke Han and Dan Hooper and Shunsaku Horiuchi and Doojin Kim and Kyoungchul Kong and Rafael F.~Lang and Qing Lin and Tim Linden and Jianglai Liu and Oscar Macias and Siddharth Mishra-Sharma and Alexander Murphy and Meshkat Rajaee and Nicholas L.~Rodd and Aditya Parikh and Jong-Chul Park and Maria Luisa Sarsa and Evan Shockley and Tracy R.~Slatyer and Volodymyr Takhistov and Felix Wagner and Jingqiang Ye and Gabrijela Zaharijas and Yi-Ming Zhong and Ning Zhou and Xiaopeng Zhou}, title = {{S}nowmass2021 {C}osmic {F}rontier {W}hite {P}aper: {P}uzzling {E}xcesses in {D}ark {M}atter {S}earches and {H}ow to {R}esolve {T}hem}, year = {2022}, eprint = {2203.06859}, note = {arXiv:2203.06859v1} }
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Intriguing signals with excesses over expected backgrounds have been observed in many astrophysical and terrestrial settings, which could potentially have a dark matter origin. Astrophysical excesses include the Galactic Center GeV gamma-ray excess detected by the Fermi Gamma-Ray Space Telescope, the AMS antiproton and positron excesses, and the 511 and 3.5 keV X-ray lines. Direct detection excesses include the DAMA/LIBRA annual modulation signal, the XENON1T excess, and low-threshold excesses in solid state detectors. We discuss avenues to resolve these excesses, with actions the field can take over the next several years.
Snowmass 2021 White Paper: The Windchime Project
Windchime Collaboration, Alaina Attanasio, Sunil A. Bhave, Carlos Blanco, Daniel Carney, Marcel Demarteau, Bahaa Elshimy, Michael Febbraro, Matthew A. Feldman, Sohitri Ghosh, Abby Hickin, Seongjin Hong, Rafael F. Lang, Benjamin Lawrie, Shengchao Li, Zhen Liu, Juan P. A. Maldonado, Claire Marvinney, Hein Zay Yar Oo, Yun-Yi Pai, et al (6)
Mar 15 2022 hep-ex astro-ph.CO hep-ph arXiv:2203.07242v1

@misc{2203.07242, author = {Windchime Collaboration and Alaina Attanasio and Sunil A.~Bhave and Carlos Blanco and Daniel Carney and Marcel Demarteau and Bahaa Elshimy and Michael Febbraro and Matthew A.~Feldman and Sohitri Ghosh and Abby Hickin and Seongjin Hong and Rafael F.~Lang and Benjamin Lawrie and Shengchao Li and Zhen Liu and Juan P.~A.~Maldonado and Claire Marvinney and Hein Zay Yar Oo and Yun-Yi Pai and Raphael Pooser and Juehang Qin and Tobias J.~Sparmann and Jacob M.~Taylor and Hao Tian and Christopher Tunnell}, title = {{S}nowmass 2021 {W}hite {P}aper: {T}he {W}indchime {P}roject}, year = {2022}, eprint = {2203.07242}, note = {arXiv:2203.07242v1} }
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The absence of clear signals from particle dark matter in direct detection experiments motivates new approaches in disparate regions of viable parameter space. In this Snowmass white paper, we outline the Windchime project, a program to build a large array of quantum-enhanced mechanical sensors. The ultimate aim is to build a detector capable of searching for Planck mass-scale dark matter purely through its gravitational coupling to ordinary matter. In the shorter term, we aim to search for a number of other physics targets, especially some ultralight dark matter candidates. Here, we discuss the basic design, open R&D challenges and opportunities, current experimental efforts, and both short- and long-term physics targets of the Windchime project.
Coherent elastic neutrino-nucleus scattering: Terrestrial and astrophysical applications
M. Abdullah, H. Abele, D. Akimov, G. Angloher, D. Aristizabal-Sierra, C. Augier, A. B. Balantekin, L. Balogh, P. S. Barbeau, L. Baudis, A. L. Baxter, C. Beaufort, G. Beaulieu, V. Belov, A. Bento, L. Berge, I. A. Bernardi, J. Billard, A. Bolozdynya, A. Bonhomme, et al (255)
Mar 15 2022 hep-ph astro-ph.HE hep-ex arXiv:2203.07361v1

@misc{2203.07361, author = {M.~Abdullah and H.~Abele and D.~Akimov and G.~Angloher and D.~Aristizabal-Sierra and C.~Augier and A.~B.~Balantekin and L.~Balogh and P.~S.~Barbeau and L.~Baudis and A.~L.~Baxter and C.~Beaufort and G.~Beaulieu and V.~Belov and A.~Bento and L.~Berge and I.~A.~Bernardi and J.~Billard and A.~Bolozdynya and A.~Bonhomme and G.~Bres and J-.L.~Bret and A.~Broniatowski and A.~Brossard and C.~Buck and M.~Cadeddu and M.~Calvo and L.~Canonica and F.~Cappella and L.~Cardani and N.~Casali and A.~Cazes and R.~Cerulli and D.~Chaize and C.~Chang and M.~Chapellier and L.~Chaplinsky and G.~Chemin and R.~Chen and I.~Colantoni and J.~Colas and P.~Coloma and E.~C.~Corcoran and S.~Crawford and A.~Cruciani and A.~Dastgheibi Fard and M.~De Jesus and P.~de Marcillac and V.~De Romeri and G.~del Castello and M.~del GalloRoccagiovine and D.~Delicato and M.~Demarteau and Y.~Deng and J.~B.~Dent and P.~B.~Denton and K.~Dering and A.~Doblhammer and F.~Dordei and S.~Dorer and L.~Dumoulin and D.~Dunford and B.~Dutta and A.~Erhart and O.~Exshaw and S.~Ferriol and E.~Figueroa-Feliciano and J.~B.~Filippini and L .J.~Flores and J.~A.~Formaggio and M.~Friedl and S.~Fuard and F.~Gao and A.~Garai and E.~A.~Garces and J.~Gascon and J.~Gehrlein and G.~Gerbier and V.~M.~Ghete and I.~Giomataris and G.~Giroux and A.~Giuliani and C.~Giunti and P.~Gorel and C.~Goupy and J.~Goupy and C.~Goy and M.~P.~Green and M.~Gros and C.~Guerin and V.~Guidi and O.~Guillaudin and E.~Guy and C.~Ha and D.~Hauff and J.~Hakenmuller and P.~M.~Harrington and S.~Hedges and S.~T.~Heine and S.~Hertel and M.~Heusch and C.~Hoarau and M.~Hoferichter and E.~W.~Hoppe and Z.~Hong and S.~Horiuchi and P.~Huber and J.~C.~Ianigro and N.~Jachowicz and E.~Jericha and Y.~Jin and J.~P.~Johnston and A.~Juillard and I.~Katsioulas and S.~Kazarcev and M.~Kaznacheeva and F.~Kelly and K.~J.~Kelly and D.~Kim and A.~Kinast and L.~Klinkenberg and H.~Kluck and P.~Knights and Y.~J.~Ko and T.~S.~Kosmas and L.~Kwon and J.~Lamblin and R.~F.~Lang and A.~Langenkamper and S.~Langrock and T.~Lasserre and H.~Lattaud and P.~Lautridou and H.~S.~Lee and B.~G.~Lenardo and D.~Lhuillier and M.~Li and S.~C.~Li and Y.~F.~Li and Z.~Li and M.~Lindner and J.~Liu and D.~Loomba and A.~Lubashevskiy and P.~A.~N.~Machado and M.~Mancuso and W.~Maneschg and D.~M.~Markoff and S.~Marnieros and R.~Martin and R.~D.~Martin and B.~Mauri and D.~W.~Mayer and A.~Mazzolari and E.~Mazzucato and J.~Menendez and J.~Minet and O.~G.~Miranda and D.~Misiak and J.-P.~Mols and A.~Monfardini and F.~Mounier and J.~F.~Muraz and T.~Neep and R.~Neilson and J.~Newby and J.~L.~Newstead and H.~Neyrial and K.~Ni and K.~Nikolopoulos and C.~Nones and D.~Norcini and V.~Pandey and P.~O'Brien and C.~A.~J.~O'Hare and L.~Oberauer and W.~Oliver and E.~Olivieri and A.~Onillon and C.~Oriol and T.~Ortmann and R.~Owen and K.~J.~Palladino and D.~K.~Papoulias and J.~C.~Park and D.~S.~Parno and P.~K.~Patel and L.~Pattavina and E.~Peinado and E.~Perbet and L.~Peters and F.~Petricca and H.~D.~Pinckney and M.-C.~Piro and D.~Ponomarev and D.~Poda and W.~Potzel and F.~Probst and F.~Pucci and F.~Rarbi and R.~Rapp and H.Ray and J.-S.Real and F.~Reindl and G.C.Rich and J.S.Ricol and T.Rink and T.Redon and R.Rogly and A.Robert and J.Rothe and S.Rozov and I.Rozova and T.Salagnac and E.Sanchez Garcia and G.Sanchez Garcia and O.Sanders and V.Sanglard and D.Santos and Y.Sarkis and V.Savu and G.Savvidis and I.~Savvidis and N.~Schermer and J.~Schieck and B.~Schmidt and S.~Schonert and K.~Scholberg and A.~Schwenk and C.~Schwertner and L.~Scola and Ye.~Shevchik and S.~Shin and V.~Sibille and I.~M.~Shoemaker and D.~P.~Snowden-Ifft and T.~Soldner and G.~Soum and N.~J.~C.~Spooner and J.~Stachurska and L.~Stodolsky and R.~Strauss and L.~E.~Strigari and A.~Stutz and B.~D.~Suh and J.~Suhonen and Z.~Tabrizi and V.~Takhistov and A.~Thompson and C.~Tomei and M.~Tortola and M.~Tripathi and L.~Vagneron and J.~W.~F.~Valle and K.~v.~Mirbach and W.~Van De Ponteseele and M.~Vignati and M.~Vivier and F.~Vazquez de Sola Fernandez and F.~Vezzu and M.~Vidal and V.~Wagner and J.~W.~Walker and R.~Ward and A.~Wex and L.~Winslow and H.~T.~Wong and M.~H.~Wood and J.~Xu and L.~Yang and E.~Yakushev and M.~Zampaolo and J.~Zettlemoyer and Y.~Y.~Zhang and D.~Zinatulina}, title = {{C}oherent elastic neutrino-nucleus scattering: {T}errestrial and astrophysical applications}, year = {2022}, eprint = {2203.07361}, note = {arXiv:2203.07361v1} }
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Coherent elastic neutrino-nucleus scattering (CE$\nu$NS) is a process in which neutrinos scatter on a nucleus which acts as a single particle. Though the total cross section is large by neutrino standards, CE$\nu$NS has long proven difficult to detect, since the deposited energy into the nucleus is $\sim$ keV. In 2017, the COHERENT collaboration announced the detection of CE$\nu$NS using a stopped-pion source with CsI detectors, followed up the detection of CE$\nu$NS using an Ar target. The detection of CE$\nu$NS has spawned a flurry of activities in high-energy physics, inspiring new constraints on beyond the Standard Model (BSM) physics, and new experimental methods. The CE$\nu$NS process has important implications for not only high-energy physics, but also astrophysics, nuclear physics, and beyond. This whitepaper discusses the scientific importance of CE$\nu$NS, highlighting how present experiments such as COHERENT are informing theory, and also how future experiments will provide a wealth of information across the aforementioned fields of physics.
Snowmass2021 Cosmic Frontier White Paper: Ultraheavy particle dark matter
Daniel Carney, Nirmal Raj, Yang Bai, Joshua Berger, Carlos Blanco, Joseph Bramante, Christopher Cappiello, Maíra Dutra, Reza Ebadi, Kristi Engel, Edward Kolb, J. Patrick Harding, Jason Kumar, Gordan Krnjaic, Rafael F. Lang, Rebecca K. Leane, Benjamin V. Lehmann, Shengchao Li, Andrew J. Long, Gopolang Mohlabeng, et al (8)
Mar 15 2022 hep-ph astro-ph.CO hep-ex arXiv:2203.06508v2

@misc{2203.06508, author = {Daniel Carney and Nirmal Raj and Yang Bai and Joshua Berger and Carlos Blanco and Joseph Bramante and Christopher Cappiello and Maíra Dutra and Reza Ebadi and Kristi Engel and Edward Kolb and J.~Patrick Harding and Jason Kumar and Gordan Krnjaic and Rafael F.~Lang and Rebecca K.~Leane and Benjamin V.~Lehmann and Shengchao Li and Andrew J.~Long and Gopolang Mohlabeng and Ibles Olcina and Elisa Pueschel and Nicholas L.~Rodd and Carsten Rott and Dipan Sengupta and Bibhushan Shakya and Ronald L.~Walsworth and Shawn Westerdale}, title = {{S}nowmass2021 {C}osmic {F}rontier {W}hite {P}aper: {U}ltraheavy particle dark matter}, year = {2022}, eprint = {2203.06508}, note = {arXiv:2203.06508v2} }
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We outline the unique opportunities and challenges in the search for "ultraheavy" dark matter candidates with masses between roughly $10~{\rm TeV}$ and the Planck scale $m_{\rm pl} \approx 10^{16}~{\rm TeV}$. This mass range presents a wide and relatively unexplored dark matter parameter space, with a rich space of possible models and cosmic histories. We emphasize that both current detectors and new, targeted search techniques, via both direct and indirect detection, are poised to contribute to searches for ultraheavy particle dark matter in the coming decade. We highlight the need for new developments in this space, including new analyses of current and imminent direct and indirect experiments targeting ultraheavy dark matter and development of new, ultra-sensitive detector technologies like next-generation liquid noble detectors, neutrino experiments, and specialized quantum sensing techniques.
Models of ultra-heavy dark matter visible to macroscopic mechanical sensing arrays
Carlos Blanco, Bahaa Elshimy, Rafael F. Lang, Robert Orlando
Jan 03 2022 hep-ph hep-ex arXiv:2112.14784v2

@misc{2112.14784, author = {Carlos Blanco and Bahaa Elshimy and Rafael F.~Lang and Robert Orlando}, title = {{M}odels of ultra-heavy dark matter visible to macroscopic mechanical sensing arrays}, year = {2022}, eprint = {2112.14784}, doi = {10.1103/PhysRevD.105.115031}, note = {arXiv:2112.14784v2} }
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In recent years, the sensitivity of opto-mechanical force sensors has improved leading to increased interest in using these devices as particle detectors. In this study we consider scenarios where dark matter with mass close to the Planck scale may be probed by a large array of opto-mechanical accelerometers. We motivate a macroscopic mechanical search for ultra-heavy dark matter, exemplified by the efforts of the Windchime collaboration, by providing a survey of the model space that would be visible to such a search. We consider two classes of models, one that invokes a new long-range unscreened force and another that is only gravitationally interacting. We identify significant regions of well-motivated, potentially visible parameter space for versatile models such as Q-balls, composite dark matter, relics of gravitational singularities, and gravitationally produced ultra-heavy particles.
Observing the Migdal effect from nuclear recoils of neutral particles with liquid xenon and argon detectors
Nicole F. Bell, James B. Dent, Rafael F. Lang, Jayden L. Newstead, Alexander C. Ritter
Dec 17 2021 hep-ph physics.ins-det arXiv:2112.08514v2

@misc{2112.08514, author = {Nicole F.~Bell and James B.~Dent and Rafael F.~Lang and Jayden L.~Newstead and Alexander C.~Ritter}, title = {{O}bserving the {M}igdal effect from nuclear recoils of neutral particles with liquid xenon and argon detectors}, year = {2021}, eprint = {2112.08514}, note = {arXiv:2112.08514v2} }
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In recent years, dark matter direct detection experiments have spurred interest in the Migdal effect, where it is employed to extend their sensitivity to lower dark matter masses. Given the lack of observation of the Migdal effect, the calculation of the signal is subject to large theoretical uncertainties. It is therefore desirable to attempt a first measurement of the Migdal effect, and to test the theoretical predictions of the Migdal effect for the calibration of the experimental response to a potential dark matter signal. In this work, we explore the feasibility of observing the Migdal effect in xenon and argon. We carry out proof-of-concept calculations for low-energy neutrons from a filtered source, and using a reactor, the Spallation Neutron Source, or $^{51}$Cr as potential neutrino sources. We perform a detector simulation for the xenon target and find that, with available technology, the low-energy neutron source is the most promising, requiring only a modest neutron flux, detector size, and exposure period.
Time variation of the atmospheric neutrino flux at dark matter detectors
Yi Zhuang, Louis E. Strigari, Rafael F. Lang
Oct 29 2021 hep-ph astro-ph.HE arXiv:2110.14723v1

@misc{2110.14723, author = {Yi Zhuang and Louis E.~Strigari and Rafael F.~Lang}, title = {{T}ime variation of the atmospheric neutrino flux at dark matter detectors}, year = {2021}, eprint = {2110.14723}, note = {arXiv:2110.14723v1} }
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The cosmic ray flux at the lowest energies, $\lesssim 10$ GeV, is modulated by the solar cycle, inducing a time variation that is expected to carry over into the atmospheric neutrino flux at these energies. Here we estimate this time variation of the atmospheric neutrino flux at five prospective underground locations for multi-tonne scale dark matter detectors (CJPL, Kamioka, LNGS, SNOlab and SURF). We find that between solar minimum and solar maximum, the normalization of the flux changes by $\sim 30\%$ at a high-latitude location such as SURF, while it changes by a smaller amount, $\lesssim 10\%$, at LNGS. A dark matter detector that runs for a period extending through solar cycles will be most effective at identifying this time variation. This opens the possibility to distinguish such neutrino-induced nuclear recoils from dark matter-induced nuclear recoils, thus allowing for the possibility of using timing information to break through the "neutrino floor."
Kiloton-scale xenon detectors for neutrinoless double beta decay and other new physics searches
A. Avasthi, T.W. Bowyer, C. Bray, T. Brunner, N. Catarineu, E. Church, R. Guenette, S.J. Haselschwardt, J.C. Hayes, M. Heffner, S.A. Hertel, P.H. Humble, A. Jamil, S. Kim, R.F. Lang, K.G. Leach, B.G. Lenardo, W.H. Lippincott, A. Marino, D.N. McKinsey, et al (14)
Oct 05 2021 physics.ins-det hep-ex hep-ph nucl-ex arXiv:2110.01537v2

@misc{2110.01537, author = {A.~Avasthi and T.W.~Bowyer and C.~Bray and T.~Brunner and N.~Catarineu and E.~Church and R.~Guenette and S.J.~Haselschwardt and J.C.~Hayes and M.~Heffner and S.A.~Hertel and P.H.~Humble and A.~Jamil and S.~Kim and R.F.~Lang and K.G.~Leach and B.G.~Lenardo and W.H.~Lippincott and A.~Marino and D.N.~McKinsey and E.H.~Miller and D.C.~Moore and B.~Mong and B.~Monreal and M.E.~Monzani and I.~Olcina and J.L.~Orrell and S.~Pang and A.~Pocar and P.C.~Rowson and R.~Saldanha and S.~Sangiorgio and C.~Stanford and A.~Visser}, title = {{K}iloton-scale xenon detectors for neutrinoless double beta decay and other new physics searches}, year = {2021}, eprint = {2110.01537}, howpublished = {Phys. Rev. D 104, 112007 (2021)}, doi = {10.1103/PhysRevD.104.112007}, note = {arXiv:2110.01537v2} }
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Large detectors employing xenon are a leading technology in existing and planned searches for new physics, including searches for neutrinoless double beta decay ($0\nu\beta\beta$) and dark matter. While upcoming detectors will employ target masses of a ton or more, further extending gas or liquid phase Xe detectors to the kton scale would enable extremely sensitive next-generation searches for rare phenomena. The key challenge to extending this technology to detectors well beyond the ton scale is the acquisition of the Xe itself. We describe the motivation for extending Xe time projection chambers (TPCs) to the kton scale and possible avenues for Xe acquisition that avoid existing supply chains. If acquisition of Xe in the required quantities is successful, kton-scale detectors of this type could enable a new generation of experiments, including searches for $0\nu\beta\beta$ at half-life sensitivities as long as $10^{30}$ yr.
Constraints on dark photon dark matter using data from LIGO's and Virgo's third observing run
LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, N. Adhikari, R. X. Adhikari, V. B. Adya, C. Affeldt, D. Agarwal, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, et al (1610)
May 28 2021 astro-ph.CO gr-qc hep-ph arXiv:2105.13085v3

@misc{2105.13085, author = {LIGO Scientific Collaboration and Virgo Collaboration and KAGRA Collaboration and R.~Abbott and T.~D.~Abbott and F.~Acernese and K.~Ackley and C.~Adams and N.~Adhikari and R.~X.~Adhikari and V.~B.~Adya and C.~Affeldt and D.~Agarwal and M.~Agathos and K.~Agatsuma and N.~Aggarwal and O.~D.~Aguiar and L.~Aiello and A.~Ain and P.~Ajith and T.~Akutsu and S.~Albanesi and A.~Allocca and P.~A.~Altin and A.~Amato and C.~Anand and S.~Anand and A.~Ananyeva and S.~B.~Anderson and W.~G.~Anderson and M.~Ando and T.~Andrade and N.~Andres and T.~Andrić and S.~V.~Angelova and S.~Ansoldi and J.~M.~Antelis and S.~Antier and S.~Appert and Koji Arai and Koya Arai and Y.~Arai and S.~Araki and A.~Araya and M.~C.~Araya and J.~S.~Areeda and M.~Arène and N.~Aritomi and N.~Arnaud and S.~M.~Aronson and K.~G.~Arun and H.~Asada and Y.~Asali and G.~Ashton and Y.~Aso and M.~Assiduo and S.~M.~Aston and P.~Astone and F.~Aubin and C.~Austin and S.~Babak and F.~Badaracco and M.~K.~M.~Bader and C.~Badger and S.~Bae and Y.~Bae and A.~M.~Baer and S.~Bagnasco and Y.~Bai and L.~Baiotti and J.~Baird and R.~Bajpai and M.~Ball and G.~Ballardin and S.~W.~Ballmer and A.~Balsamo and G.~Baltus and S.~Banagiri and D.~Bankar and J.~C.~Barayoga and C.~Barbieri and B.~C.~Barish and D.~Barker and P.~Barneo and F.~Barone and B.~Barr and L.~Barsotti and M.~Barsuglia and D.~Barta and J.~Bartlett and M.~A.~Barton and I.~Bartos and R.~Bassiri and A.~Basti and M.~Bawaj and J.~C.~Bayley and A.~C.~Baylor and M.~Bazzan and B.~Bécsy and V.~M.~Bedakihale and M.~Bejger and I.~Belahcene and V.~Benedetto and D.~Beniwal and T.~F.~Bennett and J.~D.~Bentley and M.~BenYaala and F.~Bergamin and B.~K.~Berger and S.~Bernuzzi and D.~Bersanetti and A.~Bertolini and J.~Betzwieser and D.~Beveridge and R.~Bhandare and U.~Bhardwaj and D.~Bhattacharjee and S.~Bhaumik and I.~A.~Bilenko and G.~Billingsley and S.~Bini and R.~Birney and O.~Birnholtz and S.~Biscans and M.~Bischi and S.~Biscoveanu and A.~Bisht and B.~Biswas 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M.~Korobko and K.~Kotake and M.~Kovalam and D.~B.~Kozak and C.~Kozakai and R.~Kozu and V.~Kringel and N.~V.~Krishnendu and A.~Królak and G.~Kuehn and F.~Kuei and P.~Kuijer and A.~Kumar and P.~Kumar and Rahul Kumar and Rakesh Kumar and J.~Kume and K.~Kuns and C.~Kuo and H-S.~Kuo and Y.~Kuromiya and S.~Kuroyanagi and K.~Kusayanagi and S.~Kuwahara and K.~Kwak and P.~Lagabbe and D.~Laghi and E.~Lalande and T.~L.~Lam and A.~Lamberts and M.~Landry and B.~B.~Lane and R.~N.~Lang and J.~Lange and B.~Lantz and I.~La Rosa and A.~Lartaux-Vollard and P.~D.~Lasky and M.~Laxen and A.~Lazzarini and C.~Lazzaro and P.~Leaci and S.~Leavey and Y.~K.~Lecoeuche and H.~K.~Lee and H.~M.~Lee and H.~W.~Lee and J.~Lee and K.~Lee and R.~Lee and J.~Lehmann and A.~Lemaître and M.~Leonardi and N.~Leroy and N.~Letendre and C.~Levesque and Y.~Levin and J.~N.~Leviton and K.~Leyde and A.~K.~Y.~Li and B.~Li and J.~Li and K.~L.~Li and T.~G.~F.~Li and X.~Li and C-Y.~Lin and F-K.~Lin and F-L.~Lin and H.~L.~Lin and L.~C.-C.~Lin and F.~Linde and S.~D.~Linker and J.~N.~Linley and T.~B.~Littenberg and G.~C.~Liu and J.~Liu and K.~Liu and X.~Liu and F.~Llamas and M.~Llorens-Monteagudo and R.~K.~L.~Lo and A.~Lockwood and L.~T.~London and A.~Longo and D.~Lopez and M.~Lopez Portilla and M.~Lorenzini and V.~Loriette and M.~Lormand and G.~Losurdo and T.~P.~Lott and J.~D.~Lough and C.~O.~Lousto and G.~Lovelace and J.~F.~Lucaccioni and H.~Lück and D.~Lumaca and A.~P.~Lundgren and L.-W.~Luo and J.~E.~Lynam and R.~Macas and M.~MacInnis and D.~M.~Macleod and I.~A.~O.~MacMillan and A.~Macquet and I.~Magaña Hernandez and C.~Magazzù and R.~M.~Magee and R.~Maggiore and M.~Magnozzi and S.~Mahesh and E.~Majorana and C.~Makarem and I.~Maksimovic and S.~Maliakal and A.~Malik and N.~Man and V.~Mandic and V.~Mangano and J.~L.~Mango and G.~L.~Mansell and M.~Manske and M.~Mantovani and M.~Mapelli and F.~Marchesoni and M.~Marchio and F.~Marion and Z.~Mark and S.~Márka and Z.~Márka and C.~Markakis and A.~S.~Markosyan and A.~Markowitz and E.~Maros and A.~Marquina and S.~Marsat and F.~Martelli and I.~W.~Martin and R.~M.~Martin and M.~Martinez and V.~A.~Martinez and V.~Martinez and K.~Martinovic and D.~V.~Martynov and E.~J.~Marx and H.~Masalehdan and K.~Mason and E.~Massera and A.~Masserot and T.~J.~Massinger and M.~Masso-Reid and S.~Mastrogiovanni and A.~Matas and M.~Mateu-Lucena and F.~Matichard and M.~Matiushechkina and N.~Mavalvala and J.~J.~McCann and R.~McCarthy and D.~E.~McClelland and P.~K.~McClincy and S.~McCormick and L.~McCuller and G.~I.~McGhee and S.~C.~McGuire and C.~McIsaac and J.~McIver and T.~McRae and S.~T.~McWilliams and D.~Meacher and M.~Mehmet and A.~K.~Mehta and Q.~Meijer and A.~Melatos and D.~A.~Melchor and G.~Mendell and A.~Menendez-Vazquez and C.~S.~Menoni and R.~A.~Mercer and L.~Mereni and K.~Merfeld and E.~L.~Merilh and J.~D.~Merritt and M.~Merzougui and S.~Meshkov and C.~Messenger and C.~Messick and P.~M.~Meyers and F.~Meylahn and A.~Mhaske and A.~Miani and H.~Miao and I.~Michaloliakos and C.~Michel and Y.~Michimura and H.~Middleton and L.~Milano and A.~L.~Miller and A.~Miller and B.~Miller and M.~Millhouse and J.~C.~Mills and E.~Milotti and O.~Minazzoli and Y.~Minenkov and N.~Mio and Ll.~M.~Mir and M.~Miravet-Tenés and C.~Mishra and T.~Mishra and T.~Mistry and S.~Mitra and V.~P.~Mitrofanov and G.~Mitselmakher and R.~Mittleman and O.~Miyakawa and A.~Miyamoto and Y.~Miyazaki and K.~Miyo and S.~Miyoki and Geoffrey Mo and E.~Moguel and K.~Mogushi and S.~R.~P.~Mohapatra and S.~R.~Mohite and I.~Molina and M.~Molina-Ruiz and M.~Mondin and M.~Montani and C.~J.~Moore and D.~Moraru and F.~Morawski and A.~More and C.~Moreno and G.~Moreno and Y.~Mori and S.~Morisaki and Y.~Moriwaki and B.~Mours and C.~M.~Mow-Lowry and S.~Mozzon and F.~Muciaccia and Arunava Mukherjee and D.~Mukherjee and Soma Mukherjee and Subroto Mukherjee and Suvodip Mukherjee and N.~Mukund and A.~Mullavey and J.~Munch and E.~A.~Muñiz and P.~G.~Murray and R.~Musenich and S.~Muusse and S.~L.~Nadji and K.~Nagano and S.~Nagano and A.~Nagar and K.~Nakamura and H.~Nakano and M.~Nakano and R.~Nakashima and Y.~Nakayama and V.~Napolano and I.~Nardecchia and T.~Narikawa and L.~Naticchioni and B.~Nayak and R.~K.~Nayak and R.~Negishi and B.~F.~Neil and J.~Neilson and G.~Nelemans and T.~J.~N.~Nelson and M.~Nery and P.~Neubauer and A.~Neunzert and K.~Y.~Ng and S.~W.~S.~Ng and C.~Nguyen and P.~Nguyen and T.~Nguyen and L.~Nguyen Quynh and W.-T.~Ni and S.~A.~Nichols and A.~Nishizawa and S.~Nissanke and E.~Nitoglia and F.~Nocera and M.~Norman and C.~North and S.~Nozaki and L.~K.~Nuttall and J.~Oberling and B.~D.~O'Brien and Y.~Obuchi and J.~O'Dell and E.~Oelker and W.~Ogaki and G.~Oganesyan and J.~J.~Oh and K.~Oh and S.~H.~Oh and M.~Ohashi and N.~Ohishi and M.~Ohkawa and F.~Ohme and H.~Ohta and M.~A.~Okada and Y.~Okutani and K.~Okutomi and C.~Olivetto and K.~Oohara and C.~Ooi and R.~Oram and B.~O'Reilly and R.~G.~Ormiston and N.~D.~Ormsby and L.~F.~Ortega and R.~O'Shaughnessy and 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H.~Takeda and M.~Takeda and C.~J.~Talbot and C.~Talbot and H.~Tanaka and Kazuyuki Tanaka and Kenta Tanaka and Taiki Tanaka and Takahiro Tanaka and A.~J.~Tanasijczuk and S.~Tanioka and D.~B.~Tanner and D.~Tao and L.~Tao and E.~N.~Tapia San Martin and E.~N.~Tapia San Martín and C.~Taranto and J.~D.~Tasson and S.~Telada and R.~Tenorio and J.~E.~Terhune and L.~Terkowski and M.~P.~Thirugnanasambandam and M.~Thomas and P.~Thomas and J.~E.~Thompson and S.~R.~Thondapu and K.~A.~Thorne and E.~Thrane and Shubhanshu Tiwari and Srishti Tiwari and V.~Tiwari and A.~M.~Toivonen and K.~Toland and A.~E.~Tolley and T.~Tomaru and Y.~Tomigami and T.~Tomura and M.~Tonelli and A.~Torres-Forné and C.~I.~Torrie and I.~Tosta e Melo and D.~Töyrä and A.~Trapananti and F.~Travasso and G.~Traylor and M.~Trevor and M.~C.~Tringali and A.~Tripathee and L.~Troiano and A.~Trovato and L.~Trozzo and R.~J.~Trudeau and D.~S.~Tsai and D.~Tsai and K.~W.~Tsang and T.~Tsang and J-S.~Tsao and M.~Tse and R.~Tso and K.~Tsubono and S.~Tsuchida and L.~Tsukada and D.~Tsuna and T.~Tsutsui and T.~Tsuzuki and K.~Turbang and M.~Turconi and D.~Tuyenbayev and A.~S.~Ubhi and N.~Uchikata and T.~Uchiyama and R.~P.~Udall and A.~Ueda and T.~Uehara and K.~Ueno and G.~Ueshima and F.~Uraguchi and A.~L.~Urban and T.~Ushiba and A.~Utina and H.~Vahlbruch and G.~Vajente and A.~Vajpeyi and G.~Valdes and M.~Valentini and V.~Valsan and N.~van Bakel and M.~van Beuzekom and J.~F.~J.~van den Brand and C.~Van Den Broeck and D.~C.~Vander-Hyde and L.~van der Schaaf and J.~V.~van Heijningen and J.~Vanosky and M.~H.~P.~M.~van Putten and N.~van Remortel and M.~Vardaro and A.~F.~Vargas and V.~Varma and M.~Vasúth and A.~Vecchio and G.~Vedovato and J.~Veitch and P.~J.~Veitch and J.~Venneberg and G.~Venugopalan and D.~Verkindt and P.~Verma and Y.~Verma and D.~Veske and F.~Vetrano and A.~Viceré and S.~Vidyant and A.~D.~Viets and A.~Vijaykumar and V.~Villa-Ortega and J.-Y.~Vinet and A.~Virtuoso and S.~Vitale and T.~Vo and H.~Vocca and E.~R.~G.~von Reis and J.~S.~A.~von Wrangel and C.~Vorvick and S.~P.~Vyatchanin and L.~E.~Wade and M.~Wade and K.~J.~Wagner and R.~C.~Walet and M.~Walker and G.~S.~Wallace and L.~Wallace and S.~Walsh and J.~Wang and J.~Z.~Wang and W.~H.~Wang and R.~L.~Ward and J.~Warner and M.~Was and T.~Washimi and N.~Y.~Washington and J.~Watchi and B.~Weaver and S.~A.~Webster and M.~Weinert and A.~J.~Weinstein and R.~Weiss and C.~M.~Weller and F.~Wellmann and L.~Wen and P.~Weßels and K.~Wette and J.~T.~Whelan and D.~D.~White and B.~F.~Whiting and C.~Whittle and D.~Wilken and D.~Williams and M.~J.~Williams and A.~R.~Williamson and J.~L.~Willis and B.~Willke and D.~J.~Wilson and W.~Winkler and C.~C.~Wipf and T.~Wlodarczyk and G.~Woan and J.~Woehler and J.~K.~Wofford and I.~C.~F.~Wong and C.~Wu and D.~S.~Wu and H.~Wu and S.~Wu and D.~M.~Wysocki and L.~Xiao and W-R.~Xu and T.~Yamada and H.~Yamamoto and Kazuhiro Yamamoto and Kohei Yamamoto and T.~Yamamoto and K.~Yamashita and R.~Yamazaki and F.~W.~Yang and L.~Yang and Y.~Yang and Yang Yang and Z.~Yang and M.~J.~Yap and D.~W.~Yeeles and A.~B.~Yelikar and M.~Ying and K.~Yokogawa and J.~Yokoyama and T.~Yokozawa and J.~Yoo and T.~Yoshioka and Hang Yu and Haocun Yu and H.~Yuzurihara and A.~Zadrożny and M.~Zanolin and S.~Zeidler and T.~Zelenova and J.-P.~Zendri and M.~Zevin and M.~Zhan and H.~Zhang and J.~Zhang and L.~Zhang and T.~Zhang and Y.~Zhang and C.~Zhao and G.~Zhao and Y.~Zhao and Yue Zhao and R.~Zhou and Z.~Zhou and X.~J.~Zhu and Z.-H.~Zhu and M.~E.~Zucker and J.~Zweizig}, title = {{C}onstraints on dark photon dark matter using data from {LIGO}'s and {V}irgo's third observing run}, year = {2021}, eprint = {2105.13085}, howpublished = {Phys. Rev. D 105, 063030, 2022}, doi = {10.1103/PhysRevD.105.063030}, note = {arXiv:2105.13085v3} }
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We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo's third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier Transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between $m_{\rm A} \sim 10^{-14}-10^{-11}$ eV/$c^2$, which corresponds to frequencies between 10-2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e. $U(1)_{\rm B}$ dark matter. For the cross-correlation method, the best median constraint on the squared coupling is $\sim2.65\times10^{-46}$ at $m_{\rm A}\sim4.31\times10^{-13}$ eV/$c^2$; for the other analysis, the best constraint is $\sim 2.4\times 10^{-47}$ at $m_{\rm A}\sim 5.7\times 10^{-13}$ eV/$c^2$. These limits improve upon those obtained in direct dark matter detection experiments by a factor of $\sim100$ for $m_{\rm A}\sim [2-4]\times 10^{-13}$ eV/$c^2$, and are, in absolute terms, the most stringent constraint so far in a large mass range $m_A\sim$ $2\times 10^{-13}-8\times 10^{-12}$ eV/$c^2$.
Recommended conventions for reporting results from direct dark matter searches
D. Baxter, I. M. Bloch, E. Bodnia, X. Chen, J. Conrad, P. Di Gangi, J. E. Y. Dobson, D. Durnford, S. J. Haselschwardt, A. Kaboth, R. F. Lang, Q. Lin, W. H. Lippincott, J. Liu, A. Manalaysay, C. McCabe, K. D. Mora, D. Naim, R. Neilson, I. Olcina, et al (6)
May 04 2021 hep-ex hep-ph arXiv:2105.00599v2

@misc{2105.00599, author = {D.~Baxter and I.~M.~Bloch and E.~Bodnia and X.~Chen and J.~Conrad and P.~Di Gangi and J.~E.~Y.~Dobson and D.~Durnford and S.~J.~Haselschwardt and A.~Kaboth and R.~F.~Lang and Q.~Lin and W.~H.~Lippincott and J.~Liu and A.~Manalaysay and C.~McCabe and K.~D.~Mora and D.~Naim and R.~Neilson and I.~Olcina and M.-C.~Piro and M.~Selvi and B.~von Krosigk and S.~Westerdale and Y.~Yang and N.~Zhou}, title = {{R}ecommended conventions for reporting results from direct dark matter searches}, year = {2021}, eprint = {2105.00599}, howpublished = {European Physical Journal C, 81, 907 (2021)}, doi = {10.1140/epjc/s10052-021-09655-y}, note = {arXiv:2105.00599v2} }
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The field of dark matter detection is a highly visible and highly competitive one. In this paper, we propose recommendations for presenting dark matter direct detection results particularly suited for weak-scale dark matter searches, although we believe the spirit of the recommendations can apply more broadly to searches for other dark matter candidates, such as very light dark matter or axions. To translate experimental data into a final published result, direct detection collaborations must make a series of choices in their analysis, ranging from how to model astrophysical parameters to how to make statistical inferences based on observed data. While many collaborations follow a standard set of recommendations in some areas, for example the expected flux of dark matter particles (to a large degree based on a paper from Lewin and Smith in 1995), in other areas, particularly in statistical inference, they have taken different approaches, often from result to result by the same collaboration. We set out a number of recommendations on how to apply the now commonly used Profile Likelihood Ratio method to direct detection data. In addition, updated recommendations for the Standard Halo Model astrophysical parameters and relevant neutrino fluxes are provided. The authors of this note include members of the DAMIC, DarkSide, DARWIN, DEAP, LZ, NEWS-G, PandaX, PICO, SBC, SENSEI, SuperCDMS, and XENON collaborations, and these collaborations provided input to the recommendations laid out here. Wide-spread adoption of these recommendations will make it easier to compare and combine future dark matter results.
Direct Detection Limits on Heavy Dark Matter
Michael Clark, Amanda Depoian, Bahaa Elshimy, Abigail Kopec, Rafael F. Lang, Shengchao Li, Juehang Qin
Sep 18 2020 hep-ph hep-ex arXiv:2009.07909v3

@misc{2009.07909, author = {Michael Clark and Amanda Depoian and Bahaa Elshimy and Abigail Kopec and Rafael F.~Lang and Shengchao Li and Juehang Qin}, title = {{D}irect {D}etection {L}imits on {H}eavy {D}ark {M}atter}, year = {2020}, eprint = {2009.07909}, howpublished = {Phys. Rev. D 102, 123026 (2020), including erratum Phys. Rev. D 104, 129903}, doi = {10.1103/PhysRevD.102.123026}, note = {arXiv:2009.07909v3} }
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Multiply-interacting massive particles (MIMPs) are heavy (>10^10 GeV/c^2) dark matter particles that interact strongly with regular matter, but may have evaded detection due to the low number density required to make up the local dark matter halo. These particles could leave track-like signatures in current experiments, similar to lightly-ionizing particles. We show that previously calculated limits from the MAJORANA Demonstrator on the flux of lightly-ionizing particles can be used to exclude MIMP dark matter parameter space up to a mass of 10^15 GeV/c^2. We also calculate limits from the standard XENON1T analysis in this high-mass regime, properly taking into account flux limitations and multi-scatter effects. Finally, we show that a dedicated MIMP analysis using the XENON1T dark matter search could probe unexplored parameter space up to masses of 10^18 GeV/c^2.
Mechanical Quantum Sensing in the Search for Dark Matter
Daniel Carney, Gordan Krnjaic, David C. Moore, Cindy A. Regal, Gadi Afek, Sunil Bhave, Benjamin Brubaker, Thomas Corbitt, Jonathan Cripe, Nicole Crisosto, Andrew Geraci, Sohitri Ghosh, Jack G. E. Harris, Anson Hook, Edward W. Kolb, Jonathan Kunjummen, Rafael F. Lang, Tongcang Li, Tongyan Lin, Zhen Liu, et al (15)
Aug 17 2020 physics.ins-det astro-ph.CO hep-ex hep-ph quant-ph arXiv:2008.06074v1

@misc{2008.06074, author = {Daniel Carney and Gordan Krnjaic and David C.~Moore and Cindy A.~Regal and Gadi Afek and Sunil Bhave and Benjamin Brubaker and Thomas Corbitt and Jonathan Cripe and Nicole Crisosto and Andrew Geraci and Sohitri Ghosh and Jack G.~E.~Harris and Anson Hook and Edward W.~Kolb and Jonathan Kunjummen and Rafael F.~Lang and Tongcang Li and Tongyan Lin and Zhen Liu and Joseph Lykken and Lorenzo Magrini and Jack Manley and Nobuyuki Matsumoto and Alissa Monte and Fernando Monteiro and Thomas Purdy and C.~Jess Riedel and Robinjeet Singh and Swati Singh and Kanupriya Sinha and Jacob M.~Taylor and Juehang Qin and Dalziel J.~Wilson and Yue Zhao}, title = {{M}echanical {Q}uantum {S}ensing in the {S}earch for {D}ark {M}atter}, year = {2020}, eprint = {2008.06074}, note = {arXiv:2008.06074v1} }
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Numerous astrophysical and cosmological observations are best explained by the existence of dark matter, a mass density which interacts only very weakly with visible, baryonic matter. Searching for the extremely weak signals produced by this dark matter strongly motivate the development of new, ultra-sensitive detector technologies. Paradigmatic advances in the control and readout of massive mechanical systems, in both the classical and quantum regimes, have enabled unprecedented levels of sensitivity. In this white paper, we outline recent ideas in the potential use of a range of solid-state mechanical sensing technologies to aid in the search for dark matter in a number of energy scales and with a variety of coupling mechanisms.
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.
Atmospheric neutrinos in a next-generation xenon dark matter experiment
Jayden L. Newstead, Rafael F. Lang, Louis E. Strigari
Feb 21 2020 astro-ph.CO hep-ex hep-ph arXiv:2002.08566v1

@misc{2002.08566, author = {Jayden L.~Newstead and Rafael F.~Lang and Louis E.~Strigari}, title = {{A}tmospheric neutrinos in a next-generation xenon dark matter experiment}, year = {2020}, eprint = {2002.08566}, note = {arXiv:2002.08566v1} }
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We study the sensitivity of future xenon- and argon-based dark matter and neutrino detection experiments to low-energy atmospheric neutrinos. Not accounting for experimental backgrounds, the primary obstacle for identifying nuclear recoils induced by atmospheric neutrinos is the tail of the electron recoil distribution due to $pp$ solar neutrinos. We use the NEST code to model the solar and atmospheric neutrino signals in a xenon detector and find that an exposure of 700 tonne-years will produce a $5\sigma$ detection of atmospheric neutrinos. We explore the effect of different detector properties and find that a sufficiently long electron lifetime is essential to the success of such a measurement.
A global analysis strategy to resolve neutrino NSI degeneracies with scattering and oscillation data
Bhaskar Dutta, Rafael F. Lang, Shu Liao, Samiran Sinha, Louis Strigari, Adrian Thompson
Feb 11 2020 hep-ph arXiv:2002.03066v2

@misc{2002.03066, author = {Bhaskar Dutta and Rafael F.~Lang and Shu Liao and Samiran Sinha and Louis Strigari and Adrian Thompson}, title = {{A} global analysis strategy to resolve neutrino {NSI} degeneracies with scattering and oscillation data}, year = {2020}, eprint = {2002.03066}, howpublished = {J. High Energ. Phys. 2020, 106 (2020)}, doi = {10.1007/JHEP09(2020)106}, note = {arXiv:2002.03066v2} }
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Neutrino non-standard interactions (NSI) with the first generation of standard model fermions can span a parameter space of large dimension and exhibit degeneracies that cannot be broken by a single class of experiment. Oscillation experiments, together with neutrino scattering experiments, can merge their observations into a highly informational dataset to combat this problem. We consider combining neutrino-electron and neutrino-nucleus scattering data from the Borexino and COHERENT experiments, including a projection for the upcoming coherent neutrino scattering measurement at the CENNS-10 liquid argon detector. We extend the reach of these data sets over the NSI parameter space with projections for neutrino scattering at a future multi-ton scale dark matter detector and future oscillation measurements from atmospheric neutrinos at the Deep Underground Neutrino Experiment (DUNE). In order to perform this global analysis, we adopt a novel approach using the copula method, utilized to combine posterior information from different experiments with a large, generalized set of NSI parameters. We find that the contributions from DUNE and a dark matter detector to the Borexino and COHERENT fits can improve constraints on the electron and quark NSI parameters by up to a factor of 2 to 3, even when relatively many NSI parameters are left free to vary in the analysis.
Proceedings of The Magnificent CE$\nu$NS Workshop 2018
D. Aristizabal Sierra, A.B. Balantekin, D. Caratelli, B. Cogswell, J.I. Collar, C.E. Dahl, J. Dent, B. Dutta, J. Engel, J. Estrada, J. Formaggio, S. Gariazzo, R. Han, S. Hedges, P. Huber, A. Konovalov, R.F. Lang, S. Liao, M. Lindner, P. Machado, et al (25)
Oct 17 2019 hep-ex astro-ph.IM hep-ph nucl-ex physics.ins-det arXiv:1910.07450v1

@misc{1910.07450, author = {D.~Aristizabal Sierra and A.B.~Balantekin and D.~Caratelli and B.~Cogswell and J.I.~Collar and C.E.~Dahl and J.~Dent and B.~Dutta and J.~Engel and J.~Estrada and J.~Formaggio and S.~Gariazzo and R.~Han and S.~Hedges and P.~Huber and A.~Konovalov and R.F.~Lang and S.~Liao and M.~Lindner and P.~Machado and R.~Mahapatra and D.~Marfatia and I.~Martinez-Soler and O.~Miranda and D.~Misiak and D.V.~Naumov and J.~Newby and J.~Newstead and D.~Papoulias and K.~Patton and S.~Pereverzev and M.~Pospelov and K.~Scholberg and G.~Sinev and R.~Strauss and L.~Strigari and R.~Tayloe and J.~Tiffenberg and M.~Vidal and M.~Vignati and V.~Wagner and J.~Walker and T.-T.~Yu and J.~Zettlemoyer and G.C.~Rich}, title = {{P}roceedings of {T}he {M}agnificent {CE}$\nu${NS} {W}orkshop 2018}, year = {2019}, eprint = {1910.07450}, doi = {10.5281/zenodo.3489190}, note = {arXiv:1910.07450v1} }
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The Magnificent CE$\nu$NS Workshop (2018) was held November 2 & 3 of 2018 on the University of Chicago campus and brought together theorists, phenomenologists, and experimentalists working in numerous areas but sharing a common interest in the process of coherent elastic neutrino-nucleus scattering (CE$\nu$NS). This is a collection of abstract-like summaries of the talks given at the meeting, including links to the slides presented. This document and the slides from the meeting provide an overview of the field and a snapshot of the robust CE$\nu$NS-related efforts both planned and underway.
Constraining the Spin-Dependent WIMP-Nucleon Cross Sections with XENON1T
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 (110)
Feb 11 2019 astro-ph.CO hep-ph arXiv:1902.03234v2

@misc{1902.03234, 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 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 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 D.~Wenz and C.~Wittweg and J.~Wulf and Z.~Xu and J.~Ye and Y.~Zhang and T.~Zhu and J.~P.~Zopounidis}, title = {{C}onstraining the {S}pin-{D}ependent {WIMP}-{N}ucleon {C}ross {S}ections with {XENON}1{T}}, year = {2019}, eprint = {1902.03234}, howpublished = {Phys. Rev. Lett. 122, 141301 (2019)}, doi = {10.1103/PhysRevLett.122.141301}, note = {arXiv:1902.03234v2} }
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We report the first experimental results on spin-dependent elastic weakly interacting massive particle (WIMP) nucleon scattering from the XENON1T dark matter search experiment. The analysis uses the full ton year exposure of XENON1T to constrain the spin-dependent proton-only and neutron-only cases. No significant signal excess is observed, and a profile likelihood ratio analysis is used to set exclusion limits on the WIMP-nucleon interactions. This includes the most stringent constraint to date on the WIMP-neutron cross section, with a minimum of $6.3\times10^{-42}$ cm$^2$ at 30 GeV/c${}^2$ and 90% confidence level. The results are compared with those from collider searches and used to exclude new parameter space in an isoscalar theory with an axial-vector mediator.
Foraging for dark matter in large volume liquid scintillator neutrino detectors with multiscatter events
Joseph Bramante, Benjamin Broerman, Jason Kumar, Rafael F. Lang, Maxim Pospelov, Nirmal Raj
Dec 27 2018 hep-ph astro-ph.HE hep-ex arXiv:1812.09325v2

@misc{1812.09325, author = {Joseph Bramante and Benjamin Broerman and Jason Kumar and Rafael F.~Lang and Maxim Pospelov and Nirmal Raj}, title = {{F}oraging for dark matter in large volume liquid scintillator neutrino detectors with multiscatter events}, year = {2018}, eprint = {1812.09325}, note = {arXiv:1812.09325v2} }
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We show that dark matter with a per-nucleon scattering cross section $\gtrsim 10^{-28}~{\rm cm^2}$ could be discovered by liquid scintillator neutrino detectors like BOREXINO, SNO+, and JUNO. Due to the large dark matter fluxes admitted, these detectors could find dark matter with masses up to $10^{21}$ GeV, surpassing the mass sensitivity of current direct detection experiments (such as XENON1T and PICO) by over two orders of magnitude. We derive the spin-independent and spin-dependent cross section sensitivity of these detectors using existing selection triggers, and propose an improved trigger program that enhances this sensitivity by two orders of magnitude. We interpret these sensitivities in terms of three dark matter scenarios: (1) effective contact operators for scattering, (2) QCD-charged dark matter, and (3) a recently proposed model of Planck-mass baryon-charged dark matter. We calculate the flux attenuation of dark matter at these detectors due to the earth overburden, taking into account the earth's density profile and elemental composition, and nuclear spins.
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.
CNO Solar Neutrinos in Next-Generation Dark Matter Experiments
Jayden L. Newstead, Louis E. Strigari, Rafael F. Lang
Jul 20 2018 astro-ph.SR hep-ph physics.ins-det arXiv:1807.07169v2

@misc{1807.07169, author = {Jayden L.~Newstead and Louis E.~Strigari and Rafael F.~Lang}, title = {{CNO} {S}olar {N}eutrinos in {N}ext-{G}eneration {D}ark {M}atter {E}xperiments}, year = {2018}, eprint = {1807.07169}, doi = {10.1103/PhysRevD.99.043006}, note = {arXiv:1807.07169v2} }
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We study the prospects for measuring the low-energy components of the solar neutrino flux in future direct dark matter detection experiments. We show that for a depletion of $^{136}$Xe by a factor of 100 relative to its natural abundance, and an extension to electron recoil energies of $\sim$ MeV, future xenon experiments with exposure $\sim 200$ ton-yr can detect the CNO component of the solar neutrino flux at $\sim 3 \sigma$ significance. A CNO detection will provide important insight into metallicity of the solar interior. Precise measurement of low-energy solar neutrinos, including as $pp$, $^7$Be, and $pep$ components, will further improve constraints on the "neutrino luminosity" of the Sun, thereby providing constraints on alternative sources of energy production. We find that a measurement of $L_{\nu}/L_{\odot}$ of order one percent is possible with the above exposure, improving on current bounds from a global analysis of solar neutrino data by a factor of about seven.
Dark Matter Search Results from a One Tonne$\times$Year Exposure of XENON1T
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, M. Anthony, 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, C. Capelli, et al (100)
Jun 01 2018 astro-ph.CO astro-ph.IM hep-ex hep-ph physics.ins-det arXiv:1805.12562v2

@misc{1805.12562, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and M.~Anthony 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 C.~Geis and L.~Grandi and Z.~Greene and H.~Qiu and C.~Hasterok and E.~Hogenbirk and J.~Howlett and R.~Itay and F.~Joerg and B.~Kaminsky and S.~Kazama and A.~Kish and G.~Koltman 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 J.~Mahlstedt and A.~Manfredini and T.~Marrodán Undagoitia and J.~Masbou and D.~Masson 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 B.~Pelssers and F.~Piastra and J.~Pienaar and V.~Pizzella and G.~Plante and R.~Podviianiuk and N.~Priel and D.~Ramírez García and L.~Rauch and S.~Reichard and C.~Reuter and B.~Riedel and A.~Rizzo and A.~Rocchetti and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli 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 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}, title = {{D}ark {M}atter {S}earch {R}esults from a {O}ne {T}onne$\times${Y}ear {E}xposure of {XENON}1{T}}, year = {2018}, eprint = {1805.12562}, howpublished = {Phys. Rev. Lett. 121, 111302 (2018)}, doi = {10.1103/PhysRevLett.121.111302}, note = {arXiv:1805.12562v2} }
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We report on a search for Weakly Interacting Massive Particles (WIMPs) using 278.8 days of data collected with the XENON1T experiment at LNGS. XENON1T utilizes a liquid xenon time projection chamber with a fiducial mass of $(1.30 \pm 0.01)$ t, resulting in a 1.0 t$\times$yr exposure. The energy region of interest, [1.4, 10.6] $\mathrm{keV_{ee}}$ ([4.9, 40.9] $\mathrm{keV_{nr}}$), exhibits an ultra-low electron recoil background rate of $(82\substack{+5 \\ -3}\textrm{ (sys)}\pm3\textrm{ (stat)})$ events/$(\mathrm{t}\times\mathrm{yr}\times\mathrm{keV_{ee}})$. No significant excess over background is found and a profile likelihood analysis parameterized in spatial and energy dimensions excludes new parameter space for the WIMP-nucleon spin-independent elastic scatter cross-section for WIMP masses above 6 GeV/c${}^2$, with a minimum of $4.1\times10^{-47}$ cm$^2$ at 30 GeV/c${}^2$ and 90% confidence level.
Saturated Overburden Scattering and the Multiscatter Frontier: Discovering Dark Matter at the Planck Mass and Beyond
Joseph Bramante, Benjamin Broerman, Rafael F. Lang, Nirmal Raj
Mar 23 2018 hep-ph hep-ex arXiv:1803.08044v1

@misc{1803.08044, author = {Joseph Bramante and Benjamin Broerman and Rafael F.~Lang and Nirmal Raj}, title = {{S}aturated {O}verburden {S}cattering and the {M}ultiscatter {F}rontier: {D}iscovering {D}ark {M}atter at the {P}lanck {M}ass and {B}eyond}, year = {2018}, eprint = {1803.08044}, note = {arXiv:1803.08044v1} }
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We show that underground experiments like LUX/LZ, PandaX-II, XENON, and PICO could discover dark matter up to the Planck mass and beyond, with new searches for dark matter that scatters multiple times in these detectors. This opens up significant discovery potential via re-analysis of existing and future data. We also identify a new effect which substantially enhances experimental sensitivity to large dark matter scattering cross-sections: while passing through atmospheric or solid overburden, there is a maximum number of scatters that dark matter undergoes, determined by the total number of scattering sites it passes, such as nuclei and electrons. This extends the reach of some published limits and future analyses to arbitrarily large dark matter scattering cross-sections.
Search for Bosonic Super-WIMP Interactions with the XENON100 Experiment
XENON collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, L. Althueser, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, A. Brown, E. Brown, S. Bruenner, G. Bruno, et al (102)
Sep 08 2017 astro-ph.CO hep-ex hep-ph arXiv:1709.02222v1

@misc{1709.02222, author = {XENON collaboration and E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and L.~Althueser and F.~D.~Amaro and M.~Anthony and F.~Arneodo and P.~Barrow 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 Bütikofer and J.~Calven 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 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 C.~Geis and L.~W.~Goetzke and Z.~Greene and C.~Grignon and C.~Hasterok and E.~Hogenbirk and J.~Howlett and R.~Itay and B.~Kaminsky and S.~Kazama and G.~Kessler and A.~Kish and H.~Landsman and R.~F.~Lang and D.~Lellouch and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and A.~Manfredini and I.~Maris and T.~Marrodán Undagoitia and J.~Masbou and F.~V.~Massoli and D.~Masson and D.~Mayani and M.~Messina and K.~Micheneau and A.~Molinario and K.~Morå and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and P.~Pakarha and B.~Pelssers and R.~Persiani and F.~Piastra and J.~Pienaar and V.~Pizzella and M.-C.~Piro and G.~Plante and N.~Priel and D.~Ramírez García and L.~Rauch and S.~Reichard and C.~Reuter and A.~Rizzo and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and M.~Scheibelhut and S.~Schindler and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and M.~Silva and H.~Simgen and M.~v.~Sivers and A.~Stein and D.~Thers and A.~Tiseni and G.~Trinchero and C.~Tunnell and M.~Vargas 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}, title = {{S}earch for {B}osonic {S}uper-{WIMP} {I}nteractions with the {XENON}100 {E}xperiment}, year = {2017}, eprint = {1709.02222}, note = {arXiv:1709.02222v1} }
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We present results of searches for vector and pseudo-scalar bosonic super-WIMPs, which are dark matter candidates with masses at the keV-scale, with the XENON100 experiment. XENON100 is a dual-phase xenon time projection chamber operated at the Laboratori Nazionali del Gran Sasso. A profile likelihood analysis of data with an exposure of 224.6 live days $\times$ 34\u2009kg showed no evidence for a signal above the expected background. We thus obtain new and stringent upper limits in the $(8-125)$\u2009keV/c$^2$ mass range, excluding couplings to electrons with coupling constants of $g_{ae} > 3\times10^{-13}$ for pseudo-scalar and $\alpha'/\alpha > 2\times10^{-28}$ for vector super-WIMPs, respectively. These limits are derived under the assumption that super-WIMPs constitute all of the dark matter in our galaxy.
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.
First Dark Matter Search Results from the XENON1T Experiment
E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, L. Bütikofer, et al (106)
May 19 2017 astro-ph.CO astro-ph.IM hep-ex hep-ph arXiv:1705.06655v4

@misc{1705.06655, author = {E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and F.~D.~Amaro and M.~Anthony and F.~Arneodo and P.~Barrow 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 L.~Bütikofer and J.~Calvén and J.~M.~R.~Cardoso and M.~Cervantes 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 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 R.~Gardner and C.~Geis and L.~W.~Goetzke and L.~Grandi and Z.~Greene and C.~Grignon and C.~Hasterok and E.~Hogenbirk and J.~Howlett and R.~Itay and B.~Kaminsky and S.~Kazama and G.~Kessler and A.~Kish and H.~Landsman and R.~F.~Lang and D.~Lellouch and L.~Levinson and Q.~Lin and S.~Lindemann and M.~Lindner and F.~Lombardi and J.~A.~M.~Lopes and A.~Manfredini and I.~Mariş and T.~Marrodán Undagoitia and J.~Masbou and F.~V.~Massoli and D.~Masson and D.~Mayani and M.~Messina and K.~Micheneau and A.~Molinario and K.~Morå and M.~Murra and J.~Naganoma and K.~Ni and U.~Oberlack and P.~Pakarha and B.~Pelssers and R.~Persiani and F.~Piastra and J.~Pienaar and V.~Pizzella and M.-C.~Piro and G.~Plante and N.~Priel and L.~Rauch and S.~Reichard and C.~Reuter and B.~Riedel and A.~Rizzo and S.~Rosendahl and N.~Rupp and R.~Saldanha and J.~M.~F.~dos Santos and G.~Sartorelli and M.~Scheibelhut and S.~Schindler and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and E.~Shockley and M.~Silva and H.~Simgen and M.~v.~Sivers and A.~Stein and S.~Thapa and D.~Thers and A.~Tiseni and G.~Trinchero and C.~Tunnell and M.~Vargas and N.~Upole and H.~Wang and Z.~Wang and Y.~Wei and C.~Weinheimer and J.~Wulf and J.~Ye and Y.~Zhang and T.~Zhu}, title = {{F}irst {D}ark {M}atter {S}earch {R}esults from the {XENON}1{T} {E}xperiment}, year = {2017}, eprint = {1705.06655}, howpublished = {Phys. Rev. Lett. 119, 181301 (2017)}, doi = {10.1103/PhysRevLett.119.181301}, note = {arXiv:1705.06655v4} }
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We report the first dark matter search results from XENON1T, a $\sim$2000-kg-target-mass dual-phase (liquid-gas) xenon time projection chamber in operation at the Laboratori Nazionali del Gran Sasso in Italy and the first ton-scale detector of this kind. The blinded search used 34.2 live days of data acquired between November 2016 and January 2017. Inside the (1042$\pm$12) kg fiducial mass and in the [5, 40] $\mathrm{keV}_{\mathrm{nr}}$ energy range of interest for WIMP dark matter searches, the electronic recoil background was $(1.93 \pm 0.25) \times 10^{-4}$ events/(kg $\times$ day $\times \mathrm{keV}_{\mathrm{ee}}$), the lowest ever achieved in a dark matter detector. A profile likelihood analysis shows that the data is consistent with the background-only hypothesis. We derive the most stringent exclusion limits on the spin-independent WIMP-nucleon interaction cross section for WIMP masses above 10 GeV/c${}^2$, with a minimum of 7.7 $\times 10^{-47}$ cm${}^2$ for 35-GeV/c${}^2$ WIMPs at 90% confidence level.
Supernova neutrino physics with xenon dark matter detectors: A timely perspective
Rafael F. Lang, Christopher McCabe, Shayne Reichard, Marco Selvi, Irene Tamborra
Jul 01 2016 astro-ph.HE astro-ph.SR hep-ex hep-ph arXiv:1606.09243v2

@misc{1606.09243, author = {Rafael F.~Lang and Christopher McCabe and Shayne Reichard and Marco Selvi and Irene Tamborra}, title = {{S}upernova neutrino physics with xenon dark matter detectors: {A} timely perspective}, year = {2016}, eprint = {1606.09243}, howpublished = {Phys. Rev. D 94 (2016) no.10, 103009}, note = {arXiv:1606.09243v2} }
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Dark matter detectors that utilize liquid xenon have now achieved tonne-scale targets, giving them sensitivity to all flavours of supernova neutrinos via coherent elastic neutrino-nucleus scattering. Considering for the first time a realistic detector model, we simulate the expected supernova neutrino signal for different progenitor masses and nuclear equations of state in existing and upcoming dual-phase liquid xenon experiments. We show that the proportional scintillation signal (S2) of a dual-phase detector allows for a clear observation of the neutrino signal and guarantees a particularly low energy threshold, while the backgrounds are rendered negligible during the supernova burst. XENON1T (XENONnT and LZ; DARWIN) experiments will be sensitive to a supernova burst up to 25 (35; 65) kpc from Earth at a significance of more than 5 sigma, observing approximately 35 (123; 704) events from a 27 Msun supernova progenitor at 10 kpc. Moreover, it will be possible to measure the average neutrino energy of all flavours, to constrain the total explosion energy, and to reconstruct the supernova neutrino light curve. Our results suggest that a large xenon detector such as DARWIN will be competitive with dedicated neutrino telescopes, while providing complementary information that is not otherwise accessible.
A low-mass dark matter search using ionization signals in XENON100
XENON100 Collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown S. Bruenner, G. Bruno, R. Budnik, A. Buss, L. Bütikofer, et al (91)
May 23 2016 astro-ph.CO hep-ex hep-ph physics.ins-det arXiv:1605.06262v4

@misc{1605.06262, author = {XENON100 Collaboration and E.~Aprile and J.~Aalbers and F.~Agostini and M.~Alfonsi and F.~D.~Amaro and M.~Anthony and F.~Arneodo and P.~Barrow and L.~Baudis and B.~Bauermeister and M.~L.~Benabderrahmane and T.~Berger and P.~A.~Breur and A.~Brown and E.~Brown S.~Bruenner and G.~Bruno and R.~Budnik and A.~Buss and L.~Bütikofer and J.~M.~R.~Cardoso and M.~Cervantes 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 E.~Duchovni and A.~D.~Ferella and A.~Fieguth and D.~Franco and W.~Fulgione and M.~Galloway and M.~Garbini and C.~Geis and L.~W.~Goetzke and Z.~Greene and C.~Grignon and E.~Gross and C.~Hasterok and E.~Hogenbirk and R.~Itay and B.~Kaminsky and G.~Kessler and A.~Kish and H.~Landsman and R.~F.~Lang and L.~Levinson and M.~Le Calloch and C.~Levy and F.~Linde and S.~Lindemann and M.~Lindner and J.~A.~M.~Lopes and A.~Lyashenko and A.~Manfredini and T.~Marrodán Undagoitia and J.~Masbou and F.~V.~Massoli and D.~Masson and D.~Mayani and A.~J.~Melgarejo Fernandez and Y.~Meng and M.~Messina and K.~Micheneau and B.~Miguez and A.~Molinario and M.~Murra and J.~Naganoma and U.~Oberlack and S.~E.~A.~Orrigo and P.~Pakarha and B.~Pelssers and R.~Persiani and F.~Piastra and J.~Pienaar and G.~Plante and N.~Priel and L.~Rauch and S.~Reichard and C.~Reuter and A.~Rizzo and S.~Rosendahl and N.~Rupp and J.~M.~F.~dos Santos and G.~Sartorelli and M.~Scheibelhut and S.~Schindler and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and H.~Simgen and A.~Stein and D.~Thers and A.~Tiseni and G.~Trinchero and C.~D.~Tunnell and M.~von Sivers and R.~Wall and H.~Wang and M.~Weber and Y.~Wei and C.~Weinheimer and J.~Wulf and Y.~Zhang}, title = {{A} low-mass dark matter search using ionization signals in {XENON}100}, year = {2016}, eprint = {1605.06262}, howpublished = {Phys. Rev. D 94, 092001 (2016)}, doi = {10.1103/PhysRevD.94.092001}, note = {arXiv:1605.06262v4} }
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We perform a low-mass dark matter search using an exposure of 30\u2009kg$\times$yr with the XENON100 detector. By dropping the requirement of a scintillation signal and using only the ionization signal to determine the interaction energy, we lowered the energy threshold for detection to 0.7\u2009keV for nuclear recoils. No dark matter detection can be claimed because a complete background model cannot be constructed without a primary scintillation signal. Instead, we compute an upper limit on the WIMP-nucleon scattering cross section under the assumption that every event passing our selection criteria could be a signal event. Using an energy interval from 0.7\u2009keV to 9.1\u2009keV, we derive a limit on the spin-independent WIMP-nucleon cross section that excludes WIMPs with a mass of 6\u2009GeV/$c^2$ above $1.4 \times 10^{-41}$\u2009cm$^2$ at 90\% confidence level.
Shear Viscosities from Kubo Formalism in a large-$N_{\rm c}$ Nambu--Jona-Lasinio Model
Robert Lang, Norbert Kaiser, Wolfram Weise
Jun 09 2015 hep-ph arXiv:1506.02459v2

@misc{1506.02459, author = {Robert Lang and Norbert Kaiser and Wolfram Weise}, title = {{S}hear {V}iscosities from {K}ubo {F}ormalism in a large-${N}_{\rm c}$ {N}ambu--{J}ona-{L}asinio {M}odel}, year = {2015}, eprint = {1506.02459}, howpublished = {Eur. Phys. J. A 51 (2015) 127}, doi = {10.1140/epja/i2015-15127-7}, note = {arXiv:1506.02459v2} }
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In this work the shear viscosity of strongly interacting matter is calculated within a two-flavor Nambu--Jona-Lasinio model as a function of temperature and chemical potential. The general Kubo formula is applied, incorporating the full Dirac structure of the thermal quark spectral function and avoiding commonly used on-shell approximations. Mesonic fluctuations contributing via Fock diagrams provide the dominant dissipative processes. The resulting ratio $\eta/s$ (shear viscosity over entropy density) decreases with temperature and chemical potential. Interpolating between our NJL results at low temperatures and hard-thermal-loop results at high temperatures a minimum slightly above the AdS/CFT benchmark $\eta/s=1/4\pi$ is obtained.
Testing General Relativity with Present and Future Astrophysical Observations
Emanuele Berti, Enrico Barausse, Vitor Cardoso, Leonardo Gualtieri, Paolo Pani, Ulrich Sperhake, Leo C. Stein, Norbert Wex, Kent Yagi, Tessa Baker, C. P. Burgess, Flávio S. Coelho, Daniela Doneva, Antonio De Felice, Pedro G. Ferreira, Paulo C. C. Freire, James Healy, Carlos Herdeiro, Michael Horbatsch, Burkhard Kleihaus, et al (33)
Jan 30 2015 gr-qc astro-ph.HE hep-ph hep-th arXiv:1501.07274v4

@misc{1501.07274, author = {Emanuele Berti and Enrico Barausse and Vitor Cardoso and Leonardo Gualtieri and Paolo Pani and Ulrich Sperhake and Leo C.~Stein and Norbert Wex and Kent Yagi and Tessa Baker and C.~P.~Burgess and Flávio S.~Coelho and Daniela Doneva and Antonio De Felice and Pedro G.~Ferreira and Paulo C.~C.~Freire and James Healy and Carlos Herdeiro and Michael Horbatsch and Burkhard Kleihaus and Antoine Klein and Kostas Kokkotas and Jutta Kunz and Pablo Laguna and Ryan N.~Lang and Tjonnie G.~F.~Li and Tyson Littenberg and Andrew Matas and Saeed Mirshekari and Hirotada Okawa and Eugen Radu and Richard O'Shaughnessy and Bangalore S.~Sathyaprakash and Chris Van Den Broeck and Hans A.~Winther and Helvi Witek and Mir Emad Aghili and Justin Alsing and Brett Bolen and Luca Bombelli and Sarah Caudill and Liang Chen and Juan Carlos Degollado and Ryuichi Fujita and Caixia Gao and Davide Gerosa and Saeed Kamali and Hector O.~Silva and João G.~Rosa and Laleh Sadeghian and Marco Sampaio and Hajime Sotani and Miguel Zilhao}, title = {{T}esting {G}eneral {R}elativity with {P}resent and {F}uture {A}strophysical {O}bservations}, year = {2015}, eprint = {1501.07274}, howpublished = {Class. Quantum Grav. 32, 243001 (2015)}, doi = {10.1088/0264-9381/32/24/243001}, note = {arXiv:1501.07274v4} }
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One century after its formulation, Einstein's general relativity has made remarkable predictions and turned out to be compatible with all experimental tests. Most of these tests probe the theory in the weak-field regime, and there are theoretical and experimental reasons to believe that general relativity should be modified when gravitational fields are strong and spacetime curvature is large. The best astrophysical laboratories to probe strong-field gravity are black holes and neutron stars, whether isolated or in binary systems. We review the motivations to consider extensions of general relativity. We present a (necessarily incomplete) catalog of modified theories of gravity for which strong-field predictions have been computed and contrasted to Einstein's theory, and we summarize our current understanding of the structure and dynamics of compact objects in these theories. We discuss current bounds on modified gravity from binary pulsar and cosmological observations, and we highlight the potential of future gravitational wave measurements to inform us on the behavior of gravity in the strong-field regime.
First Axion Results from the XENON100 Experiment
XENON100 Collaboration, E. Aprile, F. Agostini, M. Alfonsi, K. Arisaka, F. Arneodo, M. Auger, C. Balan, P. Barrow, L. Baudis, B. Bauermeister, A. Behrens, P. Beltrame, K. Bokeloh, A. Brown, E. Brown, S. Bruenner, G. Bruno, R. Budnik, J. M. R. Cardoso, et al (70)
Apr 08 2014 astro-ph.CO astro-ph.GA hep-ph arXiv:1404.1455v3

@misc{1404.1455, author = {XENON100 Collaboration and E.~Aprile and F.~Agostini and M.~Alfonsi and K.~Arisaka and F.~Arneodo and M.~Auger and C.~Balan and P.~Barrow and L.~Baudis and B.~Bauermeister and A.~Behrens and P.~Beltrame and K.~Bokeloh and A.~Brown and E.~Brown and S.~Bruenner and G.~Bruno and R.~Budnik and J.~M.~R.~Cardoso and A.~P.~Colijn and H.~Contreras and J.~P.~Cussonneau and M.~P.~Decowski and E.~Duchovni and S.~Fattori and A.~D.~Ferella and W.~Fulgione and F.~Gao and M.~Garbini and C.~Geis and L.~W.~Goetzke and C.~Grignon and E.~Gross and W.~Hampel and R.~Itay and F.~Kaether and G.~Kessler and A.~Kish and H.~Landsman and R.~F.~Lang and M.~Le Calloch and D.~Lellouch and C.~Levy and S.~Lindemann and M.~Lindner and J.~A.~M.~Lopes and K.~Lung and A.~Lyashenko and S.~Macmullin and T.~Marrodan Undagoitia and J.~Masbou and F.~V.~Massoli and D.~Mayani Paras and A.~J.~Melgarejo Fernandez and Y.~Meng and M.~Messina and B.~Miguez and A.~Molinario and M.~Murra and J.~Naganoma and U.~Oberlack and S.~E.~A.~Orrigo and E.~Pantic and R.~Persiani and F.~Piastra and J.~Pienaar and G.~Plante and N.~Priel and S.~Reichard and C.~Reuter and A.~Rizzo and S.~Rosendahl and J.~M.~F.~dos Santos and G.~Sartorelli and S.~Schindler and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and M.~Selvi and P.~Shagin and H.~Simgen and A.~Teymourian and D.~Thers and A.~Tiseni and G.~Trinchero and O.~Vitells and H.~Wang and M.~Weber and C.~Weinheimer}, title = {{F}irst {A}xion {R}esults from the {XENON}100 {E}xperiment}, year = {2014}, eprint = {1404.1455}, note = {arXiv:1404.1455v3} }
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We present the first results of searches for axions and axion-like-particles with the XENON100 experiment. The axion-electron coupling constant, $g_{Ae}$, has been probed by exploiting the axio-electric effect in liquid xenon. A profile likelihood analysis of 224.6 live days $\times$ 34 kg exposure has shown no evidence for a signal. By rejecting $g_{Ae}$, larger than $7.7 \times 10^{-12}$ (90\% CL) in the solar axion search, we set the best limit to date on this coupling. In the frame of the DFSZ and KSVZ models, we exclude QCD axions heavier than 0.3 eV/c$^2$ and 80 eV/c$^2$, respectively. For axion-like-particles, under the assumption that they constitute the whole abundance of dark matter in our galaxy, we constrain $g_{Ae}$, to be lower than $1 \times 10^{-12}$ (90\% CL) for mass range from 1 to 40 keV/c$^2$, and set the best limit to date as well.
Shear viscosity from Kubo formalism: NJL-model study
Robert Lang, Wolfram Weise
Nov 20 2013 hep-ph arXiv:1311.4628v2

@misc{1311.4628, author = {Robert Lang and Wolfram Weise}, title = {{S}hear viscosity from {K}ubo formalism: {NJL}-model study}, year = {2013}, eprint = {1311.4628}, howpublished = {Eur. Phys. J. A 50 (2014) 63}, doi = {10.1140/epja/i2014-14063-4}, note = {arXiv:1311.4628v2} }
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A large-$N_{\rm c}$ expansion is combined with the Kubo formalism to study the shear viscosity $\eta$ of strongly interacting matter in the two-flavor NJL model. We discuss analytical and numerical approaches to $\eta$ and investigate systematically its strong dependence on the spectral width and the momentum-space cutoff. Thermal effects on the constituent quark mass from spontaneous chiral symmetry breaking are included. The ratio $\eta/s$ and its thermal dependence are derived for different parameterizations of the spectral width and for an explicit one-loop calculation including mesonic modes within the NJL model.
Signatures of Dark Matter Scattering Inelastically Off Nuclei
L. Baudis, G. Kessler, P. Klos, R. F. Lang, J. Menendez, S. Reichard, A. Schwenk
Sep 04 2013 astro-ph.CO hep-ex hep-ph nucl-th arXiv:1309.0825v2

@misc{1309.0825, author = {L.~Baudis and G.~Kessler and P.~Klos and R.~F.~Lang and J.~Menendez and S.~Reichard and A.~Schwenk}, title = {{S}ignatures of {D}ark {M}atter {S}cattering {I}nelastically {O}ff {N}uclei}, year = {2013}, eprint = {1309.0825}, howpublished = {Phys. Rev. D 88, 115014 (2013)}, doi = {10.1103/PhysRevD.88.115014}, note = {arXiv:1309.0825v2} }
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Direct dark matter detection focuses on elastic scattering of dark matter particles off nuclei. In this study, we explore inelastic scattering where the nucleus is excited to a low-lying state of 10-100 keV, with subsequent prompt de-excitation. We calculate the inelastic structure factors for the odd-mass xenon isotopes based on state-of-the-art large-scale shell-model calculations with chiral effective field theory WIMP-nucleon currents. For these cases, we find that the inelastic channel is comparable to or can dominate the elastic channel for momentum transfers around 150 MeV. We calculate the inelastic recoil spectra in the standard halo model, compare these to the elastic case, and discuss the expected signatures in a xenon detector, along with implications for existing and future experiments. The combined information from elastic and inelastic scattering will allow to determine the dominant interaction channel within one experiment. In addition, the two channels probe different regions of the dark matter velocity distribution and can provide insight into the dark halo structure. The allowed recoil energy domain and the recoil energy at which the integrated inelastic rates start to dominate the elastic channel depend on the mass of the dark matter particle, thus providing a potential handle to constrain its mass.
Power-Spectrum Analysis of Reconstructed DAMA Data
P.A. Sturrock, E. Fischbach, J.T.Gruenwal, D. Javorsek II, J.H. Jenkins, R.F. Lang, R.H. Lee, J. Nistor, J. Scargle
May 01 2013 hep-ph astro-ph.CO arXiv:1304.8112v1

@misc{1304.8112, author = {P.A.~Sturrock and E.~Fischbach and J.T.Gruenwal and D.~Javorsek II and J.H.~Jenkins and R.F.~Lang and R.H.~Lee and J.~Nistor and J.~Scargle}, title = {{P}ower-{S}pectrum {A}nalysis of {R}econstructed {DAMA} {D}ata}, year = {2013}, eprint = {1304.8112}, note = {arXiv:1304.8112v1} }
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Claims by the DAMA (DArk MAtter) collaboration to have detected an annually varying signal consistent with models of dark matter appear to be at variance with results from other dark-matter searches. To further understand the DAMA results, we have carried out an independent analysis of DAMA data reconstructed from published figures. In addition to reexamining the Lomb-Scargle and chi-square analyses previously carried out by the DAMA collaboration, we carry out two new likelihood analyses and a new chi-square analysis, focusing attention on the treatment of experimental errors and binning. We confirm the existence of an annual oscillation, with a maximum in early June, but at a lower significance level than previously reported.
Limits on spin-dependent WIMP-nucleon cross sections from 225 live days of XENON100 data
XENON100 collaboration, E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudis, B. Bauermeister, A. Behrens, P. Beltrame, K. Bokeloh, A. Brown, E. Brown, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, A. P. Colijn, H. Contreras, et al (58)
Jan 29 2013 astro-ph.CO astro-ph.IM hep-ex hep-ph arXiv:1301.6620v2

@misc{1301.6620, author = {XENON100 collaboration and E.~Aprile and M.~Alfonsi and K.~Arisaka and F.~Arneodo and C.~Balan and L.~Baudis and B.~Bauermeister and A.~Behrens and P.~Beltrame and K.~Bokeloh and A.~Brown and E.~Brown and G.~Bruno and R.~Budnik and J.~M.~R.~Cardoso and W.-T.~Chen and B.~Choi and A.~P.~Colijn and H.~Contreras and J.~P.~Cussonneau and M.~P.~Decowski and E.~Duchovni and S.~Fattori and A.~D.~Ferella and W.~Fulgione and F.~Gao and M.~Garbini and C.~Ghag and K.-L.~Giboni and L.~W.~Goetzke and C.~Grignon and E.~Gross and W.~Hampel and F.~Kaether and A.~Kish and J.~Lamblin and H.~Landsman and R.~F.~Lang and M.~Le Calloch and D.~Lellouch and C.~Levy and K.~E.~Lim and Q.~Lin and S.~Lindemann and M.~Lindner and J.~A.~M.~Lopes and K.~Lung and T.~Marrodan Undagoitia and F.~V.~Massoli and A.~J.~Melgarejo Fernandez and Y.~Meng and M.~Messina and A.~Molinario and K.~Ni and U.~Oberlack and S.~E.~A.~Orrigo and E.~Pantic and R.~Persiani and G.~Plante and N.~Priel and A.~Rizzo and S.~Rosendahl and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and P.~R.~Scovell and M.~Selvi and P.~Shagin and H.~Simgen and A.~Teymourian and D.~Thers and O.~Vitells and H.~Wang and M.~Weber and C.~Weinheimer}, title = {{L}imits on spin-dependent {WIMP}-nucleon cross sections from 225 live days of {XENON}100 data}, year = {2013}, eprint = {1301.6620}, doi = {10.1103/PhysRevLett.111.021301}, note = {arXiv:1301.6620v2} }
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We present new experimental constraints on the elastic, spin-dependent WIMP-nucleon cross section using recent data from the XENON100 experiment, operated in the Laboratori Nazionali del Gran Sasso in Italy. An analysis of 224.6 live days x 34 kg of exposure acquired during 2011 and 2012 revealed no excess signal due to axial-vector WIMP interactions with 129-Xe and 131-Xe nuclei. This leads to the most stringent upper limits on WIMP-neutron cross sections for WIMP masses above 6 GeV, with a minimum cross section of 3.5 x 10^-40 cm^2 at a WIMP mass of 45 GeV, at 90% confidence level.
Time-Series Analysis of Reconstructed DAMA Data
Peter A. Sturrock, Ephraim Fischbach, Jere H. Jenkins, Rafael Lang, Jonathan Nistor
Oct 30 2012 hep-ph arXiv:1210.7496v1

@misc{1210.7496, author = {Peter A.~Sturrock and Ephraim Fischbach and Jere H.~Jenkins and Rafael Lang and Jonathan Nistor}, title = {{T}ime-{S}eries {A}nalysis of {R}econstructed {DAMA} {D}ata}, year = {2012}, eprint = {1210.7496}, note = {arXiv:1210.7496v1} }
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An analysis of DAMA data (as reconstructed from DAMA publications) confirms the presence of an annual oscillation, but with a lower significance level than that claimed by DAMA. The phase of their signal is 0.39 +/- 0.02, corresponding to a peak value at about May 22, which is consistent with both the DAMA estimate and the expected phase of a dark-matter signal. However, a spectrogram analysis also shows evidence for oscillations in the frequency band 11 - 13 year-1, that are similar to oscillations found in spectrograms formed from measurements of the decay rates of 36Cl and 32Si acquired at the Brookhaven National Laboratory (BNL). One component of these oscillations (at 11.44 year-1) is prominent in DAMA/NaI data, at the 0.2% significance level (99.8% confidence level). Analyses of BNL and other nuclear decay (specifically beta decay and K-capture) measurements point to a solar influence, either by neutrinos or by some currently unknown form of radiation. The phase of the annual oscillation in DAMA data is compatible with an influence of dark matter, and is unlikely to be attributable to a purely solar influence. We also find that annual oscillations in both 133Ba decay measurements and the Troitsk tritium-decay measurements are compatible with a cosmic influence but not with a purely solar influence. These considerations raise the possibility that DAMA measurements may somehow be influenced by a combination of solar neutrinos, cosmic neutrinos, and dark matter
Comment on "On the subtleties of searching for dark matter with liquid xenon detectors"
XENON Collaboration, E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudis, B. Bauermeister, A. Behrens, P. Beltrame, K. Bokeloh, E. Brown, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, D. Cline, A. P. Colijn, H. Contreras, et al (57)
Aug 29 2012 astro-ph.CO astro-ph.IM hep-ex hep-ph arXiv:1208.5762v1

@misc{1208.5762, author = {XENON Collaboration and E.~Aprile and M.~Alfonsi and K.~Arisaka and F.~Arneodo and C.~Balan and L.~Baudis and B.~Bauermeister and A.~Behrens and P.~Beltrame and K.~Bokeloh and E.~Brown and G.~Bruno and R.~Budnik and J.~M.~R.~Cardoso and W.-T.~Chen and B.~Choi and D.~Cline and A.~P.~Colijn and H.~Contreras and J.~P.~Cussonneau and M.~P.~Decowski and E.~Duchovni and S.~Fattori and A.~D.~Ferella and W.~Fulgione and F.~Gao and M.~Garbini and C.~Ghag and K.-L.~Giboni and L.~W.~Goetzke and C.~Grignon and E.~Gross and W.~Hampel and F.~Kaether and A.~Kish and J.~Lamblin and H.~Landsman and R.~F.~Lang and M.~Le Calloch and C.~Levy and K.~E.~Lim and Q.~Lin and S.~Lindemann and M.~Lindner and J.~A.~M.~Lopes and K.~Lung and T.~Marrodan Undagoitia and F.~V.~Massoli and A.~J.~Melgarejo Fernandez and Y.~Meng and A.~Molinario and E.~Nativ and K.~Ni and U.~Oberlack and S.~E.~A.~Orrigo and E.~Pantic and R.~Persiani and G.~Plante and N.~Priel and A.~Rizzo and S.~Rosendahl and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and P.~R.~Scovell and M.~Selvi and P.~Shagin and H.~Simgen and A.~Teymourian and D.~Thers and O.~Vitells and H.~Wang and M.~Weber and C.~Weinheimer}, title = {{C}omment on "{O}n the subtleties of searching for dark matter with liquid xenon detectors"}, year = {2012}, eprint = {1208.5762}, note = {arXiv:1208.5762v1} }
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In a recent manuscript (arXiv:1208.5046) Peter Sorensen claims that XENON100's upper limits on spin-independent WIMP-nucleon cross sections for WIMP masses below 10 GeV "may be understated by one order of magnitude or more". Having performed a similar, though more detailed analysis prior to the submission of our new result (arXiv:1207.5988), we do not confirm these findings. We point out the rationale for not considering the described effect in our final analysis and list several potential problems with his study.
Dark Matter Results from 225 Live Days of XENON100 Data
XENON100 Collaboration, E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudis, B. Bauermeister, A. Behrens, P. Beltrame, K. Bokeloh, E. Brown, G. Bruno, R. Budnik, J. M. R. Cardoso, W.-T. Chen, B. Choi, D. Cline, A. P. Colijn, H. Contreras, et al (58)
Jul 26 2012 astro-ph.CO hep-ex hep-ph physics.ins-det arXiv:1207.5988v2

@misc{1207.5988, author = {XENON100 Collaboration and E.~Aprile and M.~Alfonsi and K.~Arisaka and F.~Arneodo and C.~Balan and L.~Baudis and B.~Bauermeister and A.~Behrens and P.~Beltrame and K.~Bokeloh and E.~Brown and G.~Bruno and R.~Budnik and J.~M.~R.~Cardoso and W.-T.~Chen and B.~Choi and D.~Cline and A.~P.~Colijn and H.~Contreras and J.~P.~Cussonneau and M.~P.~Decowski and E.~Duchovni and S.~Fattori and A.~D.~Ferella and W.~Fulgione and F.~Gao and M.~Garbini and C.~Ghag and K.-L.~Giboni and L.~W.~Goetzke and C.~Grignon and E.~Gross and W.~Hampel and F.~Kaether and H.~Kettling and A.~Kish and J.~Lamblin and H.~Landsman and R.~F.~Lang and M.~Le Calloch and C.~Levy and K.~E.~Lim and Q.~Lin and S.~Lindemann and M.~Lindner and J.~A.~M.~Lopes and K.~Lung and T.~Marrodan Undagoitia and F.~V.~Massoli and A.~J.~Melgarejo Fernandez and Y.~Meng and A.~Molinario and E.~Nativ and K.~Ni and U.~Oberlack and S.~E.~A.~Orrigo and E.~Pantic and R.~Persiani and G.~Plante and N.~Priel and A.~Rizzo and S.~Rosendahl and J.~M.~F.~dos Santos and G.~Sartorelli and J.~Schreiner and M.~Schumann and L.~Scotto Lavina and P.~R.~Scovell and M.~Selvi and P.~Shagin and H.~Simgen and A.~Teymourian and D.~Thers and O.~Vitells and H.~Wang and M.~Weber and C.~Weinheimer}, title = {{D}ark {M}atter {R}esults from 225 {L}ive {D}ays of {XENON}100 {D}ata}, year = {2012}, eprint = {1207.5988}, howpublished = {Phys. Rev. Lett. 109, 181301 (2012)}, doi = {10.1103/PhysRevLett.109.181301}, note = {arXiv:1207.5988v2} }
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We report on a search for particle dark matter with the XENON100 experiment, operated at the Laboratori Nazionali del Gran Sasso (LNGS) for 13 months during 2011 and 2012. XENON100 features an ultra-low electromagnetic background of (5.3 \pm 0.6) \times 10^-3 events (kg day keVee)^-1 in the energy region of interest. A blind analysis of 224.6 live days \times 34 kg exposure has yielded no evidence for dark matter interactions. The two candidate events observed in the pre-defined nuclear recoil energy range of 6.6-30.5 keVnr are consistent with the background expectation of (1.0 \pm 0.2) events. A Profile Likelihood analysis using a 6.6-43.3 keVnr energy range sets the most stringent limit on the spin-independent elastic WIMP-nucleon scattering cross section for WIMP masses above 8 GeV/c^2, with a minimum of 2 \times 10^-45 cm^2 at 55 GeV/c^2 and 90% confidence level.
Shear Viscosity of a Hot Pion Gas
Robert Lang, Norbert Kaiser, Wolfram Weise
May 31 2012 hep-ph arXiv:1205.6648v2

@misc{1205.6648, author = {Robert Lang and Norbert Kaiser and Wolfram Weise}, title = {{S}hear {V}iscosity of a {H}ot {P}ion {G}as}, year = {2012}, eprint = {1205.6648}, howpublished = {Eur. Phys. J. A 48 (2012) 109}, doi = {10.1140/epja/i2012-12109-3}, note = {arXiv:1205.6648v2} }
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The shear viscosity of an interacting pion gas is studied using the Kubo formalism as a microscopic description of thermal systems close to global equilibrium. We implement the skeleton expansion in order to approximate the retarded correlator of the viscous part of the energy-momentum tensor. After exploring this in $g\phi^4$ theory we show how the skeleton expansion can be consistently applied to pions in chiral perturbation theory. The shear viscosity $\eta$ is determined by the spectral width, or equivalently, the mean free path of pions in the heat bath. We derive a new analytical result for the mean free path which is well-conditioned for numerical evaluation and discuss the temperature and pion-mass dependence of the mean free path and the shear viscosity. The ratio $\eta/s$ of the interacting pion gas exceeds the lower bound $1/4\pi$ from AdS/CFT correspondence.
Proceedings to the 13th Workshop 'What Comes Beyond the Standard Models', Bled, July 12. - 22., 2010, Slovenia
A. Ali Khan, G. Bregar, V.V. Dvoeglazov, J. Ellis, R. Erdem, A. Hernandez-Galeana, M.Yu. Khlopov, R.F. Lang, D. Lukman, N.S. Mankoc Borstnik, H. Markum, A.G. Mayorov, R. Mirman, G. Moultaka, K. Nagao, H.B. Nielsen, M. Ninomiya, M. Rosina, E.Yu. Soldatov
Dec 02 2010 hep-ph arXiv:1012.0224v1

@misc{1012.0224, author = {A.~Ali Khan and G.~Bregar and V.V.~Dvoeglazov and J.~Ellis and R.~Erdem and A.~Hernandez-Galeana and M.Yu.~Khlopov and R.F.~Lang and D.~Lukman and N.S.~Mankoc Borstnik and H.~Markum and A.G.~Mayorov and R.~Mirman and G.~Moultaka and K.~Nagao and H.B.~Nielsen and M.~Ninomiya and M.~Rosina and E.Yu.~Soldatov}, title = {{P}roceedings to the 13th {W}orkshop '{W}hat {C}omes {B}eyond the {S}tandard {M}odels', {B}led, {J}uly 12. - 22., 2010, {S}lovenia}, year = {2010}, eprint = {1012.0224}, howpublished = {J. Phys. Conf. Ser.284:012024, 2011}, note = {arXiv:1012.0224v1} }
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1. Noncommutativity and Topology within Lattice Field Theories 2. The Construction of Quantum Field Operators 3. The Bargmann-Wigner Formalism for Spin 2 Fields 4. New Light on Dark Matter from the LHC 5. Extra Dimensional Metric Reversal Symmetry and its Prospect... 6. Masses and Mixing Matrices of Families within SU(3) Flavor Symmetry ... 7. Dark Atoms of the Universe: OHe Nuclear Physics, 8. Can the Matter-Antimatter Asymmetry be Easier to Understand Within the "Spin-charge-family-theory", .. 9. Mass Matrices of Twice Four Families of Quarks and Leptons, ...in the "Spin-charge-family-theory" 10. Bohmian Quantum Mechanics or What Comes Before the Standard Model 11. Backward Causation in Complex Action Model ... 12. Is the Prediction of the "Spin-charge-family-theory" in Disagreement with the XENON100..? 13. Masses and Mixing Matrices of Families of Quarks and Leptons Within the "Spin-charge-family-theory" 14. Can the Stable Fifth Family of the "Spin-charge-family-theory" ...Form the Fifth Antibaryon Clusters with Ordinary He Nucleus? 15. Puzzles of Dark Matter - More Light on Dark Atoms? 16. Families of Spinors in d = (1 + 5)...and Masslessness 17. Are Superheavy Quark Clusters Candidates for the Dark Matter? 18. Complex Action Functioning as Cutoff and De Broglie-Bohm Particle 19. Where does the Science Go? 20. VIA Presentation
Impure Thoughts on Inelastic Dark Matter
Spencer Chang, Rafael F. Lang, Neal Weiner
Jul 19 2010 hep-ph arXiv:1007.2688v3

@misc{1007.2688, author = {Spencer Chang and Rafael F.~Lang and Neal Weiner}, title = {{I}mpure {T}houghts on {I}nelastic {D}ark {M}atter}, year = {2010}, eprint = {1007.2688}, howpublished = {Phys.Rev.Lett.106:011301,2011}, doi = {10.1103/PhysRevLett.106.011301}, note = {arXiv:1007.2688v3} }
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The inelastic dark matter scenario was proposed to reconcile the DAMA annual modulation with null results from other experiments. In this scenario, WIMPs scatter into an excited state, split from the ground state by an energy delta comparable to the available kinetic energy of a Galactic WIMP. We note that for large splittings delta, the dominant scattering at DAMA can occur off of thallium nuclei, with A~205, which are present as a dopant at the 10^-3 level in NaI(Tl) crystals. For a WIMP mass m~100GeV and delta~200keV, we find a region in delta-m-parameter space which is consistent with all experiments. These parameters in particular can be probed in experiments with thallium in their targets, such as KIMS, but are inaccessible to lighter target experiments. Depending on the tail of the WIMP velocity distribution, a highly modulated signal may or may not appear at CRESST-II.
Peaked Signals from Dark Matter Velocity Structures in Direct Detection Experiments
Rafael F. Lang, Neal Weiner
Mar 19 2010 hep-ph arXiv:1003.3664v1

@misc{1003.3664, author = {Rafael F.~Lang and Neal Weiner}, title = {{P}eaked {S}ignals from {D}ark {M}atter {V}elocity {S}tructures in {D}irect {D}etection {E}xperiments}, year = {2010}, eprint = {1003.3664}, howpublished = {JCAP06 (2010) 032}, doi = {10.1088/1475-7516/2010/06/032}, note = {arXiv:1003.3664v1} }
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In direct dark matter detection experiments, conventional elastic scattering of WIMPs results in exponentially falling recoil spectra. In contrast, theories of WIMPs with excited states can lead to nuclear recoil spectra that peak at finite recoil energies E_R. The peaks of such signals are typically fairly broad, with Delta E_R/E_peak ~ 1. We show that in the presence of dark matter structures with low velocity dispersion, such as streams or clumps, peaks from up-scattering can become extremely narrow with FWHM of a few keV only. This differs dramatically from the conventionally expected WIMP spectrum and would, once detected, open the possibility to measure the dark matter velocity structure with a fantastic accuracy. As an intriguing example, we confront the observed cluster of 3 events near 42 keV from the CRESST commissioning run with this scenario, and find a wide range of parameters capable for producing such a peak. We compare the possible signals at other experiments, and find that such a particle could also give rise to the signal at DAMA, although not from the same stream. Over some range of parameters a signal would be visible at xenon experiments. We show that such dark matter peaks are a very clear signal, and can be easily disentangled from potential backgrounds, both terrestrial or due to WIMP down-scattering, by an enhanced annual modulation signature in both the amplitude of the signal and its shape.