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A search for an eV-scale sterile neutrino using improved high-energy $\nu_\mu$ event reconstruction in IceCube
IceCube Collaboration, R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J.M. Alameddine, N. M. Amin, K. Andeen, C. Argüelles, Y. Ashida, S. Athanasiadou, L. Ausborm, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, S. Bash, et al (403)
May 15 2024 hep-ex hep-ph arXiv:2405.08070v1

@misc{2405.08070, author = {IceCube Collaboration and R.~Abbasi and M.~Ackermann and J.~Adams and S.~K.~Agarwalla and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and N.~M.~Amin and K.~Andeen and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and L.~Ausborm and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and S.~Bash and V.~Basu and R.~Bay and J.~J.~Beatty and J.~Becker Tjus and J.~Beise and C.~Bellenghi and C.~Benning and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and E.~Blaufuss and L.~Bloom and S.~Blot and F.~Bontempo and J.~Y.~Book Motzkin and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and L.~Brusa and R.~T.~Burley and D.~Butterfield and M.~A.~Campana and I.~Caracas and K.~Carloni and J.~Carpio and S.~Chattopadhyay and N.~Chau and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and R.~Corley and P.~Correa and D.~F.~Cowen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado and S.~Deng and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and P.~Dierichs and M.~Dittmer and A.~Domi and L.~Draper and H.~Dujmovic and K.~Dutta and M.~A.~DuVernois and T.~Ehrhardt and L.~Eidenschink and A.~Eimer and P.~Eller and E.~Ellinger and S.~El Mentawi and D.~Elsässer and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and K.~Fang and K.~Farrag and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and S.~Fukami and P.~Fürst and J.~Gallagher and E.~Ganster and A.~Garcia and M.~Garcia and G.~Garg and E.~Genton and L.~Gerhardt and A.~Ghadimi and C.~Girard-Carillo and C.~Glaser and T.~Glüsenkamp and J.~G.~Gonzalez and S.~Goswami and A.~Granados and D.~Grant and S.~J.~Gray and O.~Gries and S.~Griffin and S.~Griswold and K.~M.~Groth and C.~Günther and P.~Gutjahr and C.~Ha and C.~Haack and A.~Hallgren and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and M.~Handt and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and J.~Häußler and K.~Helbing and J.~Hellrung and J.~Hermannsgabner and L.~Heuermann and N.~Heyer and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and S.~Hori and K.~Hoshina and M.~Hostert and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and A.~Ishihara and W.~Iwakiri and M.~Jacquart and O.~Janik and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and N.~Kamp and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and A.~Katil and U.~Katz and M.~Kauer and J.~L.~Kelley and M.~Khanal and A.~Khatee Zathul and A.~Kheirandish and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and J.~Krishnamoorthi and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and S.~Latseva and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and J.~Liao and M.~Lincetto and Y.~T.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and W.~Luszczak and Y.~Lyu and J.~Madsen and E.~Magnus and K.~B.~M.~Mahn and Y.~Makino and E.~Manao and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and Y.~Merckx and L.~Merten and J.~Micallef and J.~Mitchell and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and M.~Nakos and U.~Naumann and J.~Necker and A.~Negi and L.~Neste and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and K.~Noda and A.~Noell and A.~Novikov and A.~Obertacke Pollmann and V.~O'Dell and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and T.~Pernice and J.~Peterson and S.~Philippen and A.~Pizzuto and M.~Plum and A.~Pontén and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and M.~Ravn and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and E.~Resconi and S.~Reusch and W.~Rhode and B.~Riedel and A.~Rifaie and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and A.~Rosted and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and P.~Schaile and M.~Schaufel and H.~Schieler and S.~Schindler and B.~Schlüter and F.~Schlüter and N.~Schmeisser and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and M.~Seikh and M.~Seo and S.~Seunarine and P.~Sevle Myhr and R.~Shah and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and P.~Soldin and G.~Sommani and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and A.~Terliuk and M.~Thiesmeyer and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and R.~Turcotte and J.~P.~Twagirayezu and M.~A.~Unland Elorrieta and A.~K.~Upadhyay and K.~Upshaw and A.~Vaidyanathan and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and M.~Venugopal and M.~Vereecken and S.~Verpoest and D.~Veske and A.~Vijai and C.~Walck and A.~Wang and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and A.~Y.~Wen and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and D.~R.~Williams and L.~Witthaus and A.~Wolf and M.~Wolf and G.~Wrede and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and R.~Young and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin and P.~Zilberman and M.~Zimmerman}, title = {{A} search for an e{V}-scale sterile neutrino using improved high-energy $\nu_\mu$ event reconstruction in {I}ce{C}ube}, year = {2024}, eprint = {2405.08070}, note = {arXiv:2405.08070v1} }
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This Letter presents the result of a 3+1 sterile neutrino search using 10.7 years of IceCube data. We analyze atmospheric muon neutrinos that traverse the Earth with energies ranging from 0.5 to 100 TeV, incorporating significant improvements in modeling neutrino flux and detector response compared to earlier studies. Notably, for the first time, we categorize data into starting and through-going events, distinguishing neutrino interactions with vertices inside or outside the instrumented volume, to improve energy resolution. The best-fit point for a 3+1 model is found to be at $\sin^2(2\theta_{24}) = 0.16$ and $\Delta m^{2}_{41} = 3.5$ eV$^2$, which agrees with previous iterations of this study. The result is consistent with the null hypothesis of no sterile neutrinos with a p-value of 3.1\%.
Methods and stability tests associated with the sterile neutrino search using improved high-energy $\nu_\mu$ event reconstruction in IceCube
IceCube Collaboration, R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J.M. Alameddine, N. M. Amin, K. Andeen, C. Argüelles, Y. Ashida, S. Athanasiadou, L. Ausborm, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, S. Bash, et al (403)
May 15 2024 hep-ex hep-ph arXiv:2405.08077v1

@misc{2405.08077, author = {IceCube Collaboration and R.~Abbasi and M.~Ackermann and J.~Adams and S.~K.~Agarwalla and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and N.~M.~Amin and K.~Andeen and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and L.~Ausborm and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and S.~Bash and V.~Basu and R.~Bay and J.~J.~Beatty and J.~Becker Tjus and J.~Beise and C.~Bellenghi and C.~Benning and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and E.~Blaufuss and L.~Bloom and S.~Blot and F.~Bontempo and J.~Y.~Book Motzkin and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and L.~Brusa and R.~T.~Burley and D.~Butterfield and M.~A.~Campana and I.~Caracas and K.~Carloni and J.~Carpio and S.~Chattopadhyay and N.~Chau and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and R.~Corley and P.~Correa and D.~F.~Cowen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado and S.~Deng and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and P.~Dierichs and M.~Dittmer and A.~Domi and L.~Draper and H.~Dujmovic and K.~Dutta and M.~A.~DuVernois and T.~Ehrhardt and L.~Eidenschink and A.~Eimer and P.~Eller and E.~Ellinger and S.~El Mentawi and D.~Elsässer and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and K.~Fang and K.~Farrag and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and S.~Fukami and P.~Fürst and J.~Gallagher and E.~Ganster and A.~Garcia and M.~Garcia and G.~Garg and E.~Genton and L.~Gerhardt and A.~Ghadimi and C.~Girard-Carillo and C.~Glaser and T.~Glüsenkamp and J.~G.~Gonzalez and S.~Goswami and A.~Granados and D.~Grant and S.~J.~Gray and O.~Gries and S.~Griffin and S.~Griswold and K.~M.~Groth and C.~Günther and P.~Gutjahr and C.~Ha and C.~Haack and A.~Hallgren and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and M.~Handt and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and J.~Häußler and K.~Helbing and J.~Hellrung and J.~Hermannsgabner and L.~Heuermann and N.~Heyer and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and S.~Hori and K.~Hoshina and M.~Hostert and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and A.~Ishihara and W.~Iwakiri and M.~Jacquart and O.~Janik and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and N.~Kamp and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and A.~Katil and U.~Katz and M.~Kauer and J.~L.~Kelley and M.~Khanal and A.~Khatee Zathul and A.~Kheirandish and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and J.~Krishnamoorthi and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and S.~Latseva and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and J.~Liao and M.~Lincetto and Y.~T.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and W.~Luszczak and Y.~Lyu and J.~Madsen and E.~Magnus and K.~B.~M.~Mahn and Y.~Makino and E.~Manao and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and Y.~Merckx and L.~Merten and J.~Micallef and J.~Mitchell and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and M.~Nakos and U.~Naumann and J.~Necker and A.~Negi and L.~Neste and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and K.~Noda and A.~Noell and A.~Novikov and A.~Obertacke Pollmann and V.~O'Dell and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and T.~Pernice and J.~Peterson and S.~Philippen and A.~Pizzuto and M.~Plum and A.~Pontén and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and M.~Ravn and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and E.~Resconi and S.~Reusch and W.~Rhode and B.~Riedel and A.~Rifaie and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and A.~Rosted and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and P.~Schaile and M.~Schaufel and H.~Schieler and S.~Schindler and B.~Schlüter and F.~Schlüter and N.~Schmeisser and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and M.~Seikh and M.~Seo and S.~Seunarine and P.~Sevle Myhr and R.~Shah and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and P.~Soldin and G.~Sommani and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and A.~Terliuk and M.~Thiesmeyer and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and R.~Turcotte and J.~P.~Twagirayezu and M.~A.~Unland Elorrieta and A.~K.~Upadhyay and K.~Upshaw and A.~Vaidyanathan and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and M.~Venugopal and M.~Vereecken and S.~Verpoest and D.~Veske and A.~Vijai and C.~Walck and A.~Wang and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and A.~Y.~Wen and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and D.~R.~Williams and L.~Witthaus and A.~Wolf and M.~Wolf and G.~Wrede and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and R.~Young and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin and P.~Zilberman and M.~Zimmerman}, title = {{M}ethods and stability tests associated with the sterile neutrino search using improved high-energy $\nu_\mu$ event reconstruction in {I}ce{C}ube}, year = {2024}, eprint = {2405.08077}, note = {arXiv:2405.08077v1} }
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We provide supporting details for the search for a 3+1 sterile neutrino using data collected over eleven years at the IceCube Neutrino Observatory. The analysis uses atmospheric muon-flavored neutrinos from 0.5 to 100\,TeV that traverse the Earth to reach the IceCube detector, and finds a best-fit point at $\sin^2(2\theta_{24}) = 0.16$ and $\Delta m^{2}_{41} = 3.5$ eV$^2$ with a goodness-of-fit p-value of 12\% and consistency with the null hypothesis of no oscillations to sterile neutrinos with a p-value of 3.1\%. Several improvements were made over past analyses, which are reviewed in this article, including upgrades to the reconstruction and the study of sources of systematic uncertainty. We provide details of the fit quality and discuss stability tests that split the data for separate samples, comparing results. We find that the fits are consistent between split data sets.
Testing Meson Portal Dark Sector Solutions to the MiniBooNE Anomaly at CCM
A.A. Aguilar-Arevalo, S. Biedron, J. Boissevain, M. Borrego, L. Bugel, M. Chavez-Estrada, J.M. Conrad, R.L. Cooper, A. Diaz, J.R. Distel, J.C. D'Olivo, E. Dunton, B. Dutta, D. Fields, J.R. Gochanour, M. Gold, E. Guardincerri, E.C. Huang, N. Kamp, D. Kim, et al (25)
Sep 07 2023 hep-ph hep-ex arXiv:2309.02599v5

@misc{2309.02599, author = {A.A.~Aguilar-Arevalo and S.~Biedron and J.~Boissevain and M.~Borrego and L.~Bugel and M.~Chavez-Estrada and J.M.~Conrad and R.L.~Cooper and A.~Diaz and J.R.~Distel and J.C.~D'Olivo and E.~Dunton and B.~Dutta and D.~Fields and J.R.~Gochanour and M.~Gold and E.~Guardincerri and E.C.~Huang and N.~Kamp and D.~Kim and K.~Knickerbocker and W.C.~Louis and J.T.M.~Lyles and R.~Mahapatra and S.~Maludze and J.~Mirabal and D.~Newmark and P.~deNiverville and V.~Pandey and D.~Poulson and H.~Ray and E.~Renner and T.J.~Schaub and A.~Schneider and M.H.~Shaevitz and D.~Smith and W.~Sondheim and A.M.~Szelc and C.~Taylor and A.~Thompson and W.H.~Thompson and M.~Tripathi and R.T.~Thornton and R.~Van Berg and R.G.~Van de Water}, title = {{T}esting {M}eson {P}ortal {D}ark {S}ector {S}olutions to the {M}ini{B}oo{NE} {A}nomaly at {CCM}}, year = {2023}, eprint = {2309.02599}, howpublished = {Phys.Rev.D 109 (2024) 9, 095017}, note = {arXiv:2309.02599v5} }
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A solution to the MiniBooNE excess invoking rare three-body decays of the charged pions and kaons to new states in the MeV mass scale was recently proposed as a dark-sector explanation. This class of solution illuminates the fact that, while the charged pions were focused in the target-mode run, their decay products were isotropically suppressed in the beam-dump-mode run in which no excess was observed. This suggests a new physics solution correlated to the mesonic sector. We investigate an extended set of phenomenological models that can explain the MiniBooNE excess as a dark sector solution, utilizing long-lived particles that might be produced in the three-body decays of the charged mesons and the two-body anomalous decays of the neutral mesons. Over a broad set of interactions with the long-lived particles, we show that these scenarios can be compatible with constraints from LSND, KARMEN, and MicroBooNE, and evaluate the sensitivity of the ongoing and future data taken by the Coherent CAPTAIN Mills experiment (CCM) to a potential discovery in this parameter space.
Searching for Decoherence from Quantum Gravity at the IceCube South Pole Neutrino Observatory
R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J.M. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, R. Bay, et al (385)
Aug 02 2023 hep-ex hep-ph hep-th arXiv:2308.00105v1

@misc{2308.00105, author = {R.~Abbasi and M.~Ackermann and J.~Adams and S.~K.~Agarwalla and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and N.~M.~Amin and K.~Andeen and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and V.~Basu and R.~Bay and J.~J.~Beatty and J.~Becker Tjus and J.~Beise and C.~Bellenghi and C.~Benning and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Y.~Book and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and R.~T.~Burley and R.~S.~Busse and D.~Butterfield and M.~A.~Campana and K.~Carloni and E.~G.~Carnie-Bronca and S.~Chattopadhyay and N.~Chau and C.~Chen and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado and S.~Deng and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and A.~Domi and H.~Dujmovic and M.~A.~DuVernois and T.~Ehrhardt and P.~Eller and E.~Ellinger and S.~El Mentawi and D.~Elsässer and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and K.~Fang and K.~Farrag and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and A.~Fritz and P.~Fürst and J.~Gallagher and E.~Ganster and A.~Garcia and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and N.~Goehlke and J.~G.~Gonzalez and S.~Goswami and D.~Grant and S.~J.~Gray and O.~Gries and S.~Griffin and S.~Griswold and K.~M.~Groth and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and K.~Helbing and J.~Hellrung and F.~Henningsen and L.~Heuermann and N.~Heyer and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and S.~Hori and K.~Hoshina and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and A.~Ishihara and M.~Jacquart and O.~Janik and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Khatee Zathul and A.~Kheirandish and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and J.~Krishnamoorthi and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and S.~Latseva and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and W.~Luszczak and Y.~Lyu and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and E.~Manao and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and Y.~Merckx and L.~Merten and J.~Micallef and J.~Mitchell and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and M.~Nakos and U.~Naumann and J.~Necker and A.~Negi and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and A.~Noell and A.~Novikov and S.~C.~Nowicki and A.~Obertacke Pollmann and V.~O'Dell and M.~Oehler and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and J.~Peterson and S.~Philippen and A.~Pizzuto and M.~Plum and A.~Pontén and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and B.~Riedel and A.~Rifaie and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and S.~E.~Sanchez Herrera and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and M.~Schaufel and H.~Schieler and S.~Schindler and L.~Schlickmann and B.~Schlüter and F.~Schlüter and N.~Schmeisser and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and M.~Seikh and S.~Seunarine and R.~Shah and A.~Sharma and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and P.~Soldin and G.~Sommani and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and M.~Thiesmeyer and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and C.~F.~Tung and R.~Turcotte and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and A.~K.~Upadhyay and K.~Upshaw and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and M.~Venugopal and M.~Vereecken and S.~Verpoest and D.~Veske and A.~Vijai and C.~Walck and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and A.~Y.~Wen and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and D.~R.~Williams and L.~Witthaus and A.~Wolf and M.~Wolf and G.~Wrede and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and R.~Young and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin and P.~Zilberman and M.~Zimmerman}, title = {{S}earching for {D}ecoherence from {Q}uantum {G}ravity at the {I}ce{C}ube {S}outh {P}ole {N}eutrino {O}bservatory}, year = {2023}, eprint = {2308.00105}, note = {arXiv:2308.00105v1} }
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Neutrino oscillations at the highest energies and longest baselines provide a natural quantum interferometer with which to study the structure of spacetime and test the fundamental principles of quantum mechanics. If the metric of spacetime has a quantum mechanical description, there is a generic expectation that its fluctuations at the Planck scale would introduce non-unitary effects that are inconsistent with the standard unitary time evolution of quantum mechanics. Neutrinos interacting with such fluctuations would lose their quantum coherence, deviating from the expected oscillatory flavor composition at long distances and high energies. The IceCube South Pole Neutrino Observatory is a billion-ton neutrino telescope situated in the deep ice of the Antarctic glacier. Atmospheric neutrinos detected by IceCube in the energy range 0.5--10 TeV have been used to test for coherence loss in neutrino propagation. No evidence of anomalous neutrino decoherence was observed, leading to the strongest experimental limits on neutrino-quantum gravity interactions to date, significantly surpassing expectations from natural Planck-scale models. The resulting constraint on the effective decoherence strength parameter within an energy-independent decoherence model is $\Gamma_0\leq 1.17\times10^{-15}$~eV, improving upon past limits by a factor of 30. For decoherence effects scaling as E$^2$, limits are advanced by more than six orders of magnitude beyond past measurements.
Search for neutrino lines from dark matter annihilation and decay with IceCube
IceCube Collaboration, R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J.M. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, et al (378)
Mar 27 2023 astro-ph.HE hep-ph arXiv:2303.13663v1

@misc{2303.13663, author = {IceCube Collaboration and R.~Abbasi and M.~Ackermann and J.~Adams and S.~K.~Agarwalla and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and N.~M.~Amin and K.~Andeen and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and V.~Basu and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and J.~Beise and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Y.~Book and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and R.~T.~Burley and R.~S.~Busse and D.~Butterfield and M.~A.~Campana and K.~Carloni and E.~G.~Carnie-Bronca and S.~Chattopadhyay and C.~Chen and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and P.~Correa and S.~Countryman and D.~F.~Cowen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado López and H.~Dembinski and S.~Deng and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and A.~Domi and H.~Dujmovic and M.~A.~DuVernois and T.~Ehrhardt and C.~El Aisati and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and K.~Fang and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and M.~Gustafsson and N.~Goehlke and J.~G.~Gonzalez and S.~Goswami and D.~Grant and S.~J.~Gray and S.~Griffin and S.~Griswold and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and T.~Hambye and H.~Hamdaoui and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and S.~Hauser and K.~Helbing and J.~Hellrung and F.~Henningsen and L.~Heuermann and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and K.~Hoshina and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and N.~Iovine and A.~Ishihara and M.~Jacquart and M.~Jansson and G.~S.~Japaridze and K.~Jayakumar and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Khatee Zathul and A.~Kheirandish and K.~Kin and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and S.~Meighen-Berger and Y.~Merckx and L.~Merten and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and M.~Nakos and U.~Naumann and J.~Necker and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and A.~Noell and S.~C.~Nowicki and A.~Obertacke Pollmann and M.~Oehler and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and J.~Peterson and S.~Philippen and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and S.Athanasiadou and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and S.~E.~Sanchez Herrera and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and M.~Schaufel and H.~Schieler and S.~Schindler and B.~Schlüter and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and G.~Sommani and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and R.~Stein and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and C.~F.~Tung and R.~Turcotte and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and A.~K.~Upadhyay and K.~Upshaw and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and M.~Venugopal and S.~Verpoest and D.~Veske and C.~Walck and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and N.~Willey and D.~R.~Williams and M.~Wolf and G.~Wrede and J.~Wulff and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and F.~Yu and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin}, title = {{S}earch for neutrino lines from dark matter annihilation and decay with {I}ce{C}ube}, year = {2023}, eprint = {2303.13663}, note = {arXiv:2303.13663v1} }
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Dark Matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for such signal, by looking at both the angular and energy information of the neutrino events. To this end, a total of five years of IceCube's DeepCore data has been used to test dark matter masses ranging from 10~GeV to 40~TeV. No significant neutrino excess was found and upper limits on the annihilation cross section, as well as lower limits on the dark matter lifetime, were set. The limits reached are of the order of $10^{-24}$~cm$^3/s$ for an annihilation and up to $10^{27}$ seconds for decaying Dark Matter. Using the same data sample we also derive limits for dark matter annihilation or decay into a pair of Standard Model charged particles.
Limits on Neutrino Emission from GRB 221009A from MeV to PeV using the IceCube Neutrino Observatory
R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, N. Aggarwal, J. A. Aguilar, M. Ahlers, J.M. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, V. Basu, et al (367)
Feb 14 2023 astro-ph.HE hep-ex hep-ph arXiv:2302.05459v3

@misc{2302.05459, author = {R.~Abbasi and M.~Ackermann and J.~Adams and S.~K.~Agarwalla and N.~Aggarwal and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and N.~M.~Amin and K.~Andeen and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and V.~Basu and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and J.~Beise and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Y.~Book and J.~Borowka and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and R.~T.~Burley and R.~S.~Busse and M.~A.~Campana and K.~Carloni and E.~G.~Carnie-Bronca and C.~Chen and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and P.~Correa and S.~Countryman and D.~F.~Cowen and C.~Dappen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado López and H.~Dembinski and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and A.~Domi and H.~Dujmovic and M.~A.~DuVernois and T.~Ehrhardt and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and N.~Goehlke and J.~G.~Gonzalez and S.~Goswami and D.~Grant and S.~J.~Gray and S.~Griffin and S.~Griswold and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and K.~Helbing and J.~Hellrung and F.~Henningsen and L.~Heuermann and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and K.~Hoshina and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Kheirandish and K.~Kin and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and S.~Meighen-Berger and Y.~Merckx and L.~Merten and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and A.~Noell and S.~C.~Nowicki and A.~Obertacke Pollmann and M.~Oehler and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and J.~Peterson and S.~Philippen and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and S.Athanasiadou and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and S.~E.~Sanchez Herrera and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and M.~Schaufel and H.~Schieler and S.~Schindler and B.~Schlüter and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and G.~Sommani and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and R.~Stein and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and C.~F.~Tung and R.~Turcotte and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and K.~Upshaw and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and M.~Venugopal and S.~Verpoest and D.~Veske and C.~Walck and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and N.~Willey and D.~R.~Williams and M.~Wolf and G.~Wrede and J.~Wulff and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and F.~Yu and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin}, title = {{L}imits on {N}eutrino {E}mission from {GRB} 221009{A} from {M}e{V} to {P}e{V} using the {I}ce{C}ube {N}eutrino {O}bservatory}, year = {2023}, eprint = {2302.05459}, howpublished = {ApJL 946 L26 (2023)}, doi = {10.3847/2041-8213/acc077}, note = {arXiv:2302.05459v3} }
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Gamma-ray bursts (GRBs) have long been considered a possible source of high-energy neutrinos. While no correlations have yet been detected between high-energy neutrinos and GRBs, the recent observation of GRB 221009A - the brightest GRB observed by Fermi-GBM to date and the first one to be observed above an energy of 10 TeV - provides a unique opportunity to test for hadronic emission. In this paper, we leverage the wide energy range of the IceCube Neutrino Observatory to search for neutrinos from GRB 221009A. We find no significant deviation from background expectation across event samples ranging from MeV to PeV energies, placing stringent upper limits on the neutrino emission from this source.
A Search for Coincident Neutrino Emission from Fast Radio Bursts with Seven Years of IceCube Cascade Events
R. Abbasi, M. Ackermann, J. Adams, N. Aggarwal, J. A. Aguilar, M. Ahlers, J.M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, et al (367)
Dec 14 2022 astro-ph.HE hep-ph arXiv:2212.06702v1

@misc{2212.06702, author = {R.~Abbasi and M.~Ackermann and J.~Adams and N.~Aggarwal and J.~A.~Aguilar and M.~Ahlers and J.M.~Alameddine and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and S.~N.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and V.~Basu and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and J.~Beise and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Y.~Book and J.~Borowka and C.~Boscolo Meneguolo and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Braun and B.~Brinson and J.~Brostean-Kaiser and R.~T.~Burley and R.~S.~Busse and M.~A.~Campana and E.~G.~Carnie-Bronca and C.~Chen and Z.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and P.~Correa and S.~Countryman and D.~F.~Cowen and C.~Dappen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado López and H.~Dembinski and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and H.~Dujmovic and M.~A.~DuVernois and T.~Ehrhardt and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and A.~T.~Fienberg and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and N.~Goehlke and J.~G.~Gonzalez and S.~Goswami and D.~Grant and S.~J.~Gray and T.~Grégoire and S.~Griffin and S.~Griswold and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and P.~Hatch and A.~Haungs and K.~Helbing and J.~Hellrung and F.~Henningsen and L.~Heuermann and S.~Hickford and A.~Hidvegi and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and K.~Hoshina and W.~Hou and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Kheirandish and K.~Kin and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and K.~Kruiswijk and E.~Krupczak and A.~Kumar and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~Lamoureux and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard DeHolton and A.~Leszczyńska and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~Love and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and S.~Marka and Z.~Marka and M.~Marsee and I.~Martinez-Soler and R.~Maruyama and F.~Mayhew and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and S.~Meighen-Berger and Y.~Merckx and L.~Merten and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and Y.~Morii and R.~Morse and M.~Moulai and T.~Mukherjee and R.~Naab and R.~Nagai and U.~Naumann and A.~Nayerhoda and J.~Necker and M.~Neumann and H.~Niederhausen and M.~U.~Nisa and A.~Noell and S.~C.~Nowicki and A.~Obertacke Pollmann and M.~Oehler and B.~Oeyen and A.~Olivas and R.~Orsoe and J.~Osborn and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and J.~Peterson and S.~Philippen and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and M.~Prado Rodriguez and B.~Pries and R.~Procter-Murphy and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and K.~Rawlins and Z.~Rechav and A.~Rehman and P.~Reichherzer and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and E.~J.~Roberts and S.~Robertson and S.~Rodan and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and L.~Ruohan and D.~Ryckbosch and S.Athanasiadou and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and S.~E.~Sanchez Herrera and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and J.~Savelberg and P.~Savina and M.~Schaufel and H.~Schieler and S.~Schindler and B.~Schlüter and T.~Schmidt and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Søgaard and D.~Soldin and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and R.~Stein and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and W.~G.~Thompson and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and C.~F.~Tung and R.~Turcotte and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and K.~Upshaw and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Vara and J.~Veitch-Michaelis and S.~Verpoest and D.~Veske and C.~Walck and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and N.~Willey and D.~R.~Williams and M.~Wolf and G.~Wrede and J.~Wulff and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin}, title = {{A} {S}earch for {C}oincident {N}eutrino {E}mission from {F}ast {R}adio {B}ursts with {S}even {Y}ears of {I}ce{C}ube {C}ascade {E}vents}, year = {2022}, eprint = {2212.06702}, note = {arXiv:2212.06702v1} }
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This paper presents the results of a search for neutrinos that are spatially and temporally coincident with 22 unique, non-repeating Fast Radio Bursts (FRBs) and one repeating FRB (FRB121102). FRBs are a rapidly growing class of Galactic and extragalactic astrophysical objects that are considered a potential source of high-energy neutrinos. The IceCube Neutrino Observatory's previous FRB analyses have solely used track events. This search utilizes seven years of IceCube's cascade events which are statistically independent of the track events. This event selection allows probing of a longer range of extended timescales due to the low background rate. No statistically significant clustering of neutrinos was observed. Upper limits are set on the time-integrated neutrino flux emitted by FRBs for a range of extended time-windows.
New Clues About Light Sterile Neutrinos: Preference for Models with Damping Effects in Global Fits
J.M. Hardin, I. Martinez-Soler, A. Diaz, M. Jin, N.W. Kamp, C.A. Argüelles, J.M. Conrad, M.H. Shaevitz
Nov 07 2022 hep-ph hep-ex arXiv:2211.02610v5

@misc{2211.02610, author = {J.M.~Hardin and I.~Martinez-Soler and A.~Diaz and M.~Jin and N.W.~Kamp and C.A.~Argüelles and J.M.~Conrad and M.H.~Shaevitz}, title = {{N}ew {C}lues {A}bout {L}ight {S}terile {N}eutrinos: {P}reference for {M}odels with {D}amping {E}ffects in {G}lobal {F}its}, year = {2022}, eprint = {2211.02610}, note = {arXiv:2211.02610v5} }
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This article reports global fits of short-baseline neutrino data to oscillation models involving light sterile neutrinos. In the commonly-used 3+1 plane wave model, there is a well-known 4.9$\sigma$ tension between data sets sensitive to appearance versus disappearance of neutrinos. We find that models that damp the oscillation prediction for the reactor data sets, especially at low energy, substantially improve the fits and reduce the tension. We consider two such scenarios. The first scenario introduces the quantum mechanical wavepacket effect that accounts for the source size in reactor experiments into the 3+1 model. We find that inclusion of the wavepacket effect greatly improves the overall fit compared to a 3$\nu$ model by $\Delta \chi^2/$DOF$=61.1/4$ ($7.1\sigma$ improvement) with best-fit $\Delta m^2=1.4$ eV$^2$ and wavepacket length of 67fm. The internal tension is reduced to 3.4$\sigma$. If reactor-data only is fit, then the wavepacket preferred length is 91 fm ($>20$ fm at 99\% CL). The second model introduces oscillations involving sterile flavor and allows the decay of the heaviest, mostly sterile mass state, $\nu_4$. This model introduces a damping term similar to the wavepacket effect, but across all experiments. Compared to a three-neutrino fit, this has a $\Delta \chi^2/$DOF$=60.6/4$ ($7\sigma$ improvement) with preferred $\Delta m^2=1.4$ eV$^2$ and decay $\Gamma = 0.35$ eV$^2$. The internal tension is reduced to 3.7$\sigma$. For many years, the reactor event rates have been observed to have structure that deviates from prediction. Community discussion has focused on an excess compared to prediction observed at 5 MeV; however, other deviations are apparent. This structure has $L$ dependence that is well-fit by the damped models. Before assuming this points to new physics, we urge closer examination of systematic effects that could lead to this $L$ dependence.
Through Iron & Ice: Searching for Sterile Neutrinos at the IceCube Neutrino Observatory
Alejandro Diaz
Oct 19 2022 hep-ex hep-ph arXiv:2210.09418v1

@misc{2210.09418, author = {Alejandro Diaz}, title = {{T}hrough {I}ron & {I}ce: {S}earching for {S}terile {N}eutrinos at the {I}ce{C}ube {N}eutrino {O}bservatory}, year = {2022}, eprint = {2210.09418}, note = {arXiv:2210.09418v1} }
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Despite the rapid progression in our understanding of neutrinos over the last half century, much is left unknown about their properties. This leaves neutrinos as the most promising portal for Beyond Standard Model (BSM) physics, and neutrinos have already provided fruitful surprises. A number of neutrino experiments in the last three decades have observed anomalous oscillation signals consistent with a mass-squared splitting of $\Delta m^2 \sim 1\ \textrm{eV}^2$, motivating the existence and search for sterile neutrinos. On the other hand, other experiments have failed to see such a signal. In this thesis, we present two analyses. The first is an update to the sterile neutrino global fits with the inclusion of recent experimental data. We find that the 3+1 model provides a better fit to the global data set compared to the null, with an improvement of $\Delta \chi^2 = 51$ with the addition of only 3 degrees of freedom, corresponding to $6.6\sigma$. While a substantial improvement, we also find a irreconcilable tension between the data sets of $5.1\sigma$, calculated using the parameter goodness-of-fit test. This motivates the exploration of expanded models: a 3+2 model, and a 3+1+Decay model. In the 3+2 model, we find negligible improvement to the fit, and an even worse tension of $5.5\sigma$. In the more exotic 3+1+Decay model, we find the tension reduced to $3.6\sigma$. While a substantial improvement compared to the 3+1 model with the introduction of only one additional parameter, the tension is still too large to assuage concerns. The second analysis is the results of an expanded IceCube sterile neutrino search. A previous sterile neutrino search found no evidence for sterile neutrinos, finding a p-value of 8%. Of the three sterile mixing angles, $\theta_{14}, \theta_{24}$, and $\theta_{34}$, only $\theta_{24}$ was fitted for, as $\theta_{14}$ was negligible and $\theta_{34} = 0$ was considered a conservative assumption. We present results of an analysis where we include $\theta_{34}$ to the fitted model. Both a frequentist and Bayesian analysis were conducted, with fits done in terms of the mass-squared splitting $\Delta m_{41}^2$ and the mixing matrix parameters $|U_{\mu4}|^2$ and $|U_{\tau4}|^2$. The frequentist analysis finds a best fit at $\Delta m_{41}^2 = 5.0\ \textrm{eV}^2$, $|U_{\mu4}|^2 = 0.04$, and $|U_{\tau4}|^2 = 0.006$, with a p-value of 5.2% assuming Wilks' Theorem with 3 degrees of freedom. Pseudoexperiments are indicating a smaller p-value 2.7%. The Bayesian analysis finds a similar best fit point at $\Delta m_{41}^2 = 5.0\ \textrm{eV}^2$, $|U_{\mu4}|^2 = 0.02$, and $|U_{\tau4}|^2 = 0.006$, with a Bayes factor indicating a ``Very Strong'' preference for this sterile hypothesis over the null hypothesis.
Searches for Connections between Dark Matter and High-Energy Neutrinos with IceCube
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, J.M. Alameddine, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. W. Barwick, et al (360)
May 26 2022 hep-ex astro-ph.HE hep-ph arXiv:2205.12950v2

@misc{2205.12950, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and J.M.~Alameddine and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Athanasiadou and S.~Axani and X.~Bai and A.~Balagopal V.~and M.~Baricevic and S.~W.~Barwick and V.~Basu and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and J.~Beise and C.~Bellenghi and S.~Benda and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Y.~Book and J.~Borowka and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and F.~Bradascio and J.~Braun and B.~Brinson and S.~Bron and J.~Brostean-Kaiser and R.~T.~Burley and R.~S.~Busse and M.~A.~Campana and E.~G.~Carnie-Bronca and C.~Chen and Z.~Chen and D.~Chirkin and K.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and A.~Connolly and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and C.~Dappen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado López and H.~Dembinski and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and H.~Dujmovic and M.~A.~DuVernois and T.~Ehrhardt and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and A.~T.~Fienberg and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and N.~Goehlke and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and S.~Griswold and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and H.~Hamdaoui and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and A.~Haungs and K.~Helbing and J.~Hellrung and F.~Henningsen and E.~C.~Hettinger and L.~Heuermann and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and K.~Hoshina and W.~Hou and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Kheirandish and K.~Kin and J.~Kiryluk and S.~R.~Klein and A.~Kochocki and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and E.~Krupczak and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard and A.~Leszczyńska and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and W.~Marie Sainte and I.~C.~Mariş and I.~Martinez-Soler and R.~Maruyama and S.~McCarthy and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and S.~Meighen-Berger and Y.~Merckx and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and R.~Morse and T.~Mukherjee and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and L.~V.~Nguy\~\^en and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and A.~Obertacke Pollmann and M.~Oehler and B.~Oeyen and A.~Olivas and J.~Osborn and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and L.~Peters and J.~Peterson and S.~Philippen and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and B.~Pries and G.~T.~Przybylski and C.~Raab and J.~Rack-Helleis and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and Z.~Rechav and A.~Rehman and P.~Reichherzer and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and E.~J.~Roberts and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and J.~Saffer and D.~Salazar-Gallegos and P.~Sampathkumar and S.~E.~Sanchez Herrera and A.~Sandrock and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Schaufel and H.~Schieler and S.~Schindler and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and N.~Shimizu and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and A.~Sogaard and D.~Soldin and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and J.~Thwaites and S.~Tilav and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and K.~Upshaw and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and J.~Veitch-Michaelis and S.~Verpoest and C.~Walck and W.~Wang and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and N.~Willey and D.~R.~Williams and M.~Wolf and G.~Wrede and J.~Wulff and X.~W.~Xu and J.~P.~Yanez and E.~Yildizci and S.~Yoshida and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin}, title = {{S}earches for {C}onnections between {D}ark {M}atter and {H}igh-{E}nergy {N}eutrinos with {I}ce{C}ube}, year = {2022}, eprint = {2205.12950}, note = {arXiv:2205.12950v2} }
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In this work, we present the results of searches for signatures of dark matter decay or annihilation into Standard Model particles, and secret neutrino interactions with dark matter. Neutrinos could be produced in the decay or annihilation of galactic or extragalactic dark matter. Additionally, if an interaction between dark matter and neutrinos exists then dark matter will interact with extragalactic neutrinos. In particular galactic dark matter will induce an anisotropy in the neutrino sky if this interaction is present. We use seven and a half years of the High-Energy Starting Event (HESE) sample data, which measures neutrinos in the energy range of approximately 60 TeV to 10 PeV, to study these phenomena. This all-sky event selection is dominated by extragalactic neutrinos. For dark matter of $\sim$ 1 PeV in mass, we constrain the velocity-averaged annihilation cross section to be smaller than $10^{-23}$cm$^3$/s for the exclusive $\mu^+\mu^-$ channel and $10^{-22}$ cm$^3$/s for the $b\bar b$ channel. For the same mass, we constrain the lifetime of dark matter to be larger than $10^{28}$ s for all channels studied, except for decaying exclusively to $b\bar b$ where it is bounded to be larger than $10^{27}$ s. Finally, we also search for evidence of astrophysical neutrinos scattering on galactic dark matter in two scenarios. For fermionic dark matter with a vector mediator, we constrain the dimensionless coupling associated with this interaction to be less than 0.1 for dark matter mass of 0.1 GeV and a mediator mass of $10^{-4}~$ GeV. In the case of scalar dark matter with a fermionic mediator, we constrain the coupling to be less than 0.1 for dark matter and mediator masses below 1 MeV.
Search for secluded dark matter towards the Galactic Centre with the ANTARES neutrino telescope
A. Albert, S. Alves, M. Andre, M. Anghinolfi, G. Anton, M. Ardid, S. Ardid, J.-J. Aubert, J. Aublin, B. Baret, S. Basa, B. Belhorma, M. Bendahman, F. Benfenati, V. Bertin, S. Biagi, M. Bissinger, J. Boumaaza, M. Bouta, M.C. Bouwhuis, et al (129)
Mar 14 2022 astro-ph.HE hep-ph arXiv:2203.06029v1

@misc{2203.06029, author = {A.~Albert and S.~Alves and M.~Andre and M.~Anghinolfi and G.~Anton and M.~Ardid and S.~Ardid and J.-J.~Aubert and J.~Aublin and B.~Baret and S.~Basa and B.~Belhorma and M.~Bendahman and F.~Benfenati and V.~Bertin and S.~Biagi and M.~Bissinger and J.~Boumaaza and M.~Bouta and M.C.~Bouwhuis and H.~Branzas and R.~Bruijn and J.~Brunner and J.~Busto and B.~Caiffi and D.~Calvo and A.~Capone and L.~Caramete and J.~Carr and V.~Carretero and S.~Celli and M.~Chabab and T.~N.~Chau and R.~Cherkaoui El Moursli and T.~Chiarusi and M.~Circella and A.~Coleiro and R.~Coniglione and P.~Coyle and A.~Creusot and A.~F.~Diaz and G.~de Wasseige and C.~Distefano and I.~Di Palma and A.~Domi and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and T.~van Eeden and D.~van Eijk and N.~El Khayati and A.~Enzenhoefer and P.~Fermani and G.~Ferrara and F.~Filippini and L.~Fusco and Y.~Gatelet and P.~Gay and H.~Glotin and R.~Gozzini and R.~Gracia Ruiz and K.~Graf and C.~Guidi and S.~Hallmann and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernandez-Rey and J.~Hoessl and J.~Hofestaedt and F.~Huang and G.~Illuminati and C.~W.~James and B.~Jisse-Jung and M.~de Jong and P.~de Jong and M.~Kadler and O.~Kalekin and U.~Katz and N.R.~Khan-Chowdhury and A.~Kouchner and I.~Kreykenbohm and V.~Kulikovskiy and C.~Lagunas Gualda and R.~Lahmann and R.~Le Breton and S.~LeStum and D.~Lefevre and E.~Leonora and G.~Levi and M.~Lincetto and D.~Lopez-Coto and S.~Loucatos and L.~Maderer and J.~Manczak and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martinez-Mora and B.~Martino and K.~Melis and P.~Migliozzi and A.~Moussa and R.~Muller and L.~Nauta and S.~Navas and E.~Nezri and B.~O Fearraigh and A.~Paun and G.E.~Pavalas and C.~Pellegrino and M.~Perrin-Terrin and V.~Pestel and P.~Piattelli and C.~Pieterse and C.~Poire and V.~Popa and T.~Pradier and N.~Randazzo and D.~Real and S.~Reck and G.~Riccobene and A.~Romanov and F.~Sala and A.~Sanchez-Losa and F.~Salesa Greus and D.~F.~E.~Samtleben and M.~Sanguineti and P.~Sapienza and J.~Schnabel and J.~Schumann and F.~Schuessler and J.~Seneca and M.~Spurio and Th.~Stolarczyk and M.~Taiuti and Y.~Tayalati and S.J.~Tingay and B.~Vallage and V.~Van Elewyck and F.~Versari and S.~Viola and D.~Vivolo and J.~Wilms and S.~Zavatarelli and A.~Zegarelli and J.D.~Zornoza and J.~Zuniga}, title = {{S}earch for secluded dark matter towards the {G}alactic {C}entre with the {ANTARES} neutrino telescope}, year = {2022}, eprint = {2203.06029}, note = {arXiv:2203.06029v1} }
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Searches for dark matter (DM) have not provided any solid evidence for the existence of weakly interacting massive particles in the GeV-TeV mass range. Coincidentally, the scale of new physics is being pushed by collider searches well beyond the TeV domain. This situation strongly motivates the exploration of DM masses much larger than a TeV. Secluded scenarios contain a natural way around the unitarity bound on the DM mass, via the early matter domination induced by the mediator of its interactions with the Standard Model. High-energy neutrinos constitute one of the very few direct accesses to energy scales above a few TeV. An indirect search for secluded DM signals has been performed with the ANTARES neutrino telescope using data from 2007 to 2015. Upper limits on the DM annihilation cross section for DM masses up to 6 PeV are presented and discussed.
MiniBooNE and MicroBooNE Combined Fit to a 3+1 Sterile Neutrino Scenario
A. A. Aguilar-Arevalo, B. C. Brown, J. M. Conrad, R. Dharmapalan, A. Diaz, Z. Djurcic, D. A. Finley, R. Ford, G. T. Garvey, S. Gollapinni, A. Hourlier, E.-C. Huang, N. W. Kamp, G. Karagiorgi, T. Katori, T. Kobilarcik, K. Lin, W. C. Louis, C. Mariani, W. Marsh, et al (19)
Jan 06 2022 hep-ex hep-ph nucl-ex arXiv:2201.01724v2

@misc{2201.01724, author = {A.~A.~Aguilar-Arevalo and B.~C.~Brown and J.~M.~Conrad and R.~Dharmapalan and A.~Diaz and Z.~Djurcic and D.~A.~Finley and R.~Ford and G.~T.~Garvey and S.~Gollapinni and A.~Hourlier and E.-C.~Huang and N.~W.~Kamp and G.~Karagiorgi and T.~Katori and T.~Kobilarcik and K.~Lin and W.~C.~Louis and C.~Mariani and W.~Marsh and G.~B.~Mills and J.~Mirabal-Martinez and C.~D.~Moore and R.~H.~Nelson and J.~Nowak and Z.~Pavlovic and H.~Ray and B.~P.~Roe and A.~D.~Russell and A.~Schneider and M.~H.~Shaevitz and J.~Spitz and I.~Stancu and R.~Tayloe and R.~T.~Thornton and M.~Tzanov and R.~G.~Van de Water and D.~H.~White and E.~D.~Zimmerman}, title = {{M}ini{B}oo{NE} and {M}icro{B}oo{NE} {C}ombined {F}it to a 3+1 {S}terile {N}eutrino {S}cenario}, year = {2022}, eprint = {2201.01724}, note = {arXiv:2201.01724v2} }
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This letter presents the results from the MiniBooNE experiment within a full "3+1" scenario where one sterile neutrino is introduced to the three-active-neutrino picture. In addition to electron-neutrino appearance at short-baselines, this scenario also allows for disappearance of the muon-neutrino and electron-neutrino fluxes in the Booster Neutrino Beam, which is shared by the MicroBooNE experiment. We present the 3+1 fit to the MiniBooNE electron-(anti)neutrino and muon-(anti)neutrino data alone, and in combination with MicroBooNE electron-neutrino data. The best-fit parameters of the combined fit with the exclusive CCQE analysis (inclusive analysis) are $\Delta m^2 = 0.29 eV^2 (0.33 eV^2)$, $|U_{e4}|^2 = 0.016 (0.500)$, $|U_{\mu 4}|^2 = 0.500 (0.500)$, and $\sin^2(2\theta_{\mu e})=0.0316 (1.0)$. Comparing the no-oscillation scenario to the 3+1 model, the data prefer the 3+1 model with a $\Delta \chi^2/\text{dof} = 24.7 / 3 (17.3 / 3)$, a $4.3\sigma (3.4\sigma)$ preference assuming the asymptotic approximation given by Wilks' theorem.
Prospects for detecting axionlike particles at the Coherent CAPTAIN-Mills experiment
A.A. Aguilar-Arevalo, D.S.M. Alves, S. Biedron, J. Boissevain, M. Borrego, L. Bugel, M. Chavez-Estrada, J.M. Conrad, R.L. Cooper, A. Diaz, J.R. Distel, J.C. D'Olivo, E. Dunton, B. Dutta, D. Fields, J.R. Gochanour, M. Gold, E. Guardincerri, E.C. Huang, N. Kamp, et al (28)
Dec 21 2021 hep-ph hep-ex arXiv:2112.09979v5

@misc{2112.09979, author = {A.A.~Aguilar-Arevalo and D.S.M.~Alves and S.~Biedron and J.~Boissevain and M.~Borrego and L.~Bugel and M.~Chavez-Estrada and J.M.~Conrad and R.L.~Cooper and A.~Diaz and J.R.~Distel and J.C.~D'Olivo and E.~Dunton and B.~Dutta and D.~Fields and J.R.~Gochanour and M.~Gold and E.~Guardincerri and E.C.~Huang and N.~Kamp and D.~Kim and K.~Knickerbocker and W.C.~Louis and J.T.M.~Lyles and R.~Mahapatra and S.~Maludze and J.~Mirabal and N.~Mishra and D.~Newmark and P.~deNiverville and V.~Pandey and D.~Poulson and H.~Ray and E.~Renner and T.J.~Schaub and A.~Schneider and M.H.~Shaevitz and D.~Smith and W.~Sondheim and A.M.~Szelc and C.~Taylor and A.~Thompson and W.H.~Thompson and M.~Tripathi and R.T.~Thornton and R.~Van Berg and R.G.~Van de Water and S.~Verma}, title = {{P}rospects for detecting axionlike particles at the {C}oherent {CAPTAIN}-{M}ills experiment}, year = {2021}, eprint = {2112.09979}, howpublished = {Phys.Rev.D 107 (2023) 9, 095036}, doi = {10.1103/PhysRevD.107.095036}, note = {arXiv:2112.09979v5} }
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We show results from the Coherent CAPTAIN Mills (CCM) 2019 engineering run which begin to constrain regions of parameter space for axion-like particles (ALPs) produced in electromagnetic particle showers in an 800 MeV proton beam dump, and further investigate the sensitivity of ongoing data-taking campaigns for the CCM200 upgraded detector. Based on beam-on background estimates from the engineering run, we make realistic extrapolations for background reduction based on expected shielding improvements, reduced beam width, and analysis-based techniques for background rejection. We obtain reach projections for two classes of signatures; ALPs coupled primarily to photons can be produced in the tungsten target via the Primakoff process, and then produce a gamma-ray signal in the Liquid Argon (LAr) CCM detector either via inverse Primakoff scattering or decay to a photon pair. ALPs with significant electron couplings have several additional production mechanisms (Compton scattering, $e^+e^-$ annihilation, ALP-bremsstrahlung) and detection modes (inverse Compton scattering, external $e^+e^-$ pair conversion, and decay to $e^+e^-$). In some regions, the constraint is marginally better than both astrophysical and terrestrial constraints. With the beginning of a three year run, CCM will be more sensitive to this parameter space by up to an order of magnitude for both ALP-photon and ALP-electron couplings. The CCM experiment will also have sensitivity to well-motivated parameter space of QCD axion models. It is only a recent realization that accelerator-based large volume liquid argon detectors designed for low energy coherent neutrino and dark matter scattering searches are also ideal for probing ALPs in the unexplored $\sim$MeV mass scale.
Search for GeV-scale Dark Matter Annihilation in the Sun with IceCube DeepCore
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, J.M. Alameddine, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, G. Anton, C. Argüelles, Y. Ashida, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, et al (360)
Nov 22 2021 astro-ph.HE hep-ph arXiv:2111.09970v3

@misc{2111.09970, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and J.M.~Alameddine and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and M.~Boddenberg and F.~Bontempo and J.~Borowka and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and F.~Bradascio and J.~Braun and B.~Brinson and S.~Bron and J.~Brostean-Kaiser and S.~Browne and A.~Burgman and R.~T.~Burley and R.~S.~Busse and M.~A.~Campana and E.~G.~Carnie-Bronca and C.~Chen and Z.~Chen and D.~Chirkin and K.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and C.~Dappen and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and D.~Delgado López and H.~Dembinski and K.~Deoskar and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and M.~Dittmer and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and K.~L.~Fan and A.~R.~Fazely and A.~Fedynitch and N.~Feigl and S.~Fiedlschuster and A.~T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and S.~Griswold and C.~Günther and P.~Gutjahr and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and A.~Haungs and D.~Hebecker and K.~Helbing and F.~Henningsen and E.~C.~Hettinger and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and K.~Hymon and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and M.~Jin and B.~J.~P.~Jones and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and L.~Kardum and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and T.~Kozynets and E.~Kun and N.~Kurahashi and N.~Lad and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard and A.~Leszczyńska and Y.~Li and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and I.~C.~Mariş and I.~Martinez-Soler and R.~Maruyama and K.~Mase and T.~McElroy and F.~McNally and J.~V.~Mead and K.~Meagher and S.~Mechbal and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and A.~Obertacke Pollmann and M.~Oehler and B.~Oeyen and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and L.~Peters and J.~Peterson and S.~Philippen and S.~Pieper and M.~Pittermann and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and B.~Pries and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and P.~Reichherzer and R.~Reimann and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and E.~J.~Roberts and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and J.~Saffer and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Schaufel and H.~Schieler and S.~Schindler and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and G.~Schwefer and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and S.~Ter-Antonyan and S.~Tilav and F.~Tischbein and K.~Tollefson and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and C.~Walck and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and N.~Whitehorn and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and J.~P.~Yanez and S.~Yoshida and S.~Yu and T.~Yuan and Z.~Zhang and P.~Zhelnin}, title = {{S}earch for {G}e{V}-scale {D}ark {M}atter {A}nnihilation in the {S}un with {I}ce{C}ube {D}eep{C}ore}, year = {2021}, eprint = {2111.09970}, howpublished = {Phys. Rev. D 105, 062004 -- Published 21 March 2022}, doi = {10.1103/PhysRevD.105.062004}, note = {arXiv:2111.09970v3} }
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The Sun provides an excellent target for studying spin-dependent dark matter-proton scattering due to its high matter density and abundant hydrogen content. Dark matter particles from the Galactic halo can elastically interact with Solar nuclei, resulting in their capture and thermalization in the Sun. The captured dark matter can annihilate into Standard Model particles including an observable flux of neutrinos. We present the results of a search for low-energy ($<$ 500 GeV) neutrinos correlated with the direction of the Sun using 7 years of IceCube data. This work utilizes, for the first time, new optimized cuts to extend IceCube's sensitivity to dark matter mass down to 5 GeV. We find no significant detection of neutrinos from the Sun. Our observations exclude capture by spin-dependent dark matter-proton scattering with cross-section down to a few times $10^{-41}$ cm$^2$, assuming there is equilibrium with annihilation into neutrinos/anti-neutrinos for dark matter masses between 5 GeV and 100 GeV. These are the strongest constraints at GeV energies for dark matter annihilation directly to neutrinos.
Cascade Appearance Signatures of Sterile Neutrinos at 1-100 TeV
Benjamin R. Smithers, Benjamin J. P. Jones, Carlos A. Argüelles, Janet M. Conrad, Alejandro Diaz
Nov 18 2021 hep-ph astro-ph.HE hep-ex arXiv:2111.08722v3

@misc{2111.08722, author = {Benjamin R.~Smithers and Benjamin J.~P.~Jones and Carlos A.~Argüelles and Janet M.~Conrad and Alejandro Diaz}, title = {{C}ascade {A}ppearance {S}ignatures of {S}terile {N}eutrinos at 1-100 {T}e{V}}, year = {2021}, eprint = {2111.08722}, note = {arXiv:2111.08722v3} }
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Neutrino telescopes provide strong sensitivity to sterile neutrino oscillations through matter-enhanced oscillation, occurring in the few TeV energy range for eV$^{2}$-scale neutrino mass-squared splittings. Prior searches have focused on $\nu_\mu$ disappearance, which has a particularly strong sensitivity to the mixing angle $\theta_{24}$ via $\nu_\mu\rightarrow\nu_s$ transitions. Nowadays, the $\nu_\mu\rightarrow\nu_e$ and $\nu_\mu\rightarrow\nu_\tau$ appearance channels have been considered less promising at neutrino telescopes, due in part to the much smaller target volume for cascades relative to tracks. This work explores the detectability of these signatures at neutrino telescopes given present constraints on sterile neutrino mixing, and as an example, forecasts the sensitivity of the IceCube Neutrino Observatory to the mixing angles $\theta_{14}$, $\theta_{24}$, and $\theta_{34}$ in the 3+1 sterile neutrino model using the cascade channel with ten years of data. We find that $\nu_\tau$ appearance signatures consistent with the existing IceCube $\nu_\mu$ disappearance best-fit point are discoverable for values of $\theta_{34}$ consistent with world constraints, and that the sterile neutrino parameters favored by the BEST and gallium anomalies are expected to be testable at the 95\% confidence level.
Combined sensitivity of JUNO and KM3NeT/ORCA to the neutrino mass ordering
KM3NeT Collaboration, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, et al (257)
Aug 16 2021 hep-ex hep-ph arXiv:2108.06293v1

@misc{2108.06293, author = {KM3NeT Collaboration and S.~Aiello and A.~Albert and M.~Alshamsi and S.~Alves Garre and Z.~Aly and A.~Ambrosone and F.~Ameli and M.~Andre and G.~Androulakis and M.~Anghinolfi and M.~Anguita and M.~Ardid and S.~Ardid and J.~Aublin and C.~Bagatelas and B.~Baret and S.~Basegmez du Pree and M.~Bendahman and F.~Benfenati and E.~Berbee and A.M.~van den Berg and V.~Bertin and S.~Biagi and M.~Boettcher and M.~Bou Cabo and J.~Boumaaza and M.~Bouta and M.~Bouwhuis and C.~Bozza and H.Brânzaş and R.~Bruijn and J.~Brunner and R.~Bruno and E.~Buis and R.~Buompane and J.~Busto and B.~Caiffi and D.~Calvo and S.~Campion and A.~Capone and V.~Carretero and P.~Castaldi and S.~Celli and M.~Chabab and N.~Chau and A.~Chen and S.~Cherubini and V.~Chiarella and T.~Chiarusi and M.~Circella and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and M.~Colomer Molla and R.~Coniglione and P.~Coyle and A.~Creusot and A.~Cruz and G.~Cuttone and R.~Dallier and B.~De Martino and I.~Di Palma and A.F.~Díaz and D.~Diego-Tortosa and C.~Distefano and A.~Domi and C.~Donzaud and D.~Dornic and M.~Dörr and D.~Drouhin and T.~Eberl and A.~Eddyamoui and T.~van Eeden and D.~van Eijk and I.~El Bojaddaini and A.~Enzenhöfer and V.~Espinosa and P.~Fermani and G.~Ferrara and M.~D.~Filipovic and F.~Filippini and L.~A.~Fusco and T.~Gal and J.~García Méndez and A.~Garcia Soto and F.~Garufi and Y.~Gatelet and C.~Gatius and N.~Geisselbrecht and L.~Gialanella and E.~Giorgio and S.~R.~Gozzini and R.~Gracia and K.~Graf and G.~Grella and D.~Guderian and C.~Guidi and B.~Guillon and M.~Gutiérrez and J.~Haefner and S.~Hallmann and H.~Hamdaoui and H.~van Haren and A.~Heijboer and A.~Hekalo and L.~Hennig and J.~J.~Hernández-Rey and J.~Hofestädt and F.~Huang and W.~Idrissi Ibnsalih and G.~Illuminati and C.W.~James and M.~de Jong and P.~de Jong and B.~J.~Jung and P.~Kalaczynski and O.~Kalekin and U.~F.~Katz and N.~R.~Khan Chowdhury and G.~Kistauri and F.~van der Knaap and P.~Kooijman and A.~Kouchner and V.~Kulikovskiy and M.~Labalme and R.~Lahmann and M.~Lamoureux and G.~Larosa and C.~Lastoria and A.~Lazo and R.~Le Breton and S.~Le Stum and G.~Lehaut and O.~Leonardi and F.~Leone and E.~Leonora and N.~Lessing and G.~Levi and M.~Lincetto and M.~Lindsey Clark and T.~Lipreau and C.~Llorens Alvarez and F.~Longhitano and D.~Lopez-Coto and A.~Lygda and L.~Maderer and J.~Majumdar and J.~Mańczak and A.~Margiotta and A.~Marinelli and C.~Markou and L.~Martin and J.A.~Martínez-Mora and A.~Martini and F.~Marzaioli and S.~Mastroianni and K.W.~Melis and G.~Miele and P.~Migliozzi and E.~Migneco and P.~Mijakowski and L.~S.~Miranda and C.~M.~Mollo and M.~Moser and A.~Moussa and R.~Muller and M.~Musumeci and L.~Nauta and S.~Navas and C.A.~Nicolau and B.~Nkosi and B.~Ó Fearraigh and M.~O'Sullivan and M.~Organokov and A.~Orlando and J.~Palacios González and G.~Papalashvili and R.~Papaleo and A.~M.~Păun and G.E.~Păvălaş and C.~Pellegrino and M.~Perrin-Terrin and V.~Pestel and P.~Piattelli and C.~Pieterse and O.~Pisanti and C.~Poirè and V.~Popa and T.~Pradier and I.~Probst and S.~Pulvirenti and G.~Quéméner and N.~Randazzo and S.~Razzaque and D.~Real and S.~Reck and G.~Riccobene and A.~Romanov and A.~Rovelli and F.~Salesa Greus and D.~F.~E.~Samtleben and A.~Sánchez Losa and M.~Sanguineti and D.~Santonocito and P.~Sapienza and J.~Schnabel and M.F.~Schneider and J.~Schumann and H.~M.~Schutte and J.~Seneca and I.~Sgura and R.~Shanidze and A.~Sharma and A.~Sinopoulou and B.~Spisso and M.~Spurio and D.~Stavropoulos and S.M.~Stellacci and M.~Taiuti and Y.~Tayalati and H.~Thiersen and S.~Tingay and S.~Tsagkli and V.~Tsourapis and E.~Tzamariudaki and D.~Tzanetatos and V.~Van Elewyck and G.~Vasileiadis and F.~Versari and D.~Vivolo and G.~de Wasseige and J.~Wilms and R.~Wojaczyński and E.~de Wolf and T.~Yousfi and S.~Zavatarelli and A.~Zegarelli and D.~Zito and J.D.~Zornoza and J.~Zúñiga and N.~Zywucka and JUNO Collaboration members and S.~Ahmad and J.~P.~A.~M.~de André and E.~Baussan and C.~Bordereau and A.~Cabrera and C.~Cerna and G.~Donchenko and E.~A.~Doroshkevich and M.~Dracos and F.~Druillole and C.~Jollet and L.~N.~Kalousis and P.~Kampmann and K.~Kouzakov and A.~Lokhov and B.~K.~Lubsandorzhiev and S.~B.~Lubsandorzhiev and A.~Meregaglia and L.~Miramonti and F.~Perrot and L.~F.~Piñeres Rico and A.~Popov and R.~Rasheed and M.~Settimo and K.~Stankevich and H.~Steiger and M.~R.~Stock and A.~Studenikin and A.~Triossi and W.~Trzaska and M.~Vialkov and B.~Wonsak and J.~Wurtz and F.~Yermia}, title = {{C}ombined sensitivity of {JUNO} and {KM}3{N}e{T}/{ORCA} to the neutrino mass ordering}, year = {2021}, eprint = {2108.06293}, note = {arXiv:2108.06293v1} }
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This article presents the potential of a combined analysis of the JUNO and KM3NeT/ORCA experiments to determine the neutrino mass ordering. This combination is particularly interesting as it significantly boosts the potential of either detector, beyond simply adding their neutrino mass ordering sensitivities, by removing a degeneracy in the determination of $\Delta m_{31}^2$ between the two experiments when assuming the wrong ordering. The study is based on the latest projected performances for JUNO, and on simulation tools using a full Monte Carlo approach to the KM3NeT/ORCA response with a careful assessment of its energy systematics. From this analysis, a $5\sigma$ determination of the neutrino mass ordering is expected after 6 years of joint data taking for any value of the oscillation parameters. This sensitivity would be achieved after only 2 years of joint data taking assuming the current global best-fit values for those parameters for normal ordering.
All-flavor constraints on nonstandard neutrino interactions and generalized matter potential with three years of IceCube DeepCore data
IceCube Collaboration, R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, R. An, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, Y. Ashida, S. Axani, X. Bai, A. Balagopal V., et al (354)
Jun 16 2021 hep-ex hep-ph arXiv:2106.07755v2

@misc{2106.07755, author = {IceCube Collaboration and R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and R.~An and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and Y.~Ashida and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and F.~Bontempo and J.~Borowka and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and S.~Browne and A.~Burgman and R.~S.~Busse and M.~A.~Campana and C.~Chen and D.~Chirkin and K.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and H.~Erpenbeck and J.~Evans and P.~A.~Evenson and A.~R.~Fazely and S.~Fiedlschuster and A.T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and A.~Garcia and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and S.~Griswold and M.~Gündüz and C.~Günther and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and A.~Haungs and S.~Hauser and D.~Hebecker and K.~Helbing and F.~Henningsen and E.~C.~Hettinger and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and R.~Joppe and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and T.~Kontrimas and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and N.~Kurahashi and A.~Kyriacou and N.~Lad and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and J.~W.~Lee and K.~Leonard and A.~Leszczyńska and Y.~Li and M.~Lincetto and Q.~R.~Liu and M.~Liubarska and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and T.~McElroy and F.~McNally and K.~Meagher and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and J.~Micallef and D.~Mockler and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and L.~V.~Nguyên and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and L.~Paul and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and M.~Pittermann and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and B.~Pries and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and J.~Saffer and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and C.~Spannfellner and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and A.~Terliuk and S.~Tilav and F.~Tischbein and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and N.~Valtonen-Mattila and J.~Vandenbroucke and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and T.~B.~Watson and C.~Weaver and P.~Weigel and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and B.~J.~Whelan and N.~Whitehorn and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and S.~Yoshida and S.~Yu and T.~Yuan and Z.~Zhang}, title = {{A}ll-flavor constraints on nonstandard neutrino interactions and generalized matter potential with three years of {I}ce{C}ube {D}eep{C}ore data}, year = {2021}, eprint = {2106.07755}, howpublished = {Phys. Rev. D104(Oct, 2021) 072006}, doi = {10.1103/PhysRevD.104.072006}, note = {arXiv:2106.07755v2} }
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We report constraints on nonstandard neutrino interactions (NSI) from the observation of atmospheric neutrinos with IceCube, limiting all individual coupling strengths from a single dataset. Furthermore, IceCube is the first experiment to constrain flavor-violating and nonuniversal couplings simultaneously. Hypothetical NSI are generically expected to arise due to the exchange of a new heavy mediator particle. Neutrinos propagating in matter scatter off fermions in the forward direction with negligible momentum transfer. Hence the study of the matter effect on neutrinos propagating in the Earth is sensitive to NSI independently of the energy scale of new physics. We present constraints on NSI obtained with an all-flavor event sample of atmospheric neutrinos based on three years of IceCube DeepCore data. The analysis uses neutrinos arriving from all directions, with reconstructed energies between 5.6 GeV and 100 GeV. We report constraints on the individual NSI coupling strengths considered singly, allowing for complex phases in the case of flavor-violating couplings. This demonstrates that IceCube is sensitive to the full NSI flavor structure at a level competitive with limits from the global analysis of all other experiments. In addition, we investigate a generalized matter potential, whose overall scale and flavor structure are also constrained.
Explaining the MiniBooNE Excess Through a Mixed Model of Oscillation and Decay
Stefano Vergani, Nicholas W. Kamp, Alejandro Diaz, Carlos A. Argüelles, Janet M. Conrad, Michael H. Shaevitz, Melissa A. Uchida
May 14 2021 hep-ph hep-ex arXiv:2105.06470v5

@misc{2105.06470, author = {Stefano Vergani and Nicholas W.~Kamp and Alejandro Diaz and Carlos A.~Argüelles and Janet M.~Conrad and Michael H.~Shaevitz and Melissa A.~Uchida}, title = {{E}xplaining the {M}ini{B}oo{NE} {E}xcess {T}hrough a {M}ixed {M}odel of {O}scillation and {D}ecay}, year = {2021}, eprint = {2105.06470}, note = {arXiv:2105.06470v5} }
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The electron-like excess observed by the MiniBooNE experiment is explained with a model comprising a new low mass state ($\mathcal{O}(1)$ eV) participating in neutrino oscillations and a new high mass state ($\mathcal{O}(100)$ MeV) that decays to $\nu+\gamma$. Short-baseline oscillation data sets are used to predict the oscillation parameters. Fitting the MiniBooNE energy and scattering angle data, there is a narrow joint allowed region for the decay contribution at 95% CL. The result is a substantial improvement over the single sterile neutrino oscillation model, with $\Delta \chi^2/dof$ = 19.3/2 for a decay coupling of $2.8 \times 10^{-7}$ GeV$^{-1}$, high mass state of 376 MeV, oscillation mixing angle of $7\times 10^{-4}$ and mass splitting of $1.3$ eV$^2$. This model predicts that no clear oscillation signature will be observed in the FNAL short baseline program due to the low signal-level.
LeptonInjector and LeptonWeighter: A neutrino event generator and weighter for neutrino observatories
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, R. An, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, et al (346)
Dec 22 2020 physics.comp-ph hep-ex hep-ph arXiv:2012.10449v2

@misc{2012.10449, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and R.~An and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and R.~S.~Busse and M.~A.~Campana and C.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and J.~Evans and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and S.~Fiedlschuster and A.T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and C.~Glaser and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~A.~Harnisch and A.~Haungs and S.~Hauser and D.~Hebecker and K.~Helbing and F.~Henningsen and E.~C.~Hettinger and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and R.~Joppe and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kurahashi and A.~Kyriacou and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and F.~McNally and K.~Meagher and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and B.~Pries and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and M.~Renschler and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and A.~Sharma and S.~Shefali and M.~Silva and B.~Skrzypek and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and S.~Tilav and F.~Tischbein and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and M.~A.~Unland Elorrieta and N.~Valtonen-Mattila and J.~Vandenbroucke and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and S.~Yoshida and T.~Yuan and Z.~Zhang}, title = {{L}epton{I}njector and {L}epton{W}eighter: {A} neutrino event generator and weighter for neutrino observatories}, year = {2020}, eprint = {2012.10449}, note = {arXiv:2012.10449v2} }
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We present a high-energy neutrino event generator, called LeptonInjector, alongside an event weighter, called LeptonWeighter. Both are designed for large-volume Cherenkov neutrino telescopes such as IceCube. The neutrino event generator allows for quick and flexible simulation of neutrino events within and around the detector volume, and implements the leading Standard Model neutrino interaction processes relevant for neutrino observatories: neutrino-nucleon deep-inelastic scattering and neutrino-electron annihilation. In this paper, we discuss the event generation algorithm, the weighting algorithm, and the main functions of the publicly available code, with examples.
Detection of astrophysical tau neutrino candidates in IceCube
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, et al (345)
Nov 10 2020 hep-ex astro-ph.HE hep-ph arXiv:2011.03561v3

@misc{2011.03561, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and R.~S.~Busse and M.~A.~Campana and C.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and J.~Evans and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and S.~Fiedlschuster and A.T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~Haungs and S.~Hauser and D.~Hebecker and K.~Helbing and F.~Henningsen and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and R.~Joppe and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and F.~McNally and K.~Meagher and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and G.~Neer and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and M.~Renschler and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and S.~Shefali and M.~Silva and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and N.~L.~Strotjohann and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and S.~Tilav and F.~Tischbein and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and N.~Wandkowsky and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and T.~R.~Wood and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and S.~Yoshida and T.~Yuan and Z.~Zhang}, title = {{D}etection of astrophysical tau neutrino candidates in {I}ce{C}ube}, year = {2020}, eprint = {2011.03561}, howpublished = {Eur. Phys. J. C 82, 1031 (2022)}, doi = {10.1140/epjc/s10052-022-10795-y}, note = {arXiv:2011.03561v3} }
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High-energy tau neutrinos are rarely produced in atmospheric cosmic-ray showers or at cosmic particle accelerators, but are expected to emerge during neutrino propagation over cosmic distances due to flavor mixing. When high energy tau neutrinos interact inside the IceCube detector, two spatially separated energy depositions may be resolved, the first from the charged current interaction and the second from the tau lepton decay. We report a novel analysis of 7.5 years of IceCube data that identifies two candidate tau neutrinos among the 60 ``High-Energy Starting Events'' (HESE) collected during that period. The HESE sample offers high purity, all-sky sensitivity, and distinct observational signatures for each neutrino flavor, enabling a new measurement of the flavor composition. The measured astrophysical neutrino flavor composition is consistent with expectations, and an astrophysical tau neutrino flux is indicated at 2.8$\sigma$ significance.
The IceCube high-energy starting event sample: Description and flux characterization with 7.5 years of data
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, et al (346)
Nov 10 2020 astro-ph.HE hep-ex hep-ph arXiv:2011.03545v1

@misc{2011.03545, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and R.~S.~Busse and M.~A.~Campana and C.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and J.~Evans and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and S.~Fiedlschuster and A.T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~Haungs and S.~Hauser and D.~Hebecker and K.~Helbing and F.~Henningsen and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and R.~Joppe and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and T.~Katori and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and S.~Mandalia and I.~C.~Mariş and R.~Maruyama and K.~Mase and F.~McNally and K.~Meagher and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and G.~Neer and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and M.~Renschler and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and S.~Shefali and M.~Silva and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and N.~L.~Strotjohann and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and S.~Tilav and F.~Tischbein and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and J.~Vandenbroucke and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and N.~Wandkowsky and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and T.~R.~Wood and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and S.~Yoshida and T.~Yuan and Z.~Zhang}, title = {{T}he {I}ce{C}ube high-energy starting event sample: {D}escription and flux characterization with 7.5 years of data}, year = {2020}, eprint = {2011.03545}, note = {arXiv:2011.03545v1} }
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The IceCube Neutrino Observatory has established the existence of a high-energy all-sky neutrino flux of astrophysical origin. This discovery was made using events interacting within a fiducial region of the detector surrounded by an active veto and with reconstructed energy above 60 TeV, commonly known as the high-energy starting event sample, or HESE. We revisit the analysis of the HESE sample with an additional 4.5 years of data, newer glacial ice models, and improved systematics treatment. This paper describes the sample in detail, reports on the latest astrophysical neutrino flux measurements, and presents a source search for astrophysical neutrinos. We give the compatibility of these observations with specific isotropic flux models proposed in the literature as well as generic power-law-like scenarios. Assuming $\nu_e:\nu_\mu:\nu_\tau=1:1:1$, and an equal flux of neutrinos and antineutrinos, we find that the astrophysical neutrino spectrum is compatible with an unbroken power law, with a preferred spectral index of ${2.87}^{+0.20}_{-0.19}$ for the $68.3\%$ confidence interval.
Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, A. A. Alves Jr., N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, S. Axani, X. Bai, A. Balagopal V., A. Barbano, S. W. Barwick, B. Bastian, et al (345)
Nov 10 2020 hep-ex astro-ph.HE hep-ph arXiv:2011.03560v1

@misc{2011.03560, author = {R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and A.~A.~Alves Jr.~and N.~M.~Amin and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and S.~Axani and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and C.~Bellenghi and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and R.~S.~Busse and M.~A.~Campana and C.~Chen and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and J.~Evans and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and S.~Fiedlschuster and A.T.~Fienberg and K.~Filimonov and C.~Finley and L.~Fischer and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and P.~Fürst and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and A.~Ghadimi and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and S.~Goswami and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and M.~Ha Minh and K.~Hanson and J.~Hardin and A.~Haungs and S.~Hauser and D.~Hebecker and K.~Helbing and F.~Henningsen and S.~Hickford and J.~Hignight and C.~Hill and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and R.~Joppe and D.~Kang and W.~Kang and X.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and K.~Kin and T.~Kintscher and J.~Kiryluk and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kovacevich and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and C.~Lagunas Gualda and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and F.~McNally and K.~Meagher and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and R.~Naab and R.~Nagai and U.~Naumann and J.~Necker and G.~Neer and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and E.~O'Sullivan and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and M.~Renschler and G.~Renzi and E.~Resconi and S.~Reusch and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and G.~Roellinghoff and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and S.~Shefali and M.~Silva and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and N.~L.~Strotjohann and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and S.~Tilav and F.~Tischbein and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and J.~P.~Twagirayezu and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and N.~Wandkowsky and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and M.~Weyrauch and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and M.~Wolf and T.~R.~Wood and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and S.~Yoshida and T.~Yuan and Z.~Zhang}, title = {{M}easurement of the high-energy all-flavor neutrino-nucleon cross section with {I}ce{C}ube}, year = {2020}, eprint = {2011.03560}, note = {arXiv:2011.03560v1} }
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The flux of high-energy neutrinos passing through the Earth is attenuated due to their interactions with matter. The interaction rate is modulated by the neutrino interaction cross section and affects the flux arriving at the IceCube Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the Antarctic ice sheet. We present a measurement of the neutrino cross section between 60 TeV and 10 PeV using the high-energy starting events (HESE) sample from IceCube with 7.5 years of data. The result is binned in neutrino energy and obtained using both Bayesian and frequentist statistics. We find it compatible with predictions from the Standard Model. Flavor information is explicitly included through updated morphology classifiers, proxies for the the three neutrino flavors. This is the first such measurement to use the three morphologies as observables and the first to account for neutrinos from tau decay.
Updated MiniBooNE Neutrino Oscillation Results with Increased Data and New Background Studies
MiniBooNE Collaboration, A. A. Aguilar-Arevalo, B. C. Brown, J. M. Conrad, R. Dharmapalan, A. Diaz, Z. Djurcic, D. A. Finley, R. Ford, G. T. Garvey, S. Gollapinni, A. Hourlier, E. C. Huang, N. W. Kamp, G. Karagiorgi, T. Katori, T. Kobilarcik, K. Lin, W. C. Louis, C. Mariani, et al (22)
Jul 01 2020 hep-ex hep-ph nucl-ex arXiv:2006.16883v3

@misc{2006.16883, author = {MiniBooNE Collaboration and A.~A.~Aguilar-Arevalo and B.~C.~Brown and J.~M.~Conrad and R.~Dharmapalan and A.~Diaz and Z.~Djurcic and D.~A.~Finley and R.~Ford and G.~T.~Garvey and S.~Gollapinni and A.~Hourlier and E.~C.~Huang and N.~W.~Kamp and G.~Karagiorgi and T.~Katori and T.~Kobilarcik and K.~Lin and W.~C.~Louis and C.~Mariani and W.~Marsh and G.~B.~Mills and J.~Mirabal-Martinez and C.~D.~Moore and R.~H.~Nelson and J.~Nowak and I.~Parmaksiz and Z.~Pavlovic and H.~Ray and B.~P.~Roe and A.~D.~Russell and A.~Schneider and M.~H.~Shaevitz and H.~Siegel and J.~Spitz and I.~Stancu and R.~Tayloe and R.~T.~Thornton and M.~Tzanov and R.~G.~Van de Water and D.~H.~White and E.~D.~Zimmerman}, title = {{U}pdated {M}ini{B}oo{NE} {N}eutrino {O}scillation {R}esults with {I}ncreased {D}ata and {N}ew {B}ackground {S}tudies}, year = {2020}, eprint = {2006.16883}, howpublished = {Physical Review D103,052002 (2021)}, doi = {10.1103/PhysRevD.103.052002}, note = {arXiv:2006.16883v3} }
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The MiniBooNE experiment at Fermilab reports a total excess of $638.0 \pm 132.8$ electron-like events ($4.8 \sigma$) from a data sample corresponding to $18.75 \times 10^{20}$ protons-on-target in neutrino mode, which is a 46\% increase in the data sample with respect to previously published results, and $11.27 \times 10^{20}$ protons-on-target in antineutrino mode. The additional statistics allow several studies to address questions on the source of the excess. First, we provide two-dimensional plots in visible energy and cosine of the angle of the outgoing lepton, which can provide valuable input to models for the event excess. Second, we test whether the excess may arise from photons that enter the detector from external events or photons exiting the detector from $\pi^0$ decays in two model independent ways. Beam timing information shows that almost all of the excess is in time with neutrinos that interact in the detector. The radius distribution shows that the excess is distributed throughout the volume, while tighter cuts on the fiducal volume increase the significance of the excess. We conclude that models of the event excess based on entering and exiting photons are disfavored.
An eV-scale sterile neutrino search using eight years of atmospheric muon neutrino data from the IceCube Neutrino Observatory
M. G. Aartsen, R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, H. Bagherpour, X. Bai, A. Balagopal V., A. Barbano, et al (357)
May 28 2020 hep-ex hep-ph arXiv:2005.12942v4

@misc{2005.12942, author = {M.~G.~Aartsen and R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and N.~M.~Amin and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and J.~Auffenberg and S.~Axani and H.~Bagherpour and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and C.~Bohm and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and J.~Buscher and R.~S.~Busse and T.~Carver and C.~Chen and E.~Cheung and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and A.~Fedynitch and J.~Felde and A.~T.~Fienberg and K.~Filimonov and C.~Finley and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Günder and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and K.~Hanson and J.~Hardin and A.~Haungs and S.~Hauser and D.~Hebecker and D.~Heereman and P.~Heix and K.~Helbing and R.~Hellauer and F.~Henningsen and S.~Hickford and J.~Hignight and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and F.~Jonske and R.~Joppe and D.~Kang and W.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and T.~Kintscher and J.~Kiryluk and T.~Kittler and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and J.~Lünemann and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and G.~Maggi and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and R.~Maunu and F.~McNally and K.~Meagher and M.~Medici and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and T.~Meures and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and P.~Muth and R.~Nagai and U.~Naumann and G.~Neer and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and A.~O'Murchadha and E.~O'Sullivan and T.~Palczewski and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and E.~Pinat and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and L.~Rauch and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and B.~Relethford and M.~Renschler and G.~Renzi and E.~Resconi and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and S.~Shefali and M.~Silva and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and M.~Song and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and A.~Stößl and N.~L.~Strotjohann and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and A.~Terliuk and S.~Tilav and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and W.~Van Driessche and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and M.~Wallraff and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and L.~Wills and M.~Wolf and T.~R.~Wood and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and G.~Yodh and S.~Yoshida and T.~Yuan and Z.~Zhang and M.~Zöcklein}, title = {{A}n e{V}-scale sterile neutrino search using eight years of atmospheric muon neutrino data from the {I}ce{C}ube {N}eutrino {O}bservatory}, year = {2020}, eprint = {2005.12942}, howpublished = {Phys. Rev. Lett. 125, 141801 (2020)}, doi = {10.1103/PhysRevLett.125.141801}, note = {arXiv:2005.12942v4} }
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The results of a 3+1 sterile neutrino search using eight years of data from the IceCube Neutrino Observatory are presented. A total of 305,735 muon neutrino events are analyzed in reconstructed energy-zenith space to test for signatures of a matter-enhanced oscillation that would occur given a sterile neutrino state with a mass-squared differences between 0.01\u2009eV$^2$ and 100\u2009eV$^2$. The best-fit point is found to be at $\sin^2(2\theta_{24})=0.10$ and $\Delta m_{41}^2 = 4.5{\rm eV}^2$, which is consistent with the no sterile neutrino hypothesis with a p-value of 8.0\%.
Searching for eV-scale sterile neutrinos with eight years of atmospheric neutrinos at the IceCube neutrino telescope
M. G. Aartsen, R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, N. M. Amin, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, H. Bagherpour, X. Bai, A. Balagopal V., A. Barbano, et al (357)
May 28 2020 hep-ex hep-ph arXiv:2005.12943v2

@misc{2005.12943, author = {M.~G.~Aartsen and R.~Abbasi and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and N.~M.~Amin and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and J.~Auffenberg and S.~Axani and H.~Bagherpour and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Basu and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and C.~Bohm and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and J.~Buscher and R.~S.~Busse and T.~Carver and C.~Chen and E.~Cheung and D.~Chirkin and S.~Choi and B.~A.~Clark and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and A.~Desai and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and S.~Dharani and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and M.~A.~DuVernois and E.~Dvorak and T.~Ehrhardt and P.~Eller and R.~Engel and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and A.~Fedynitch and J.~Felde and A.~T.~Fienberg and K.~Filimonov and C.~Finley and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Günder and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and K.~Hanson and J.~Hardin and A.~Haungs and S.~Hauser and D.~Hebecker and D.~Heereman and P.~Heix and K.~Helbing and R.~Hellauer and F.~Henningsen and S.~Hickford and J.~Hignight and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and B.~J.~P.~Jones and F.~Jonske and R.~Joppe and D.~Kang and W.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and M.~Kellermann and J.~L.~Kelley and A.~Kheirandish and J.~Kim and T.~Kintscher and J.~Kiryluk and T.~Kittler and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and P.~Koundal and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and Y.~Li and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and A.~Ludwig and J.~Lünemann and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and G.~Maggi and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and R.~Maunu and F.~McNally and K.~Meagher and M.~Medici and A.~Medina and M.~Meier and S.~Meighen-Berger and J.~Merz and T.~Meures and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and P.~Muth and R.~Nagai and U.~Naumann and G.~Neer and L.~V.~Nguyen and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and A.~O'Murchadha and E.~O'Sullivan and T.~Palczewski and H.~Pandya and D.~V.~Pankova and N.~Park and G.~K.~Parker and E.~N.~Paudel and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and E.~Pinat and A.~Pizzuto and M.~Plum and Y.~Popovych and A.~Porcelli and M.~Prado Rodriguez and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and L.~Rauch and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and B.~Relethford and M.~Renschler and G.~Renzi and E.~Resconi and W.~Rhode and M.~Richman and B.~Riedel and S.~Robertson and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk Cantu and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Scharf and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and S.~Shefali and M.~Silva and B.~Smithers and R.~Snihur and J.~Soedingrekso and D.~Soldin and M.~Song and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and A.~Stößl and N.~L.~Strotjohann and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and A.~Terliuk and S.~Tilav and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and W.~Van Driessche and D.~van Eijk and N.~van Eijndhoven and D.~Vannerom and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and M.~Wallraff and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and D.~R.~Williams and L.~Wills and M.~Wolf and T.~R.~Wood and K.~Woschnagg and G.~Wrede and J.~Wulff and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and G.~Yodh and S.~Yoshida and T.~Yuan and Z.~Zhang and M.~Zöcklein}, title = {{S}earching for e{V}-scale sterile neutrinos with eight years of atmospheric neutrinos at the {I}ce{C}ube neutrino telescope}, year = {2020}, eprint = {2005.12943}, note = {arXiv:2005.12943v2} }
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We report in detail on searches for eV-scale sterile neutrinos, in the context of a 3+1 model, using eight years of data from the IceCube neutrino telescope. By analyzing the reconstructed energies and zenith angles of 305,735 atmospheric $\nu_\mu$ and $\bar{\nu}_\mu$ events we construct confidence intervals in two analysis spaces: $\sin^2 (2\theta_{24})$ vs. $\Delta m^2_{41}$ under the conservative assumption $\theta_{34}=0$; and $\sin^2(2\theta_{24})$ vs. $\sin^2 (2\theta_{34})$ given sufficiently large $\Delta m^2_{41}$ that fast oscillation features are unresolvable. Detailed discussions of the event selection, systematic uncertainties, and fitting procedures are presented. No strong evidence for sterile neutrinos is found, and the best-fit likelihood is consistent with the no sterile neutrino hypothesis with a p-value of 8\% in the first analysis space and 19\% in the second.
A search for IceCube events in the direction of ANITA neutrino candidates
IceCube Collaboration, M. G. Aartsen, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, P. Backes, H. Bagherpour, X. Bai, A. Balagopal V., A. Barbano, et al (341)
Jan 08 2020 astro-ph.HE hep-ph arXiv:2001.01737v2

@misc{2001.01737, author = {IceCube Collaboration and M.~G.~Aartsen and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and J.~Auffenberg and S.~Axani and P.~Backes and H.~Bagherpour and X.~Bai and A.~Balagopal V.~and A.~Barbano and S.~W.~Barwick and B.~Bastian and V.~Baum and S.~Baur and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and S.~BenZvi and D.~Berley and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and C.~Bohm and S.~Böser and O.~Botner and J.~Böttcher and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and J.~Buscher and R.~S.~Busse and T.~Carver and C.~Chen and E.~Cheung and D.~Chirkin and S.~Choi and K.~Clark and L.~Classen and A.~Coleman and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and E.~Dvorak and B.~Eberhardt and T.~Ehrhardt and P.~Eller and R.~Engel and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and J.~Felde and K.~Filimonov and C.~Finley and D.~Fox and A.~Franckowiak and E.~Friedman and A.~Fritz and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and K.~Ghorbani and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and D.~Grant and T.~Grégoire and Z.~Griffith and S.~Griswold and M.~Günder and M.~Gündüz and C.~Haack and A.~Hallgren and R.~Halliday and L.~Halve and F.~Halzen and K.~Hanson and A.~Haungs and D.~Hebecker and D.~Heereman and P.~Heix and K.~Helbing and R.~Hellauer and F.~Henningsen and S.~Hickford and J.~Hignight and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and T.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and M.~Jansson and G.~S.~Japaridze and M.~Jeong and K.~Jero and B.~J.~P.~Jones and F.~Jonske and R.~Joppe and D.~Kang and W.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Kheirandish and J.~Kim and T.~Kintscher and J.~Kiryluk and T.~Kittler and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and N.~Kurahashi and A.~Kyriacou and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and A.~Leszczyńska and M.~Leuermann and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and J.~Lünemann and W.~Luszczak and Y.~Lyu and W.~Y.~Ma and J.~Madsen and G.~Maggi and K.~B.~M.~Mahn and Y.~Makino and P.~Mallik and K.~Mallot and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and R.~Maunu and F.~McNally and K.~Meagher and M.~Medici and A.~Medina and M.~Meier and S.~Meighen-Berger and G.~Merino and T.~Meures and J.~Micallef and D.~Mockler and G.~Momenté and T.~Montaruli and R.~W.~Moore and R.~Morse and M.~Moulai and P.~Muth and R.~Nagai and U.~Naumann and G.~Neer and H.~Niederhausen and M.~U.~Nisa and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and M.~Oehler and A.~Olivas and A.~O'Murchadha and E.~O'Sullivan and T.~Palczewski and H.~Pandya and D.~V.~Pankova and N.~Park and P.~Peiffer and C.~Pérez de los Heros and S.~Philippen and D.~Pieloth and S.~Pieper and E.~Pinat and A.~Pizzuto and M.~Plum and A.~Porcelli and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and L.~Rauch and K.~Rawlins and I.~C.~Rea and A.~Rehman and R.~Reimann and B.~Relethford and M.~Renschler and G.~Renzi and E.~Resconi and W.~Rhode and M.~Richman and S.~Robertson and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Schaufel and H.~Schieler and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and F.~G.~Schröder and L.~Schumacher and S.~Sclafani and S.~Seunarine and S.~Shefali and M.~Silva and R.~Snihur and J.~Soedingrekso and D.~Soldin and M.~Song and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and A.~Stößl and N.~L.~Strotjohann and T.~Stürwald and T.~Stuttard and G.~W.~Sullivan and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and A.~Terliuk and S.~Tilav and K.~Tollefson and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and A.~Trettin and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and W.~Van Driessche and D.~van Eijk and N.~van Eijndhoven and J.~van Santen and S.~Verpoest and M.~Vraeghe and C.~Walck and A.~Wallace and M.~Wallraff and N.~Wandkowsky and T.~B.~Watson and C.~Weaver and A.~Weindl and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and L.~Wille and D.~R.~Williams and L.~Wills and M.~Wolf and J.~Wood and T.~R.~Wood and K.~Woschnagg and G.~Wrede and D.~L.~Xu and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and G.~Yodh and S.~Yoshida and T.~Yuan and M.~Zöcklein}, title = {{A} search for {I}ce{C}ube events in the direction of {ANITA} neutrino candidates}, year = {2020}, eprint = {2001.01737}, howpublished = {The Astrophysical Journal, Volume 892, Number 1 (2020)}, doi = {10.3847/1538-4357/ab791d}, note = {arXiv:2001.01737v2} }
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During the first three flights of the Antarctic Impulsive Transient Antenna (ANITA) experiment, the collaboration detected several neutrino candidates. Two of these candidate events were consistent with an ultra-high-energy up-going air shower and compatible with a tau neutrino interpretation. A third neutrino candidate event was detected in a search for Askaryan radiation in the Antarctic ice, although it is also consistent with the background expectation. The inferred emergence angle of the first two events is in tension with IceCube and ANITA limits on isotropic cosmogenic neutrino fluxes. Here, we test the hypothesis that these events are astrophysical in origin, possibly caused by a point source in the reconstructed direction. Given that any ultra-high-energy tau neutrino flux traversing the Earth should be accompanied by a secondary flux in the TeV-PeV range, we search for these secondary counterparts in seven years of IceCube data using three complementary approaches. In the absence of any significant detection, we set upper limits on the neutrino flux from potential point sources. We compare these limits to ANITA's sensitivity in the same direction and show that an astrophysical explanation of these anomalous events under standard model assumptions is severely constrained regardless of source spectrum.
Dark Matter Annihilation to Neutrinos
Carlos A. Argüelles, Alejandro Diaz, Ali Kheirandish, Andrés Olivares-Del-Campo, Ibrahim Safa, Aaron C. Vincent
Dec 23 2019 hep-ph astro-ph.HE arXiv:1912.09486v3

@misc{1912.09486, author = {Carlos A.~Argüelles and Alejandro Diaz and Ali Kheirandish and Andrés Olivares-Del-Campo and Ibrahim Safa and Aaron C.~Vincent}, title = {{D}ark {M}atter {A}nnihilation to {N}eutrinos}, year = {2019}, eprint = {1912.09486}, note = {arXiv:1912.09486v3} }
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We review the annihilation of dark matter into neutrinos over a range of dark matter masses from MeV$/c^2$ to ZeV$/c^2$. Thermally-produced models of dark matter are expected to self-annihilate to standard model products. As no such signal has yet been detected, we turn to neutrino detectors to constrain the ``most invisible channel.'' We review the experimental techniques that are used to detect neutrinos, and revisit the expected contributions to the neutrino flux at current and upcoming neutrino experiments. We place updated constraints on the dark matter self-annhilation cross section to neutrinos $\langle \sigma v \rangle$ using the most recently available data, and forecast the sensitivity of upcoming experiments such as Hyper-Kamiokande, DUNE, and IceCube Gen-2. Where possible, limits and projections are scaled to a single set of dark matter halo parameters for consistent comparison. We consider Galactic and extragalactic signals of $s$, $p$, and $d$-wave annihilation processes directly into neutrino pairs, yielding constraints that range from $\langle \sigma v \rangle \sim 2.5\times10^{-26}~{\rm cm}^3 {\rm s}^{-1}$ at 30 MeV$/c^2$ to $10^{-17}~{\rm cm}^3{\rm s}^{-1}$ at 10$^{11}$ GeV$/c^2$. Experiments that report directional and energy information of their events provide much stronger constraints, outlining the importance of making such data public.
Combining Sterile Neutrino Fits to Short Baseline Data with IceCube Data
M.H. Moulai, C.A. Argüelles, G.H. Collin, J.M. Conrad, A. Diaz, M.H. Shaevitz
Oct 31 2019 hep-ph hep-ex arXiv:1910.13456v2

@misc{1910.13456, author = {M.H.~Moulai and C.A.~Argüelles and G.H.~Collin and J.M.~Conrad and A.~Diaz and M.H.~Shaevitz}, title = {{C}ombining {S}terile {N}eutrino {F}its to {S}hort {B}aseline {D}ata with {I}ce{C}ube {D}ata}, year = {2019}, eprint = {1910.13456}, howpublished = {Phys. Rev. D 101, 055020, 2020}, doi = {10.1103/PhysRevD.101.055020}, note = {arXiv:1910.13456v2} }
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Recent global fits to short-baseline neutrino oscillation data have been performed finding preference for a sterile neutrino solution (3+1) over null. In the most recent iteration, it was pointed out that an unstable sterile neutrino (3+1+decay) may be a better description of the data. This is due to the fact that this model significantly reduces the tension between appearance and disappearance datasets. In this work, we add a one-year IceCube dataset to the global fit obtaining new results for the standard 3+1 and 3+1+decay sterile neutrino scenarios. We find that the 3+1+decay model provides a better fit than the 3+1, even in the presence of IceCube, with reduced appearance to disappearance tension. The 3+1+decay model is a 5.4$\sigma$ improvement over the null hypothesis and a 2.8$\sigma$ improvement over the standard 3+1 model.
Where Are We With Light Sterile Neutrinos?
A. Diaz, C.A. Argüelles, G.H. Collin, J.M. Conrad, M.H. Shaevitz
Jun 04 2019 hep-ex hep-ph arXiv:1906.00045v3

@misc{1906.00045, author = {A.~Diaz and C.A.~Argüelles and G.H.~Collin and J.M.~Conrad and M.H.~Shaevitz}, title = {{W}here {A}re {W}e {W}ith {L}ight {S}terile {N}eutrinos?}, year = {2019}, eprint = {1906.00045}, note = {arXiv:1906.00045v3} }
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We review the status of searches for sterile neutrinos in the $\sim 1$ eV range, with an emphasis on the latest results from short baseline oscillation experiments and how they fit within sterile neutrino oscillation models. We present global fit results to a three-active-flavor plus one-sterile-flavor model (3+1), where we find an improvement of $\Delta \chi^2=35$ for 3 additional parameters compared to a model with no sterile neutrino. This is a 5$\sigma$ improvement, indicating that an effect that is like that of a sterile neutrino is highly preferred by the data. However we note that separate fits to the appearance and disappearance oscillation data sets within a 3+1 model do not show the expected overlapping allowed regions in parameter space. This "tension" leads us to explore two options: 3+2, where a second additional mass state is introduced, and a 3+1+decay model, where the $\nu_4$ state can decay to invisible particles. The 3+1+decay model, which is also motivated by improving compatibility with cosmological observations, yields the larger improvement, with a $\Delta \chi^2=8$ for 1 additional parameter beyond the 3+1 model, which is a $2.6\sigma$ improvement. Moreover the tension between appearance and disappearance experiments is reduced compared to 3+1, although disagreement remains. In these studies, we use a frequentist approach and also a Bayesean method of finding credible regions. With respect to this tension, we review possible problems with the global fitting method. We note multiple issues, including problems with reproducing the experimental results, especially in the case of experiments that do not provide adequate data releases. We discuss an unexpected 5 MeV excess, observed in the reactor flux energy spectrum, that may be affecting the oscillation interpretation of the short baseline reactor data. We emphasize the care that must be taken in mapping to the true neutrino energy in the case of oscillation experiments that are subject to multiple interaction modes and nuclear effects. We point to problems with the "Parameter-Goodness-of-Fit test" that is used to quantify the tension. Lastly, we point out that analyses presenting limits often receive less scrutiny that signals. While we provide a snapshot of the status of sterile neutrino searches today and global fits to their interpretation, we emphasize that this is a fast-moving field. We briefly review experiments that are expected to report new data in the immediate future. Lastly, we consider the 5-year horizon, where we propose that decay-at-rest neutrino sources are the best method of finally resolving the confusing situation.
Development of an analysis to probe the neutrino mass ordering with atmospheric neutrinos using three years of IceCube DeepCore data
M. G. Aartsen, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, C. Alispach, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, P. Backes, H. Bagherpour, X. Bai, A. Barbano, S. W. Barwick, V. Baum, et al (316)
Feb 22 2019 hep-ex hep-ph arXiv:1902.07771v2

@misc{1902.07771, author = {M.~G.~Aartsen and M.~Ackermann and J.~Adams and J.~A.~Aguilar and M.~Ahlers and M.~Ahrens and C.~Alispach and K.~Andeen and T.~Anderson and I.~Ansseau and G.~Anton and C.~Argüelles and J.~Auffenberg and S.~Axani and P.~Backes and H.~Bagherpour and X.~Bai and A.~Barbano and S.~W.~Barwick and V.~Baum and R.~Bay and J.~J.~Beatty and K.-H.~Becker and J.~Becker Tjus and S.~BenZvi and D.~Berley and E.~Bernardini and E.~Bernardini and D.~Z.~Besson and G.~Binder and D.~Bindig and E.~Blaufuss and S.~Blot and C.~Bohm and M.~Börner and S.~Böser and O.~Botner and E.~Bourbeau and J.~Bourbeau and F.~Bradascio and J.~Braun and H.-P.~Bretz and S.~Bron and J.~Brostean-Kaiser and A.~Burgman and R.~S.~Busse and T.~Carver and C.~Chen and E.~Cheung and D.~Chirkin and K.~Clark and L.~Classen and G.~H.~Collin and J.~M.~Conrad and P.~Coppin and P.~Correa and D.~F.~Cowen and R.~Cross and P.~Dave and J.~P.~A.~M.~de André and C.~De Clercq and J.~J.~DeLaunay and H.~Dembinski and K.~Deoskar and S.~De Ridder and P.~Desiati and K.~D.~de Vries and G.~de Wasseige and M.~de With and T.~DeYoung and A.~Diaz and J.~C.~Díaz-Vélez and H.~Dujmovic and M.~Dunkman and E.~Dvorak and B.~Eberhardt and T.~Ehrhardt and P.~Eller and J.J.~Evans and P.~A.~Evenson and S.~Fahey and A.~R.~Fazely and J.~Felde and K.~Filimonov and C.~Finley and A.~Franckowiak and E.~Friedman and A.~Fritz and T.~K.~Gaisser and J.~Gallagher and E.~Ganster and S.~Garrappa and L.~Gerhardt and K.~Ghorbani and T.~Glauch and T.~Glüsenkamp and A.~Goldschmidt and J.~G.~Gonzalez and D.~Grant and Z.~Griffith and M.~Günder and M.~Gündüz and C.~Haack and A.~Hallgren and L.~Halve and F.~Halzen and K.~Hanson and D.~Hebecker and D.~Heereman and K.~Helbing and R.~Hellauer and F.~Henningsen and S.~Hickford and J.~Hignight and G.~C.~Hill and K.~D.~Hoffman and R.~Hoffmann and T.~Hoinka and B.~Hokanson-Fasig and K.~Hoshina and F.~Huang and M.~Huber and K.~Hultqvist and M.~Hünnefeld and R.~Hussain and S.~In and N.~Iovine and A.~Ishihara and E.~Jacobi and G.~S.~Japaridze and M.~Jeong and K.~Jero and B.~J.~P.~Jones and W.~Kang and A.~Kappes and D.~Kappesser and T.~Karg and M.~Karl and A.~Karle and U.~Katz and M.~Kauer and J.~L.~Kelley and A.~Kheirandish and J.~Kim and T.~Kintscher and J.~Kiryluk and T.~Kittler and S.~R.~Klein and R.~Koirala and H.~Kolanoski and L.~Köpke and C.~Kopper and S.~Kopper and D.~J.~Koskinen and M.~Kowalski and K.~Krings and G.~Krückl and N.~Kulacz and S.~Kunwar and N.~Kurahashi and A.~Kyriacou and M.~Labare and J.~L.~Lanfranchi and M.~J.~Larson and F.~Lauber and J.~P.~Lazar and K.~Leonard and M.~Leuermann and Q.~R.~Liu and E.~Lohfink and C.~J.~Lozano Mariscal and L.~Lu and F.~Lucarelli and J.~Lünemann and W.~Luszczak and J.~Madsen and G.~Maggi and K.~B.~M.~Mahn and Y.~Makino and K.~Mallot and S.~Mancina and I.~C.~Mariş and R.~Maruyama and K.~Mase and R.~Maunu and K.~Meagher and M.~Medici and A.~Medina and M.~Meier and S.~Meighen-Berger and T.~Menne and G.~Merino and T.~Meures and S.~Miarecki and J.~Micallef and G.~Momenté and T.~Montaruli and R.~W.~Moore and M.~Moulai and R.~Nagai and R.~Nahnhauer and P.~Nakarmi and U.~Naumann and G.~Neer and H.~Niederhausen and S.~C.~Nowicki and D.~R.~Nygren and A.~Obertacke Pollmann and A.~Olivas and A.~O'Murchadha and E.~O'Sullivan and T.~Palczewski and H.~Pandya and D.~V.~Pankova and N.~Park and P.~Peiffer and C.~Pérez de los Heros and D.~Pieloth and E.~Pinat and A.~Pizzuto and M.~Plum and P.~B.~Price and G.~T.~Przybylski and C.~Raab and A.~Raissi and M.~Rameez and L.~Rauch and K.~Rawlins and I.~C.~Rea and R.~Reimann and B.~Relethford and G.~Renzi and E.~Resconi and W.~Rhode and M.~Richman and S.~Robertson and M.~Rongen and C.~Rott and T.~Ruhe and D.~Ryckbosch and D.~Rysewyk and I.~Safa and S.~E.~Sanchez Herrera and A.~Sandrock and J.~Sandroos and M.~Santander and S.~Sarkar and S.~Sarkar and K.~Satalecka and M.~Schaufel and P.~Schlunder and T.~Schmidt and A.~Schneider and J.~Schneider and L.~Schumacher and S.~Sclafani and D.~Seckel and S.~Seunarine and M.~Silva and R.~Snihur and J.~Soedingrekso and D.~Soldin and S.~Söldner-Rembold and M.~Song and G.~M.~Spiczak and C.~Spiering and J.~Stachurska and M.~Stamatikos and T.~Stanev and A.~Stasik and R.~Stein and J.~Stettner and A.~Steuer and T.~Stezelberger and R.~G.~Stokstad and A.~Stößl and N.~L.~Strotjohann and T.~Stuttard and G.~W.~Sullivan and M.~Sutherland and I.~Taboada and F.~Tenholt and S.~Ter-Antonyan and A.~Terliuk and S.~Tilav and L.~Tomankova and C.~Tönnis and S.~Toscano and D.~Tosi and M.~Tselengidou and C.~F.~Tung and A.~Turcati and R.~Turcotte and C.~F.~Turley and B.~Ty and E.~Unger and M.~A.~Unland Elorrieta and M.~Usner and J.~Vandenbroucke and W.~Van Driessche and D.~van Eijk and N.~van Eijndhoven and S.~Vanheule and J.~van Santen and M.~Vraeghe and C.~Walck and A.~Wallace and M.~Wallraff and N.~Wandkowsky and T.~B.~Watson and C.~Weaver and M.~J.~Weiss and J.~Weldert and C.~Wendt and J.~Werthebach and S.~Westerhoff and B.~J.~Whelan and N.~Whitehorn and K.~Wiebe and C.~H.~Wiebusch and L.~Wille and D.~R.~Williams and L.~Wills and M.~Wolf and J.~Wood and T.~R.~Wood and K.~Woschnagg and G.~Wrede and S.~Wren and D.~L.~Xu and X.~W.~Xu and Y.~Xu and J.~P.~Yanez and G.~Yodh and S.~Yoshida and T.~Yuan}, title = {{D}evelopment of an analysis to probe the neutrino mass ordering with atmospheric neutrinos using three years of {I}ce{C}ube {D}eep{C}ore data}, year = {2019}, eprint = {1902.07771}, howpublished = {Eur. Phys. J C80, 9 (2020)}, doi = {10.1140/epjc/s10052-019-7555-0}, note = {arXiv:1902.07771v2} }
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The Neutrino Mass Ordering (NMO) remains one of the outstanding questions in the field of neutrino physics. One strategy to measure the NMO is to observe matter effects in the oscillation pattern of atmospheric neutrinos above $\sim 1\,\mathrm{GeV}$, as proposed for several next-generation neutrino experiments. Moreover, the existing IceCube DeepCore detector can already explore this type of measurement. We present rthe development and application of two independent analyses to search for the signature of the NMO with three years of DeepCore data. These analyses include a full treatment of systematic uncertainties and a statistically-rigorous method to determine the significance for the NMO from a fit to the data. Both analyses show that the dataset is fully compatible with both mass orderings. For the more sensitive analysis, we observe a preference for Normal Ordering with a $p$-value of $p_\mathrm{IO} = 15.3\%$ and $\mathrm{CL}_\mathrm{s}=53.3\%$ for the Inverted Ordering hypothesis, while the experimental results from both analyses are consistent within their uncertainties. Since the result is independent of the value of $\delta_\mathrm{CP}$ and obtained from energies $E_\nu \gtrsim 5\,\mathrm{GeV}$, it is complementary to recent results from long-baseline experiments. These analyses set the groundwork for the future of this measurement with more capable detectors, such as the IceCube Upgrade and the proposed PINGU detector.
Measuring the atmospheric neutrino oscillation parameters and constraining the 3+1 neutrino model with ten years of ANTARES data
ANTARES Collaboration, A. Albert, M. André, M. Anghinolfi, G. Anton, M. Ardid, J.-J. Aubert, J. Aublin, T. Avgitas, B. Baret, J. Barrios-Martí, S. Basa, B. Belhorma, V. Bertin, S. Biagi, R. Bormuth, J. Boumaaza, S. Bourret, M.C. Bouwhuis, H. Brânzaş, et al (116)
Dec 21 2018 hep-ex hep-ph arXiv:1812.08650v3

@misc{1812.08650, author = {ANTARES Collaboration and A.~Albert and M.~André and M.~Anghinolfi and G.~Anton and M.~Ardid and J.-J.~Aubert and J.~Aublin and T.~Avgitas and B.~Baret and J.~Barrios-Martí and S.~Basa and B.~Belhorma and V.~Bertin and S.~Biagi and R.~Bormuth and J.~Boumaaza and S.~Bourret and M.C.~Bouwhuis and H.~Brânzaş and R.~Bruijn and J.~Brunner and J.~Busto and A.~Capone and L.~Caramete and J.~Carr and S.~Celli and M.~Chabab and R.~Cherkaoui El Moursli and T.~Chiarusi and M.~Circella and A.~Coleiro and M.~Colomer and R.~Coniglione and H.~Costantini and P.~Coyle and A.~Creusot and A.~F.~Díaz and A.~Deschamps and C.~Distefano and I.~Di Palma and A.~Domi and R.~Donà and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and I.~El Bojaddaini and N.~El Khayati and D.~Elsässer and A.~Enzenhöfer and A.~Ettahiri and F.~Fassi and P.~Fermani and G.~Ferrara and L.~Fusco and P.~Gay and H.~Glotin and R.~Gozzini and T.~Grégoire and R.~Gracia Ruiz and K.~Graf and S.~Hallmann and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernández-Rey and J.~Hößl and J.~Hofestädt and G.~Illuminati and C.~W.~James and M.~de Jong and M.~Jongen and M.~Kadler and O.~Kalekin and U.~Katz and N.R.~Khan-Chowdhury and A.~Kouchner and M.~Kreter and I.~Kreykenbohm and V.~Kulikovskiy and C.~Lachaud and R.~Lahmann and R.~Le Breton and D.~Lefèvre and E.~Leonora and G.~Levi and M.~Lincetto and M.~Lotze and S.~Loucatos and G.~Maggi and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martínez-Mora and R.~Mele and K.~Melis and P.~Migliozzi and A.~Moussa and S.~Navas and E.~Nezri and C.~Nielsen and A.~Nuñez and M.~Organokov and G.E.~Păvălaş and C.~Pellegrino and M.~Perrin-Terrin and P.~Piattelli and V.~Popa and T.~Pradier and L.~Quinn and C.~Racca and N.~Randazzo and G.~Riccobene and A.~Sánchez-Losa and A.~Salah-Eddine and I.~Salvadori and D.~F.~E.~Samtleben and M.~Sanguineti and P.~Sapienza and F.~Schüssler and M.~Spurio and Th.~Stolarczyk and M.~Taiuti and Y.~Tayalati and T.~Thakore and A.~Trovato and B.~Vallage and V.~Van Elewyck and F.~Versari and S.~Viola and D.~Vivolo and J.~Wilms and D.~Zaborov and J.D.~Zornoza and J.~Zúñiga}, title = {{M}easuring the atmospheric neutrino oscillation parameters and constraining the 3+1 neutrino model with ten years of {ANTARES} data}, year = {2018}, eprint = {1812.08650}, note = {arXiv:1812.08650v3} }
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The ANTARES neutrino telescope has an energy threshold of a few tens of GeV. This allows to study the phenomenon of atmospheric muon neutrino disappearance due to neutrino oscillations. In a similar way, constraints on the 3+1 neutrino model, which foresees the existence of one sterile neutrino, can be inferred. Using data collected by the ANTARES neutrino telescope from 2007 to 2016, a new measurement of $\Delta m^2_{32}$ and $\theta_{23}$ has been performed - which is consistent with world best-fit values - and constraints on the 3+1 neutrino model have been derived.
Significant Excess of ElectronLike Events in the MiniBooNE Short-Baseline Neutrino Experiment
MiniBooNE Collaboration, A. A. Aguilar-Arevalo, B. C. Brown, L. Bugel, G. Cheng, J. M. Conrad, R. L. Cooper, R. Dharmapalan, A. Diaz, Z. Djurcic, D. A. Finley, R. Ford, F. G. Garcia, G. T. Garvey, J. Grange, E.-C. Huang, W. Huelsnitz, C. Ignarra, R. A. Johnson, G. Karagiorgi, et al (28)
May 31 2018 hep-ex hep-ph arXiv:1805.12028v2

@misc{1805.12028, author = {MiniBooNE Collaboration and A.~A.~Aguilar-Arevalo and B.~C.~Brown and L.~Bugel and G.~Cheng and J.~M.~Conrad and R.~L.~Cooper and R.~Dharmapalan and A.~Diaz and Z.~Djurcic and D.~A.~Finley and R.~Ford and F.~G.~Garcia and G.~T.~Garvey and J.~Grange and E.-C.~Huang and W.~Huelsnitz and C.~Ignarra and R.~A.~Johnson and G.~Karagiorgi and T.~Katori and T.~Kobilarcik and W.~C.~Louis and C.~Mariani and W.~Marsh and G.~B.~Mills and J.~Mirabal and J.~Monroe and C.~D.~Moore and J.~Mousseau and P.~Nienaber and J.~Nowak and B.~Osmanov and Z.~Pavlovic and D.~Perevalov and H.~Ray and B.~P.~Roe and A.~D.~Russell and M.~H.~Shaevitz and J.~Spitz and I.~Stancu and R.~Tayloe and R.~T.~Thornton and M.~Tzanov and R.~G.~Van de Water and D.~H.~White and D.~A.~Wickremasinghe and E.~D.~Zimmerman}, title = {{S}ignificant {E}xcess of {E}lectron{L}ike {E}vents in the {M}ini{B}oo{NE} {S}hort-{B}aseline {N}eutrino {E}xperiment}, year = {2018}, eprint = {1805.12028}, note = {arXiv:1805.12028v2} }
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The MiniBooNE experiment at Fermilab reports results from an analysis of $\nu_e$ appearance data from $12.84 \times 10^{20}$ protons on target in neutrino mode, an increase of approximately a factor of two over previously reported results. A $\nu_e$ charged-current quasielastic event excess of $381.2 \pm 85.2$ events ($4.5 \sigma$) is observed in the energy range $200<E_\nu^{QE}<1250$~MeV. Combining these data with the $\bar \nu_e$ appearance data from $11.27 \times 10^{20}$ protons on target in antineutrino mode, a total $\nu_e$ plus $\bar \nu_e$ charged-current quasielastic event excess of $460.5 \pm 99.0$ events ($4.7 \sigma$) is observed. If interpreted in a two-neutrino oscillation model, ${\nu}_{\mu} \rightarrow {\nu}_e$, the best oscillation fit to the excess has a probability of $21.1\%$, while the background-only fit has a $\chi^2$ probability of $6 \times 10^{-7}$ relative to the best fit. The MiniBooNE data are consistent in energy and magnitude with the excess of events reported by the Liquid Scintillator Neutrino Detector (LSND), and the significance of the combined LSND and MiniBooNE excesses is $6.0 \sigma$. A two-neutrino oscillation interpretation of the data would require at least four neutrino types and indicate physics beyond the three neutrino paradigm.Although the data are fit with a two-neutrino oscillation model, other models may provide better fits to the data.
Status of Sterile Neutrino fits with Global Data
Alejandro Diaz
Oct 13 2017 hep-ex hep-ph arXiv:1710.04360v2

@misc{1710.04360, author = {Alejandro Diaz}, title = {{S}tatus of {S}terile {N}eutrino fits with {G}lobal {D}ata}, year = {2017}, eprint = {1710.04360}, note = {arXiv:1710.04360v2} }
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A number of short baseline neutrino oscillation experiments have observed an anomalous excess of neutrinos in the low energy range. This may hint towards the existence of additional neutrino mass splittings. If true, additional sterile (non-interacting) neutrino states above the current 3 neutrino model would be required. On the other hand, many parameters of the allowed space are limited by experiments that have seen no anomaly. We will introduce models which accommodate these additional neutrinos, and then discuss our work towards fitting these models to the available global high $\Delta m^{2}$ oscillation data. We will then present the latest results of these fits.
Intrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the KM3NeT/ORCA detector
S. Adrián-Martínez, M. Ageron, S. Aiello, A. Albert, F. Ameli, E. G. Anassontzis, M. Andre, G. Androulakis, M. Anghinolfi, G. Anton, M. Ardid, T. Avgitas, G. Barbarino, E. Barbarito, B. Baret, J. Barrios-Martí, A. Belias, E. Berbee, A. van den Berg, V. Bertin, et al (233)
Dec 19 2016 physics.ins-det hep-ex hep-ph arXiv:1612.05621v2

@misc{1612.05621, author = {S.~Adrián-Martínez and M.~Ageron and S.~Aiello and A.~Albert and F.~Ameli and E.~G.~Anassontzis and M.~Andre and G.~Androulakis and M.~Anghinolfi and G.~Anton and M.~Ardid and T.~Avgitas and G.~Barbarino and E.~Barbarito and B.~Baret and J.~Barrios-Martí and A.~Belias and E.~Berbee and A.~van den Berg and V.~Bertin and S.~Beurthey and V.~van Beveren and N.~Beverini and S.~Biagi and A.~Biagioni and M.~Billault and M.~Bondì and R.~Bormuth and B.~Bouhadef and G.~Bourlis and S.~Bourret and C.~Boutonnet and M.~Bouwhuis and C.~Bozza and R.~Bruijn and J.~Brunner and E.~Buis and R.~Buompane and J.~Busto and G.~Cacopardo and L.~Caillat and M.~Calamai and D.~Calvo and A.~Capone and L.~Caramete and S.~Cecchini and S.~Celli and C.~Champion and S.~Cherubini and V.~Chiarella and T.~Chiarusi and M.~Circella and L.~Classen and D.~Cobas and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and S.~Colonges and R.~Coniglione and M.~Cordelli and A.~Cosquer and P.~Coyle and A.~Creusot and G.~Cuttone and C.~D'Amato and A.~D'Amico and A.~D'Onofrio and G.~De Bonis and C.~De Sio and I.~Di Palma and A.~F.~Díaz and C.~Distefano and C.~Donzaud and D.~Dornic and Q.~Dorosti-Hasankiadeh and E.~Drakopoulou and D.~Drouhin and M.~Durocher and T.~Eberl and S.~Eichie and D.~van Eijk and I.~El Bojaddaini and D.~Elsaesser and A.~Enzenhöfer and M.~Favaro and P.~Fermani and G.~Ferrara and G.~Frascadore and L.~A.~Fusco and T.~Gal and S.~Galatà and F.~Garufi and P.~Gay and M.~Gebyehu and F.~Giacomini and L.~Gialanella and V.~Giordano and N.~Gizani and R.~Gracia and K.~Graf and T.~Grégoire and G.~Grella and A.~Grmek and R.~Habel and S.~Hallmann and H.~van Haren and S.~Harissopulos and T.~Heid and A.~Heijboer and E.~Heine and S.~Henry and J.~J.~Hernández-Rey and M.~Hevinga and J.~Hofestädt and C.~M.~F.~Hugon and G.~Illuminati and C.~W.~James and P.~Jansweijer and M.~Jongen and M.~de Jong and M.~Kadler and O.~Kalekin and A.~Kappes and U.~F.~Katz and P.~Keller and G.~Kieft and D.~Kießling and E.~N.~Koffeman and P.~Kooijman and A.~Kouchner and M.~Kreter and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and A.~Leisos and F.~Leone and E.~Leonora and M.~Lindsey Clark and A.~Liolios and C.~D.~Llorens Alvarez and D.~Lo Presti and H.~Löhner and A.~Lonardo and M.~Lotze and S.~Loucatos and E.~Maccioni and K.~Mannheim and M.~Manzali and A.~Margiotta and A.~Marinelli and O.~Mariş and C.~Markou and J.~A.~Martínez-Mora and A.~Martini and F.~Marzaioli and R.~Mele and K.~W.~Melis and T.~Michael and P.~Migliozzi and E.~Migneco and P.~Mijakowski and A.~Miraglia and C.~M.~Mollo and M.~Mongelli and M.~Morganti and A.~Moussa and P.~Musico and M.~Musumeci and S.~Navas and C.~A.~Nicolau and I.~Olcina and C.~Olivetto and A.~Orlando and A.~Orzelli and A.~Papaikonomou and R.~Papaleo and G.~E.~Păvălaş and H.~Peek and G.~Pellegrini and C.~Pellegrino and C.~Perrina and M.~Pfutzner and P.~Piattelli and K.~Pikounis and M.-O.~Pleinert and G.~E.~Poma and V.~Popa and T.~Pradier and F.~Pratolongo and G.~Pühlhofer and S.~Pulvirenti and L.~Quinn and C.~Racca and F.~Raffaelli and N.~Randazzo and T.~Rauch and D.~Real and L.~Resvanis and J.~Reubelt and G.~Riccobene and C.~Rossi and A.~Rovelli and M.~Saldaña and I.~Salvadori and D.~F.~E.~Samtleben and A.~Sánchez García and A.~Sánchez Losa and M.~Sanguineti and A.~Santangelo and D.~Santonocito and P.~Sapienza and F.~Schimmel and J.~Schmelling and J.~Schnabel and V.~Sciacca and M.~Sedita and T.~Seitz and I.~Sgura and F.~Simeone and V.~Sipala and B.~Spisso and M.~Spurio and G.~Stavropoulos and J.~Steijger and S.~M.~Stellacci and D.~Stransky and M.~Taiuti and Y.~Tayalati and F.~Terrasi and D.~Tézier and S.~Theraube and P.~Timmer and C.~Tönnis and L.~Trasatti and R.~Travaglini and A.~Trovato and A.~Tsirigotis and S.~Tzamarias and E.~Tzamariudaki and B.~Vallage and V.~Van Elewyck and J.~Vermeulen and P.~Vicini and S.~Viola and D.~Vivolo and M.~Volkert and L.~Wiggers and J.~Wilms and E.~de Wolf and K.~Zachariadou and J.~D.~Zornoza and J.~Zúñiga}, title = {{I}ntrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the {KM}3{N}e{T}/{ORCA} detector}, year = {2016}, eprint = {1612.05621}, howpublished = {The KM3NeT collaboration, Adri{\'a}n-Mart{\'\i}nez, S., Ageron, M. et al. J. High Energ. Phys. (2017) 2017: 8}, doi = {10.1007/JHEP05(2017)008}, note = {arXiv:1612.05621v2} }
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Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA detector are investigated. These processes include the composition of the hadronic fragmentation products, the subsequent particle propagation and the photon-sampling fraction of the detector. GEANT simulations of neutrino interactions in seawater produced by GENIE are used to study the effects in the 1 - 20 GeV range. It is found that fluctuations in the hadronic cascade in conjunction with the variation of the inelasticity y are most detrimental to the resolutions. The effect of limited photon sampling in the detector is of significantly less importance. These results will therefore also be applicable to similar detectors/media, such as those in ice.