Improved limits on dark matter annihilation in the Sun with the 79-string IceCube detector and implications for supersymmetry

Aartsen, M. G.; Abraham, K.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, Tyler; Ansseau, I.; Anton, Gisela; Archinger, M.; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K.-H.; Beiser, E.; BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz, H.-P.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Collin, Gabriel; Conrad, J. M.; Cowen, D. F.; Silva, A. H.Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Rosendo, E. del Pino; Dembinski, H.-P.; Ridder, S. De; Desiati, P.; Vries, Krijn de; Wasseige, G. de; DeYoung, T.; Díaz-Vélez, J. C.; Lorenzo, V. di; Dumm, J. P.; Dunkman, M.; Eberhardt, B.; Edsjö, Joakim; Ehrhardt, Thomas; Eichmann, B.; Euler, S.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.; Fösig, C.-C.; Fuchs, T.; Gaisser, T. K.; Gaïor, R.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Gier, D.; Gladstone, L.; Glagla, M.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Góra, D.; Grant, D.; Griffith, Z.; Groß, A.; Ha, C.; Haack, Christian; Ismail, A. Haj; Hallgren, A.; Halzen, F.; Hansen, E.; Hansmann, B.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Holzapfel, K.; Homeier, A.; Hoshina, K.; Huang, F.; Huber, Matthías; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, Minjin; Jero, K.; Jones, B. J. P.; Jurković, M.; Kappes, A.; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kemp, J.; Kheirandish, Ali; Kiryluk, J.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Konietz, R.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, G.; Kroll, M.; Krückl, G.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leuner, J.; Lu, Lu; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, Kendall; Mandelartz, M.; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meier, Maximilian; Meli, A.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Middell, E.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Pollmann, A. Obertacke; Olivas, A.; Omairat, A.; O’Murchadha, A.; Palczewski, T.; Pandya, Hershal; Pankova, D. V.; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Quinnan, M.; Raab, Christoph; Rädel, L.; Rameez, M.; Rawlins, K.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Richter, S.; Riedel, Benedikt; Robertson, S.; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Sabbatini, L.; Sander, H. G.; Sandrock, A.; Sandroos, J.; Sarkar, S.; Savage, Christopher; Schatto, K.; Schimp, Michael; Schlunder, P.; Schmidt, T.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schulte, L.; Schumacher, Lisa Johanna; Scott, Pat; Seckel, D.; Seunarine, S.; Silverwood, H.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stahlberg, M.; Stamatikos, M.; Stanev, T.; Stasik, A.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola, H.; Taboada, I.; Tatar, J.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou, M.; Turcati, A.; Unger, E.; Usner, M.; Vallecorsa, S.; Vandenbroucke, J.; Eijndhoven, N. van; Vanheule, S.; Santen, J. V.; Veenkamp, J.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Yunlin; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zoll, M.

doi:10.1088/1475-7516/2016/04/022

Cited by 132 publications

(243 citation statements)

References 54 publications

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“…The IceCube limits for DM annihilating dominantly to W W , ZZ or tt are stronger than the XENON100 limits (on SD DM-neutron cross-section) for dark matter masses above about 100 GeV [34]. In the upper panels of figure 1 SD crosssections are shown with superimposed XENON100 and IceCube limits.…”

Section: Jhep03(2016)179mentioning

confidence: 91%

“…Upper panels: the solid lines show the LSP spindependent cross-section on neutrons (lower) and protons (upper) for positive (purple) and negative (cyan) values of parameter µ. The dashed and dotted lines denote the corresponding upper limits from, respectively, XENON100 [33] and IceCube [34] (see details in text). For all used experimental bounds we assume that the relic density of the LSP is equal to the observed value [7] (otherwise these bounds should be re-scaled by the ratio Ω observed /Ω LSP ).…”

Section: Without Scalar Mixingmentioning

confidence: 99%

“…The most stringent model independent upper bound on SD cross-section is provided by XENON100 for neutrons [33]. The limits on the SD DM-proton cross-section, provided by the indirect detection experiment IceCube [34], depend strongly on assumed dominant annihilation channels of dark matter particles. Generically in NMSSM with small tan β and decoupled scalars the singlino-dominated LSP annihilates mainly into tt (if the LSP mass is above the top quark mass) while the Higgsino-dominated LSP annihilates mainly into W W and ZZ -10 -…”

Section: Without Scalar Mixingmentioning

confidence: 99%

“…We have verified with MicrOMEGAs that for |κ| ∼ O(0.1) this is indeed the dominant annihilation channel for a singlino-dominated LSP. The IceCube collaboration [34] does not provide ) with the SI cross-section that can be below the neutrino background for m χ µ > 0 (red) and m χ µ < 0 (blue), while keeping 10 −3 ≤ |∆ mix | ≤ 1 GeV and 5·10 −3 ≤ |κ| ≤ 0.3. Right: the same as in the left panel but as a function of |µ| and fixed λ = 0.6.…”

Section: Jhep03(2016)179mentioning

confidence: 99%

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Blind spots for neutralino dark matter in the NMSSM

Badziak

Olechowski

Szczerbiak

2016

J. High Energ. Phys.

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Spin-independent cross-section for neutralino dark matter scattering off nuclei is investigated in the NMSSM. Several classes of blind spots for direct detection of singlinoHiggsino dark matter are analytically identified, including such that have no analog in the MSSM. It is shown that mixing of the Higgs doublets with the scalar singlet has a big impact on the position of blind spots in the parameter space. In particular, this mixing allows for more freedom in the sign assignment for the parameters entering the neutralino mass matrix, required for a blind spot to occur, as compared to the MSSM or the NMSSM with decoupled singlet. Moreover, blind spots may occur for any composition of a singlino-Higgsino LSP. Particular attention is paid to cases with the singlet-dominated scalar lighter than the 125 GeV Higgs for which a vanishing tree-level spin-independent scattering cross-section may result from destructive interference between the Higgs and the singlet-dominated scalar exchange. Correlations of the spin-independent scattering cross-section with the Higgs observables are also discussed.

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Section: Jhep03(2016)179mentioning

confidence: 91%

Section: Without Scalar Mixingmentioning

confidence: 99%

Section: Without Scalar Mixingmentioning

confidence: 99%

Section: Jhep03(2016)179mentioning

confidence: 99%

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Blind spots for neutralino dark matter in the NMSSM

Badziak

Olechowski

Szczerbiak

2016

J. High Energ. Phys.

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“…[18,19]), fully frequentist Neyman constructions are typically not possible. A popular alternative to Bayesian inference is to examine the priorindependent profile likelihood.…”

Section: Introductionmentioning

confidence: 99%

Comparison of statistical sampling methods with ScannerBit, the GAMBIT scanning module

Martinez¹,

McKay²,

Farmer³

et al. 2017

Eur. Phys. J. C

100

160

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We introduce ScannerBit, the statistics and sampling module of the public, open-source global fitting framework GAMBIT. ScannerBit provides a standardised interface to different sampling algorithms, enabling the use and comparison of multiple computational methods for inferring profile likelihoods, Bayesian posteriors, and other statistical quantities. The current version offers random, grid, raster, nested sampling, differential evolution, Markov Chain Monte Carlo (MCMC) and ensemble Monte Carlo samplers. We also announce the release of a new standalone differential evolution sampler, Diver, and describe its design, usage and interface to ScannerBit. We subject Diver and three other samplers (the nested sampler MultiNest, the MCMC GreAT, and the native ScannerBit implementation of the ensemble Monte Carlo algorithm T-Walk) to a battery of statistical tests. For this we use a realistic physical likelihood function, based on the scalar singlet model of dark matter. We examine the performance of each sampler as a function of its adjustable settings, and the dimensionality of the sampling problem. We evaluate performance on four metrics: optimality of the best fit found, completeness in exploring the best-fit region, number of likelihood evaluations, and total runtime. For Bayesian posterior estimation at high resolution, T-Walk provides the most accurate and timely mapping of the full parameter space. For profile likelihood analysis in less than about ten dimensions, we find that Diver and MultiNest score similarly in terms of best fit and speed, outperforming GreAT a

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Aspects of WIMP Dark Matter Searches at Colliders and Other Probes

Morgante

2017

Springer Theses

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UNIVERSITÉ DE GENÈVE FACULTÉ DES SCIENCES AbstractThe problem of Dark Matter is one of the most longstanding problems in cosmology and particle physics, and surely one of the most interesting. A number of astrophysical and cosmological evidences point to the existence of a large amount of non luminous matter, whose nature is still a mistery. The simplest possible solution to this puzzle is in terms of new neutral and stable particles with weak-scale mass and couplings (named WIMPs for weakly interacting massive particles), which would not only reproduce naturally the observed cosmological Dark Matter abundance, but also fit very well in many well-motivated theories for physics beyond the Standard Model. In this thesis I discuss the present status of WIMP searches and of our understanding of the theoretical issues involved in them, with a particular emphasis to searches at the Large Hadron Collider.iii iv ABSTRACT List of publicationsPapers that appear in this thesis [1] ResuméLe problème de la matière noire (DM, de l'anglais Dark Matter) peut être résumé comme suit : plusieurs anomalies ont été observées, depuis 1933, à partir des échelles galactiques jusqu'à celles des plus large structures, qu'on ne peut pas expliquer que par l'existence de quelques éléments pas lumineux qui constituent plus de 80% de la masse totale des galaxies et des amas de galaxies, ou sinon par quelques modifications supplé-mentaires de la Relativité Générale. La quelle des deux solutions est correcte est encore matière à débat, même si une modification du contenu de la matière est généralement considéré plus probable. De plus, c'est un résultat bien établi le fait que les objets astrophysiques exotiques peuvent constituer seulement une petite partie du total de la Matière noire contenu dans l'Univers, avec seulement quelques petites fenêtres laissées ouvertes par l'observation astrophysique. à cause de ça, la solution la plus plausible du puzzle semble être dans la forme des particules subatomiques.Notre connaissance actuelle de la physique des particules est fondée sur l'ainsi nommé Modèle Standard (SM). La seule candidate de DM dans le Modèle Standard est le neutrino, mais, comme on verra dans le chapitre 1.3, les neutrinos ne peuvent pas constituer toute la DM, et l'introduction des nouvelles particules est necessaire. Deux faits très intéressants se présentent à ce moment. D'un côté, un simple calcul de l'abondance de la DM dans le modèle du Big Bang chaud indique qu'une particule avec une masse et une constante de couplage typiques des interactions faibles aurait la juste abondance aujourd'hui. Cette coïncidence est appelée le "WIMP miracle", pour weakly interacting massive particle. De l'autre côté, le SM souffre l'ainsi nommé "problème de la hiérarchie de l'échelle électrofaible", ça veut dire que l'échelle électrofaible est instable contre les corrections quantiques et, en supposant que le SM n'est que la limite de basse energie d'une physique plus fondamentale, peut-être à l'échelle de Planck, un choix ajusté finement...

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Improved limits on dark matter annihilation in the Sun with the 79-string IceCube detector and implications for supersymmetry

Cited by 132 publications

References 54 publications

Blind spots for neutralino dark matter in the NMSSM

Blind spots for neutralino dark matter in the NMSSM

Comparison of statistical sampling methods with ScannerBit, the GAMBIT scanning module

Aspects of WIMP Dark Matter Searches at Colliders and Other Probes

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