Limits on Spin-Dependent WIMP-Nucleon Cross Sections from 225 Live Days of XENON100 Data

Aprile, E.; Alfonsi, M.; Arisaka, K.; Arneodo, F.; Bălan, C.; Baudis, L.; Bauermeister, B.; Behrens, A.; Beltrame, P.; Bokeloh, K.; Brown, A.; Brown, E.; Bruno, G.; Budnik, R.; Cardoso, J. M. R.; Chen, W. T.; Choi, Bernard C. K.; Colijn, A. P.; Contreras, H.; Cussonneau, J. P.; Decowski, M. P.; Duchovni, E.; Fattori, S.; Ferella, A. D.; Fulgione, W.; Gao, F.; Garbini, M.; Ghag, C.; Giboni, Karl; Goetzke, L. W.; Grignon, C.; Gross, E.; Hampel, W.; Kaether, F.; Kish, A.; Lamblin, J.; Landsman, H.; Lang, R. F.; Calloch, M. Le; Lellouch, D.; Lévy, C.; Lim, K. E.; Lin, Q.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Lung, K.; Undagoitia, T. Marrodán; Massoli, F. V.; Fernandez, A. J. Melgarejo; Meng, Y.; Messina, M.; Molinario, A.; Ni, K.; Oberlack, U.; Orrigo, S. E. A.; Pantic, E.; Persiani, R.; Plante, G.; Priel, N.; Rizzo, A.; Rosendahl, S. S.E.; Santos, J.M.F. dos; Sartorelli, G.; Schreiner, J.; Schümann, M.; Lavina, L. Scotto; Scovell, P. R.; Selvi, M.; Shagin, P.; Simgen, H.; Teymourian, A.; Thers, D.; Vitells, O.; Wang, H.; Weber, M.; Weinheimer, C.

doi:10.1103/physrevlett.111.021301

Cited by 258 publications

(268 citation statements)

References 53 publications

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“…Accelerator and direct detection experiments are most sensitive to DM particles with mass below a few hundred GeV. Positive results for signals of ∼10 GeV DM reported by some direct-searches experiments [7][8][9][10] could not be confirmed by other detectors, and are in tension with results obtained by XENON100 [11,12] and LUX [13]. On the other hand, the rather heavy Higgs boson [14] and the lack of indications of new physics at the Large Hadron Collider, strongly constrain the existence of a WIMP at the electroweak scale.…”

Section: Introductioncontrasting

confidence: 49%

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Aleksić

2016

Springer Theses

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Abstract. We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ∼500 GeV dark matter particle annihilating into τ + τ − , and is of order σ ann v ≃ 1.2×10 −24 cm 3 s −1 -a factor ∼40 above the σ ann v thermal value.

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Section: Introductioncontrasting

confidence: 49%

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Aleksić

2016

Springer Theses

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“…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%

“…On the other hand, this region may be probed with DM detection experiments sensitive to SD interactions. 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.…”

Section: Without Scalar Mixingmentioning

confidence: 99%

“…Green line correspond to the standard blind spot condition (4.2). Brown points on the green line for |µ| ≈ 120−250 GeV are excluded by the XENON100 constraints on the SD scattering cross-section [33] (see also figure 6). All points are consistent with the LHC Higgs data at 2σ.…”

Section: Jhep03(2016)179mentioning

confidence: 99%

“…Right: the same as in the left panel but as a function of |µ| for λ = 0.6. Black (brown) region is excluded by the XENON100 constraints on the SD scattering cross-section [33] for m χ µ < 0 (m χ µ > 0). All points are consistent with the LHC and LEP Higgs data at 2σ.…”

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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Dark matter searches

Baudis

2015

Annalen der Physik

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One of the major challenges of modern physics is to decipher the nature of dark matter. Astrophysical observations provide ample evidence for the existence of an invisible and dominant mass component in the observable universe, from the scales of galaxies up to the largest cosmological scales. The dark matter could be made of new, yet undiscovered elementary particles, with allowed masses and interaction strengths with normal matter spanning an enormous range. Axions, produced non-thermally in the early universe, and weakly interacting massive particles (WIMPs), which froze out of thermal equilibrium with a relic density matching the observations, represent two well-motivated, generic classes of dark matter candidates. Dark matter axions could be detected by exploiting their predicted coupling to two photons, where the highest sensitivity is reached by experiments using a microwave cavity permeated by a strong magnetic field. WIMPs could be directly observed via scatters off atomic nuclei in underground, ultra low-background detectors, or indirectly, via secondary radiation produced when they pair annihilate. They could also be generated at particle colliders such as the LHC, where associated particles produced in the same process are to be detected. After a brief motivation and an introduction to the phenomenology of particle dark matter detection, I will discuss the most promising experimental techniques to search for axions and WIMPs, addressing their current and future science reach, as well as their complementarity.Comment: 10 pages, 8 figure

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Limits on Spin-Dependent WIMP-Nucleon Cross Sections from 225 Live Days of XENON100 Data

Cited by 258 publications

References 53 publications

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Blind spots for neutralino dark matter in the NMSSM

Dark matter searches

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