Light stops, blind spots, and isospin violation in the MSSM

Crivellin, Andreas; Hoferichter, Martin; Procura, Massimiliano; Tunstall, Lewis C.

doi:10.1007/jhep07(2015)129

Cited by 51 publications

(52 citation statements)

References 175 publications

(397 reference statements)

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“…On the other hand, we note that before applying these constraints, and even afterwards at the 95 % CL, there are values for σ SI p that go far below this neutrino 'floor', highlighting the complementarity of direct detection experiments and searches at the LHC. Since these very low values of σ SI p are due to cancellations between different contributions to the spinindependent scattering matrix element [138][139][140][141][142], one may ask whether the spin-independent cross sections on proton and neutron targets could be very different when this cancellation occurs [143,144]. More specifically, one may wonder whether, for models in which σ SI p is below the neutrino 'floor', the cross section σ SI n for scattering on a neutron target may be less suppressed, perhaps remaining above the neutrino 'floor'?…”

Section: Direct Dark Matter Detectionmentioning

confidence: 99%

The pMSSM10 after LHC run 1

et al. 2015

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We present a frequentist analysis of the parameter space of the pMSSM10, in which the following ten soft SUSY-breaking parameters are specified independently at the mean scalar top mass scale M SUSY ≡ √ mt 1 mt 2 :the gaugino masses M 1,2,3 , the first-and second-generation squark masses mq 1 = mq 2 , the third-generation squark mass mq 3 , a common slepton mass m˜ and a common trilinear mixing parameter A, as well as the Higgs mixing parameter μ, the pseudoscalar Higgs mass M A and tan β, the ratio of the two Higgs vacuum expectation values. We use the MultiNest sampling algorithm with ∼1.2 ×10 9 points to sample the pMSSM10 parameter space. A dedicated study shows that the sensitivities to strongly interacting sparticle masses of ATLAS and CMS searches for jets, leptons + / E T signals depend only weakly on many of the other pMSSM10 parameters. With the aid of the Atom and Scorpion codes, we also implement the LHC searches for electroweakly interacting sparticles and light stops, so as to confront the pMSSM10 parameter space with all relevant SUSY searches. In addition, our analysis includes Higgs mass and rate measurements using the HiggsSignals code, SUSY Higgs exclusion bounds, the measurements of BR(B s → μ + μ − ) by LHCb and CMS, other B-physics observables, electroweak precision observables, the cold dark matter density and the XENON100 and LUX searches for spin-independent dark matter scattering, assuming that the cold dark matter is mainly provided by the lightest neutralinoχ 0 1 . We show that the pMSSM10 is able to provide a supersymmetric interpretation of (g − 2) μ , unlike the CMSSM, NUHM1 and NUHM2. As a result, we find (omitting Higgs rates) that the minimum χ 2 = 20.5 with 18 degrees of freedom (d.o.f.) in the pMSSM10, corresponding to a χ 2 probability of 30.8 %, to be compared with χ 2 /d.o.f. = 32.8/24 (31.1/23) (30.3/22) in the CMSSM (NUHM1) (NUHM2). We display the one-dimensional likelihood functions for sparticle masses, and we show that they may be significantly lighter in the pMSSM10 than in the other models, e.g., the gluino may be as light as ∼1250 GeV at the 68 % CL, and squarks, stops, electroweak gauginos and sleptons may be much lighter than in the CMSSM, NUHM1 and NUHM2. We discuss the discovery potential of future LHC runs, e + e − colliders and direct detection experiments.

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Section: Direct Dark Matter Detectionmentioning

confidence: 99%

The pMSSM10 after LHC run 1

et al. 2015

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“…The discrepancy between the two values and its impact in the SI cross section is studied in more detail in Refs. [107,108].…”

Section: Implications For Direct Detectionmentioning

confidence: 99%

Dark matter protohalos in a nine parameter MSSM and implications for direct and indirect detection

2015

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Dark matter protohalos in a nine parameter MSSM and implications for direct and indirect detection Diamanti, R.; Cabrera Catalan, M.E.; Ando, S. General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. Download date: 24 Mar 2019Dark matter protohalos in a nine parameter MSSM and implications for direct and indirect detection We study how the kinetic decoupling of dark matter within a minimal supersymmetric extension of the standard model, by adopting nine independent parameters (MSSM-9), could improve our knowledge of the properties of the dark matter protohalos. We show that the most probable neutralino mass regions, which satisfy the relic density and the Higgs mass constraints, are those with the lightest supersymmetric neutralino mass around 1 TeV and 3 TeV, corresponding to Higgsino-like and winolike neutralino, respectively. The kinetic decoupling temperature in the MSSM-9 scenario leads to a most probable protohalo mass in a range of M ph ∼ 10 −12 -10 −7 M ⊙ . The part of the region closer to ∼2 TeV gives also important contributions from the neutralino-stau coannihilation, reducing the effective annihilation rate in the early Universe. We also study how the size of the smallest dark matter substructures correlates to experimental signatures, such as the spin-dependent and spin-independent scattering cross sections, relevant for direct detection of dark matter. Improvements on the spin-independent sensitivity might reduce the most probable range of the protohalo mass between ∼10 −9 M ⊙ and ∼10 −7 M ⊙ , while the expected spindependent sensitivity provides weaker constraints. We show how the boost of the luminosity due to dark matter annihilation increases, depending on the protohalo mass. In the Higgsino case, the protohalo mass is lower than the canonical value often used in the literature (∼10 −6 M ⊙ ), while hσvi does not deviate from hσvi ∼ 10 −26 cm 3 s −1 ; there is no significant enhancement of the luminosity. On the contrary, in the wino case, the protohalo mass is even lighter, and hσvi is two orders of magnitude larger; as its consequence, we see a substantial enhancement of the luminosity.

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“…3). This is a summary of a general analysis [7] concerning parameter space regions where the χ-nucleon scattering cross-section is strongly suppressed. A key feature of our work is that in the vicinity of these so-called blind spots [8,9], isospin-violation may be much larger than typically expected in the MSSM.…”

Section: The Dark Matter Puzzlementioning

confidence: 99%

“…In our work [7], we have examined several simplified models where all but a few superpartners are decoupled from the spectrum. Not only does this allow us to focus on dark matter signals of interest, it also allows us to develop an analytical framework with which to explore the underlying parameter space.…”

Section: Pos(cd15)088mentioning

confidence: 99%

“…Not only does this allow us to focus on dark matter signals of interest, it also allows us to develop an analytical framework with which to explore the underlying parameter space. Here we consider the effects of isospin violation in two simplified models [8,9] where χ-quark scattering is mediated by Higgs exchange in the t-channel: for an analysis of scenarios involving the exchange of light 3 rd generation squarks, we refer the reader to [7]. In these models, the lightest neutralino χ is an admixture of bino, wino, and Higgsino interaction eigenstates, obtained by diagonalising the mass matrix The simplest possible dark matter model in the MSSM consists of a light Higgs h with properties consistent with the SM, and a neutralino LSP which we assume to be predominantly bino-like, i.e.…”

Section: Pos(cd15)088mentioning

confidence: 99%

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Hadronic uncertainties and isospin violation in supersymmetric dark matter models

Tunstall¹,

Crivellin²,

Hoferichter³

et al. 2016

Proceedings of the 8th International Workshop on Chiral Dynamics — PoS(CD15)

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Current limits from dark matter direct-detection experiments place a powerful constraint on the parameter space of the Minimal Supersymmetric Standard Model (MSSM). The interpretation of these limits, however, depends sensitively on the hadronic uncertainties associated with the scattering of supersymmetric dark matter particles off nucleons. For spin-independent scattering, we review the role of 2-and 3-flavour chiral perturbation theory in the determination of these hadronic uncertainties, and quantify the amount of isospin violation within several simplified versions of the MSSM. In each case, we identify parameter-space configurations that produce (almost) vanishing cross sections and examine the complementarity of constraints due to directdetection, flavour, and collider experiments. In the vicinity of these so-called blind spots, we find that isospin violation may be much larger than typically expected in the MSSM.

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Light stops, blind spots, and isospin violation in the MSSM

Cited by 51 publications

References 175 publications

The pMSSM10 after LHC run 1

The pMSSM10 after LHC run 1

Dark matter protohalos in a nine parameter MSSM and implications for direct and indirect detection

Hadronic uncertainties and isospin violation in supersymmetric dark matter models

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