Light relic neutralinos

Bottino, A.; Fornengo, N.; Scopel, S.

doi:10.1103/physrevd.67.063519

Cited by 208 publications

(344 citation statements)

References 51 publications

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“…In the large tan β region, the contribution of such light Higgses can be sufficient to bring the relic density below the upper bound even if one is quite far from the s-channel pole due to the enhanced coupling of the Higgs to b quarks and τ 's. This opens up a new region of parameter space for light neutralinos (mχ0 1 < 18 GeV) as was pointed out in [74,39].…”

Section: Limits On the Lspmentioning

confidence: 88%

Lower limit on the neutralino mass in the general MSSM

Bélanger¹,

Boudjema²,

Cottrant³

et al. 2004

J. High Energy Phys.

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We discuss constraints on SUSY models with non-unified gaugino masses and R P conservation. We derive a lower bound on the neutralino mass combining the direct limits from LEP, the indirect limits from (g − 2) µ , b → sγ, B s → µ + µ − and the relic density constraint from WMAP. The lightest neutralino mχ0 1 ≈ 6 GeV is found in models with a light pseudoscalar with M A < 200 GeV and a large value for tan β. Models with heavy pseudoscalars lead to mχ0 1 > 18(29) GeV for tan β = 50(10). We show that even a very conservative bound from the muon anomalous magnetic moment can increase the lower bound on the neutralino mass in models with µ < 0 and/or large values of tan β. We then examine the potential of the Tevatron and the direct detection experiments to probe the SUSY models with the lightest neutralinos allowed in the context of light pseudoscalars with high tan β. We also examine the potential of an e + e − collider of 500 GeV to produce SUSY particles in all models with neutralinos lighter than the W . In contrast to the mSUGRA models, observation of at least one sparticle is not always guaranteed.

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Section: Limits On the Lspmentioning

confidence: 88%

Lower limit on the neutralino mass in the general MSSM

Bélanger¹,

Boudjema²,

Cottrant³

et al. 2004

J. High Energy Phys.

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“…Though such models formally violate the LEP lower bound on the mass of the lightest neutralino m χ > ∼ 50 GeV, this latter bound implicitly assumes gaugino mass unification at the GUT scale. When this assumption is dropped, m χ ≈ 5 GeV neutralinos remain a viable dark matter candidate [45]. It is seen, that with respect to SBBN, the 7 Li overproduction problem is hardly alleviated, while such models produce 6 Li in excess of that observed in Pop II stars.…”

Section: ) One Thusmentioning

confidence: 96%

Did something decay, evaporate, or annihilate during big bang nucleosynthesis?

Jedamzik

2004

Phys. Rev. D

246

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Results of a detailed examination of the cascade nucleosynthesis resulting from the putative hadronic decay, evaporation, or annihilation of a primordial relic during the Big Bang nucleosynthesis (BBN) era are presented. It is found that injection of energetic nucleons around cosmic time 10 3 sec may lead to an observationally favored reduction of the primordial 7 Li/H yield by a factor 2 − 3. Moreover, such sources also generically predict the production of the 6 Li isotope with magnitude close to the as yet unexplained high 6 Li abundances in low-metallicity stars. The simplest of these models operate at fractional contribution to the baryon density Ω b h 2 > ∼ 0.025, slightly larger than that inferred from standard BBN. Though further study is required, such sources, as for example due to the decay of the next-to-lightest supersymmetric particle into GeV gravitinos or the decay of an unstable gravitino in the TeV range of abundance ΩGh 2 ∼ 5 × 10 −4 show promise to explain both the 6 Li and 7 Li abundances in low metallicity stars.Big Bang nucleosynthesis has since long been known as one of the most precise and furthest back-reaching probes of cosmic conditions and the cosmic matter content of the early Universe. It thus, for example, has significantly contributed to the notion that a large fraction of matter in present-day galaxies is believed to be of non-baryonic nature as well as considerably limited some extensions of the standard model of particle physics. Paramount to having become such a useful tool of cosmology was and is, not only the examination of early synthesis of light elements in it's simplest standard version, but also in a variety of non-standard, alternative scenarios, relaxing a priori non-verified assumptions entering the calculations of a standard BBN (SBBN). Depending on the light element yields obtained in these latter scenarios, such calculations may then either favor a modified version of BBN, or strengthen the case for the SBBN. In either case, calculations of non-standard BBN may be used to place limits on the cosmic condition in the early Universe. In this spirit, technically advanced calculations of BBN including decaying particles during, or after BBN, an inhomogeneous baryon distribution, small-scale antimatter domains, neutrino degeneracy, or varying fundamental constants (for reviews cf.[1]), among others, have been performed over the years, rendering SBBN (also by the principle of Occam's razor) as our preferred scenario for BBN On the observational side significant advances have been made with the advent of high-resolution spectrographs on the Keck-and VLT-telescopes and the resulting capability to perform D/H abundance determinations of unprecedented accuracy in a few simple high-redshift quasar absorption line (QAL) systems. Furthermore an independent determination of the fractional contribution of baryons to the critical density, Ω b , from precision measurements of the cosmic microwave background radiation (CMB) by various balloon missions and the WMAP [2] sattelite has...

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“…is an attractive possibility, because the parameter space selected by this scenario unavoidably corresponds to a large scattering cross-section with nuclei (up to σ SI 10 −41 cm 2 ), so that the signals at DAMA [12,13], CoGeNT [14], CRESST-II [15] and the three events recently reported by CDMS [16] could be nicely explained [7,17,18,19]. However, recent LHC results exclude light DM in this parameter region of the MSSM.…”

Section: Light Neutralino Dm In the Mssmmentioning

confidence: 99%

“…As an illustration, in the left panel of Fig.5 we plot σ SI (weighted by ξ ≡ Ω DM h 2 /0.119) versus m χ 0 1 for m A = 2 TeV and the default micrOMEGAs value of the quark masses and the hadronic matrix elements. 7 As we can see, XENON100 already represents a relevant constraint on the light neutralino parameter space and the expected sensitivity of XENON1T has the potential of completely testing our scenario. We checked, however, that, if we allow m A to be O (10) TeV, the H contribution would finally decouple and the SI cross-section would be decreased by almost a factor of three, so that most of the points would escape from the XENON100 bound, although probably still being within the future XENON1T sensitivity.…”

Section: Direct and Indirect Dark Matter Searchesmentioning

confidence: 99%

Cornering light neutralino dark matter at the LHC

Calibbi

Lindert

Ota

et al. 2013

J. High Energ. Phys.

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We investigate the current status of the light neutralino dark matter scenario within the minimal supersymmetric standard model (MSSM) taking into account latest results from the LHC. A discussion of the relevant constraints, in particular from the dark matter relic abundance, leads us to a manageable simplified model defined by a subset of MSSM parameters. Within this simplified model we reinterpret a recent search for electroweak supersymmetric particle production based on a signature including multi-taus plus missing transverse momentum performed by the ATLAS collaboration. In this way we derive stringent constraints on the light neutralino parameter space. In combination with further experimental information from the LHC, such as dark matter searches in the monojet channel and constraints on invisible Higgs decays, we obtain a lower bound on the lightest neutralino mass of about 24 GeV. This limit is stronger than any current limit set by underground direct dark matter searches or indirect detection experiments. With a mild improvement of the sensitivity of the multi-tau search, light neutralino dark matter can be fully tested up to about 30 GeV.

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Light relic neutralinos

Cited by 208 publications

References 51 publications

Lower limit on the neutralino mass in the general MSSM

Lower limit on the neutralino mass in the general MSSM

Did something decay, evaporate, or annihilate during big bang nucleosynthesis?

Cornering light neutralino dark matter at the LHC

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