002008528 001__ 2008528
002008528 003__ SzGeCERN
002008528 005__ 20220813042159.0
002008528 0248_ $$aoai:cds.cern.ch:2008528$$pcerncds:CERN$$pcerncds:CERN:FULLTEXT$$pcerncds:FULLTEXT
002008528 0247_ $$2DOI$$a10.1103/PhysRevD.92.015011
002008528 035__ $$9arXiv$$aoai:arXiv.org:1504.02486
002008528 035__ $$9Inspire$$a1358942
002008528 037__ $$9arXiv$$aarXiv:1504.02486$$chep-ph
002008528 037__ $$aCERN-PH-TH-2015-078
002008528 041__ $$aeng
002008528 088__ $$aCERN-PH-TH-2015-078
002008528 084__ $$2CERN Library$$aTH-2015-078
002008528 100__ $$aDelgado, Antonio$$uCERN$$uNotre Dame U.$$vTheory Division, Physics Department , CERN, CH-1211 Geneva 23, Switzerland$$vDepartment of Physics, University of Notre Dame , 225 Nieuwland Science Hall, Notre Dame, Indiana 46556, USA
002008528 245__ $$aDark Matter from the Supersymmetric Custodial Triplet Model
002008528 269__ $$aGeneva$$bCERN$$c09 Apr 2015
002008528 260__ $$c2015-07-14
002008528 300__ $$a16 p
002008528 500__ $$aComments: 26 pages, 8 figures
002008528 500__ $$9arXiv$$a26 pages, 8 figures; v2 revised comments on classification method and indirect detection section. Results unchanged, matches PRD published version
002008528 520__ $$aThe Supersymmetric Custodial Triplet Model (SCTM) adds to the particle content of the MSSM three $SU(2)_L$ triplet chiral superfields with hypercharge $Y=(0,\pm1)$. At the superpotential level the model respects a global $SU(2)_L \otimes SU(2)_R$ symmetry only broken by the Yukawa interactions. The pattern of vacuum expectation values of the neutral doublet and triplet scalar fields depends on the symmetry pattern of the Higgs soft breaking masses. We study the cases where this symmetry is maintained in the Higgs sector, and when it is broken only by the two doublets attaining different vacuum expectation values. In the former case, the symmetry is spontaneously broken down to the vectorial subgroup $SU(2)_V$ and the $\rho$ parameter is protected by the custodial symmetry. However in both situations the $\rho$ parameter is protected at tree level, allowing for light triplet scalars with large vacuum expectation values. We find that over a large range of parameter space, a light neutralino can supply the correct relic abundance of dark matter either through resonant s-channel triplet scalar funnels or well tempering of the Bino with the triplet fermions. Direct detection experiments have trouble probing these model points because the custodial symmetry suppresses the coupling of the neutralino and the $Z$ and a small Higgsino component of the neutralino suppresses the coupling with the Higgs. Likewise the annihilation cross sections for indirect detection lie below the Fermi-LAT upper bounds for the different channels.
002008528 520__ $$9APS$$aThe supersymmetric custodial triplet model adds to the particle content of the minimal supersymmetric standard model three SU(2)L triplet chiral superfields with hypercharge Y=(0,±1). At the superpotential level, the model respects a global SU(2)L⊗SU(2)R symmetry only broken by the Yukawa interactions. The pattern of vacuum expectation values of the neutral doublet and triplet scalar fields depends on the symmetry pattern of the Higgs soft breaking masses. We study the cases in which this symmetry is maintained in the Higgs sector and in which it is broken only by the two doublets attaining different vacuum expectation values. In the former case, the symmetry is spontaneously broken down to the vectorial subgroup SU(2)V, and the ρ parameter is protected by the custodial symmetry. However, in both situations, the ρ parameter is protected at tree level, allowing for light triplet scalars with large vacuum expectation values. We find that over a large range of parameter space a light neutralino can supply the correct relic abundance of dark matter either through resonant s-channel triplet scalar funnels or well tempering of the Bino with the triplet fermions. Direct detection experiments have trouble probing these model points because the custodial symmetry suppresses the coupling of the neutralino and the Z, and a small Higgsino component of the neutralino suppresses the coupling with the Higgs. Likewise, the annihilation cross sections for indirect detection lie below the Fermi-LAT upper bounds for the different channels.
002008528 520__ $$9arXiv$$aThe Supersymmetric Custodial Triplet Model (SCTM) adds to the particle content of the MSSM three $SU(2)_L$ triplet chiral superfields with hypercharge $Y=(0,\pm1)$. At the superpotential level the model respects a global $SU(2)_L \otimes SU(2)_R$ symmetry only broken by the Yukawa interactions. The pattern of vacuum expectation values of the neutral doublet and triplet scalar fields depends on the symmetry pattern of the Higgs soft breaking masses. We study the cases where this symmetry is maintained in the Higgs sector, and when it is broken only by the two doublets attaining different vacuum expectation values. In the former case, the symmetry is spontaneously broken down to the vectorial subgroup $SU(2)_V$ and the $\rho$ parameter is protected by the custodial symmetry. However in both situations the $\rho$ parameter is protected at tree level, allowing for light triplet scalars with large vacuum expectation values. We find that over a large range of parameter space, a light neutralino can supply the correct relic abundance of dark matter either through resonant s-channel triplet scalar funnels or well tempering of the Bino with the triplet fermions. Direct detection experiments have trouble probing these model points because the custodial symmetry suppresses the coupling of the neutralino and the $Z$ and a small Higgsino component of the neutralino suppresses the coupling with the Higgs. Likewise the annihilation cross sections for indirect detection lie below the Fermi-LAT upper bounds for the different channels.
002008528 540__ $$aarXiv nonexclusive-distrib. 1.0$$barXiv$$uhttp://arxiv.org/licenses/nonexclusive-distrib/1.0/
002008528 540__ $$3preprint$$aCC-BY-4.0
002008528 540__ $$3publication$$aCC-BY-3.0
002008528 542__ $$3preprint$$dCERN$$g2015
002008528 542__ $$3publication$$dThe Author(s)$$g2015
002008528 595__ $$aOA
002008528 595__ $$aCERN-TH
002008528 595__ $$aLANL EDS
002008528 65017 $$2arXiv$$aParticle Physics - Phenomenology
002008528 695__ $$9LANL EDS$$ahep-ph
002008528 690C_ $$aARTICLE
002008528 690C_ $$aCERN
002008528 700__ $$aGarcia-Pepin, Mateo$$uBarcelona, IFAE$$vInstitut de Física d’Altes Energies, Universitat Autònoma de Barcelona , 08193 Bellaterra, Barcelona, Spain
002008528 700__ $$aOstdiek, Bryan$$iINSPIRE-00378886$$uNotre Dame U.$$vDepartment of Physics, University of Notre Dame , 225 Nieuwland Science Hall, Notre Dame, Indiana 46556, USA
002008528 700__ $$aQuiros, Mariano$$uBarcelona, IFAE$$uICREA, Barcelona$$vInstitució Catalana de Recerca i Estudis Avançats (ICREA) and Institut de Física d’Altes Energies, Universitat Autònoma de Barcelona , 08193 Bellaterra, Barcelona, Spain$$vInstitut de Física d’Altes Energies, Universitat Autònoma de Barcelona , 08193 Bellaterra, Barcelona, Spain
002008528 710__ $$5PH-TH
002008528 773__ $$c015011$$oPhys. Rev. D 92, 015011 (2015)$$pPhys. Rev. D$$v92$$y2015
002008528 8564_ $$uhttp://arxiv.org/pdf/1504.02486.pdf$$yPreprint
002008528 8564_ $$81083385$$s1127335$$uhttp://cds.cern.ch/record/2008528/files/arXiv:1504.02486.pdf
002008528 8564_ $$81083374$$s100561$$uhttp://cds.cern.ch/record/2008528/files/CompPlot.png$$y00005 Composition of the LSP in terms of gauge eigenstates. The top row shows $\tan\beta=1$ and the bottom shows $\tan\beta=2$. The columns correspond to $\mu=(200,250,400)~\gev$ respectively while the tripletino mass is set to $\mu_{\Delta}=250~\gev$. The Wino has been decoupled with $M_2=1~\tev$. Note in top middle and top right plots the presence of a triplet like eigenvalue, which is totally decoupled from the rest of the neutralino mass matrix, made out of only $\tilde{\psi},\tilde{\phi}$ and $\tilde{\chi}$. It corresponds to an $SU(2)_V$ fiveplet in the custodial basis.
002008528 8564_ $$81083377$$s12205$$uhttp://cds.cern.ch/record/2008528/files/lambdaplotMax.png$$y00001 Top row: Maximal values of $v_{\Delta}$ which allow $\lambda$ to set the Higgs mass to $125~\gev$ and yield a minimized potential as a function of $\mu$. Bottom: Value of $\lambda$ needed to attain the observed Higgs mass for $v_{\Delta}=10~\gev$. The triplet supersymmetric mass is set to $\mu_{\Sigma}=250~\gev$, and the other values are as Eq.~\eqref{eqn:benchmark}.
002008528 8564_ $$81083382$$s1263$$uhttp://cds.cern.ch/record/2008528/files/SpectrumLegend.png$$y00004 The left panels show the spectrum of the neutral light scalars when $v_{\Delta}=10~\gev$ and $\lambda$ is changed to set the Higgs mass. The right panels use the maximum allowed value for $v_{\Delta}$ for each $\mu$ value. The upper (lower) panels contain $\tan\beta=1$ ($\tan\beta=2$). Changing $\tan\beta$ greatly affects the mass of $H_2^0$ and $A_2^0$ but $H_3^0$'s mass is similar for both choices.
002008528 8564_ $$81083380$$s12918$$uhttp://cds.cern.ch/record/2008528/files/lambdaplotConst.png$$y00002 Top row: Maximal values of $v_{\Delta}$ which allow $\lambda$ to set the Higgs mass to $125~\gev$ and yield a minimized potential as a function of $\mu$. Bottom: Value of $\lambda$ needed to attain the observed Higgs mass for $v_{\Delta}=10~\gev$. The triplet supersymmetric mass is set to $\mu_{\Sigma}=250~\gev$, and the other values are as Eq.~\eqref{eqn:benchmark}.
002008528 8564_ $$81083383$$s1710$$uhttp://cds.cern.ch/record/2008528/files/LegendCompPlot.png$$y00006 Composition of the LSP in terms of gauge eigenstates. The top row shows $\tan\beta=1$ and the bottom shows $\tan\beta=2$. The columns correspond to $\mu=(200,250,400)~\gev$ respectively while the tripletino mass is set to $\mu_{\Delta}=250~\gev$. The Wino has been decoupled with $M_2=1~\tev$. Note in top middle and top right plots the presence of a triplet like eigenvalue, which is totally decoupled from the rest of the neutralino mass matrix, made out of only $\tilde{\psi},\tilde{\phi}$ and $\tilde{\chi}$. It corresponds to an $SU(2)_V$ fiveplet in the custodial basis.
002008528 8564_ $$81083388$$s17889$$uhttp://cds.cern.ch/record/2008528/files/sdplot.png$$y00011 Spin-dependent dark matter nucleon cross sections. Each point meets the correct relic abundance with the annihilation mode marked. The parity violating $Z$ couplings vanish in the custodial case.
002008528 8564_ $$81083376$$s18340$$uhttp://cds.cern.ch/record/2008528/files/vdplotMax.png$$y00000 Top row: Maximal values of $v_{\Delta}$ which allow $\lambda$ to set the Higgs mass to $125~\gev$ and yield a minimized potential as a function of $\mu$. Bottom: Value of $\lambda$ needed to attain the observed Higgs mass for $v_{\Delta}=10~\gev$. The triplet supersymmetric mass is set to $\mu_{\Sigma}=250~\gev$, and the other values are as Eq.~\eqref{eqn:benchmark}.
002008528 8564_ $$81083386$$s22110$$uhttp://cds.cern.ch/record/2008528/files/siplot.png$$y00010 Spin-independent dark matter nucleon cross sections. Each point meets the correct relic abundance with the annihilation mode marked. Points with smaller Higgsino components have a lower spin-independent cross section.
002008528 8564_ $$81083384$$s2412$$uhttp://cds.cern.ch/record/2008528/files/TypeLegend.png$$y00009 Points which yield the correct relic abundance of dark matter. The upper row is for the custodial case while the lower has $\tan\beta=2$. The left panels keep $v_{\Delta}$ constant, and the right panels use the maximum allowed value for $v_{\Delta}$ for each $\mu$ value. The points are labelled corresponding to which annihilation channel dominates in the early universe.Spin-independent dark matter nucleon cross sections. Each point meets the correct relic abundance with the annihilation mode marked. Points with smaller Higgsino components have a lower spin-independent cross section.Spin-dependent dark matter nucleon cross sections. Each point meets the correct relic abundance with the annihilation mode marked. The parity violating $Z$ couplings vanish in the custodial case.
002008528 8564_ $$81083387$$s3960$$uhttp://cds.cern.ch/record/2008528/files/IndirectLegend.png$$y00013 Annihilation cross section times velocity of dark matter in the galaxy in the current universe. Each point meets the correct relic abundance with the annihilation mode in the early universe marked. The lines mark the limits assuming the annihilation occurs $100\%$ of the time through the given channel, each resulting in different spectrum of photons measured here on Earth.
002008528 8564_ $$81083381$$s39900$$uhttp://cds.cern.ch/record/2008528/files/MuChi1.png$$y00008 Points which yield the correct relic abundance of dark matter. The upper row is for the custodial case while the lower has $\tan\beta=2$. The left panels keep $v_{\Delta}$ constant, and the right panels use the maximum allowed value for $v_{\Delta}$ for each $\mu$ value. The points are labelled corresponding to which annihilation channel dominates in the early universe.
002008528 8564_ $$81083379$$s6718$$uhttp://cds.cern.ch/record/2008528/files/raplot.png$$y00007 Relic abundance for the model with $\mu=200~\gev$, $\mu_{\Delta}=250~\gev$, $v_{\Delta}=10~\gev$, and $\tan\beta=1$. The grey line marks the observed relic abundance in the universe today. As the mass of the LSP crosses over half the mass of one of the scalars in the model, the annihilation cross section greatly increases, leading to lower relic abundances. When the LSP mass gets close to the mass of the Higgsino, the mixing and co-annihilations take over and the relic abundance stays below the observed value.
002008528 8564_ $$81083375$$s68547$$uhttp://cds.cern.ch/record/2008528/files/IndirectDetection2015Update.png$$y00012 Annihilation cross section times velocity of dark matter in the galaxy in the current universe. Each point meets the correct relic abundance with the annihilation mode in the early universe marked. The lines mark the limits assuming the annihilation occurs $100\%$ of the time through the given channel, each resulting in different spectrum of photons measured here on Earth.
002008528 8564_ $$81083378$$s79938$$uhttp://cds.cern.ch/record/2008528/files/Spectrum.png$$y00003 The left panels show the spectrum of the neutral light scalars when $v_{\Delta}=10~\gev$ and $\lambda$ is changed to set the Higgs mass. The right panels use the maximum allowed value for $v_{\Delta}$ for each $\mu$ value. The upper (lower) panels contain $\tan\beta=1$ ($\tan\beta=2$). Changing $\tan\beta$ greatly affects the mass of $H_2^0$ and $A_2^0$ but $H_3^0$'s mass is similar for both choices.
002008528 8564_ $$81234943$$s1100683$$uhttp://cds.cern.ch/record/2008528/files/PhysRevD.92.015011.pdf$$yAPS Open Access article
002008528 8564_ $$81234943$$s2556020$$uhttp://cds.cern.ch/record/2008528/files/PhysRevD.92.015011.pdf?subformat=pdfa$$xpdfa$$yAPS Open Access article
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