Dark Matter Phenomenology - PDF Free Download

Dark Matter Phenomenology Peisi Huang Texas A&M University PPC 207, TAMU-CC PH, C. Wagner arxiv:404.0392 PH, R. Roglans, D. Spiegel, Y. Sun and C. Wagner arxiv:70.02737

Neutralino Dark Matter Phenomenology Peisi Huang Texas A&M University PPC 207, TAMU-CC PH, C. Wagner arxiv:404.0392 PH, R. Roglans, D. Spiegel, Y. Sun and C. Wagner arxiv:70.02737

Neutralino Dark Matter, (or anything with a Higgs exchange) -- Where is it? χ SM χ SM Direct Detection The direct detection experiments are pushing rapidly into the region with a Higgs exchange Suppress the neutralino direct detection rate?

Outline How to suppress the neutralino direct detection rate? Blind Spot scenarios Deviations from the Blind Spots Current constraints Future reaches How to probe the blind spot scenarios? LHC IceCube

Suppress the Neutralino Direct Detection Rate Consider a neutralino scattering off a down-type quark. In gauge eigenstates Amplitude Couplings

Suppress the neutralino direct detection rate Loop Effects When st&2nd gen squarks are heavy, ϵd is suppressed

Suppress the Neutralino Direct Detection Rate Pierce, Shah, and Freese. arxiv:309.735

Blind Spot in Dark Matter Direct Detection 25 GeV Higgs Exchange Heavy Higgs Exchange Blind Spot at (m 0 + µ sin 2 ) =0. F d (p) 0.5, F U (p) 0.4 See Cheung, Hall, Pinner, and Ruderman. arxiv:2.4873 Han, Kling, Su, and Wu. arxiv:62.02387 Higgsino mass μ < 0 PH, C. Wagner, 4 Suppress the lightest neutralino coupling to 25 GeV Higgs Destructive interference between the 25 GeV Higgs and the heavy Higgs exchange Reduce the pmssm parameter space to M, μ, tanβ, and m A For a full pmssm study, see Cahill-Rowley et al, 405.676. For a loop level analysis, see Berlin, Hooper, and McDermott, arxiv:508.05390

Blind Spot and the Relic Density Relevant parameters: M, μ, tanβ, and m A Under Abundant Over Abundant m A is chosen to minimize the DD rate Two branches well tempered M ~μ A-funnel m χ ~m A /2

Outline How to suppress the neutralino direct detection rate? Blind Spot scenarios Deviations from the Blind Spots Current constraints Future reach How to probe the blind spot scenarios? LHC IceCube

Current Direct Detection Constraints m A upper bound Assume the right relic density In the well-tempered region, m A < 350-400 GeV The A-funnel region is allowed by LUX and relic density considerations Neutralino higgs coupling vanishes

Current Direct Detection Constraints m A upper bound Rescale according to the local density In the well-tempered region, m A < 350-400 GeV relaxed ma bound to the left of the welltempered region Will discuss direct heavy Higgs search and precision Higgs later

Future Reach next generation experiments will push m A to be smaller than 300 GeV in the well-tempered region

Probe the Blind Spots Scenarios Collider Searches Well-tempered region : open for tanβ < 6 completely ruled out for tanβ 7 A-funnel region starts to get excluded as tanβ increases Well-tempered A-funnel

Probe the Blind Spots Scenarios Collider Searches hbb coupling g hbb g SM hbb = sin cos =sin( ) tan cos( ) hvv coupling ~ One loop level, sizable tanβ tan cos( ) ' m 2 H m 2 h apple m 2 h + m 2 Z + controls the modification A t 3 M s, vacuum stability 3m4 t A 4 2 v 2 MS 2 t µ tan A 2 t 6M 2 S Ms TeV, proper Higgs mass m A 350 GeV to be consistent with the current Higgs data.

Probe the Blind Spots Scenarios Collider Searches In tension with the current Higgs data Extended the Higgs sector tan cos( ) ' m 2 H m 2 h apple m 2 h + m 2 Z + 3m4 t A 4 2 v 2 MS 2 t µ tan A 2 t 6M 2 S tan cos( ) ' m 2 H m 2 h apple m 2 h + m 2 Z 2 v 2 + 3m4 t A 4 2 v 2 MS 2 t µ tan A 2 t 6M 2 S λ 0.6-07, even for m H 200 GeV, the modification in SM Higgs coupling is small enough. Blind spot scenarios in NMSSM, see Badziak, Olechowski, and Szczerbiak, arxiv:52.02472

earches at LHC become relevant. The most stringent with M, µ < 200 GeV. The neutralinos and charginos are Probe the Blind Spots Scenarios udying the decay products of the associated production of our slepton masses have been set high, the branching Collider Searches Since our slepton masses have been set high, the branching LHC become relevant. The most stringent of gkino thesearches decay atproducts of the associated production est neutralino and the lightest chargino0 e02±, e±, into lightest neutralino and the lightest chargino e2, e, into 3 neutralinos, (mixtures of bino 0and ±Higgsinos), the lighest 0e ± ± 0,, the e, since m e02 m 'em < M + m decay of, e into A ' m < M + m the decay of e e A 2, 2e into e chargino(higgsino-like) 0 400 CMS Preliminary 35.9 fb- (3 TeV) H Z m m χ 0+ = m χ 0+ Expected Observed χ± m χ± 200 = χ± m = m χ0 250 m 300 Moriond 207 SUS-6-039, 2l SS + 3l (WH) SUS-6-034, 2l OS (WZ) SUS-6-039, 3l (WZ) SUS-6-048, soft 2-lep (WZ) 350 8 pp χ02 χ± m χ [GeV] 0 ± ± W he0 e0 0 0 00 e00 and e0 e0±! ible. This leaves e! W Z e This leaves e02 ee±! W Z e e and e e 2 2 e 2! W he m ± 0 0 2 50 00 50 0 00 200 300 400 500 600 m χ = m χ [GeV] 0 2 ±

Probe the Blind Spots scenarios IceCube bb, weak Dark matter-proton cross-section SD,p (cm 2 ) 0 33 0 34 0 35 0 36 0 37 0 38 0 39 0 40 0 4 0 42 IC79 gg b b hh t t IceCube Collaboration 206 W + W ZZ + 0 0 2 0 3 0 4 Dark matter mass m (GeV) tt, Wh, Zh, ha, WW, ZZ..

Probe the Blind Spots scenarios IceCube exclude the well-tempered region for m χ 200 GeV Dark matter-proton cross-section SD,p (cm 2 ) 0 33 0 34 0 35 0 36 0 37 0 38 0 39 0 40 0 4 0 42 IC79 gg b b hh t t IceCube Collaboration 206 W + W ZZ + 0 0 2 0 3 0 4 Dark matter mass m (GeV)

Conclusion Identify a blind spot scenario for neutralino dark matter Possible probes LHC - Heavy Higgs searches, precision Higgs, and Electroweakinos searches IceCube

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Positive μ /pb SI σ p 0 8 µ = - 600 GeV µ = 600 GeV 9 0 0 0 0 2 0 200 400 600 800 000 200 M A /GeV Larger Higgs Neutralino coupling Constructive interference lower bound on m A

A funnel and the LUX limit

Exclusions

Exclusions, ma upper bound

EW-ino production cross section