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Cosmology in the SUSY DFSZ Axion Model

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Cosmology in the SUSY DFSZ Axion Model COSMOLOGY OF SUSY DFSZ AXION MODEL ! Kyu Jung Bae, ! Department of Physics and Astronomy, University of Oklahoma ! based on KJB, Baer, Chun 1309.0515, 1309.5365 ! Phenoworkshop@KIAS Nov. 15, 2013 OUTLINE • Introduction & Motivation • Neutralino & Axion DM • Cosmology of SUSY DFSZ • Summary SUSY & PQ Higgs discovery & Gauge hierarchy: m =125.8 0.5 (stat) 0.2 (syst) GeV (CMS) H ± ± 126.8 0.2 (stat) 0.7 (syst) GeV (ATLAS) ± ± At the quantum level, ⇤2 H 2 ⇠ cuto↵| | Introducing SUSY, it is removed, m2 log ⇤2 H 2 ⇠ soft | | Strong CP-problem: 2 gs a ˜aµ⌫ QCD θ-term, ✓ = ✓ Gµ⌫ G ✓(E B) L 32⇡2 ) · 11 From neutron EDM, ✓ < 10− a g2 = + ✓ s Ga Gaµ⌫ With Peccei-Quinn symmetry, L f 32⇡2 µ⌫ ✓ a ◆ 2 2 e f⇡m⇡ 2 2 V = mu + md +2mumd cos(a/Fa + ✓) −mu + md q a/F + ✓ =0 h a i μ-problem of MSSM: WMSSM = µHuHd + Yukawas μ-term is supersymmetric; basically fundamental scale, Λ. For the natural EWSB, μ is required to be 100 GeV order. Howard Baer’s talk SUSY DFSZ realization of μ-term: assigning PQ charges to Higgs multiplets (S, H H )=(1, 2) u d − to forbid bare μ-term. Instead, 2 S A/vP Q WKN = λ HuHd with PQ breaking field, S = vPQe MP 2 10 2 λvPQ 10 GeV µ 18 100 GeV Kim-Nilles mechanism! ⇠ MP ⇠ 10 GeV ⇠ NEUTRALINO & AXION 2 DM candidates: neutralino & axion 5 0.64 0.16 events from ER leakage are expected below are- obtainedneutralino for each WIMP DM mass fromin fullMSSM: simulations. admixture of bino, wino and Higgsinos the NR± mean, for the search dataset. The spatial distribution of the events matches that expected from the ER backgrounds in full detector simulations. We select constrains the size of mixing the upper bound of 30 phe (S1) for the signal estimation ) 2 analysis to avoid additional background from the 5 keVee Z1 B,W Hu,d Z1 x-ray from 127Xe. X X −44 10 1.3 keV 2.6 ee e e f e e h 2.4 1.8 6 8 10 12 2.2 −40 10 nucleon cross section (cm − 2 3.5 −45 q q 4.6 10 −42 WIMP 10 1.8 5.9 7.1 /S1) x,y,z corrected b favors more mass gap between 1.6 −44 10 (S2 1 2 3 10 10 10 10 1.4 2 higgsinos and gauginos log m (GeV/c ) WIMP 1.2 3 6 9 12 15 18 21 24 27 30 keV FIG. 5. The LUX 90% confidence limit on the spin- 1 nr 0 10 20 30 40 50 independent- LHC elastic search WIMP-nucleon limit cross for section gluino (blue), (m g˜ 1 . 4 TeV ) pushes up the gaugino S1 x,y,z corrected (phe) together with the 1σ variation from repeated trials, where & trials fluctuating below± the expected number of events for FIG. 4. The LUX WIMP signal region. Events in the zeromasses BG are forced (under to 2.3 (blue shaded).assumption We also show of gaugino unification) 118 kg fiducial volume during the 85.3 live-day exposure are Edelweiss II [41] (dark yellow line), CDMS II [42] (green line), shown. Lines as shown in Fig. 3, with vertical dashed cyan ZEPLIN-III [43] (magenta line) and XENON100 100 live- lines showing the 2-30 phe range used for the signal estimation day- [44] prefers (orange line), andHiggsino-like 225 live-day [45] (red line) neutralino results. analysis. The inset (same axis units) also shows the regions measured from annual modulation in CoGeNT [46] (light red, shaded), along with exclusion limits from low threshold re-analysis of CDMS II data [47] (upper green line), 95% allowed Confidence intervals on the spin-independent WIMP- region from CDMS II silicon detectors [48] (green shaded) nucleon cross section are set using a profile likelihood and centroid (green x), 90% allowed region from CRESST ratio (PLR) test statistic [35], exploiting the separation II [49] (yellow shaded) and DAMA/LIBRA allowed region [50] of signal and background distributions in four physical interpreted by [51] (grey shaded). quantities: radius, depth, light (S1), and charge (S2). The fit is made over the parameter of interest plus three Gaussian-constrained nuisance parameters which encode The observed PLR for zero signal is entirely consistent uncertainty in the rates of 127Xe, γ-rays from internal with its simulated distribution, giving a p-value for the components and the combination of 214Pb and 85Kr. background-only hypothesis of 0.35. The 90% C. L. The distributions, in the observed quantities, of the four upper limit on the number of expected signal events model components are as described above and do not ranges, over WIMP masses, from 2.4 to 5.3. A variation vary in the fit: with the non-uniform spatial distributions of one standard deviation in detection efficiency shifts of γ-ray backgrounds and x-ray lines from 127Xe obtained the limit by an average of only 5%. The systematic from energy-deposition simulations [31]. uncertainty in the position of the NR band was estimated The energy spectrum of WIMP-nucleus recoils is by averaging the di↵erence between the centroids of modeled using a standard isothermal Maxwellian velocity simulated and observed AmBe data in log(S2b/S1). This distribution [36], with v0 = 220 km/s; vesc = 544 km/s; yielded an uncertainty of 0.044 in the centroid, which 3 1 ⇢0 =0.3 GeV/c ; average Earth velocity of 245 km s− , propagates to a maximum uncertainty of 25% in the high and Helm form factor [37, 38]. We conservatively model mass limit. no signal below 3.0 keVnr (the lowest energy for which The 90% upper C. L. cross sections for spin- direct NR yield measurements exist [30, 40]). We do independent WIMP models are thus shown in Fig. 5 46 2 not profile the uncertainties in NR yield, assuming a with a minimum cross section of 7.6 10− cm for a model which provides excellent agreement with LUX WIMP mass of 33 GeV/c2. This represents⇥ a significant data (Fig. 1 and [39]), in addition to being conservative improvement over the sensitivities of earlier searches [42, compared to past works [23]. We also do not account 43, 45, 46]. The low energy threshold of LUX permits for uncertainties in astrophysical parameters, which are direct testing of low mass WIMP hypotheses where beyond the scope of this work. Signal models in S1 and S2 there are potential hints of signal [42, 46, 49, 50]. Higgsino DM: ⌦ h2 0.10 (µ/1 TeV)2 H ⇠ For µ = 150 GeV , Higgsinoe DM is less than 10% of the total DM. 1.19 Axion DM: 2 2 Fa ⇤QCD Turner; KJB, Huh, Kim; 13 ⌦ah =0.18 ✓1 12 10 Gev 400 MeV Visinelli, Gondolo ✓ ◆ ✓ ◆ ma !eV" 10!3 10!4 10!5 10!6 10!7 10!8 10!9 T = T1 1.0 R˙ 3 m R ⇠ a 0.8 0.6 ! "! Π a CDM # i Θ 0.4 axion can be !a #!CDM sizable DM component 0.2 for proper θ1 and fa 0.0 109 1010 1011 1012 1013 1014 1015 1016 ! " fa GeV Visinelli and Gondolo FIG. 2: The misalignment angle θi necessary for the axion to be 100% of the cold dark matter in 17 Scenario II (fa >HI/2π), as a function of fa.Abovethecurve,Ωa > ΩCDM.Forfa > 10 GeV, ∼ 17 3/4 19 one has θi 0.001(fa/10 GeV)− ;inparticular,forfa > 10 GeV, the initial misalignment ≃ ∼ 5 angle θi has to assume values θi < 10− . ∼ > 17 < 10 < For fa 10 GeV (ma 10− eV or θi 0.001), one has f(θi) 1andEq.(50) ∼ ∼ ∼ ≃ simplifies to 3/4 3 fa − 17 θ 0.84 10− , for f > 10 GeV, (51) i ≃ × 1017 GeV a ! " ∼ or 3/4 3 ma 10 − < − θi 1.2 10 10 , for ma 10 eV. (52) ≃ × 10− eV ∼ > 19 # $ In particular, for fa 10 GeV, the initial misalignment angle θi has to assume values ∼ 5 θi < 10− .Thiswasalsonotedin[17,28].Thesesmallvaluesofθi may be uncomfortable ∼ in a cosmological scenario. In the other limit of θ π,theformofthefunctionf(θ )assumedinEq.(40)gives i ≃ i eπ C/fa < 10 π θi e− , for fa 2 10 GeV, (53) − ≃ 2 ∼ × with C =7.48 1010 GeV. So, as θ approaches π from below, the corresponding f ap- × i a proaches 0. This gives rise to the linear dependence of fa on HI in the lower left corner of Keys for the DM cosmology: - 2 DM components: Higgsino-like neutralino and axion - not a simple composition; supersymmetrization the axion sector 1 2 a A = (s + ia)+p2✓a˜ + ✓ A ! p2 F long-lived saxion/axino production & decay affect DM density What we do: - Extensive study of saxion & axino decay: including all tree-level processes - Consider the DM re-annihilation from both saxion & axino decay - Dark Radiation and entropy are also considered - DM density is calculated depending on PQ parameters a" SUA 1000 100 " f !1010 GeV 10 a GeV ! ! 12 ã fa 10 GeV D T 1 14 fa!10 GeV 0.1 0 2 4 6 8 10 mã !TeV" b" SOA 106 104 " 10 fa!10 GeV GeV 100 ! ! 12 ã fa 10 GeV D T ! 14 1 fa 10 GeV 0.01 0 2 4 6 8 10 mã !TeV" 12 Figure 6: Axino decay temperature for fa = 10 GeV and for a) SUA and b) SOA benchmark points. Previous studies for KSVZ model: - Effectiveanomaly interaction: interaction of dimension 1-loop 5: suppressed √2α = s d2θAW aW a +h.c.
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