WIMP Dark Matter + SUSY

Transcription

1 WIMP Dark Matter + SUSY Clifford Cheung Dark Matter in Southern California

2 Ingredients for a miracle (WIMP): #1) Particle is neutral + stable. #2) Particle couples to SM with weak scale annihilation cross-section. These are ubiquitous in models that address the hierarchy problem.

3 #1) Lots of examples of stabilizing symmetry! theory Z2 Supersymmetry R-parity Extra Dimensions KK-parity Little Higgs T-parity Parities help with other exp l constraints.

4 #2) Lots of weak scale masses + couplings! xxx ^> c* Such couplings are mandatory to solve the hierarchy problem.

5 SUSY offers a sandbox for WIMP DM. DM is among primary virtues of SUSY: dark matter hierarchy problem gauge coupling unification

6 SUSY offers a sandbox for WIMP DM. DM is among primary virtues of SUSY: dark matter hierarchy problem? gauge coupling unification

7 DM probes offer a crucial experimental referendum on our motivations for SUSY. What is the present status of neutralino DM and what is in its future?

8 Focus on neutralino DM that is an admixture of gauginos and Higgsinos: ( b, w, h) The parameter space is small, manageable: (M 1,M 2, µ, tan )

9 Focus on neutralino DM that is an admixture of gauginos and Higgsinos: ( b, w, h) singlets, triplets, doublets The parameter space is small, manageable: (M 1,M 2, µ, tan )

10 simplifications a) Ignore all scalars but light Higgs. resonant effects (Higgs funnels) scalar coannihilation (squark, etc) b) Ignore all CP phases.

11 relic abundance We allow for a range cosmology scenarios: thermal obs = = (th) non-thermal obs = 6= (th) sub-component obs > = (th)

12 relic abundance We allow for a range cosmology scenarios: thermal obs = = (th) } theory parameters constrained non-thermal obs = 6= (th) sub-component obs > = (th)

13 relic abundance We allow for a range cosmology scenarios: thermal obs = = (th) } theory parameters constrained non-thermal obs = 6= (th) sub-component obs > = (th) exp. limits }weaker

14 Well-tempering is needed for correct relic abundance in many theories - including SUSY. W h ò B é -like W obs ± 3s bino - higgsino m = 500 GeV M 2 decoupled tan b = M H é -like ô 1000

15 experiments Consider present limits and future reach for direct detection / neutrinos experiments. spin independent (SI) scattering: XENON, LUX spin dependent (SD) scattering: XENON, IceCube

16 10-43 SI XENON D LUX SuperCDMS chcc XENON1T m

17 10-43 SI XENON D LUX SuperCDMS chcc XENON1T m

18 SD XENON D XENON1T IceCube tt IceCube W + W czcc m

19 SD XENON D XENON1T IceCube tt IceCube W + W czcc m

20 At zeroth order, XENON100 introduces tension for neutralino dark matter: c h. 0.1 versus g g 0.65

21 At zeroth order, XENON100 introduces tension for neutralino dark matter: g c h. 0.1 versus g 0.65 Because contributions are of order the limit, cancellations will occur generically, e.g. (2 1) 2 (2 + 1) 2

22 how does DM hide? purity c h! 0 as M 1,M 2,µ!1 blind spots c h =0 as M 1,M 2,µ=finite

23 purity state SI(h) SI(Z) SD(Z) b inert inert inert w no renorm. operator no renorm. operator no renorm. operator h u, h d no renorm. operator present but inelastic no renorm. operator

24 blind spots (SI) Reinstate the Higgs boson:! L h = 1 m (v + h) 2 = 1 2 m (v) + 1 (v) h + O(h 2 Higgs coupling cancellation at: c h =0

25 current Take bino-higgsino DM ( ). non-thermal b é êh é limits M 2!1 tan b = W c HthL LEP c - c c hcc = W obs bino-like IceCube W + W - Higgsino-like Fermi XENON100 SI 1000 bino-like tan b = 20

26 current non-thermal b é êh é limits tan b = W c HthL W obs Fermi LEP c - c c hcc = IceCube W + W XENON100 SI tan b = 20

27 current non-thermal b é êh é limits tan b = W c HthL W obs Fermi LEP c - c c hcc = IceCube W + W well-tempered neutralino allowed 10 XENON100 SI well-tempered tan b = 20 neutralino excluded

28 current tan b = W c HthL W obs Fermi LEP c - c c hcc = IceCube W + W XENON100 SI : Current limits on bino/higgsino DM with = obs for tan =2(upp

29 future tan b = W c HthL = W obs LEP c - c + Fermi 1000 c hcc = 0 LUX SI XENON1T SI XENON1T SD

30 future tan b = W c HthL = W obs LEP c - c + Fermi 1000 c hcc = 0 LUX SI XENON1T SI XENON1T SD blind spot

31 future tan b = W c HthL = W obs LEP c - c + Fermi 1000 c hcc = 0 LUX SI XENON1T SI XENON1T SD blind spot SD complements SI

32 future tan b = W c HthL = W obs LEP c - c + Fermi 1000 c hcc = 0 XENON1T SD LUX SI XENON1T SI

33 current 40 current limits LEP c - c + 20 tan b IceCube W + W - Xenon100 SD Xenon100 SI c hcc =

34 current 40 well-tempered neutralino is alive and well current limits LEP c - c + 20 tan b IceCube W + W - Xenon100 SD Xenon100 SI c hcc =

35 LUX and IceCube reach H~2013L LEP c - c + 20 LUX SI 10 tan b 5 IceCube tt HreachL IceCube W + W - HreachL 2 c hcc = XENON 1T reach H~2017L

36 XENON 1T reach H~2017L LEP c - c Xenon1T SI tan b 5 Xenon1T SD 2 c hcc =

37 XENON 1T reach H~2017L LEP c - c Xenon1T SI tan b 5 Xenon1T SD 2 c hcc = soon, nothing left but blind spot

38 Are there any theory motivated blind spots? Higgsino DM at tan beta ~ 1 hard to probe. SI scattering is in blind spot. SD scattering is in blind spot. Higgsino DM at tan beta ~ 1 is motivated. natural theories (lambda SUSY) unnatural theories (split SUSY)

39 Low tan beta preferred by theory (gaugino/ scalar hierarchy) and experiment (flavor). Arvanitaki et al. [ ]

40 Low tan beta preferred by theory (gaugino/ scalar hierarchy) and experiment (flavor). Arvanitaki et al. [ ]

41 XENON100 has just cut into the Higgs scattering region of thermal neutralino DM! XENON100 m > 0 2 D LUX XENON1T m < m

42 thanks!