Prospects and Blind Spots for Neutralino Dark Matter
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1 Prospects and Blind Spots for Neutralino Dark Matter Josh Ruderman October 6 GGI 01 Cliff Cheung, Lawrence Hall, David Pinner, JTR 111.xxxx
2 ] WIMP-Nucleon Cross Section [cm DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL) Expected limit of this run: ± 1! expected ±! expected SIMPLE (01) CDMS (010/11) COUPP (01) ZEPLIN-III (01) XENON100 (011) WIMP Mass [GeV/c ]
3 ] WIMP-Nucleon Cross Section [cm DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL) Expected limit of this run: ± 1! expected ±! expected SIMPLE (01) CDMS (010/11) COUPP (01) ZEPLIN-III (01) XENON100 (011) WIMP Mass [GeV/c ] what is status of SUSY DM?
4 the plan 1. experimental status. neutralino DM in SUSY 3. bino-higgsino 4. bino-wino-(higgsino)
5 experimental status XENON1T
6 types of scattering: 1. spin independent: χχ NN χ χ y χχh σ SI cm y 0.1 q h q
7 types of scattering: 1. spin independent: χχ NN χ χ y χχh σ SI cm y 0.1 q h q. spin-dependent: χγ µ γ 5 χ Nγ µ γ 5 N c χγ µ γ 5 χ Z µ χ χ σ SD cm c 0.1 q Z q
8 spin independent status spin independent Xenon Σp,n cm cχχh m DM GeV
9 spin independent status spin independent Xenon Σp,n cm LUX cχχh m DM GeV
10 spin independent status spin independent Xenon Σp,n cm LUX cχχh Xenon1T m DM GeV
11 what about the strange quark? f q = m q m N N q q N σ f f = Σ q f q lattice Giedt et al. f f Μ default traditional ΠN f s Giedt, Thomas, Young
12 spin dependent status spin dependent Xenon Σp,n cm cχχz m DM GeV
13 spin dependent status spin dependent Xenon IceCube tt Σp,n cm IceCube W W 0.01 cχχz m DM GeV
14 spin dependent status spin dependent Xenon IceCube tt Σp,n cm IceCube W W 0.01 cχχz Xenon1T m DM GeV
15 indirect
16 indirect thermal
17 collider LEP: LHC: m χ GeV µ, M 100 GeV [GeV] 0 1! m" CMS Preliminary pp % "! 0 combined observed combined observed (±1$ -1 s = 7 TeV, L = 4.98 fb int theory combined median expected combined expected (±1$) lj observed trilepton (M ) observed "! ± 1 T miss % WZ+E T ) % CL UL $#BF [fb] m 0 = m ± [GeV]! "! " 1
18 neutralino DM in SUSY
19 fermionic dark matter a SM + B, W, H assume scalar superpartners can be decoupled when computing: σ χn, Ω assume CP parameters: M 1, M, µ, tan β
20 m h is the weak scale natural?
21 is the weak scale natural? m h 15 GeV
22 is the weak scale natural? m h 15 GeV natural unnatural
23 is the weak scale natural? m h 15 GeV natural unnatural λ SH u H d
24 is the weak scale natural? m h 15 GeV natural unnatural λ SH u H d split SUSY
25 is the weak scale natural? m h 15 GeV natural unnatural λ SH u H d split SUSY χ neutralino DM interesting for both!
26 fermionic DM in unnatural SUSY the LSP is at the weak scale to avoid overclosure Ω 1 σ m Ñ the DM mass is crucial for LHC observability m g >m χ
27 fermionic DM in unnatural SUSY fermionic DM is a simplified limit of natural SUSY mz m we assume any physics that raises the Higgs mass does not modify DM properties 4 θñ1 S 1 DM mass is important for naturalness: µ m χ m χ m h
28 Ω in this talk I ll consider two cases: 1. non-thermal Ω freezeout = Ω dm. thermal Ω freezeout = Ω dm
29 pure eigenstate DM bino overcloses higgsino m H 1 TeV H H W H W + wino m W.7 TeV
30 well-tempered neutralino N. Arkani-Hamed, A. Delgado, G. Giudice
31 well-tempered neutralino N. Arkani-Hamed, A. Delgado, G. Giudice
32 hidden dark matter χ h χ
33 hidden dark matter χ h χ
34 hidden dark matter χ h χ 1. purity χ B, W, H turn y χχh 0 off mixing by decoupling higgsinos or gauginos. blindspots
35 hidden dark matter χ h χ 1. purity χ B, W, H y χχh 0 decouple higgsinos or gauginos. blindspots y χχh =0 due to cancellation
36 purity tree-level Higgs coupling vanishes for pure higgsino or Wino loop contribution smaller than expected χ 0 χ 0 ψ ± ( η 0 ) χ 0 χ 0 ψ ± ( η 0 ) W ± (Z 0 ) h 0 W ± W ± (Z 0 ) (Z 0 ) q (q) q q q q χ 0 ψ± ( η 0 ) χ 0 χ 0 χ 0 ψ ± ( η 0 ) χ 0 χ 0 ψ ± W ± (Z 0 ) h 0 Q /q W ± W ± Q (Q) W ± (Z 0 (Q/q) W ± ) (Z 0 ) (Z 0 ) (Z 0 ) g Q g g g Q/q g Q g Hisano, Ishiwata, Nagata, Takesako Hill, Solon
37 blindspots y χχh =0
38 blindspots y χχh =0 bino m χ = M 1 1 M 1 +sinβ µ =0
39 blindspots y χχh =0 bino m χ = M 1 1 M 1 +sinβ µ =0 higgsino m χ = µ tan β =1 sign(µ) = sign(m 1 )
40 blindspots y χχh =0 1 bino m χ = M 1 M 1 +sinβ µ =0 higgsino m χ = µ tan β =1 sign(µ) = sign(m 1 ) wino m χ = M 3 M +sinβ µ =0 4 M 1 = M sign(µ) = sign(m 1, )
41 bino-higgsino
42 bino-higgsino decouple wino M 1 g cos β v g sin β g cos β v 0 µ g sin β v µ 0 v parameters M 1,µ,tan β
43 non-thermal tan Β 5000 LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ Μ GeV tan Β LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ Μ GeV
44 non-thermal tan Β 5000 LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ 0 M 1 +sinβ µ = Μ GeV tan Β 0 LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ Μ GeV
45 tan β 1 sign(µ) = sign(m 1 ) 5000 non-thermal tan Β LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ Μ GeV tan Β LEP Χ Χ thermal cdm M1 GeV 1000 c hχχ Μ GeV
46 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ Μ GeV tan Β LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ Μ GeV
47 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ Μ GeV tan Β 0 XENON LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 XENON Μ GeV
48 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV tan Β 0 XENON LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV XENON100
49 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV tan Β 0 LUX 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV LUX
50 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV tan Β 0 XENON1T 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 IceCube WW Μ GeV XENON1T
51 non-thermal tan Β 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 XENON1TSD Μ GeV tan Β 0 XENON1TSI 5000 LEP Χ Χ thermal cdm Fermi M1 GeV 1000 c hχχ 0 XENON1TSD Μ GeV XENON1TSI
52 well-tempered Ω (M 1,µ,tan β) =Ω DM solve for: M 1 (µ, tan β)
53 well-tempered
54 M 1 +sinβ µ =0 well-tempered
55 well-tempered
56 well-tempered
57 well-tempered
58 well-tempered
59 well-tempered
60 target ] WIMP-Nucleon Cross Section [cm DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL) Expected limit of this run: ± 1! expected ±! expected SIMPLE (01) CDMS (010/11) COUPP (01) ZEPLIN-III (01) XENON100 (011) WIMP Mass [GeV/c ]
![target ] WIMP-Nucleon Cross Section [cm 10 10 10 10 10 10-39 -40-41 -4-43 -44 DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL)](/docs-images/96/127737379/images/61-0.jpg "Expected limit of this run: ± 1! expected ±!")
61 target ] WIMP-Nucleon Cross Section [cm DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL) Expected limit of this run: ± 1! expected ±! expected SIMPLE (01) CDMS (010/11) COUPP (01) ZEPLIN-III (01) XENON100 (011) WIMP Mass [GeV/c ]
62 target ] WIMP-Nucleon Cross Section [cm DAMA/Na CoGeNT XENON10 (011) DAMA/I CRESST-II (01) SIMPLE (01) EDELWEISS (011/1) XENON100 (01) observed limit (90% CL) Expected limit of this run: ± 1! expected ±! expected CDMS (010/11) COUPP (01) ZEPLIN-III (01) XENON100 (011) Σ cm XENON100 LUX XENON1T Μ 0 Μ WIMP Mass [GeV/c ] m Χ GeV
63 bino-wino-(higgsino)
64 bino-wino-(higgsino) M 1 0 g cos β g cos β g sin β v g cos β 0 M v g sin β v g cos β v 0 µ g sin β v g sin β v µ 0 v v parameters M 1,M,µ,tan β
65 non-thermal tan β = µ = 750 GeV
66 non-thermal tan β = µ = 750 GeV M 1 +sinβ µ =0
67 non-thermal tan β = µ = 750 GeV M +sinβ µ =0
68 non-thermal tan β = µ = 750 GeV M 1 = M
69 non-thermal tan β = µ = 750 GeV
70 non-thermal tan β = µ = 750 GeV
71 non-thermal tan β = µ = 750 GeV
72 non-thermal tan β = µ = 750 GeV
73 well-tempered Ω (M 1,M,µ,tan β) =Ω DM solve for: M 1 (M,µ,tan β)
74 bino/wino coannihilation H W B M 1 0 g cos β g sin β v g cos β 0 M v g sin β g cos β v g cos β v 0 µ g sin β v g sin β v µ 0 v v
75 bino/wino coannihilation H W B M 1 0 g cos β g sin β v g cos β 0 M v g sin β g cos β v g cos β v 0 µ g sin β v g sin β v µ 0 v v how heavy can the higgsino be?
76 bino/wino coannihilation H W B M 1 0 g cos β g sin β v g cos β 0 M v g sin β g cos β v g cos β v 0 µ g sin β v g sin β v µ 0 v v how heavy can the higgsino be? coannihilation: σ eff v = Σ i,j w i w j σ ij v (Σ i w i ) w i = mi m 1 3/ e x mi m 1 1
77 well-tempered tan β =
78 well-tempered tan β =
79 well-tempered tan β = B/ W
80 well-tempered B/ H tan β =
81 well-tempered tan β = M 1 +sinβ µ =0
82 well-tempered tan β = M 1 M sign(µ) = sign(m 1, )
83 well-tempered tan β =
84 well-tempered tan β =
85 well-tempered tan β =
86 well-tempered tan β =
87 well-tempered tan β =
88 take away points direct detection is finally probing neutralino DM large parameter space remains blindspots with small spin-independent cross-section evade Xenon1T
89 backup
90 overclose LUX SI Xenon1T SI Μ GeV Xenon1T SD tan Β 0 Μ 0 Xenon100 SI ATLAS 7 TeV 00 m g TeV g decoupled m q 1, GeV
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