SUSY Implications from WIMP Annihilation into scalars at the - - PowerPoint PPT Presentation

SUSY Implications from WIMP Annihilation into scalars at the Galactic Center

Anibal D. Medina

The University of Melbourne

11th Feb 2015, HPNP2015 Toyama

In collaboration with T.Gherghetta, B.v.Harling, M.A.Schmidt and T.Trott [1502.xxxx] JHEP 1302 (2013) 032 [1212.5243]

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 1/18

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Fermi Satellite Experiment

fermi.gsfc.nasa.gov

• launched 11 June 2008
• running 5 - 10 years

Fermi-LAT

• Observation of γ-rays
• E = 30MeV −500GeV
• High energy resolution: < 15% at

energies > 100 MeV

• large field of view 2.4 sr

fermi.gsfc.nasa.gov

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 2/18

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Dark Matter Interpretation of Fermi GeV Excess

DM dN dE = ∑

f

⟨σv⟩f 8πm2

χ

dN f

γ

dE ∫

l.o.s.

ds ρ2(r(s, ψ)) Generalized NFW profile ρ(r) = ρ⊙ ( r r⊙ )−γ (1 + r⊙/rs 1 + r/rs )3−γ

10-2 10-1 100 101 102 103 r[kpc] 10-6 10-5 10-4 10-3 10-2 10-1 100 101 102 103 104 ρ[GeVcm−2 ] r ⊙ =8.5 kpc ρ ⊙ =0.4 GeV cm−3 rs =20 kpc γ =1.2 contracted NFW profile

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 3/18

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Dark Matter Interpretation of Fermi GeV Excess

DM dN dE = ∑

f

⟨σv⟩f 8πm2

χ

dN f

γ

dE ∫

l.o.s.

ds ρ2(r(s, ψ))

100 101 102 E [GeV] 10−8 10−7 10−6 10−5 E2dN/dE [GeV cm−2s−1sr−1] broken PL PL with exp. cutoff DM ¯ bb DM τ +τ − GC excess spectrum with

• stat. and corr. syst. errors

Calore, Cholis, Weniger [1409.0042]

p-values broken PL p = 0.47 exp cutoff p = 0.16 DM b¯ b p = 0.43 DM τ +τ − p = 0.065

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 3/18

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DM Fits: 3σ Regions

101 102

mχ [GeV]

10−27 10−26 10−25

σv /A [cm3s−1] τ +τ− ¯ qq ¯ cc ¯ bb gg W +W − ZZ hh ¯ tt

Calore, Cholis, McCabe, Weniger [1411.4647]

Uncertainties in DM halo A = [0.17, 5.3] (J = [0.19, 3])

⟨σv⟩ mχ χ2

min

p-value ¯ bb 1.75+0.28

−0.26

48.7+6.4

−5.2

23.9 0.35 ¯ tt 5.8+0.8

−0.8

173.3+2.8

−0

43.9 0.003 hh 5.33+0.68

−0.68

125.7+3.1

−0

29.5 0.13 W +W − 3.52+0.48

−0.48

80.4+1.3

−0

36.7 0.026 ZZ 4.12+0.55

−0.55

91.2+1.53

−0

35.3 0.036

Calore,Cholis,McCabe,Weniger [1411.4647]

hh WW tt bb ZZ Σ2.21026cm3s

50 100 150 200 250 2 4 6 8 10 mΧGeV Σ 1026cm3s Agrawal, Batell, Fox, Harnik [1411.2592]

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 4/18

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Annihilation into ha and aa in type II 2HDM

• Independent of additional scalar singlets (includes the NMSSM).
• Fits with a Higgs at 125 GeV with SM couplings and setting

tan β = 3.

• Consider the dominant decay channels b¯

b, τ +τ −, c¯ c, γγ and gg and simulate the prompt photon spectra using PYTHIA 8.201.

• For intermediate tan β ⇒

Br(a → γγ)/Br(hSM → γγ) ∼ 1/(10 × tan4 β).

• Spectral line from a → γγ barely distinguishable from the

continuum for ma ∼ 150 GeV and tan β ∼ 1 using Fermi-LAT resolution.

• 2-peak structure in ha may be detectable in future

experiments.

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 5/18

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Spectral Fit for ha

100 101 102 E [GeV] 10-8 10-7 10-6 E2 dN/dE [GeVcm−2 s−1 sr−1 ]

ha, ma =63 GeV ha, ma =90 GeV ha, ma =120 GeV ha, ma =150 GeV b¯ b hh

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 6/18

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Spectral Fit for aa

100 101 102 E [GeV] 10-8 10-7 10-6 E2 dN/dE [GeVcm−2 s−1 sr−1 ]

aa, ma =63 GeV aa, ma =90 GeV aa, ma =120 GeV aa, ma =150 GeV b¯ b hh

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 7/18

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Best fit regions for ha

40 60 80 100 120 140 160 180 mχ [GeV] 1 2 3 4 5 6 7 8

• σv
• /A [10−26 cm3 s−1 ]

ha, ma =63 GeV ha, ma =90 GeV ha, ma =120 GeV ha, ma =150 GeV b¯ b hh

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 8/18

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Best fit regions for aa

40 60 80 100 120 140 160 180 mχ [GeV] 1 2 3 4 5 6 7 8

• σv
• /A [10−26 cm3 s−1 ]

aa, ma =63 GeV aa, ma =90 GeV aa, ma =120 GeV aa, ma =150 GeV b¯ b hh

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 9/18

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channel ma [GeV] mDM [GeV] ⟨σv⟩0 [10−26cm3/s] χ2

min

p-value b¯ b 49.5+8.1

−6.3

1.8+0.3

−0.3

24.5 0.32 hh 125.0+2.3

0.0

4.9+1.0

−0.9

30.0 0.12 ha 63 94.0+4.2

0.0

4.2+0.8

−0.8

22.4 0.43 90 107.5+3.4

0.0

4.3+0.8

−0.8

25.3 0.28 120 122.5+3.0

0.0

4.5+0.9

−0.9

30.3 0.11 150 137.5+2.7

0.0

4.7+1.0

−1.0

36.0 0.03 aa 63 73.0+15.4

−10.0

3.1+0.6

−0.6

24.3 0.33 90 90.0+10.9

0.0

3.7+0.5

−0.8

24.4 0.33 120 120.0+4.9

0.0

4.1+0.8

−0.8

31.0 0.10 150 150.0+4.4

0.0

4.5+1.0

−1.0

41.4 0.01

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 10/18

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Dark Matter Annihilation in the NMSSM

• ˜

χ˜ χ → b¯ b Annihilation

˜ χ ˜ χ ¯ b b a ˜ χ ˜ χ ¯ b b Z

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 11/18

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Dark Matter Annihilation in the NMSSM

• ˜

χ˜ χ → a1h Annihilation

˜ χ ˜ χ h a a∗

˜ χ ˜ χ h a ˜ χ0

i

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 12/18

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Early and late time cross sections for ha case

1 2 3 5 7 10 20 σvTF[10−26cm3/s] 0.7 0.8 1.0 2.0 3.0 4.0 σahv0[10−26cm3/s]

dSph limit bino-like singlino-like

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 13/18

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Direct Detection for ha case

100 110 120 130 140 150 m˜

χ[GeV]

10−48 10−47 10−46 10−45 σSI

p [cm2]

LUX LUX 300d Xenon1T LZ bino-like singlino-like

Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 14/18

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Resonance Condition for b¯ b case with DSph bounds

30 35 40 45 50 m˜

χ[GeV]

0.90 0.95 1.00 1.05 1.10

2m˜

χ

ma σb¯

bv0 ∈ [1, 1.5] × 10−26cm3/s

a singlet-like a doublet-like correct Ω˜

χ Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 15/18

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Direct Detection and Invisible decay for b¯ b case

30 35 40 45 50 m˜

χ[GeV]

10−47 10−46 10−45 σSI

p [cm2] LUX LUX 300d Xenon1T a singlet-like a doublet-like correct Ω˜

χ Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 16/18

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Direct Detection and Invisible decay for b¯ b case

30 35 40 45 50 m˜

χ[GeV]

0.00 0.05 0.10 0.15 0.20 0.25 0.30 0.35 0.40 Br(h → inv)

Br(h → inv) limit CMS 300fb−1 CMS 3000fb−1 a singlet-like a doublet-like correct Ω˜

χ Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 16/18

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Conclusions

• Fermi GeV Excess stands all tests
• Dark matter annihilations to b¯

b as well as hh close to threshold provide a good fit

• We showed that annihilations to ha also provide a good fit and

are naturally present in NMSSM

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