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] 1 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 1/18
Fermi Satellite Experiment Fermi-LAT • Observation of γ -rays • E = 30 MeV − 500 GeV • High energy resolution: < 15 % at energies > 100 MeV • large field of view 2 . 4 sr fermi.gsfc.nasa.gov • launched 11 June 2008 fermi.gsfc.nasa.gov • running 5 - 10 years 2 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 2/18
Dark Matter Interpretation of Fermi GeV Excess dN f dN ⟨ σv ⟩ f ∫ γ ∑ ds ρ 2 ( r ( s, ψ )) DM dE = 8 πm 2 dE χ l.o.s. f ( r ) − γ ( 1 + r ⊙ /r s ) 3 − γ Generalized NFW profile ρ ( r ) = ρ ⊙ r ⊙ 1 + r/r s 10 4 contracted NFW profile 10 3 10 2 10 1 ρ [GeVcm − 2 ] 10 0 10 -1 10 -2 10 -3 10 -4 γ =1 . 2 r ⊙ =8 . 5 kpc ρ ⊙ =0 . 4 GeV cm − 3 10 -5 r s =20 kpc 10 -6 10 -2 10 -1 10 0 10 1 10 2 10 3 r [kpc] 3 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 3/18
Dark Matter Interpretation of Fermi GeV Excess dN f dN ⟨ σv ⟩ f ∫ ∑ γ ds ρ 2 ( r ( s, ψ )) DM dE = 8 πm 2 dE l.o.s. χ f 10 − 5 p-values broken PL DM τ + τ − PL with exp. cutoff GC excess spectrum with E 2 dN/dE [GeV cm − 2 s − 1 sr − 1 ] stat. and corr. syst. errors DM ¯ bb broken PL 10 − 6 p = 0 . 47 exp cutoff p = 0 . 16 10 − 7 DM b ¯ b p = 0 . 43 DM τ + τ − 10 − 8 10 0 10 1 10 2 p = 0 . 065 E [GeV] Calore, Cholis, Weniger [1409.0042] 3 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 3/18
DM Fits: 3 σ Regions p -value ⟨ σv ⟩ m χ χ 2 min ¯ 1 . 75 +0 . 28 48 . 7 +6 . 4 23.9 0.35 bb 10 − 25 − 0 . 26 − 5 . 2 ¯ 5 . 8 +0 . 8 173 . 3 +2 . 8 43.9 0.003 tt τ + τ − W + W − − 0 . 8 − 0 5 . 33 +0 . 68 125 . 7 +3 . 1 29.5 0.13 ¯ qq ZZ hh − 0 . 68 − 0 cc ¯ hh 3 . 52 +0 . 48 80 . 4 +1 . 3 36.7 0.026 W + W − − 0 . 48 − 0 ¯ ¯ bb tt 4 . 12 +0 . 55 91 . 2 +1 . 53 35.3 0.036 ZZ − 0 . 55 − 0 gg � σv � / A [cm 3 s − 1 ] Calore,Cholis,McCabe,Weniger [1411.4647] 10 − 26 10 hh W � W � tt bb 8 � Σ � � � � 10 � 26 cm 3 � s � ZZ 6 � Σ � � � 2.2 � 10 � 26 cm 3 � s 10 − 27 10 1 10 2 4 m χ [GeV] Calore, Cholis, McCabe, Weniger [1411.4647] 2 Uncertainties in DM halo 0 0 50 100 150 200 250 A = [0 . 17 , 5 . 3] ( J = [0 . 19 , 3] ) m Χ � GeV � Agrawal, Batell, Fox, Harnik [1411.2592] 4 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 4/18
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( h SM → γγ ) ∼ 1 / (10 × tan 4 β ) . • Spectral line from a → γγ barely distinguishable from the continuum for m a ∼ 150 GeV and tan β ∼ 1 using Fermi-LAT resolution. • 2-peak structure in ha may be detectable in future experiments. 5 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 5/18
Spectral Fit for ha ha, m a =63 GeV E 2 d N/ d E [GeVcm − 2 s − 1 sr − 1 ] ha, m a =90 GeV ha, m a =120 GeV 10 -6 ha, m a =150 GeV b ¯ b hh 10 -7 10 -8 10 0 10 1 10 2 E [GeV] 6 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 6/18
Spectral Fit for aa aa, m a =63 GeV E 2 d N/ d E [GeVcm − 2 s − 1 sr − 1 ] aa, m a =90 GeV aa, m a =120 GeV 10 -6 aa, m a =150 GeV b ¯ b hh 10 -7 10 -8 10 0 10 1 10 2 E [GeV] 7 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 7/18
Best fit regions for ha 8 ha, m a =63 GeV 7 ha, m a =90 GeV / A [10 − 26 cm 3 s − 1 ] ha, m a =120 GeV 6 ha, m a =150 GeV b ¯ b 5 hh 4 3 � σv 2 � 1 40 60 80 100 120 140 160 180 m χ [GeV] 8 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 8/18
Best fit regions for aa 8 aa, m a =63 GeV 7 aa, m a =90 GeV / A [10 − 26 cm 3 s − 1 ] aa, m a =120 GeV 6 aa, m a =150 GeV b ¯ b 5 hh 4 3 � σv 2 � 1 40 60 80 100 120 140 160 180 m χ [GeV] 9 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 9/18
channel m a [GeV] m DM [GeV] p -value ⟨ σv ⟩ 0 [10 − 26 cm 3 / s] χ 2 min b ¯ 49 . 5 +8 . 1 1 . 8 +0 . 3 b 24 . 5 0 . 32 − 6 . 3 − 0 . 3 125 . 0 +2 . 3 4 . 9 +1 . 0 hh 30 . 0 0 . 12 0 . 0 − 0 . 9 94 . 0 +4 . 2 4 . 2 +0 . 8 63 22 . 4 0 . 43 0 . 0 − 0 . 8 107 . 5 +3 . 4 4 . 3 +0 . 8 90 25 . 3 0 . 28 ha 0 . 0 − 0 . 8 122 . 5 +3 . 0 4 . 5 +0 . 9 120 30 . 3 0 . 11 0 . 0 − 0 . 9 137 . 5 +2 . 7 4 . 7 +1 . 0 150 36 . 0 0 . 03 0 . 0 − 1 . 0 73 . 0 +15 . 4 3 . 1 +0 . 6 63 24 . 3 0 . 33 − 10 . 0 − 0 . 6 90 . 0 +10 . 9 3 . 7 +0 . 5 90 24 . 4 0 . 33 aa 0 . 0 − 0 . 8 120 . 0 +4 . 9 4 . 1 +0 . 8 120 31 . 0 0 . 10 0 . 0 − 0 . 8 150 . 0 +4 . 4 4 . 5 +1 . 0 150 41 . 4 0 . 01 0 . 0 − 1 . 0 10 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 10/18
Dark Matter Annihilation in the NMSSM χ → b ¯ b Annihilation • ˜ χ ˜ ¯ ¯ χ ˜ b χ ˜ b a Z χ ˜ b χ ˜ b 11 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 11/18
Dark Matter Annihilation in the NMSSM χ → a 1 h Annihilation • ˜ χ ˜ χ h ˜ χ ˜ h a ∗ χ 0 ˜ i a χ ˜ a χ ˜ 12 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 12/18
Early and late time cross sections for ha case 4 . 0 dSph limit bino-like 3 . 0 singlino-like � σ ah v � 0 [10 − 26 cm 3 / s] 2 . 0 1 . 0 0 . 8 0 . 7 1 2 3 5 7 10 20 � σv � T F [10 − 26 cm 3 / s] 13 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 13/18
Direct Detection for ha case 10 − 45 p [cm 2 ] 10 − 46 σ SI LUX LUX 300d Xenon1T 10 − 47 LZ bino-like singlino-like 10 − 48 100 110 120 130 140 150 χ [GeV] m ˜ 14 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 14/18
Resonance Condition for b ¯ b case with DSph bounds 1 . 10 a singlet-like a doublet-like correct Ω ˜ χ 1 . 05 2 m ˜ χ 1 . 00 m a 0 . 95 b v � 0 ∈ [1 , 1 . 5] × 10 − 26 cm 3 / s � σ b ¯ 0 . 90 30 35 40 45 50 m ˜ χ [GeV] 15 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 15/18
Direct Detection and Invisible decay for b ¯ b case 10 − 45 p [cm 2 ] σ SI 10 − 46 LUX LUX 300d Xenon1T a singlet-like a doublet-like correct Ω ˜ χ 10 − 47 30 35 40 45 50 χ [GeV] m ˜ 16 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 16/18
Direct Detection and Invisible decay for b ¯ b case 0 . 40 Br( h → inv) limit 0 . 35 CMS 300fb − 1 CMS 3000fb − 1 0 . 30 a singlet-like a doublet-like Br ( h → inv) 0 . 25 correct Ω ˜ χ 0 . 20 0 . 15 0 . 10 0 . 05 0 . 00 30 35 40 45 50 χ [GeV] m ˜ 16 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 16/18
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 17 / 18 Anibal D. Medina The University of Melbourne SUSY Implications from WIMP Annihilation into scalars at the Galactic Center 17/18
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