Dark Radiation Constraints on Mixed Axion/Neutralino Dark Matter
André Lessa University of São Paulo
Moriond - March 11th, 2013
H. Baer, K. J. Bae, AL, arXiv:1301.7428 Outline
What is Dark Radiation?
Axions and Dark Radiation Supersymmetric Axion
CMB Constraints
Conclusions What is Dark Radiation? What is Dark Radiation?
◮ Number of relativistic species during matter-radiation decoupling (T ∼eV):
ρR = ργ + Nν ρν + ???
"Radiation" Neutrinos Dark Radiation What is Dark Radiation?
◮ Number of relativistic species during matter-radiation decoupling (T ∼eV):
ρR = ργ + Nν ρν + ???
"Radiation" Neutrinos Dark Radiation
◮ N Nν ρν +ρX 3 04 Or: eff = ρν → . (SM) What is Dark Radiation?
◮ Number of relativistic species during matter-radiation decoupling (T ∼eV):
ρR = ργ + Nν ρν + ???
"Radiation" Neutrinos Dark Radiation
◮ N Nν ρν +ρX 3 04 Or: eff = ρν → . (SM)
6000 Neff and CMB:
5000 )
2 Neff = 2
• Affects expansion rate K µ 4000 N = 3.04
) ( eff
→ shifts peak π
/(2 N = 4.34 3000 eff • Changes time of matter-radiation equality TT l → enhances 1st and 2nd peaks 2000 l(l+1)C
• ... 1000
102 103 Multipole Moment (l) Dark Radiation
2011: WMAP7 Neff = 4.34 ± 0.88 arXiv:1212.5226 SPT Neff = 3.86 ± 0.42 ACT Neff = 4.6 ± 0.80
2012-2013: WMAP9 Neff = 3.84 ± 0.40 WMAP9 NSPT 3 71 ± 0 35 SPT eff = . . ACT ACT Neff = 3.50 ± 0.42
2013-: Planck Neff =?? ± 0.2 Dark Radiation
2011: WMAP7 Neff = 4.34 ± 0.88 arXiv:1212.5226 SPT Neff = 3.86 ± 0.42 ACT Neff = 4.6 ± 0.80
2012-2013: WMAP9 Neff = 3.84 ± 0.40 WMAP9 NSPT 3 71 ± 0 35 SPT eff = . . ACT ACT Neff = 3.50 ± 0.42
2013-: Planck Neff =?? ± 0.2
SM → ✞∆Neff ≡ Neff − Neff < 1.6 (95% C.L.) ☎ ✝ ✆ Dark Radiation
2011: WMAP7 Neff = 4.34 ± 0.88 arXiv:1212.5226 SPT Neff = 3.86 ± 0.42 ACT Neff = 4.6 ± 0.80
2012-2013: WMAP9 Neff = 3.84 ± 0.40 WMAP9 NSPT 3 71 ± 0 35 SPT eff = . . ACT ACT Neff = 3.50 ± 0.42
2013-: Planck Neff =?? ± 0.2
SM → ✞∆Neff ≡ Neff − Neff < 1.6 (95% C.L.) ☎ ✝ ✆ ◮ What if the excess is real? Dark Radiation
2011: WMAP7 Neff = 4.34 ± 0.88 arXiv:1212.5226 SPT Neff = 3.86 ± 0.42 ACT Neff = 4.6 ± 0.80
2012-2013: WMAP9 Neff = 3.84 ± 0.40 WMAP9 NSPT 3 71 ± 0 35 SPT eff = . . ACT ACT Neff = 3.50 ± 0.42
2013-: Planck Neff =?? ± 0.2
SM → ✞∆Neff ≡ Neff − Neff < 1.6 (95% C.L.) ☎ ✝ ✆ ◮ What if the excess is real? • New relativistic species at T & eV
• mDR . eV (usually) → suppressed interactions with SM Dark Radiation
2011: WMAP7 Neff = 4.34 ± 0.88 arXiv:1212.5226 SPT Neff = 3.86 ± 0.42 ACT Neff = 4.6 ± 0.80
2012-2013: WMAP9 Neff = 3.84 ± 0.40 WMAP9 NSPT 3 71 ± 0 35 SPT eff = . . ACT ACT Neff = 3.50 ± 0.42
2013-: Planck Neff =?? ± 0.2
SM → ✞∆Neff ≡ Neff − Neff < 1.6 (95% C.L.) ☎ ✝ ✆ ◮ What if the excess is real? • New relativistic species at T & eV
• mDR . eV (usually) → suppressed interactions with SM • DR candidates: (light) sterile neutrinos, gravitinos, axions, ... Axion = Dark Radiation?
◮ QCD axion (Strong CP Problem)
6 ◮ 10 GeV ma ∼ 6 eV fa
g ◮ 9 fa & 10 GeV (astrophysical bounds) a αs ∝ ✔ fa → ma . meV g → small couplings ✔ Axion = Dark Radiation?
◮ QCD axion (Strong CP Problem)
6 ◮ 10 GeV ma ∼ 6 eV fa
g ◮ 9 fa & 10 GeV (astrophysical bounds) a αs ∝ ✔ fa → ma . meV g → small couplings ✔
◮ Coherent Oscillations → CDM Axion = Dark Radiation?
◮ QCD axion (Strong CP Problem)
6 ◮ 10 GeV ma ∼ 6 eV fa
g ◮ 9 fa & 10 GeV (astrophysical bounds) a αs ∝ ✔ fa → ma . meV g → small couplings ✔
◮ Coherent Oscillations → CDM
◮ Also produced thermally: g a Relativistic ✔
g
g g Axion = Dark Radiation?
◮ QCD axion (Strong CP Problem)
6 ◮ 10 GeV ma ∼ 6 eV fa
g ◮ 9 fa & 10 GeV (astrophysical bounds) a αs ∝ ✔ fa → ma . meV g → small couplings ✔
◮ Coherent Oscillations → CDM
◮ Also produced thermally: g a Relativistic ✔
−2 g → ✞∆Neff < 10 ☎→ Below CMB sensitivity
g g (Can✝ not explain possible✆ excess) Axion = Dark Radiation?
◮ QCD axion (Strong CP Problem)
6 ◮ 10 GeV ma ∼ 6 eV fa
g ◮ 9 fa & 10 GeV (astrophysical bounds) a αs ∝ ✔ fa → ma . meV g → small couplings ✔
◮ Coherent Oscillations → CDM
◮ Also produced thermally: g a Relativistic ✔
−2 g → ✞∆Neff < 10 ☎→ Below CMB sensitivity
g g (Can✝ not explain possible✆ excess)
◮ Non-thermal production? Supersymmetric Axion
◮ fa ≫ EW scale → Hierarchy Problem → Supersymmetry Supersymmetric Axion
◮ fa ≫ EW scale → Hierarchy Problem → Supersymmetry ◮ Supersymmetric Axion:
a → Aˆ → s + i a + a˜ saxion axion axino
• SM + a → MSSM + a, s, a˜ = PQMSSM Supersymmetric Axion
◮ fa ≫ EW scale → Hierarchy Problem → Supersymmetry ◮ Supersymmetric Axion:
a → Aˆ → s + i a + a˜ saxion axion axino
• SM + a → MSSM + a, s, a˜ = PQMSSM
• Couplings:
g g g˜ g a → a, s s a˜
g g g˜ g˜
a˜ a + s s
a˜ a Supersymmetric Axion
◮ fa ≫ EW scale → Hierarchy Problem → Supersymmetry ◮ Supersymmetric Axion:
a → Aˆ → s + i a + a˜ saxion axion axino
• SM + a → MSSM + a, s, a˜ = PQMSSM
• Couplings:
g g g˜ g a → a, s s a˜
g g g˜ g˜
a˜ ✛ a✘ + s s → Non-thermal axion production (if ms > 2ma) a˜ a
✚ ✙ Supersymmetric Axion
◮ PQMSSM Masses:
PQMSSM
q˜1,2, ˜l
Mass Scale g˜
˜t, b˜
LSP SM Supersymmetric Axion
◮ PQMSSM Masses:
PQMSSM
q˜1,2, ˜l s
Mass Scale g˜
˜t, b˜
LSP SM Supersymmetric Axion
◮ PQMSSM Masses:
PQMSSM
q˜1,2, ˜l s
Mass Scale g˜
˜t, b˜
LSP SM
a Supersymmetric Axion
◮ PQMSSM Masses:
PQMSSM
q˜1,2, ˜l s a˜ Mass Scale g˜
˜t, b˜
LSP SM
We assume: a
mLSP = me < m . ms ∼ mSUSY Z1 a˜ Supersymmetric Axion
s → a + a ◮ PQMSSM Masses: 1
PQMSSM 10-1 s → ~a + ~a q˜1 2, ˜l , 10-2 s BF a˜ s → g + g
Mass Scale -3 g˜ 10 m = 1.6 TeV ~g s → ~g + ~g ˜ -4 ˜t, b 10 m~a = 0.5 TeV
LSP 10-5 3 4 SM 10 10 ms (GeV) We assume: a
mLSP = me < m . ms ∼ mSUSY Z1 a˜ Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM) Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM)
◮ Dark Radiation = Axions Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM)
◮ Dark Radiation = Axions • Production: TP s → a + a Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM)
◮ Dark Radiation = Axions • Production: TP s → a + a
• ∆Neff & 1 → large saxion production Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM)
◮ Dark Radiation = Axions • Production: TP s → a + a
• ∆Neff & 1 → large saxion production
• CMB constrains saxion production! Supersymmetric Axion
◮ Dark Matter = Neutralino + Axions • Neutralino production: TP (∼ MSSM) e a˜ → g + g˜ → ...Z1 + X • Axion production: coherent oscillations (CDM)
◮ Dark Radiation = Axions • Production: TP s → a + a
• ∆Neff & 1 → large saxion production
• CMB constrains saxion production!
How are saxions produced in the early universe? Saxion Production
◮ Thermal Production g s
TP 2 g → ρs ∝ TR/fa
g g
g a˜
TP 2 g → ρa˜ ∝ TR/fa
g g˜ Saxion Production
◮ Thermal Production ◮ Coherent Oscillations: g s
TP 2 → ρ ∝ TR/f g s a CO 2 2 → ρs ∝ θs fa g g
• θs is UV dependent (inflation) g a˜ (θsfa ≡ s0)
TP 2 g → ρa˜ ∝ TR/fa
g g˜ Saxion Production
◮ Thermal Production ◮ Coherent Oscillations: g s
TP 2 → ρ ∝ TR/f g s a CO 2 2 → ρs ∝ θs fa g g
• θs is UV dependent (inflation) g a˜ (θsfa ≡ s0) • TP 2 Dominates at large fa and low TR g → ρa˜ ∝ TR/fa
g g˜
• Dominates at small fa and high TR CMB Constraints on TP
◮ Thermal Production of Saxions:
102 ∆ 10 CMB Excluded ( Neff > 1.6) 1 s(TP) 10-1 eff
N -2
∆ 10 10-3 10-4 10-5 107 108 109 1010 1011 1012 1013 T R (GeV)
• Saxion production increases with TR CMB Constraints on TP
◮ Thermal Production of Saxions:
102 ∆ 10 CMB Excluded ( Neff > 1.6) 1 s(TP) 10-1 eff
N -2
∆ 10 10-3 10-4 10-5 107 108 109 1010 1011 1012 1013 T R (GeV)
• Saxion production increases with TR ...but axino production increases at the same rate! CMB Constraints on TP
◮ Thermal Production of Saxions:
102 ∆ 10 CMB Excluded ( Neff > 1.6) 1 s(TP) 10-1 eff
N -2
∆ 10 10-3 10-4 10-5 107 108 109 1010 1011 1012 1013 T R (GeV)
• Saxion production increases with TR ...but axino production increases at the same rate!
ρ(s→aa) ∆Neff ∼ e ργ +ρ(a˜→Z1+γ) CMB Constraints on TP
◮ Thermal Production of Saxions:
102 ∆ 10 CMB Excluded ( Neff > 1.6) 1 s(TP) 10-1 eff
N -2
∆ 10 s(TP) + ~a(TP) 10-3 10-4 10-5 107 108 109 1010 1011 1012 1013 T R (GeV)
• Saxion production increases with TR ...but axino production increases at the same rate!
ρ(s→aa) ρ(s→aa) ∆Neff ∼ e → e ργ +ρ(a˜→Z1+γ) ρ(a˜→Z1+γ) CMB Constraints on TP
◮ Thermal Production of Saxions:
102 ∆ 10 CMB Excluded ( Neff > 1.6) 1 s(TP) 10-1 eff
N -2
∆ 10 s(TP) + ~a(TP) 10-3 10-4 10-5 107 108 109 1010 1011 1012 1013 T R (GeV)
• Saxion production increases with TR ...but axino production increases at the same rate!
ρ(s→aa) ρ(s→aa) ∆Neff ∼ e → e . 0.2 ργ +ρ(a˜→Z1+γ) ρ(a˜→Z1+γ) → Below WMAP9 sensitivity! CMB Constraints on CO
◮ Coherent Oscillation Production of Saxions: CMB Constraints on CO
◮ Coherent Oscillation Production of Saxions:
• Relevant at large fa → suppresses TP (no axino dilution) CMB Constraints on CO
◮ Coherent Oscillation Production of Saxions:
• Relevant at large fa → suppresses TP (no axino dilution)
CO 2 2 • ρs ∝ fa θs CMB Constraints on CO
◮ Coherent Oscillation Production of Saxions:
• Relevant at large fa → suppresses TP (no axino dilution)
CO 2 2 • ρs ∝ fa θs
• ∆Neff < 1.6 → Upper bound on fa! CMB Constraints on CO
◮ Coherent Oscillation Production of Saxions:
• Relevant at large fa → suppresses TP (no axino dilution)
CO 2 2 • ρs ∝ fa θs
• ∆Neff < 1.6 → Upper bound on fa!
1016 1016 θ θ s = 1 6 GeV) s fa = M /100 15 = 10 15 P 10 > 1.6 (T R 10 ∆ Neff 14 10 GeV) 14 10 = 10 10 > 1.6 (T R 13 ∆ Neff 13 10 |g |min = 6× 10-16 (ADMX) 10 |g |min = 6× 10-16 (ADMX) a γγ a γγ
(GeV) 12 (GeV) 12 -15 6 a 10 min × -15 a 10 min × GeV) f |g | = 6 10 (ADMX-II) f |g | = 6 10 (ADMX-II) a γγ a γγ = 10 10 GeV) 11 11 R 10 10 = 10 > 1.6 (T R eff 10 10 ∆ N 10 10 > 1.6 (T eff ∆ N
1 10 102 103 104 105 1 10 102 103 104 105 ms (GeV) ms (GeV) CMB Constraints
◮ Dark Matter:
e 2 • a˜ → ...Z1 + X → Ωe h enhancement Z1 2 • s → g + g → Ωe h dilution Z1 CMB Constraints
◮ Dark Matter:
e 2 • a˜ → ...Z1 + X → Ωe h enhancement Z1 2 • s → g + g → Ωe h dilution Z1
104 103 Xe100 Excluded 2 2 10 (Ω~ h > 0.026) Z 10 1 1 10-1 10-2 MSSM 2 -3 Ω~ h
2 10 Z1 -4 h
1 10 ~ Z 10-5 Ω 10-6 10-7 ∆ Neff > 1.6 10-8 10-9 10-10 10-11 10-12 109 1010 1011 1012 1013 1014 1015 1016 f a (GeV) Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data
• Large CO saxion production is already excluded by ∆Neff < 1.6 13 (fa . 10 GeV) Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data
• Large CO saxion production is already excluded by ∆Neff < 1.6 13 (fa . 10 GeV)
2 MSSM 2 • ∆Neff < 1.6 → Ωe h > Ωe h Z1 Z1 e → DM ∼ Z1 (WIMP Signal) Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data
• Large CO saxion production is already excluded by ∆Neff < 1.6 13 (fa . 10 GeV)
2 MSSM 2 • ∆Neff < 1.6 → Ωe h > Ωe h Z1 Z1 e → DM ∼ Z1 (WIMP Signal)
◮ If Planck confirms the excess in ∆Neff : Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data
• Large CO saxion production is already excluded by ∆Neff < 1.6 13 (fa . 10 GeV)
2 MSSM 2 • ∆Neff < 1.6 → Ωe h > Ωe h Z1 Z1 e → DM ∼ Z1 (WIMP Signal)
◮ If Planck confirms the excess in ∆Neff :
• ”evidence” for CO saxions (large fa → ADMX) or Conclusions
◮ Current CMB data starts to become sensitive to SUSY axion models
◮ In the mixed axion/neutralino DM scenario: • TP of saxions is still unconstrained...... will start to be probed by Planck data
• Large CO saxion production is already excluded by ∆Neff < 1.6 13 (fa . 10 GeV)
2 MSSM 2 • ∆Neff < 1.6 → Ωe h > Ωe h Z1 Z1 e → DM ∼ Z1 (WIMP Signal)
◮ If Planck confirms the excess in ∆Neff :
• ”evidence” for CO saxions (large fa → ADMX) or • axino LSP → no WIMP signal! What is Dark Radiation? Axions and Dark Radiation CMB Constraints Conclusions Backup
14/20 Cosmological Evolution
◮ Thermal Production:
1025
1021 Time 1015 SM
109 ) 4 103
1014
1013
-3 1012 (GeV 10
ρ 1011
1010
9 a (DR) -9 10 s ~ ~ 10 8 10 a Z1 7 10
106
-15 5 10 10 a (DM)
8 9 10 10
10-21
105 106 107 108 109 1010 1011 1012 1013 1014 R/R0 CMB Constraints
◮ Scan over parameter space:
104 CMB Excluded 103 ∆ ( Neff > 1.6) 102
10 ∆ Nmax(TP) 1 eff 10-1
-2
eff 10
N 10-3 ∆ 10-4
-5 -4 10 s0/fa = 10 10-6 s0/fa < 1 10-7 ≥ s0/fa 1 10-8 10-9 109 1010 1011 1012 1013 1014 1015 1016 f a (GeV) Experimental Constraints
L. Rosenberg’s talk @ Axions 2010, UF J.L. Hewett et al., arXiv:1205.2671 Dark Matter and Dark Radiation
MSSM 2 ◮ Bino LSP (Ωe h > 0.11) Z1
6 10 WMAP Excluded 5 10 Ω 2 4 ( ~ h > 0.12) 10 Z1 103 102 10 MSSM 2 1 Ω~ h Z
2 1 10-1 h 1 -2 ~ Z 10
Ω -3 10 BBN Allowed 10-4 10-5 BBN Excluded -6 ∆ 10 Neff > 1.6 10-7 10-8 10-9
109 1010 1011 1012 1013 1014 1015 1016 f a (GeV) Dark Matter and Dark Radiation
MSSM 2 ◮ Higgsino LSP (Ωe h < 0.11) Z1
104 103 Xe100 Excluded 2 2 10 (Ω~ h > 0.026) Z 10 1 1 10-1 10-2 MSSM 2 -3 Ω~ h
2 10 Z1 -4 h
1 10 ~ Z 10-5 Ω 10-6 10-7 ∆ Neff > 1.6 10-8 10-9 10-10 10-11 10-12 109 1010 1011 1012 1013 1014 1015 1016 f a (GeV) Supersymmetric Axion
◮ Axion production: coherent oscillations** (CDM) T ≫ ΛQCD: ma = 0 T ≪ ΛQCD: ma =6 0
CO CO 2 2 2 ρa = 0 ρa ∝ V(ai) = maθi fa − ◮ CO behave as cold matter (ρ ∝ R 3)
◮ Saxions can also oscillate, if θs =6 0
◮ θi is a random number of order 1