Supersymmetric dark matter with low reheating temperature of the Universe

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1 Supersymmetric dark matter with low reheating temperature of the Universe Sebastian Trojanowski National Center for Nuclear Research, Warsaw COSMO 204 Chicago, August 29, 204 L. Roszkowski, ST, K. Turzyński hep-ph/ /2 Supersymmetric dark matter with low reheating temperature of the Universe

2 Motivation What is the nature of dark matter (DM)? Lightest Supersymmetric Particle(?) LHC bounds SUSY scale M S TeV popular higgsino DM with m χ TeV......but what else? It s difficult to get neutralino dark matter with m χ > TeV Any prospects for discovery such heavy DM? Gravitino DM typically discussed upper limit on the reheating temperature T R GeV What about lower limit on T R? 2/2 Supersymmetric dark matter with low reheating temperature of the Universe

3 Reheating period in the evolution of the Universe At the end of a period of cosmological inflation: T 0 large potential energy of the inflaton field φ is transformed into the kinetic energy of recreated particles then T (reheating) If instantaneous reheating: Γ φ = H = 8π ρ 3M Pl 2 φ and ρ φ = ρ rad (T R ) TR 4 Γ φ = 4π3 g (T R ) 45 T R 2 M Pl defines reheating temperature T R If non-instantaneous reheating Boltzmann equations: dρ φ dt dρ R dt dn X dt G. F. Giudice, E. W. Kolb, A. Riotto hep-ph/000523, G. Gelmini et al. hep-ph/ = 3Hρ φ Γ φ ρ φ inflaton field = 4Hρ R + Γ φ ρ φ + σv 2 E X [ nx 2 (n eq X )2] = 3Hn X σv [ ( nx 2 (n eq X )2] + b ) Γ φ ρ φ m φ Radiation dominated (RD) epoch begins when T T R, radiation dark matter before the reheating period 3/2 Supersymmetric dark matter with low reheating temperature of the Universe

4 Reheating period evolution of the total supersymmetric yield Y = n / s Y = n s with n = i n i n n eq n n χ freeze-out (low T R ) reheating period (low T R ) freeze-out (high T R ) x = m χ / T T n χ RD epoch (low T R ) dilution due to fast expansion high T R low T R Dark matter particles freeze-out in the reheating period: freeze-out occurs at a slightly higher temperatures than in the standard case after freeze-out, but before the end of the reheating period, the DM particles are effectively diluted away Ω χh 2 (low T R ) ( ) 3 ( ) TR T old T fo new fo T fo new Ω χh 2 (high T R ) G. F. Giudice, E. W. Kolb, A. Riotto hep-ph/ Ω χh 2 (low T R ) < Ω χh 2 (high T R ) (w/o inflaton decays to DM) 4/2 Supersymmetric dark matter with low reheating temperature of the Universe

5 Supersymmetric dark matter with low T R in the (N)MSSM the lightest neutralino is natural DM candidate (R-parity conservation) depending on its composition it can be:, higgsino, wino, singlino (NMSSM) or a mixed state for or singlino DM relic density can vary by several orders of magnitude for a fixed m χ ( ) 2 ( ) 2 for DM Ω Bh 2 (high T R ) g /2 m l m l,fo 460 GeV m B M. Drees et al. hep-ph/ , J. D. Wells hep-ph/ Ω DM h 2 (high T R ) for higgsino and wino DM Ω χh 2 m 2 χ, wino DM Sommerfeld effect Ω DM h 2 = T R = GeV T R = 0 GeV higgsino wino p0mssm T R = 50 GeV T R = 00 GeV T R = 200 GeV high T R m DM (TeV) Ω DM h 2 (high T R ) Ω DM h 2 = GeV T R = 0 GeV p3nmssm (95% CL) singlino comp. > 99% > 95% T R = 50 GeV T R = 00 GeV T R = 200 GeV high T R m DM (TeV) 5/2 Supersymmetric dark matter with low reheating temperature of the Universe

6 Higgsino DM high T R correct relic density for m χ TeV testable DM direct detection σ SI p (XenonT) low T R (w/o inflaton decays to DM) correct relic density for m χ TeV still testable 0-7 p0mssm (95% CL) 0-8 higgsino high T R LUX p0mssm (95% CL) 0-7 higgsino 0-8 T R = 00 GeV LUX 0-9 Xenon T 0-9 Xenon T σ p SI (pb) 0-0 σ p SI (pb) m χ (TeV) m χ (TeV) 6/2 Supersymmetric dark matter with low reheating temperature of the Universe

7 Bino DM high T R correct relic density in the bulk region or with some specific conditions: (co)annihilations, resonances only partly testable in DM direct detection experiments possibly some hints from colliders (stau-coannihilation region) Bino DM low T R (w/o inflaton decays to DM) correct relic density for wide range of m χ depending on T R w/o specific mass patterns p0mssm (95% CL) T R = 0 GeV LUX p0mssm (95% CL) 0-7 higgsino 0-8 T R = 50 GeV LUX 0-9 Xenon T 0-9 Xenon T σ p SI (pb) 0-0 σ p SI (pb) m χ (TeV) m χ (TeV) 7/2 Supersymmetric dark matter with low reheating temperature of the Universe

8 Wino DM high T R correct relic density for m W 3 TeV (including Sommerfeld effect) J. Hisano et al. hep-ph/060249,a. Hryczuk et al. hep-ph/ excluded by DM indirect detection (γ-ray line) for m W 3.5 TeV T. Cohen et al. hep-ph/ , J. Fan et al. hep-ph/ , A. Hryczuk et al. hep-ph/ Wino DM low T R (w/o inflaton decays to DM) correct relic density for heavy wino DM testable direct and/or indirect DM detection p0mssm (95% CL) 0-7 higgsino 0-8 wino LUX T R = 50 GeV 200 Ω W ~ h 2 = 0.2 with Sommerfeld effect w/o Sommerfeld effect p0mssm (95% CL) σ p SI (pb) Xenon T T R [GeV] wino (ID excl.) m χ (TeV) m W ~ [TeV] 8/2 Supersymmetric dark matter with low reheating temperature of the Universe

9 Gravitino G DM superpartner of graviton extremely weakly interacting massive particle (EWIMP) interaction rate suppressed by M Pl 0 8 GeV not directly testable, but some hints from the LHC may be possible cosmological constraints Gravitino relic density Ω G h 2 = Ω NTP G h 2 + Ω TP Non-Thermal Production late decays of the next-to-lsp G h2 low T R Ω NTP h G 2 = m G m χ Ω χh 2 Big Bang Nucleosynthesis (BBN) constraints Thermal production scatterings of superparticles in the thermal plasma late-time decays of the next-to-lsp to gravitino initiate electromagnetic and hadronic cascades that destroy light nuclei in the early Universe this alters BBN predictions constraints depend on the next-to-lsp s lifetime τ and relic density Ω χh 2 as well as on the hadronic branching fraction B h K. Jedamzik hep-ph/060425, M. Kawasaki et al. hep-ph/ K. Jedamzik hep-ph/ , M. Kawasaki hep-ph/ /2 Supersymmetric dark matter with low reheating temperature of the Universe

10 mg e mnlsp ΩGe h2 = Gravitino DM low TR ΩNLSP h2 Bino next-to-lsp 0/2 Slepton next-to-lsp Bh & 0. τ m2e G m5e B lower Ωel h2 larger mge for mbe mg low Bh BBN requires τ. 0. s m 2/5 e G mbe &.4 GeV TeV ΩG~h2 = BBN excl. TR = 200 GeV NTP high TR too low ΩG~h2 mg~ = TeV higgsino wino stau sneutrino 3 BBN excl. 02 TR = 00 GeV 0 TR = 200 GeV l G me m2e 0 TR = 00 GeV 0 2 TR = 0 GeV 0 ΩG~h2 = 0.2 ΩLOSPh (high TR) ΩLOSPh2 (high TR) 05 TR = GeV G me5 6 higgsino wino stau sneutrino 0 m2e l mg~ = 0 GeV 6 4 τ 3 4 mlosp (TeV) 5 6 NTP high TR 2 too low ΩG~h mlosp (TeV) Supersymmetric dark matter with low reheating temperature of the Universe

11 Gravitino DM lower limit on T R BBN + relic density constraints lower limit on T R min T R (GeV) m τ ~ < 5 TeV m τ ~ < 0 TeV m τ ~ < 5 TeV LOSP min T R (GeV) sneutrino LOSP stau LOSP m G ~ (GeV) m G ~ (GeV) /2 Supersymmetric dark matter with low reheating temperature of the Universe

12 Conclusions for low enough reheating temperature T R neutralino freeze-out may occur before the RD epoch in the reheating period......this opens up new regions with neutralino dark matter regions with heavy higgsino or wino DM can be tested in direct/indirect detection experiments wino DM can be again allowed DM correct relic density w/o specific mass patterns gravitino DM in such scenario is only produced in non-thermal production BBN constraints in case of gravitino DM introduce lower limit T R 00 GeV 2/2 Supersymmetric dark matter with low reheating temperature of the Universe