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Monday colloquium

Monday colloquium. Probing Kaluza-Klein dark matter with neutrino telescopes Phys.Rev D67,055003 (2003) D.Hooper et.al. 2009 5/18 田中　隆之. Dark Matter （暗黒物質）.

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Monday colloquium

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  1. Monday colloquium Probing Kaluza-Klein dark matter with neutrino telescopes Phys.Rev D67,055003 (2003) D.Hooper et.al. 2009 5/18 田中　隆之

  2. Dark Matter（暗黒物質） • Must exist in the Universe(From the observation of the CMB, galactic rotation etc….). They has no radiation and it’s difficult to detect in the detector. Candidates: • Baryonic Brown and white dwarfs, neutron stars、　Black hole • Hot dark matter -> almost rejected Have the relativistic velocity particle decouple neutrino • Cold darkmatter Have the non- relativistic velocity particle decouple Weak Interacting Massive Particles = WIMP （SUSY-LSP, Axion , Kaluza-kleinparticle）

  3. Dark energy　～73％ Cold dark matter　～23％ Baryonic　～4％ Expected component of the Universe from the observation of large structure of the universe and CMB. Dark Matter2 Dark energy → Many theory is establishing. Collect the precise data about expanding universe Cold dark matter　→　direct search, indirect search Baryonic ＤＭ　→　search invisible bodies (ＭＯＡ)

  4. Cold Dark matter • The most appealing candidate for cold dark matter is WIMP(Weakly interacting Massive Particle) • Amount of the dark matter density can be obtained from the thermal relic of a weakly interacting stable neutral particle.(100GeV~10TeV) • WIMP requires new framework beyond the standard theory.(Search in the colliders also)

  5. SUSY WIMP The most popular and studied candidate is the lightest super symmetric particle(LSP) which is odd under R-parity. SUSY = Symmetry between fermion and boson Ex) lepton ⇔　slepton Gaugino ⇔　Gauge boson R-parity : parity between SM particle and SUSY particle ＬＳＰ　→　Ａ＋Ｂ＋・・　 １、If A,B ・・・=SM particle -> contradict due to R-Parity ２、If one of A,B ・・・　＝SUSY particle -> not ‘Lightest’ →LSP is stable and can become the Dark Matter (Neutralino, Gravitino)

  6. To detect the signal from DM WIMPs Indirect detection Direct detection Detect the signal of nuclear recoil in the detector (DAMA, XENON10,XMASS) Detect the particles(radiation) induced from WIMP annihilation (SK, Ice-cube, Fermi) WIMP Scatter WIMP ＷＩＭＰ　ＤＭ Scatter Annihilate Target nuclei Neutrino, Gamma … The earth Detector

  7. Other approach to make the CDM Super string and extra dimension of Universe 素粒子の正体は紐の振動 開いたひも とじたひも 10－35m 激しい振動→　大きな質量 緩やかな振動　→　小さな質量 一般相対論の導出や重力を含む統一力の記述が可能 →　ここに超対称性理論を仮定すると、超ひもの世界は10次元で安定である。（6次元は巻き上げられている）

  8. Brane宇宙 われわれの宇宙は10次元空間に浮かぶブレーン（膜）宇宙。 →　重力やGauge boson, SM場がそれぞれのブレーン間に染み出す。（これがダークマターやダークエネルギー源？）　これで標準理論の階層性問題も解決。 本論文では、Super stringを仮定してはおらず、「一つのコンパクトな」余剰次元が「TeV付近に折りたたまれて」存在するとして書かれている。（5次元） また、SM場が染み出す“Universal” extra dimension（UED模型）を仮定。

  9. UED模型

  10. KK number & KK parity XX次元における運動量保存則　＋　コンパクト化　 　　　　　　　　　　　　　　　　　　　　　　　　　→　KK parity LSPの場合と同じく、中性なLighest 1stKK particle(LKP) は安定である。

  11. LKP candidate Assuming mB1= 600 -1200GeV, and thermal equilibrium of LKP, relic density become ΩB1h2=0.16±0.04 ,which is the favorable region.

  12. Annihilation Channel Cross section from some approximation. Basically determined by SM couplings . Further study we must consider mass spectrum of the first KK level.

  13. Feature of the KK annihilation B1 interact with another KK particle also. • Coannihilation with the SU(2) singlet KK leptons reduced the effective cross section and hence reduces the predicted LKP mass, in contrast to SUSY. • Coannihilation with doublet KK leptons and KK quarks increases the effective cross section and the predicted LKP mass, due to larger SU(2) and SU(3) gauge couplings.

  14. Capture and Annihilation in the Sun • Basically calculation method is same as the case: WIMP is neutralino 1, Compute the interaction cross section of WIMPs in the Sun(DM density is given). 2, Assuming equilibrium, compare the capture rate with the annihilation rate. 3, Consider both SD and SI interaction

  15. SD and SI capture rate in the Sun SD : WIMP – proton interaction SI: WIMP- proton&Helium interaction SD cross section is typically three to for orders of magnitude larger than the SI cross section. -> SI scattering in the Sun is negligible.

  16. Approximated B1 cross section Scattering cross section is dominated by exchange of the right-handed KK quarks due to their larger hypercharge over left-handed KK quarks. Fractions of the spin carried by constituent quark q are written Therefore WIMP-proton SD cross section is written as

  17. Annihilation rate Change of the WIMP number in the Sun(N) is written as C: Capture rate A: annihilation cross section Annihilation cross section : Effective volume of the core : WIMP annihilation rate is written as t : the age of Solar system

  18. For the case of the Earth Earth: Small , Only occur scalar interaction WIMP capture is much slowly Consider optimistic case (mB1=500GeV, σH~106pb) 10-10 in the annihilation rate compared with Sun. It’s not realistic to B1 induced signal search from the Earth.

  19. Indirect Event Rate Relative annihilation fraction for each mode. (left side: assume all KK has same mass right side: assume heavy KK quark(more realistic)) Using the same equation as Edsjo, estimate the neutrino flux, upmu flux. (considering oscillation, neutrino E loss the Sun , upmu propagation …)

  20. Spectrum of muons at the Earth 600GeV WIMP 1000GeV WIMP

  21. Expected number of event From the expectation of R, 0.1<rqR<0.2 Solid sections is the region which give appropriate relic density. (ΩB1h2=0.14±0.04 ) Ice Cube can see the signal from a few to tens of events per year.

  22. Back Ground • Atmospheric neutrino -> low neutrino flux at the high energy (>100GeV) region(~ten event above 100GeV at 1km2 detector for the Sun direction) . Can simulate the rate. • Solar-atmospheric neutrino -> come from the Sun, and difficult to estimate. (< a few event per year at 1km2 detector? )

  23. Conclusion • Indirect detection of B1 dark matter is very promising at kilometer scale neutrino telescope. Considering mB1=600-800GeV, a few to tens of event can be detected. • Some model such as 6 dimension model indicate the more neutrino flux. Probably it will be soon excluded if large detector start the operation.

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