Phenomenology of Wino Dark Matter

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Phenomenology of Wino Dark Matter. Shigeki Matsumoto (Kavli IPMU). Why Wino? What is the physics behind it? D irect & indirect detections of the wino. W ino dark matter detections at the LHC. Summary. 2/17. Why Wino?. ~ From viewpoint of cosmology ~. - PowerPoint PPT Presentation

Text of Phenomenology of Wino Dark Matter

Searching signals at the Nightmare scenario

Phenomenology ofWino Dark Matter Shigeki Matsumoto (Kavli IPMU)Why Wino? What is the physics behind it? Direct & indirect detections of the wino. Wino dark matter detections at the LHC. Summary.41 CMB, Circular velocity, Galactic clusters, LSS, Bullet clusters, etc. Why Wino? From viewpoint of cosmology Direct detection of DM, Indirect detections of DM (g, p, e, n, )- Electrically (color) neutral Non-baryonic (not p or n) Stable (or enough stable) Its motion is non-relativistic Its interactions are weak. WDMh2 = 0.110 (10-6 GeV/c.c.)Among those conditions, the most remarkable one is the stability of the dark matter. Why the dark matter is stable? Answer will be that there is a symmetry which guarantees the DM stability. 2/172 Why Wino?When DM has a non-zero B-L DM is ADM! mDM = 5 GeV/(B-L)DM. [M. Ibe, S.M., T. Yanagida, PLB708, 2012] We are focusing on the DM of B-L charge 0 Fermionic dark matter! SM contains fermions (of BL charge 1) & bosons (of BL charge 0)SM fermionSM bosonDMSM fermionSM fermionDM(DM is fermion w/ even BL charge)(DM is boson w/ odd BL charge)Which symmetry stabilizes the dark matter? U(1)B-L gauge symmetry. (Gauged U(1)BL (3 x R-neutrinos) Tiny neutrino masses & Leptogenesis) U(1)B-L is expected to be broken at higher scale by a VEV with (B-L) = 2, aso that a residual discrete symmetry, Z2 = (-1)B L U(1) B-L, remains.3/173 Why Wino? SUSY naturally provides a fermionic dark matter of B-L charge 0.Recent LHC results are saying SM-like higgs of 125 GeV. No SUSY signals observed.MSUSY 10 TeV when tanb 1 MSUSY 100 TeV when tanb 1 Fine tuning of 10-3 10-5 is required for mh=125 GeV. No SUSY-Flavor/CP problem. Consistent with negative results of the LHC exp. From viewpoint of particle physics Larger MSUSY than expected. L-R mixing of stops is large. Existence of extra-matters

[G. Degrassi,, arXiv:1205.649]How large should MSUSY be?4/174 Why Wino? What kind of SUSY model is there behind the high MSUSY scenario? Pure Gravity Mediation Model [M. Ibe, S.M., T. Yanagida, PRD85, 2012]MSSM SectorSUSY SectorR SectorNo singletsScalar fields in MSSM obtain softSUSY mass terms by tree-levelinteractions in supergravity; m0 m3/2 O(100) TeV SUSY scalar tri-linear couplings are expected to be suppressed in supergravity at tree level; A0 0 m3/2Supersymmetric and SUSY higgsmass parameters are generatedthrough tree-level interactionsin supergravity without havinga singlet SUSY breaking field; m B m3/2 O(100) TeV [K. Inoue, M. Kawasaki, M. Yamaguchi, T, Yanagida, PRD45, 1992; M. Ibe, T. Moroi, T. Yanagida, PLB 644, 2007] tanb = O(1) No gravitino problem [M. Kawasaki, K. Kohri, T. Moroi, PRD71, 2005; M. Kawasaki, K. Kohri, T. Moroi, A. Yotsuyanagi, PRD78, 2008] No Polonyi problem [G. D. Coughlan, W. Fischler, E. W. Kolb, S. Raby, G. G. Ross, PLB131, 1983]5/175 Why Wino? What kind of SUSY model is there behind the high MSUSY scenario? Pure Gravity Mediation Model [M. Ibe, S.M., T. Yanagida, PRD85, 2012]Gaugino masses are dominated byone-loop contributions in super-gravity, i.e. the anomaly mediatedcontributions. The gaugino massesare therefore suppressed by loopfactor in comparison with m0.Furthermore, higgsino thresholdcontributions is of the order ofa loop factor times m3/2, which gives sizable effects on massesof gauginos (Bino and Winos). [G. F. Giudice, M. A. Luty, H. Murayama, R. Rattazzi, JHEP9812, 1998. L. Randall, R. Sundrum,NPB557, 1999; M. Dine, D. MacIntire, PRD46, 1992; T. Gherghetta, G. F. Giudice, J. D. Wells, NPB559, 1999; M. Ibe, T. Moroi, T. Yanagida, PLB644, 2007] Neutral Wino is the dark matter Only gauginos are directly accessible in the near future.

6/176Thermal production m < 2.7TeV Non-thermal production (Wh2)NT = 0.16(m/300 GeV)(TR/1010 GeV) For successful leptogenesis, TR > 109.5 GeV m < 1 TeVHow heavy the wino can be?

Hisano, S.M., Nagai, Saito, Senami, PLB646 (2007). Why Wino?7/177 Direct & indirect detections of Wino dark matter(Ge, Xe, etc.)Using underground instruments,dark matter will be detected by observing recoil energies caused by scattering with nucleus. Scattering cross section betweenWino dark matter and a nucleonis estimated to be 10-47 cm2 when the higgs mass is 125 GeV. [J. Hisano, K. Ishiwata, N. Nagata, PLB690, 2010]DMNucleusDirect detection of the Wino dark matter

Scattering cross section should be smaller than 3 x 10-45 cm2 for mDM =100 GeV and 2 x 10-44 cm2 for mDM = 1 TeV because of the latest result of the XENON100. Scattering cross section of the wino is two orders of magnitude smatter than the above limit.8/178We are here!Extra Galactic g(Clusters, dSphs)p, p, e -gDark matter will (may) be detected by observing the products (gamma, anti-p, etc.) coming from dark matter annihilations in our galaxy (or nearby galaxies). Wino dark matter annihilates first into W boson pairs, and the annihilation products are provided through complicated cascade decays of the W bosons.

130 GeV line gamma-ray as well as the PAMEL anomaly cannot be reproduced by the Wino dark matter with being consistent with other indirect detections.DM halog

0.010.11100.10.511.5Wino mass (TeV)Annihilation cross section (in unit of 1024 cm3 /s)Wino + Wino W+ WTreeSommerfeld enhanced[Hisano, S.M., Nojiri, PRL92, 2004] Direct & indirect detections of Wino dark matter9/17

[A.Abdo et al. (LAT), APJ, Suppl.188, 2010]

Indirect detection using gamma ray Where it comes from? Galactic center Galactic clusters Galactic cluster Diffused gamma Milky-way satellites (dSphs) At present, observation of dSphs gives the most severe limit on sv. There are some ambiguities in the calculation of the g ray flux, which is caused by DM profiles in dSphs. (Especially, for ultra faint ones)

Fermi-LATHESSObservationSince g-ray signal from DM annihilation has not been observed yet, we have a limit on its cross section (sv). For Wino DM, sv is directly related to its mass.

mWino > 300 500 GeV Direct & indirect detections of Wino dark matter10/1710 Indirect detection using anti-protons PAMELAAMS-02

Observation Since anti-protons change their directions during the propagation in our galaxy, signal is observed as an anomalous excess of cosmic ray There are some ambiguities in the calculation of anti-proton fluxes, which is caused by DM profile in the galactic center as well as the propagation model. The latter one will be refined by the on-going experiment, say AMS-02.

Since anti-p signal from annihilationof DM has not been observed yet, we have a limit on its cross section (sv).

PAMELA: mWino > 210-700 GeV AMS-02: mWino > O(1000) GeV

Direct & indirect detections of Wino dark matter11/1711Signal is observed as an anomalousexcess of the e-component of CR.Since electron/positron loses itsenergy during the propagation viainverse Compton scatterings. Allthe energetic electrons/positronsoriginate in some sources close tothe solar system. Uncertainties ofthe propagation is small comparedto that of the anti-p observation.On the other hand, some BG exists which mimics the signal. PEMALE-AnomalyDark matter or astro-activity

Dark matter: Some models exist Astro-activity: Rotating PulsarsPAMELAAMS-02

Direct & indirect detections of Wino dark matter Indirect detection using electron/positron Observation12/17 Indirect detection using CMB anisotropy

WMAPPLANCKObservation The dark matter annihilation at recombination epoch may affect the spectrum of CMB anisotropy. The cross section of the dark matter annihilation is larger, the energy injection to cosmic environment is larger, resulting in the modification of spectrum. Cosmological and astrophysical uncertainties are quite small.Since the observed CMB spectrum is reproduced without DM effects, we have a limit on its cross section (sv).

WMAP: mWino > 230 GeV PLANCK: mWino > 500 GeV

[Ibe, S.M., Yanagida, 2012] Direct & indirect detections of Wino dark matter13/1713 Wino dark matter detections at LHC Conventional analysis (multi-jets + ET) Signal events topology Since all squarks are very heavy,the important signal process is the gluino pair production. Once the gluino is produced, it decays into a neutral/charged wino by emitting two quarks. As a result, its signal topology is multi-jets + ET.

The mass difference between the neutral and charged wino is about 160MeV [J. L. Feng, T. Moroi, L. Randall, M. Strassler, S. f. Su, PRL83, 1999], &the charged wino eventually decays into a neutral wino by emitting one soft pion, though this pion is hardly detected in a usual manner. [B. Bhattacherjee, B. Feldstein, M. Ibe, S. M., T. Yanagida,arXiv:1207.5453.]/GluinoGluinojetjetjetjetWinoWino

No signal has been detected, so that some parameter region in Pure Gravity Mediation model has been excluded

7TeV: mGluino > 1TeV & mWino > 300GeV 14TeV: mGluino > 2.3TeV mWino > 1 TeV 14/1714


Wino dark matter detections at LHC Hunting for disappearing chargino tracks Signal events topology

When at least one chargino exists in the final state of gluino pair production, it may be possible to detect the charged track caused by the chargino. This chargino eventually decays after traveling 10 cm, so that the track can be detected as a disappearing track.[S. Asai, T. Moroi, T. Yanagida, PLB664, 2008]

At present, TRT is used to