1 / 22

Phenomenology of Wino Dark Matter

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 ～.

gema
Download Presentation

Phenomenology of Wino Dark Matter

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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.

  2. 2/17 Why Wino? ～ From viewpoint of cosmology ～ CMB, Circular velocity, Galactic clusters, LSS, Bullet clusters, etc. ＋ - 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 (10-6GeV/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.

  3. 3/17 Why Wino? Which symmetry stabilizes the dark matter?  U(1)B-L gauge symmetry. (Gauged U(1)B–L ∃(3 x R-neutrinos)  Tiny neutrino masses & Leptogenesis) U(1)B-Lis 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. SM contains fermions (of B–L charge 1) & bosons (of B–L charge 0) SM fermion SM fermion DM DM SM boson SM fermion (DM is fermion w/ even B–L charge) (DM is boson w/ odd B–L charge) 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!

  4. 4/17 Why Wino? ～ From viewpoint of particle physics ～ 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. ・Larger MSUSY than expected. ・ L-R mixing of stops is large. ・ Existence of extra-matters How large should MSUSY be? 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. [G. Degrassi, et.al., arXiv:1205.649]

  5. 5/17 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] Supersymmetric 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] MSSM Sector No singlets SUSY Sector R Sector Scalar fields in MSSM obtain softSUSY mass terms by tree-levelinteractionsin supergravity; m0～ m3/2～ O(100) TeV ・ 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] SUSY scalar tri-linear couplings are expected to be suppressed in supergravity at tree level; A0～ 0 ≪ m3/2

  6. 6/17 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.

  7. 7/17 Why Wino? How heavy the wino can be? Hisano, S.M., Nagai, Saito, Senami, PLB646 (2007). Thermal 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 TeV

  8. Direct & indirect detections of Wino dark matter • 8/17 Direct detection of the Wino dark matter (Ge, Xe, etc.) DM Nucleus 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 cm2when the higgs mass is 125 GeV. [J. Hisano, K. Ishiwata, N. Nagata, PLB690, 2010] 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.

  9. Direct & indirect detections of Wino dark matter • 9/17 10 Annihilation cross section (in unit of 10–24 cm3 /s) 1 Extra Galactic g (Clusters, dSphs) Sommerfeld enhanced DM halo g 0.1 Tree g Wino + Wino  W+ W– 0.01 1.5 0.5 1 0.1 We are here! - p, p, e± Wino mass (TeV) [Hisano, S.M., Nojiri, PRL92, 2004] Dark 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.

  10. Direct & indirect detections of Wino dark matter • 10/17 ～ Indirect detection using gamma ray ～ Observation Fermi-LAT HESS 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) [A.Abdo et al. (LAT), APJ, Suppl.188, 2010] Since 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

  11. Direct & indirect detections of Wino dark matter • 11/17 ～ Indirect detection using anti-protons ～ Observation PAMELA AMS-02 Since anti-protons change their directions during the propagation in our galaxy, signal is observedas 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 onewill 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

  12. Direct & indirect detections of Wino dark matter • 12/17 ～ Indirect detection using electron/positron ～ Observation PAMELA AMS-02 Signal 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-Anomaly！ Dark matteror astro-activity？ Dark matter: Some models exist Astro-activity: Rotating Pulsars

  13. Direct & indirect detections of Wino dark matter • 13/17 ～ Indirect detection using CMB anisotropy ～ Observation WMAP PLANCK 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. [Ibe, S.M., Yanagida, 2012] • 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

  14. 14/17 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.] jet jet Wino Gluino Gluino jet / jet Wino 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>1TeV

  15. 15/17 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 find the track. Since TRT is 1m away from the beam pipe,the current limit is notstronger than that of conventional one. If more inner detectors is used in near future, the limit will be much stronger. [B. Bhattacherjee, B. Feldstein, M. Ibe, S. M., T. Yanagida,arXiv:1207.5453.] 100cm 50cm 30cm 10cm The charged track of chargino has not been observed, so that some parameter region of the model has been excluded. 7TeV: Weaker than conventional one 14TeV: mGluino< 2.5 will be explored.

  16. 16/17 Wino dark matter detections at LHC ～ Direct production of the Wino dark mater ～ EWinteraction at LHCWhen the gluino is too heavy to be produced at the LHC, we have to consider the direct production of the Wino through EW interactions. Several production processes are considered so far, for example, (i) Wino production with a jet. [M. Ibe, T. Moroi, T. Yanagida, PLB644, 2007] (ii) Wino production via VBF.[B. Bhattacherjee, B. Feldstein, M. Ibe, S. M., T. Yanagida, arXiv:1207.5453] Since the cross sections of these processes are smaller than that of the gluino pair production, to find the chargino track is mandatory to extract the signal from SM BG. Estimation of the BG is difficult without use of real data. q g q (1-jet) Wino W q Wino q q W Wino Wino (VBF) Wino W q q (1jet): Cross section is not so small. BG against the track is large? (2jets): Cross section is very small. The BG is expected to be small.

  17. 17/17 Summary • From both viewpoints of cosmology & particle physics, the neutral Wino dark matter is now understood as one of attractive candidates for dark matter. • There is a simplest SUSY model behind the Wino dark matter, that is the pure gravity mediation of the SUSY breaking, which seems to be consistent with present LHC results as well as cosmological observations. • It is interesting to carefully consider indirect detection signals because the annihilation cross section of Wino is not suppressed (even if its mass is ～ 1TeV) due to the Sommerfeld enhancement. Current limit is mwino > 0.3TeV. • LHC currently gives limits on Wino and gluino masses to m gluino > 1TeV & mwino > 0.3TeV. Find tracks of chargino will be important in the future for both the gluino pair production and direct production of the Wino.

  18. Backup

  19. BU-2 Properties of the Wino Neutral wino mass Thermal production  m < 2.7 TeV Non-thermal production(Wh2)NT = 0.16(m/300 GeV)(TR/1010 GeV) For the successful leptogenesis,TR > 109.5 GeV  m < 1 TeV Hisano, S.M., Nagai, Saito, Senami, PLB646 (2007). Charged wino mass Charged wino is highly degeneratedwith neutral wino in their masses. Dm～ 165 MeV when m = 0.1-1 TeV Charged wino decays into a neutralwino by emitting a (soft) pion.c+  c0 + p+ (Decay length ～ 5 cm) Disappearing track at the LHC! Mass difference between neutral & charged winos.

  20. BU-3 Properties of the Wino Gluino mass Because of the higgsinothreshold contribution,L, the relation betweenGluino, Wino, and Binomasses is changed from the conventional anomaly mediation model such as Gluino Bino Wino mgluino/mwino > 3 (mgluino/mbino～ 3) Wino cross sections SI scattering X-sectionbetween wino & p(n)is O(10–47 ) cm2. Annihilation X-sectioninto W bosonsis 10–23 -10–24 cm3/s (Sommerfeld enhanced) Hisano, Ishiwata, NagataPLB690 (2010) Hisano, Matsumoto, Nojiri, PRL92 (2004)

  21. BU-4 Cross section: J. Hisano et al., PRL92, 031303 (2004) A. Hryczuk et al., JHEP1201, 163 (2012) Anti-proton: O. Adriani et al., PRL105, 121101 (2010) C. Evoli et al., arXiv:1108.0664. Gamma-ray: M. Ackermann et al., PRL107, 241302 (2011) A. Charbonnier et al., Mon. Not. R. Astron. Soc..418, 1526 (2011) CMB (Recombination): J. Hisano at al., PRD83, 123511 (2011) G. Hutsi et at., Astron. Astrophys. 535, A26 (2011) Ibe, Matsumoto, Yanagida, PRD85, (2012) Anti-proton: Currently large uncertainties from CR propagations. The situation will be improved at the AMS-02 experiment. (850 days PAMELA data. Assuming 1yr data taking with A eff = 0.25 m2 sr using DRAGON code @ AMS-02) Gamma-ray: From (Classical & Super-faint) dSphs with 2yrs data. ∃Uncertainties because of DM profiles inside dSphs. CMB (Recombination): DM annihilation affects the recombination history. Astrophysical uncertainties are very small.

  22. BU-5 Gluino pair production (w/o charged tracks):Signal is multiple jets with large missing energy. ATLAS collaboration, ATLAS-CONF-2012-033. CMS collaboration, CMS PAS SUS-12-002. Gluino pair production w/ charged tracks:Signal is multiple jets with large missing energy and charged disappearing track at the TRT. ATLAS collaboration, arXiv:1202.4847. ATLAS collaboration, ATLAS-CONF-2012-034. Direct production of charged wino w/ tracks: Signal is mono/two jets with missing energy and charged disappearing track at the TRT. Ibe, et.al., PLB644, 355 (2007). http://atlas.kek.jp/sub/documents/jps201203/. Bhattacherjee, Ibe, Matsumoto, Yanagida, in preparation. Gluino pair production (without charged tracks): Typical SUSY signal. Signal cross section (times acceptance) obtained using 11 categories of kinematical selections. Gluino pair production with charged tracks. It does not provide the most severe bound for the TRT is currently used. If SCT is used, it will give the severest one. Direct production of charged wino with their tracks. Signal can be detected even if the gluino is beyond the reach of the LHC experiment. No official result reported yet. LEP bound is only the one currently available, which is from the radiative return process of the wino pair production.

More Related