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 重い SUSY ？（その動機と暗黒物質）

最近の BICEP2 の影響に ついて も言及する！ [Harigaya, Ibe, Ichikawa, Kaneta, S.M., arXiv:1403.5880].  重い SUSY ？（その動機と暗黒物質）. 松本 重貴　 ( カブリ 数物 連携宇宙研究機構 ). 重い ＳＵＳＹの定義、そしてその動機について 重いＳＵＳＹの予言する暗黒物質とＬＨＣ 実験 重いＳＵＳＹのまとめと今後の展望. 1/11. 重いＳＵＳＹについて. 全て のスカラー粒子（ヒッグスを除く）が 10—100TeV と重い SUSY 模型 ↓

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 重い SUSY ？（その動機と暗黒物質）

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  1. 最近のBICEP2の影響についても言及する！ [Harigaya, Ibe, Ichikawa, Kaneta, S.M., arXiv:1403.5880] 重いSUSY？（その動機と暗黒物質） 松本 重貴　(カブリ数物連携宇宙研究機構) 重いＳＵＳＹの定義、そしてその動機について 重いＳＵＳＹの予言する暗黒物質とＬＨＣ実験 重いＳＵＳＹのまとめと今後の展望

  2. 1/11 重いＳＵＳＹについて 全てのスカラー粒子（ヒッグスを除く）が10—100TeVと重いSUSY模型 ↓ フェルミオニック超対称粒子は？ 様々な可能性 Mass (TeV) Split-SUSY Pure Gravity Focus point Super-split Scalars Scalars Scalars Scalars Higgsinos 10-100 Gauginos Higgsinos Gauginos Higgsinos Higgsinos Gauginos 0.1-1 Gauginos [M. Ibe, T. Moroi, & T. T. Yanagida, PLB644, 2007] [J. Feng, T. Moroi, and K. Matchev, PRD61, 2000] [There must be several papers, since long ago.] [N. Arkani-Hamed & S. Dimopoulos, JHEP 0506, 2005] もっと重かった これ中心にいく 横崎君トーク ≒ SM

  3. 2/11 重いＳＵＳＹについて • ～ 現象論の観点からの重いSUSYを考える動機 ～ • Phenomenological advantages • Higgs mass of 126GeV • SUSY Flavor/CP prob. relaxed • Dark matter candidate • No gravitino problem • Compatible w/ leptogenesis • GUT works (永田君トーク） Mass(TeV) Gravitino, Scalars,Higgsinos 100 標準模型 vs. 重いSUSY (PGM) 10 標準模型 重いSUSY Gluinos ◎ ○ Higgs mass Flavor/CP Gravitino Dark matter Coupling U. Naturalness Bino 1 ◎ ○ Winos ○ ○ Higgs ◎ × 0.1 × ◎ △ ×

  4. 3/11 重いＳＵＳＹについて • ～ 模型構築の観点からの重いSUSYを考える動機 ～ Mass(TeV) Gravitino, Scalars,Higgsinos Scalar masses: [Gravitino mass is fixed to be O(100)TeV] [Inoue, Kawasaki, Yamaguchi, Yanagida, 1992] m-term: 100 Minimal (Simplest) Setup! SUGRA interactions MSSM SUSY No singlets → 10 Gluinos Anomaly Mediation: [H.Murayama, et. al., 1998; L.Randall, et. al., 1999] Bino 1 Winos [Hisano, S.M., Nagai, Saito, Senami, 2007 (TH); T. Moroi, et. al., 1999 (NT),] Dark Matter: Higgs 0.1 Higgs mass: [Okada, Yamaguchi, Yanagida, 1990;Ellis, et. al., 1990] = A conjecture on SUSY breaking mediation [Ibe, Moroi, Yanagida (2007), Ibe, Yanagida (2011), Ibe, Matsumoto, Yanagida (2012)]

  5. 4/11 重いＳＵＳＹについて 長井君トーク ・ Effective Lagrangian: Mass (TeV) Gravitino, Scalars,Higgsinos 佐藤君トーク ・ Gaugino masses (@ MSUSY scale): + other contributions 100 + other contributions + other contributions [From PQ sector [K. Nakayama & T. T. Yanagida, PLB722, 2013] [Vector Matters [K. Harigaya, M. Ibe, T. T. Yanagida, JHEP1312] 10 Gluinos ・ Charged wino mass (Dm ～ 150—164 MeV) Bino [Independent of the gaugino mass] 1 Winos [Y. Yamada, PLB682, 2010; M.Ibe, S.M., R. Sato, PLB721, 2013] Higgs ・ Several DM regions: 0.1 1. Bino DM  This region has already been ruled out.2. Wino DM  [Hisano, S.M., Nagai, Saito, Senami, 2007]3. Coannihilation regions  [Harigaya, Kaneta, S. M., 2014]

  6. 5/11 重いＳＵＳＹの暗黒物質 • ～ Wino dark matter region ～ Thermal relic abundance: Annihilations modes are w0w0, w＋w－, w0w±, w±w±. Wino DM with its mass ofabout 3.1TeV explains the Planck data. • [J.Hisano, S.M., M.Nagai, • O.Saito,M.Senami, 2007] Non-thermal contribution: Gravitino produced after inflation.  Its decay into DM at late time. DWDMh2 = 0.16(m/0.3TeV) ×(TR/1010GeV). [Gherghetta, Giudice; Wells, Moroi, Randall, 1999] Wino DM with its mass less than 3.1TeV explains the Planck data. The BICEP2 Result • [M. Ibe, T. T. Yanagida, 2011]

  7. 6/11 重いＳＵＳＹの暗黒物質 • ～ Wino dark matter region ～ 2.3 3.1 0.27 0.32 mwino 0.5TeV 5TeV 0.1TeV 1TeV From Collider (LHC) experiment: From DM indirect detections: BICEP2 Fermi-LAT Limit [PRD88, 2013] Continuum g H.E.S.S. Limit Disappearingtrack search! Line g • Wino mass up to 500GeV will be explored in future (100fb-1@14TeV). • Is it possible to use “the double disappearing tracks search” at HL-LHC? • Chargino productions via VBF is useful? [s~ 0.4fb@14TeV, |Dh| > 4.2][Bhattacherjee, Feldstein, Ibe, S.M., Yanagida, PRD87, 2013, Snowmass rept. arXiv:1308.0355]

  8. 7/11 重いＳＵＳＹの暗黒物質 • ～ Bino-Gluino coannihilation ～ Thermal relic abundance: Annihilations modes:gluino + gluino (Sommerfeld) gluino + bino (Suppressed) bino + bino (Suppressed) Chemical equilibrium between gluino and bino maintains due to conversion processes, etc. BICEP2 • Dark matter can be as heavy as several TeV with the mass differencebetween gluino and wino being of the order of O(100)GeV. • No signals are expected in direct and indirect DM observations. • The only possible way to explore the DM is the use of “Hadron Collider”. • Process at the LHC is pp  gluino + gluino (gluino  bino + two jets),where the gluino is degenerated with the bino dark matter. • Initial state radiations play important roles, pp  gluino+gluino+jet(s).Bino mass up to 1TeV will be covered in near future (green/blue lines). • [B. Bhattacherjee, et. al., PRD89, 2014, S. Mukhopadhyay, M. Nojiri, T. T. Yanagida, arXiv:1403.6028]

  9. 8/11 重いＳＵＳＹの暗黒物質 • ～ Wino-Gluino coannihilation ～ Thermal relic abundance: Annihilations modes:gluino + gluino (Sommerfeld) gluino + wino (Suppressed) wino + wino (Sommerfeld) Chemical equilibrium between gluino and bino maintains due to conversion processes, etc. • The mass of the dark matter is predicted to be 3—7 TeV in this region, where it is smoothly connected to 3.1TeV predicted by the wino DM. • In order to explore the DM in this coannihilation region, we have to rely on the indirect DM detection utilizing (monochromatic) g-rays, so that future air Cherenkov telescopes (CTA) will play important roles. • If we impose the limit from the line g-ray observation at H.E.S.S. with adopting the cuspy profile, the wino mass up to 3.3TeV is ruled out. [ T. Cohen, M. Lisanti, A. Pierce, and T. R. Slatyer, JCAP10, 061, 2013 ] • Even in such a case, we find the allowed mass region of 3.5—7 TeV.

  10. 9/11 重いＳＵＳＹの暗黒物質 • ～ Bino-Wino coannihilation ～ Thermal relic abundance: Annihilations modes: wino + wino (Sommerfeld) wino + bino (Suppressed) bino + bino (Suppressed) Chemical equilibrium between gluino and bino maintains due to conversion processes, etc. BICEP2 • The mass of the bino DM can be as heave as about 2TeV with the mass difference between the bino DM and the wino being 10—40GeV. • The bino mass less than 90GeV has already been ruled out by LEPII. • The most important process to explore the DM at the LHC is the wino production (charged wino + neutral wino, two charged wino modes).☆ Charged wino decays into W* + bino with almost 100% branching.☆ Neutral wino decays into Z* + bino, l+l– + bino, h* + bino, and their branching fractions depend on the masses of higgsino & sleptons. • The best process is pp  charged and neutral winos  llln + 2binos.

  11. 10/11 重いＳＵＳＹの暗黒物質 • ～ Wino-Bino coannihilation ～ Thermal relic abundance: Annihilations modes: bino + bino(Suppressed) bino + wino (Suppressed) wino + wino (Sommerfeld) Chemical equilibrium between gluino and bino maintains due to conversion processes, etc. • The mass of the wino DM is predicted to be smaller than 3.1TeV, with the mass difference between the bino DM and wino being 100—200 GeV. • In order to explore the DM in this coannihilation region, we have to rely on the indirect DM detection utilizing (monochromatic) g-rays, so that future air Cherenkov telescopes (CTA) will play important roles. • If we impose the limit from the line g-ray observation at H.E.S.S. with adopting the cuspy (Einasto or NFW) dark matter profile, the whole parameter (mass) space in this coannihilation region is ruled out.

  12. 11/11 重いSUSYのまとめと今後の展望 • 重いSUSYのシナリオ（Pure Gravity Mediation type）は、現象論及び理論の両側面から非常に魅力的。しかもゲージーノは軽いので、現在及び近い将来に行われる実験・観測でシグナルが見える可能性が有る。 • 重いSUSYのシナリオ（Pure Gravity Mediation type)が予言する暗黒物質（領域）とそれら検出に関する今後の展望は以下の通り。☆ Bino DM Region：ノーマルな宇宙論を考えると既に排除済み。☆ Wino DM Region：3.1TeV or (0.3—3.1TeV)を予言。質量が低い 領域はLHC（消失荷電トラック検出）が、高い領域はγ線を用いた暗黒物質の間接検出が有効。 • 　☆ Bino(DM)-Gluino:0.5—8TeVを予言。ハドロン加速器がアクセス可。　　　　　　　　　　　　　　　　特に縮退系のグルイーノ対生成の検出が大事。　　☆ Wino(DM)-Gluino:3.1—7TeVを予言。γ線を用いた暗黒物質の間接検出（銀河中心からのラインγ線）が大事。　　☆ Bino (DM)-Wino: 0.1—3TeVを予言。加速器における荷電&中性　　　　　　　　　　　　　　　　ウィーノ生成からのトリ・レプトン検出が大事。 • ☆ Wino (DM)-Bino: 2.8—3.1TeVを予言。γ線を用いた暗黒物質の間 接検出（銀河中心からのラインγ線）が大事。 BICEP2の結果を考慮すると (TR = 2 x 109GeVを仮定) 0.9TeV 0.5-1TeV 0.9-1TeV 0.1-0.9TeV 0.9TeV

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