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![Page 1: 重いSUSY?(その動機と暗黒物質) 1. 重いSUSYの定義、そしてその動機について 2. 重いSUSYの予言する暗黒物質とLHC実験](https://reader033.fdocuments.net/reader033/viewer/2022061608/5697bff71a28abf838cbeb21/html5/thumbnails/1.jpg)
重い SUSY ?(その動機と暗黒物質)
1. 重いSUSYの定義、そしてその動機について
2. 重いSUSYの予言する暗黒物質とLHC実験
3. 重いSUSYのまとめと今後の展望
松本 重貴 ( カブリ数物連携宇宙研究機構 )
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]
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1/11
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
10-100
Mass (TeV)
0.1-1
Scalars
GauginosHiggsinos
Scalars
Gauginos
HiggsinosScalarsGauginos
Higgsinos
Scalars
GauginosHiggsinos
Split-SUSY Pure Gravity Focus point Super-split
[N. Arkani-Hamed & S. Dimopoulos, JHEP 0506, 2005]
[M. Ibe, T. Moroi, & T. T. Yanagida, PLB644, 2007]
[J. Feng, T. Moroi, and K. Matchev, PRD61, 2000]
もっと重かった これ中心にいく 横崎君トーク
[There must be several papers, since long ago.]
≒ SM
重いSUSYについて
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Gluinos
~ 現象論の観点からの重い SUSY を考える動機 ~
Mass(TeV)
100
10
1
0.1
BinoWinos
Gravitino,Scalars,Higgsinos
Higgs
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)標準模型 vs. 重い SUSY (PGM)
Higgs mass
Flavor/CP
Gravitino
Dark matter
Coupling U.
Naturalness
○
標準模型 重い SUSY
◎
◎ ○
○ ○
◎
◎
△
×
×
×
重いSUSYについて
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重いSUSYについて
Gluinos
~ 模型構築の観点からの重い SUSY を考える動機 ~Mass
(TeV)
100
10
1
0.1
BinoWinos
Higgs
MSSM SUSYNo singlets →
SUGRA interactions
[Inoue, Kawasaki,
Yamaguchi, Yanagida, 1992]
Gravitino,Scalars,Higgsinos
Minimal (Simplest) Setup!
[Okada, Yamaguchi, Yanagida, 1990; Ellis, et. al., 1990]
[H.Murayama, et. al., 1998;
L.Randall, et. al., 1999][Hisano, S.M., Nagai, Saito, Senami, 2007 (TH);
T. Moroi, et. al., 1999 (NT),]
= A conjecture on SUSY breaking mediation[Ibe, Moroi, Yanagida (2007), Ibe, Yanagida (2011), Ibe, Matsumoto, Yanagida (2012)]
Anomaly Mediation:
Dark Matter:
m-term:
Higgs mass:
[Gravitino mass is fixed to be O(100)TeV]Scalar masses:
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重いSUSYについて
Gluinos
Mass(TeV)
100
10
1
0.1
BinoWinos
Higgs
・ Effective Lagrangian: 長井君トーク
佐藤君トーク・ Gaugino masses (@ MSUSY scale):
+ other contributions
+ other contributions
+ other contributions
[From PQ sector [K. Nakayama & T. T. Yanagida, PLB722, 2013][Vector Matters [K. Harigaya, M. Ibe, T. T. Yanagida, JHEP1312]
・ Charged wino mass (Dm ~ 150—164 MeV)
・ Several DM regions:
[Independent of the gaugino mass]
[Y. Yamada, PLB682, 2010; M.Ibe, S.M., R. Sato, PLB721, 2013]
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]
Gravitino,Scalars,Higgsinos
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重いSUSYの暗黒物質
[J.Hisano, S.M., M.Nagai, O.Saito, M.Senami, 2007]
~ Wino dark matter region ~
Thermal relic abundance: Annihilations modes are w0w0, w + w - , w0w±, w±w±.
Wino DM with its mass of about 3.1TeV explains the Planck data.
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.
[M. Ibe, T. T. Yanagida, 2011]
The BICEP2 Result
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重いSUSYの暗黒物質~ Wino dark matter region ~
mwino
0.1TeV 0.5TeV 1TeV 5TeV
0.27 0.32 2.3 3.1
[PRD88, 2013]
Disappearingtrack search!
From Collider (LHC) experiment: From DM indirect detections:
• 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]
Continuum g
Fermi-LAT Limit
Line g
H.E.S.S. Limit
BICEP2
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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.
• 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]
BICEP2
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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.
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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.
• 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.
BICEP2
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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.
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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。
11/11
0.9TeV
0.5-1TeV
0.1-0.9TeV
BICEP2 の結果を考慮すると(TR = 2 x 109GeV を仮定 )
0.9-1TeV
0.9TeV
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