Chao-Qiang Geng - PowerPoint PPT Presentation

��� Dark Matter, Dark Energy & Neutrino Mass 暗物质，暗能量和中微⼦质量 Chao-Qiang Geng 理论物理前沿暑期讲习班 —— 暗物质，中微⼦与粒⼦物理前沿 中山⼤学广州校区南校园 2017 年 7 ⽉ 3-28 ⽇

Lecture 1: Introduction to Particle Physics and Cosmology Lecture 2: Some Basic Backgrounds of the Standard Model of Particle Physics Lecture 3: Neutrino Mass Generation Lecture 4: Theoretical Understanding of Dark Matter Detections Lecture 5: Dark Energy and Gravitational Waves

Lecture 4: Theoretical Understanding of Dark Matter Detections Outline • Introduction • Indirect Searches for Dark Matter • Direct Detections for Dark Matter • Conclusions

• Introduction

• Introduction 95% of the cosmic Have we seen matter/energy is a Dark Matter yet? mystery.

An Odyssey of Searching for Dark Matter ‭ ( ‬ DM ‭ ) ‬ 1783 J. Michell light can be affected by gravity 1844 F. Bessel the observed motion of Sirius and Procyon ~ dark stars 1846 the anomalous precession of the perihelion of Mercury ~ dark planet U. L. Verrier 1877 A. Secchi research on a nebulae ~ unseen matter scattered in space ~ dark clouds Lord Kelvin estimated the quantity of unseen matter in the galaxy & presented the End of 19 th upper limit on the density of matter century H. Poincare “ matiere obscure (French)” 1922 J. Kapteyn a quantitative model to address the possible existence of dark matter 1932 J. Oort analyzed and derived the value of the unseen matter’s local density 1933 F. Zwicky Studied the Coma cluster ~ high mass density needed to maintain the velocity dispersion of the galaxies ~ “dark matter” 1970 V. Rubin & The rotational velocities of the spiral galaxies are independent of the K. Ford distance away from galactic center ~ no “Keplerian decline”

☞ ☝ Cosmological scale Observations Galaxy cluster scale Galactic scale support Dark Matter at SNe Ia Concordance region: LSS CMB

Dark Matter: 26.8% Dark matter cannot be the particle in the standard model, which has to be: Massive Non baryonic No charge (electric or color) Stable ( τ > 10 26 s, τ universe ~ 10 17 s) WIMP Axion Sterile neutrino . . . . . .

Some Dark Matter Candidate Particles 24 10 21 10 18 10 15 10 12 10 Q-ball 9 10 6 10 Black Hole Remnant 3 10 0 10 -3 ! int (pb) 10 neutrinos WIMPs : wimpzilla -6 neutralino 10 -9 KK photon 10 branon -12 10 LTP -15 10 -18 10 -21 10 axion axino -24 10 -27 SuperWIMPs : 10 -30 10 fuzzy CDM gravitino -33 KK graviton 10 -36 10 -39 10 -12 10 -9 10 -6 10 -3 10 0 10 3 10 6 10 9 10 12 10 15 10 -33 10 -30 10 -27 10 -24 10 -21 10 -18 10 -15 10 18 10 mass (GeV) How to observe dark matter?

What is the real nature of Dark Matter ︖ Beyond the SM DARK MATTER ? DM

What is the real nature of Dark Matter ︖ Beyond the SM DARK MATTER ?

What is the real nature of Dark Matter ︖ Beyond the SM DARK MATTER ?

What is the real nature of Dark Matter ︖ Beyond the SM DARK MATTER ? ?

Search for Dark Matter: Some interaction beyond gravitation DM DM DM SM Direct Indirect detection detection SM SM DM SM Relic abundance Ω DM h 2 = 0.1196±0.0031 Ω DM : Ω OM ~ 5:1 DM DM SM DM Collider Astrophysical detection probes DM DM SM DM

Indirect detection: Search for Dark Matter: (cosmic-ray experiments) Direct detection: (underground experiments) Collider searches: ( LHC) AMS-02 Space Station

~2400m ������� ����������� CMDS-II DAMA, Xenon

• Indirect Searches for Dark Matter DM SM DM SM

Space Station AMS-02 Cosmic Ray Experiments Satellite Fermi PAMELA Balloon ATIC

☞ 12/8/ e + and e + +e - excesses Cosmic Ray Anomalies 2016 4/19/ 11/16/ 7/31/ 9/26/ 2/2/ 5/2/ 7/7/ 9/26/ 12/8/ 2013 2009 2010 2014 2015 2015 2015 2016 2016 Cited Fermi: Phys.Rev.Lett. 102 (2009) 181101 793 900 909 769 802 642 744 323 181 Online on May 4, 2009 arXiv:0905.0025 [astro-ph.HE] 807 822 701 692 556 627 657 345 ATIC: Nature 456 (2008) 362 258 PAMELA: Nature 458 (2009) 607 386 564 1040 1298 1372 1452 1481 1721 1748 arXiv:0810.4995 [astro-ph] Pulsars ...? Anomalies Dark Matter ? New theory of DM on arXiv every day! >200 570 300 500 630 635 550 590 600 2011/5/19 （ Endeavour ） Physics Result published on April 3, 2013 598 618 393 316 366 AMS-2: Phys.Rev.Lett. 110 (2013) 141102 12 240 74 208 233 0 35 58 AMS-02: Two new PRLs published on Sept. 19, 2014 47 152 169 0 22 38 - AMS days at CERN: p/p on April 15-17, 2015 (S. Ting) 15 30 -- 6 AMS-02: PRL117 (2016) 091103 (Aug. 26, 2016) 0 12

It can discriminate (9430 e + collected) background

It can discriminate (9430 e + collected) background

It can discriminate (9430 e + collected) (errors statistical only, larger at high energy) Solar activity below 10 GeV background

☞ It can discriminate (9430 e + collected) (errors statistical only, larger at high energy) Solar activity below 10 GeV background Steep e+ excess above 10 GeV with very large flux

Consistent with the background

It cannot discriminate e + and e - An e + +e - excess 300-800 GeV

Fermi’s result: PRL102(09)181101 It cannot discriminate e + and e - arXiv:0905.0025 [astro-ph.HE] Fermi Data 4 million events conflict with ATIC

2011/5/19「奮進號」 （Endeavour）太空梭

AMS is an International Collaboration 16 Countries, 60 Institutes and 600 Physicists, 17 years FINLAND HELSINKI UNIV. RUSSIA UNIV. OF TURKU I.K.I. ITEP DENMARK KURCHATOV INST. MOSCOW STATE UNIV. UNIV. OF AARHUS NETHERLANDS GERMANY ESA-ESTEC NIKHEF RWTH-I KOREA RWTH-III NLR USA MAX-PLANK INST. EWHA FLORIDA A&M UNIV. UNIV. OF KARLSRUHE KYUNGPOOK NAT.UNIV. FLORIDA STATE UNIVERSITY MIT - CAMBRIDGE FRANCE ROMANIA CHINA BISEE (Beijing) NASA GODDARD SPACE FLIGHT CENTER GAM MONTPELLIER ISS NASA JOHNSON SPACE CENTER IEE (Beijing) LAPP ANNECY UNIV. OF BUCHAREST TEXAS A&M UNIVERSITY IHEP (Beijing) LPSC GRENOBLE UNIV. OF MARYLAND - DEPT OF PHYSICS SWITZERLAND NLAA (Beijing) YALE UNIVERSITY - NEW HAVEN SJTU (Shanghai) ETH-ZURICH SEU (Nanjing) 中山⼤学，广州 UNIV. OF GENEVA SPAIN TAIWAN SYSU (Guangzhou) �� CIEMAT - MADRID ACAD. SINICA (Taiwan) SDU (Jinan) ITALY I.A.C. CANARIAS. AIDC (Taiwan) ASI CSIST (Taiwan) CARSO TRIESTE NCU (Chung Li) MEXICO IROE FLORENCE NCKU (Tainan) UNAM INFN & UNIV. OF BOLOGNA NSPO (Hsinchu) NCTU (Hsinchu) PORTUGAL INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA LAB. OF INSTRUM. LISBON INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA The detectors were built all over the world and assembled at CERN, near Geneva, Switzerland

Fermi with earth Mag.F. AMS-02:PRL110,141102(2013) PRL108,011103(2002) AMS02 4/3/2013 4x10 5 e + collected AMS02 consistent with PAMELA but not Fermi

PRL(9/19/2014)

PRL(9/19/2014) PRL(9/19/2014) PRL(4/3/2013)

PRL(9/19/2014) Recent&Development& � PRL113, 221102 (2014) Nov. 28, 2014

AMS days at CERN: anti-proton on April 15-17, 2015 (S. Ting) (AMS-02: 290,000 antiprotons selected) PRL117 (2016) 091103 (Aug. 26, 2016)

AMS days at CERN: anti-proton on April 15-17, 2015 (S. Ting) (AMS-02: 290,000 antiprotons selected) H.B.Jin,Y.L.Wu,Y.F.Zhou arXiv:1404.04604 [hep-ph] AMS-02 data Consistent with the background - PRL117 (2016) 091103 (Aug. 26, 2016)

Six conditions for the evidence of Dark Matter ! (S.Ting)

AMS-2: six conditions for Dark Matter with five seen! ?

AMS-2: six conditions for Dark Matter with five seen! ? 5. The rate at which it falls beyond the turning point.

AMS-2: six conditions for Dark Matter with five seen! 2016 ? It would be observed in 2024! 丁肇中 Talk at CERN on Dec. 8, 2016 中國 `` 悟空 ’’ 衛星

Possible interpretations: e + and e + +e - excesses Astrophysics: nearby pulsars ...... Particle physics: Dark Matter (DM) Dark matter annihilation: DM DM SM SM Dark matter decay: DM 2 or 3 SMs M ≥ 1 TeV, τ ≥ 10 26 s Note:

���������� �������� �������� a Kaluza-Klein mass of 620 GeV

Phys.Lett. B675, 77 (2009) C.H.Chen, C.Q.Geng, D.Zhuridov, JCAP 0910, 001 (2009) [0906.1646 [hep-ph]], Neutrino Masses, Leptogenesis and Decaying Dark Matter C.Q.Geng, D.Huang, L.H.Tsai, PRD89, 055021 (2014) [1312.0366 [hep-ph]], Imprint of Multicomponent Dark Matter on AMS-02 C.Q.Geng, D.Huang, C.Lai, PRD91, (2015) [1411.3813 [astro-ph]], Revisiting Multicomponent Dark Matter with New AMS-02 Data

The total e - and e + fluxes are: κ κ : the uncertainty in primary e - normalization Background: Secondary e - (e + ) produced in propagation, modeled by GALPROP e - (e + ) diffusion eq. and Two$Component+Decaying+DM � solved numerically by GALPROP DM source terms: Half% Density � ρ(x): DM density distribu3on, here we use isothermal profile τ i : DM life3me M i : DM Mass DM decay processes: model-dependent