1. Yifang Wang Institute of High Energy Physics, CAS
IHEP
Yifang Wang
Institute of High Energy Physics, CAS

2. Accelerator: BEPC & BEPCII
ADONE
BEPCII
CESRc
BEPC
SPEAR
DORIS I
BEPCII/BESIII Upgrade:

3. Starting Point: Cosmic-rays
Since 50’s: Cosmic-rays at high altitude in Yunnan & Tibet using emulsion & cloud chambers
Since 90’s: Asg (China-Japan coll.) & ARGO (China-Italy coll.) in Tibet
Latest result: Asg observed high energy g-rays, up to 450 TeV, from Crab Nebula  important for the understanding of the origin and the acceleration mechanism of cosmic-rays
Yunnan, 3200m, 60’s
Cloud Chamber, 60’s
Tibet, 4200m
Tibet, 4200m, 90’s

4. Next: LHAASO (Large High Altitude Air Shower Observatory)
A large air shower array for cosmic-rays and g-astronomy
A combination of plastic scintillators, water and flourescent Cherenkov detectors
Complementary to CTA：
Time-variant and extended sources
Fast indication for CTA
¼ Construction completed. Full construction by 2020.
Sichuan, m a.s.l.
Main Array:
5195 scintillator detectors every 15 m
& 1146 –detectors every 30 m
Water Cherenkov Detector
80,000 m2

5. CMB at Tibet：AliCPT
AliCPT(5250m) is the best site in the north hemisphere for CMB: a great opportunity
Moisture in winter: 1.0 mm
Nearby(~6000m): 0.5 mm
Best in the world
Existing infrastructure
Good sky coverage
Goal:
Polarization of CMB for primordial gravitational waves
Prove of inflation at the very beginning of big bang
Status: under construction

6. X-ray astronomy in Space
Insight-HXMT
Insight-HXMT satellite was launched on June 15, 2017
Smooth operation
A number of papers published, including the search for EW signal during the neutron-star merger with GW detected ME LE HE
11.5 m × 8.78 m × 4.74m
eXTP
eXTP is the next generation telescope for“Enhanced X-ray Timing and Polarization Mission”
A leading flagship observatory for black holes, neutron stars and extreme physics
A large international collaboration

7. Cosmic-Rays in Space AMS02
3D crystal calorimeter for dark matter searches and cosmic-rays
Acceptance & energy range  10
Collaboration with Italy, Sweden, Switzerland, …
To be launched in 2025
X0(λ)
∆E/E for e
e/p sep GF
m2sr
HERD (2020)
55(3) 1%
10-6
3.1
Fermi (2008) 10
12%
10-3
0.9
AMS02 (2011) 17 2%
0.12
DAMPE (2015) 31
10-4
0.3
CREAM (2015)
20(1.5) --

8. Underground n Experiment: Daya Bay
Redundancy !!! n1 n2 n3
Solar n Oscillation
sin22q12 ~ 0.9
Atm. n Oscillation
Sin22q23 ~ 1
q13 ?
Cross check; Reduce errors by 1/N

9. A New Type of n Oscillation
Electron anti-neutrino disappearance observed in 2012:
R = ±0.011 (stat) ±0.004 (syst)
Sin22q13 =  0.016(stat)  0.005(syst)
c2/NDF = 4.26/4, σ for non-zero θ13
F.P. An et al., Phys. Rev. Lett. 108, (2012) ; citation > 2000

10. Implications and Prospects
sin22q13: One of 28 free parameters of the Standard Model; one of 6 oscillation parameters; complete the oscillation pattern.
Precision improved from ~ 20% to ~ 3%; Combined with T2K & Nova, leptonic CP Phase is estimated to be ~ -90o at 2s level
New experiments start: JUNO, DUNE/LBNF, HyperK,…
H. O’keeffe,

11. Next Step: The JUNO Experiment
NPP
Daya Bay
Huizhou
Lufeng
Yangjiang
Taishan
Status
Operational
Planned
Under construction
Power
17.4 GW
18.4 GW
Overburden ~ 700 m
20 kt Liquid Scintillator
Yangjiang NPP
Taishan NPP
Daya Bay NPP
Huizhou NPP
Lufeng NPP
53 km
Hong Kong
Macau
Guang Zhou
Shen Zhen
Zhu Hai
2.5 h drive
Daya Bay
JUNO
Previous site candidate
by 2020: 26.6 GW

12. Physics at JUNO
Mass Hierarchy sensitivity with 6 years' data(Thanks to large q13):
Properties of each kind of supernova n
Ref: Y.F Li et al,
PRD 88, (2013)
Relative Meas.
(a)Use absolute Dm2
(b)Realistic case 3s 4s
Precision measurement of mixing parameters
Current
JUNO
Dm212 4%
0.6%
Dm223
sin2q12 6%
0.7%
sin2q23
10%
N/A
sin2q13
6% 4%
~ 15%
Discovery of diffused Supernova n

13. JUNO Detector and Challenges
Largest LS detector   20 KamLAND，  40 Borexino
Highest light yield   2 Borexino，  5 KamLAND
Hugh cavern:
~ 50m 70m
Largest Acrylic tank:
F 35.4m(
20 kt LS
Best attenuation length: 25m Daya Bay)
” PMT
Highest photon detection efficiency : 30%*100% = SuperK）
44.5m
43.5m

14. JUNO Collaboration
17 countries/regions，77 institutions，~620 members

15. Neutrino Physics: Future
In ten years from now, oscillation will be completely understood. MH and CP phase will be determined
0n bb decay will be the next breakthrough
Hints from cosmology: mn < ~1 eV
Guess from Oscillation: mn ~1 meV
Katrin will probe to mn ~ 0.2 eV
0n bb decay should target for ~ 1meV
(m ve)eff =[Σi | Uei |2 m2 vi ]1/2
<Mee> = | Σi (Uei )2 m vi |
Isotopes
Mass(t)
<mbb>,meV
nEXO
136Xe 5
7-22
GERDA/Majorana
76Ge 1
10-40
SNO+
130Te 8
19-46
KamLAND-Zen
~20
JUNO-bb 50
4-12
Insert a balloon filled with 136Xe-loaded LS(or 130Te) into the JUNO detector
Zhao et al., arXiv: , CPC 41（2017）5

16. Accelerator: BEPC & BEPCII
ADONE
BEPCII
CESRc
BEPC
SPEAR
DORIS I
BEPCII/BESIII Upgrade:

17. Next Step: CEPC
Since 2005, we were discussing the next machine after BEPC/BEPCII
Thanks to the low mass Higgs, there is the possibility to build a Higgs Factory: Circular e+e- Collider(CEPC)
Looking for Hints (from Higgs)  direct searches
The tunnel will allow us to build pp, AA, ep colliders in the far future: Super proton-proton Collider(SppC)
The idea to build a circular Higgs factory followed by a proton machine, was discussed for the first time at the Higgs factory workshop in Oct. 2012

18. Precision Higgs Physics at CEPC
No signal at At LHC:
Direct searches: M ~ 1 TeV
10% precision: M ~ 1 TeV
Look for signals at CEPC:
1% precision  M ~10 TeV
CEPC preCDR Volume 1 (p.9)
Precision EW test, QCD & flavor physics are also important
10 TeV: New Physics < 10 TeV ?

19. Public release of printed CDR volumes in IHEP on 14th Nov., 2018
From Pre-CDR to CDR
CEPC CDR was released in Aug. & Oct., 2018
Public release of printed CDR volumes in IHEP on 14th Nov., 2018

20. CEPC Baseline Layout Lumi. Higgs W Z Z(2T) 1034 2.93 11.5 16.6 32.1
Baseline design: 100 km, 30MW/beam
Switchable between H and Z/W w/o hardware change (magnet switch)
Upgradable to 50MW/beam, ttbar & high Lumi Z
Lumi.
Higgs W Z
Z(2T)
1034
2.93
11.5
16.6
32.1
Luminosities exceed those in the pre-CDR

21. Accelerator R&D ……

22. International Collaboration
“China initiated large international science projects”
Goal: 1/3 international contributions
Seriously discussed at the European HEP strategy
International advisory board established
MOUs signed with many institutions
Workshop on CEPC-EU edition
May 24-26, 2018, Rome, Italy
April 15-17, 2019, Oxford
Next: May, 2020, Marseille
1/3 international participation

23. Other Accelerator Facilities
CSNS: 100 kW  500 kW
ADS injector: mA
250 mA  mA
HEPS: nmrad

24. Particle & Astro-Particle Physics at IHEP
Current
Future
Accelerator-based
Precision frontier
BESIII
ILC，FCC
CEPC  SppC
Belle II、PANDA、COMET，GlueX，LHCb
Energy frontier
CMS、ATLAS
Non-accelerator-based
Underground
Daya Bay
JUNO
nEXO
EXO
Surface
ARGO/ASg
LHASSO
AliCPT
Space
AMS
HERD
eXTP
HXMT