1. What Atomic Physics Can Do for Neutrino and Direct Dark Matter Detection? Jiunn-Wei Chen National Taiwan U. Collaborators: Chih-Liang Wu, Chih-Pang Wu (NTU) Chen-Pang Liu, Hsin-Chang Chih (NDHU) Keh-Ning Huang, Hao-Tse Shiao, Hao-Bin Li, Henry T. Wong, Lakhwinder Singh (AS)

2. Neutrino and Dark Matter are Portals to New Physics

4. Neutrino: Challenges and Opportunities Mass: hierarchy and absolute values Dirac or Majorana? CP phase(s) Sterile neutrinos? Electromagnetic properties: magnetic moments? Charge Radius?... Those are probes of new physics!

5. 5 How neutrino magnetic moment arises in SM? i jlW  i j lW

6. Neutrino Magnetic Moment (NMM) Flavor changing MM Flavor unchanging MM Dirac Majorana × (forbiden by CTP) (forbiden by CTP) ○○ ○ A probe of new physics!

7. Dark Matter (DM) Bigger density than the visible Universe Its existence hints that there might be a dark sector

8. Portals to the Dark Sector Other dark matter candidates include MACHOs: MAssive Compact Halo Objects WIMPs: Weakly Interacting Massive Particles

10. Why Atomic Physics? Energy scales: Atomic (~ eV) Reactor neutrino (~ MeV) WIMP (~ GeV) Neutrino: NNM atomic ionization signal larger at lower energy scattering (current Ge detector threshold 0.1 keV) DM: direct detection, velocity slow (~ 1/1000), max energy 1 keV for mass 1 GeV DM. Opportunity: Applying atomic physics at keV (low for nuclear physics but high for atomic physics)

11. Neutrino Atomic Ionization The complete set of neutrino electromagnetic form factor is can be constrained:

12. scattering Weak Interaction Magnetic moment Should go for low T (energy transfered)!

13. Two Approximations ---I Equivalent Photon Approx. proposed by Henry Wong et al. ( PRL 105 061801) photon q 2 ～ 0 : relativistic beam or soft photons q μ ～ 0 several orders of magnitude enhancement → tighen the μ ν constraint with the same set of data

14. Two Approximations --- II Free Electron Approx. revisited by Voloshin et al. ( PRL 105 201801) sum rule and Hydrogen-like calculation FEA works well at sub-keV regime

15. Toy: ν-H atomic ionization, exact result obtained (1307.2857)

17. Two Approximations Free Electron Approx. (revisited by Voloshin et.al) Equivalent Photon Approx. binding momentum of hydrogen: αm e ↓

18. 18 Ge atomic ionization: ab initio MCRRPA Theory MCRRPA: multiconfiguration relativistic random phase approx. Reducing the N-body problem to a 1-body problem by solving the 1-body effective potential self consistently. Hartree-Fock : RPA: RRPA: MCRRPA: ↓ Including 2 particle 2 hole excitations ↓ Correcting the relativistic effect ↓ More than one configurations in Hartree-Fock; Important for open shell system like Ge where the energy gap is smaller than the closed shell case

19. MCRRPA Theory N-electron relativistic Hamiltonian ↓ Dirac Hamiltonian + Coulomb interaction The rest of EM interaction Solve initial wavefucntion of atom Solve final wavefunction by time evolution ↓ ↓

20. Benchmark: Ge Photoionization Exp. data: Ge solid Theory: Ge atom (gas) Above 100 eV error under 5%. JWC et. al. arXiv: 1311.5294

21. Ge atomic ionization with ab initio MCRRPA Theory JWC et. al. arXiv: 1311.5294

22. Ge atomic ionization with ab initio MCRRPA Theory JWC et. al. arXiv: 1311.5294

23. Ge atomic ionization with ab initio MCRRPA Theory JWC et. al. 1411.0574

24. JWC et. al. arXiv: 1411.0574

25. Direct Dark Matter Detection RPP 2014

26. What Can Atomic Physics Contribute? Light dark matter detection: Electron recoil background from solar neutrinos for a LXe detector Large LXe detectors can be used as a neutrino/axion detectors as well (measuring NNM w/ a source nearby)

27. Electron Recoil Background for DARWIN (Lxe) L. Baudis et al 1309.7024

28. Summary Neutrinos and dark matter particles are portals to new physics Ab initio calculations of Ge neutrino atomic ionization performed with 5-10% estimated error. Xe can be done as well. Ongoing: dark matter atomic ionization

29. Searching for the QCD Critical End Point Jiunn-Wei Chen National Taiwan U. JWC, Jian Deng, Lance Labun 1410.5454

30. Universality In the scaling region, physics is the same within the same universality class---an effective field theory argument. QCD near CEP ~ Ising model (Stephanov)

31. 4 th moment CPOD 2014

32. 3 rd moment CPOD 2014

33. When the Imaginary is a Real Alternative Jiunn-Wei Chen National Taiwan U. Phys.Rev.Lett. 110 (2013) 262301 Collaborators: Jens Braun, Jian Deng, Joaquin E. Drut, Bengt Friman, Chen-Te Ma, Yu-Dai Tsai

34. From the hottest to the coolest, and back?

35. When Mr. Berry Meets Mr. Wigner Jiunn-Wei Chen National Taiwan U. JWC, Shi Pu, Qun Wang, Xin-Nian Wang Phys.Rev.Lett. 110 (2013) 262301

36. Flavor Structure of the Nucleon Sea from Lattice QCD Jiunn-Wei Chen National Taiwan U. arXiv:1402.1462 [hep-ph] Collaborators: Huey-Wen Lin, Saul D. Cohen, Xiangdong Ji

38. Backup slides

39. Solar Neutrino Flux

40. 40 Case study: NMM Reactor antineutrino ( ) GEMMA : Ge detector with threshold 1.5keV TEXONO: Ge detector with threshold 5keV Solar neutrino Borexino Astrophysical limit ( model dependent )

41. 41 scattering Weak Interaction Magnetic moment

42. How low i s low enough? Now sub-keV Ge detector is available!

44. Parton Physics on a Euclidean Lattice X. Ji, PRL, 2013

45. Schematic QCD Phase Diagram The location of the critical point (CEP)is still unknown. Th: Difficult to apply LQCD to the low T / high chemical potential region.

46. Our Contribution JWC, Jian Deng, Lance Labun,1410.5454 Work out the mapping in a simple model: 1+1dim Gross-Neveu model in the large N limit. Not in the same universality class--- different critical exponents but behavior similar. More diagrams not included are also important in the power counting: