Very Weak Interactions or, what is 23% of the universe made of?

1. Very Weak Interactionsor, what is 23% of the universe made of? Itay Yavin New York University Rutgers University January 25, 2011

2. The Search for New Physics In particle physics, we are interested in the fundamental building blocks of nature. We are not just looking to discover new particles, but new principles and symmetries as well. We often call this quest for the basic interactions “the search for new physics”. How do we look for new physics? Where should we look for it? What is new physics ? How do we make sure we don’t miss it?

3. Principle Based Searches • Many searches are based on theoretical principles • Top discovery – anomaly free gauge-theory • Unitarization of W-boson scattering - Unitarity • Higgs boson – Renormalizability • Supersymmetry – solution to the hierarchy problem

4. Phenomenological Searches • Other searches are more phenomenological in nature • The discovery of Quantum Mechanics • Neutrinos and their properties • The discovery of the tau • Dark matter and weakly coupled physics

5. Theoretical Efforts How can theorists aid phenomenological searches? • Construct new models (hard, no obvious principals to follow) • Propose new searches • Suggest alternative explanations for observed anomalies • Critically examine and integrate all the known results • Calculate experimental observables

6. Missing Things Neutrinos were first noticed as missing energy-momentum in beta decays. It took 23 years before their existence was confirmed. It took another 50 years to discover that neutrinos have a mass. Dark matter was first observed by Zwicky in cluster of galaxies. Over the past 70 years observers have seen evidence for dark matter over many length scales. But how does it interact? SNO – neutrino observatory

7. Content • Weakly Interacting Matter • The Exposure Frontier • Weak Interactions • The Energy Frontier

8. Weakly Interacting MatterThe Exposure Frontier

9. WMAP Bullet Cluster Lensing Effect Rotation curves Indirect Detection Dark Matter Direct Production Direct Detection

10. Getting Pushed by Dark Matter(or Direct Detection Experiments) Dark Matter leaves Dark Matter entering target Nuclear recoil event CDMS: 0912.3592

11. Detection Schemes CoGeNT From P. Salati’s review on Dark Matter CRESST-II

12. XENON10 CDMS CRESST A Tale of Two Experiments DAMA CoGeNT XENON100 Chang, Liu, Pierce, Weiner, and IY - 1004.0697 CoGeNT is NOT seeing light dark matter elastically scattering against the nucleus.

13. Magnetic inelastic Dark Matter How is DAMA different from the other experiments? Is there a dark matter candidate that would show up in DAMA, but not in other experiments? (inspired by inelastic dark matter, Tucker-Smith and Weiner hep-ph/0101138) Chang, Weiner, and IY - 1007.4200 A Magnetic dipole interaction: • DAMA’s crystals are made NaI: • Heavy target (iodide) • Large magnetic dipole

14. Event Rate How many events do we get for a given cross-section? astrophysics Particle physics

15. Experimental Signatures It can be searched for by other experiments and enjoys an additional unique signature. After the collision, the excited state travels some distance before it de-excites and emits a photon, CDMS Such a DM state explains the annular modulations seen by DAMA while avoiding the other null results of other experiments. CRESST-II XENON10 KIMS ZPELIN-III Standard cuts will likely miss these events, but with some care it may not be hard to distinguish from background.

16. Open Questions • Are there any bounds from experiments looking for neutrinos from the Sun? (not as strong as for the original iDM scenario – Nussinov, Wang, and IY, 0905.1333) • Can such a scenario lead to the correct relic abundance? • What are the bounds from collider searches? • Are there convincing models that exhibit such a phenomenology? • Will it be seen by the XENON100 experiment? Inelastic, Exothermic, Magnetic DM Maybe the most important result of such scenarios is that they force us to think beyond the usual elastic scattering phenomenology. Inelastic, Exothermic, and Magnetic DM all result in unique experimental signatures. Elastic Scattering

17. Weak ForcesEnergy Frontier

18. Probing Weak Forces Muon anomalous magnetic moment Precision measurements of atomic transitions Lepton-Jets Low-energy colliders

19. Holdom Boson – A Case Study A very simple theoretical example of a weak force is illustrated through the Holdom effect (Holdom, Phys.Lett. B166), The mixing term results in a coupling of the new boson to the electromagnetic current, The story becomes even more intricate once supersymmetry is included and new scales can emerge – Cheung, Ruderman, Wang, and IY, 0902.3246

20. Example: Rare Z Decay Let’s consider the rare decay of the Z boson into a Holdom-boson and some extra scalar. New and interesting type of objects appear, Lepton Jets - A collimated collection of energetic leptons with a small opening angle(Arkani-Hamed and Weiner, 0810.0714) A’ Dark Cascades A’ q q A’

21. Dark/Hidden Sectors This phenomenon is very general. It occurs when we consider new light states coupled to the Standard Model, Irrelevant Operators Marginal Operators (Motivated by recent astrophysical anomalies – Arkani-Hamed et al. 0810.0713) Dark sectors phenomenology, Baumgart, Cheung, Ruderman, Wang, and IY, 0901.0283 Hidden Valleys, Strassler and Zurek, hep-ph/0604261 Lepton-jets are the hallmarks of an extra weakly coupled sector with a low scale.

22. Full Evolution We implemented the relevant physics into a Monte-Carlo based simulation,

23. Lepton Jets Lepton Jets - Cheung, Ruderman, Wang, and IY, 0909.0290 This definition grew out of a very fruitful exchange with the experimentalists who actually conducted the search for these objects.

24. Experimental Search Y. Gershtein and A. Haas have recently concluded the first search for these exotic objects at the Tevatron for D0 - Phys.Rev.Lett. 105 (2010) More searches are planned for the LHC in both CMS and ATLAS.

25. TeV GeV MeV keV Frontiers Tevatron, LHC Energy Frontier Weakly coupled physics be here Exposure Frontier Large targets (Sun,Earth) Exposure (CDMS,XENON) Luminosity (CHARM,Babar) Precision Frontier Atomic physics

26. Conclusions There is no guarantee any of the searches I described will succeed. There is no deep principle that ensures us something will definitely show up. But, the frontiers are expanding and many promising explorations are underway. By casting a wide net we hope to catch something interesting. Keep in mind that . . . Dark Matter 23% Dark Energy 73% “Us” 4%

27. Thank You

28. Muonic Hydrogen The long-waited measurement of the proton radius in muonic hydrogen was released this summer from the Paul Scherrer Institute (PSI). The surprising result is that it differs by 5 s.d. from the world’s average. (reminder: original Lamb shift was the first observation of a QED effect – circa 1947) Pohl et al. Nature 466:213-216,2010

29. A New Force? The discrepancy can be the result of a new force between the proton and the muon. It can also help explain the long standing discrepancy in the muon anomalous magnetic moment (Tucker-Smith and IY, 1011.4922). Vector force fit to muon g-2 • Constraints: • Neutron-Lead scattering • Lamb-shift in ordinary hydrogen • Neutrino reactions • It is yet unclear whether such a force can be obtained from a simple particle physics model. Measured deviation Scalar force fit to muon g-2 Cannot be a Holdom boson type of force – would have been seen in ordinary Hydrogen

30. Predictions • More measurements in muonic systems are planned in PSI and elsewhere. This framework allows for concrete predictions about these systems, • Muonic Deuterium • Muonic Helium • True Muonium