The Low Energy Physics Frontier of the Standard Model at the MAMI accelerator

1. Concettina Sfienti Johannes Gutenberg-Universität - Institut für Kernphysik, Mainz The low energy physics frontier @Mami: Results and Perspectives Sunday, April 13, 2014

2. The low energy physics frontier @Mami: Results and Perspectives Sunday, April 13, 2014

3. Why? How? Who? Where? The low energy physics frontier @Mami: Results and Perspectives Sunday, April 13, 2014

4. EU-DE-MZ-JGU-KPH Sunday, April 13, 2014

7. The MAMI Legacy Sunday, April 13, 2014

8. The MAMI Legacy Sunday, April 13, 2014

9. Upgrade to ... MAMI-C Harmonic Double Sided Microtron (2007) up to E = 1.6 GeV HIGH Intensity up to 100 µA Resolution σE < 0.100 MeV Polarization up to 80% @ 40µA Reliability 85% (7000 h/y) The MAMI Legacy Sunday, April 13, 2014

10. The Wheelers !"!"#$%&'()*"+&,-%(.*/" 01(%%"#$%&'()*+,-.+/"23%&'()4%'%(+" 01213'"456'78#9' Sunday, April 13, 2014

11. The Wheelers !"!"#$%&'()*"+&,-%(.*/" 01(%%"#$%&'()*+,-.+/"23%&'()4%'%(+" 01213'"456'78#9' !"#$%&'($)*+,+-$./'0&12-3! ! $!"##$%&41&566,1'*(78)*+,+-6$ ! !"#8.&,9:#$;1<6,'($4'((=$>!).$ Sunday, April 13, 2014

12. The Wheelers !"!"#$%&'()*"+&,-%(.*/" 01(%%"#$%&'()*+,-.+/"23%&'()4%'%(+" 01213'"456'78#9' !"#$%&'($)*+,+-$./'0&12-3! ! $!"##$%&41&566,1'*(78)*+,+-6$ ! !"#8.&,9:#$;1<6,'($4'((=$>!).$ !"#$%&'()*$+(,-&.,/$(/$(/$01$0-&2.3$23&40'(/5$ !"#$%&'!("#')*+,,&-."&*/012'3$ ! $%678$9&-,'(:0)0'$$ Sunday, April 13, 2014

13. The Realm Sunday, April 13, 2014

14. The Middle Earth of the Nuclear Realm LRP Nuclear Science Advisory Committee(2008) Resolution Complexity Simplicity Hot and dense quark-gluon matter Hadron structure Nuclear structure Nuclear reactions Nuclear astrophysics Applications of nuclear science Hadron-Nuclear interface Sunday, April 13, 2014

15. What is it all about? Sunday, April 13, 2014

16. Scales and Phases of Nuclear Matter Courtesy R.F.Carsten (WNSL) LOOKING INWARD Nucleon Nuclear Structure Nuclear Astrophysics Neutron Stars Hypernuclei Hot and Dense Matter OUTWARD LOOKING Sunday, April 13, 2014

17. First Constraint „If the Lord Almighty had consulted me before embarking upon creation, I would have recommended something simpler.“ King Alphonse X. of Castille and Léon (1221-1284), on having the Ptolemaic system of epicycles explained to him QCD in the non-perturbative regime F. Wilczek “QCD made simple” (http://www.frankwilczek.com/) Sunday, April 13, 2014

18. First Constraint Modern nuclear physics is about... !Linking QCD to many body systems UNEDF SciDAC Collaboration Universal Nuclear Energy Density Functional Sunday, April 13, 2014

19. The Beauty of the Electromagnetic Probe Clean probe of hadron structure " Electron-vertex well- known from QED " One-photon exchange dominates " Higher-order exchange diagrams are suppressed " Vary the wavelength of the probe to view deeper inside the hadron Sunday, April 13, 2014

20. The Proton Sunday, April 13, 2014

21. The Proton ...ask Prof. Wiki Sunday, April 13, 2014

22. The Proton Mass(MeV) One Millennium Quest Generation of Mass Not the elementary mass of the fermions ! Higgs Sector But the actual mass of the “Macroscopic” Hadron and its Composites Sunday, April 13, 2014

23. Nuclear Physics @ A=1 ≡ Nucleon Properties Introduction – Nucleon properties Proton / Neutron mass mp = 938.272046(21) MeV/c2 Discovered by E. Rutherford (1919) mn = 939.565379(21) MeV/c2 Discovered by J. Chadwick (1939) size moments of electric charge and magnetization distribution derived from form factor measurements shape departure from spherical symmetry determined in N −→ ∆ measurements stiffness electric and magnetic polarizabilities extracted from Virtual Compton scattering (VCS) Sunday, April 13, 2014

26. “ Diamonds are for ever ... Sunday, April 13, 2014

27. “ Diamonds are for ever ... Form Factors are e!ernal ” http://hyperphysics.phy-astr.gsu.edu/ Rutherford Scattering + relativistic electrons + nuclear recoil + magnetic moments = Mott Scattering Sunday, April 13, 2014

28. “ Diamonds are for ever ... Form Factors are e!ernal ” http://hyperphysics.phy-astr.gsu.edu/ Rutherford Scattering + relativistic electrons + nuclear recoil + magnetic moments = Mott Scattering Hofstadter, R., et al., Phys. Rev. 92, 978 (1953). d" d# = d" d# $ % & ' ( ) Mott * G(q) 2 Sunday, April 13, 2014

29. Form Factors from Elastic ep scattering Classical picture form factor: G(q2) = 1 e ∞ 0 ρ(r) sin qr qr 4πr2 dr dipole e.g. proton formfactor|G(q 2 )|! gaussian e.g. 6 Li momentum transfer |q| ! oscillating e.g. 40 Ca Fourier ⇔ Transform exponential chargedensity!(r) gaussian radius r sphere with diffuse edge charge distribution: ρ(r) = e (2π)3 ∞ 0 G(q2 ) sin qr qr 4πq2 dq Sunday, April 13, 2014

30. Cross section for one photon exchange (Rosenbluth-cross section + Separation at constant Q2) ... and the slope of GE charge distribution distribution of magnetic moments # Separated GE(Q2) and GM(Q2) $ but contribution from two photon exchange (TPE) Form Factors from Elastic ep scattering Sunday, April 13, 2014

31. ● Statistical precision σ 0.1% ● δθ 0.5 mrad vertical and horizontal ● Control of luminosity and systematic errors The latest MAMI measurement The experiment designed for ... high precision by redundancy % All quantities measured by more than one method Sunday, April 13, 2014

32. Rosenbluth with a twist “Super-Rosenbluth Separation”: fit of form factor models DIRECTLY to cross sections ● All Q2 and ε data are used in one ﬁt ● No projection to constant Q2 % no limit of kinematics ● One “estimator” % stat. theory “robust estimator” Sunday, April 13, 2014

33. Strong Interactions Hadron Structure Hadron Spectroscopy High-Energy Physics Precision Physics Atomic Physics Astrophysics The Low Energy Frontier !# $%'(#)*+%,-# %+./01 ...the Atomic Physics frontier Sunday, April 13, 2014

34. The Low Energy FrontierThe radius puzzle – Lamb shift in µH Nature 466, 213-216 (8 July 2010) Sunday, April 13, 2014

35. “WE are famous!” (ED) ! ! !!#$%#!'()*+, !!-).!/*+.!01.#%#+.0123 !4#+.+!)*%!.5#)%#.06'7!*18#%+.'18012! )!9%).)1 !:'80*+!)!9%).)1!0+!8)(01'1.! *16#%.'01.;!01!('1;!=!9%)6#++#+! ! ! !!#$%#!'()*+, !!-).!/*+.!01.#%#+.0123 !4#+.+!)*%!.5#)%#.06'7!*18#%+.'18012! )!9%).)1 !:'80*+!)!9%).)1!0+!8)(01'1.! *16#%.'01.;!01!('1;!=!9%)6#++#+! ....not just interesting: Tests our theoretical understanding of proton Radius of proton is dominant uncertainty in many QED processes Sunday, April 13, 2014

36. R. Pohl et al., Nature 466, (2010) 213 The Radius Puzzle Discrepancy is between muonic and electronic measurements Sunday, April 13, 2014

37. R. Pohl et al., Nature 466, (2010) 213 The Radius Puzzle Discrepancy is between muonic and electronic measurements Proton Radius Puzzle 57 muonic hydrogen 1962 1963 1974 1980 1994 1996 1997 1999 2000 2001 2003 2007 2008 2010 2011 0.780 0.800 0.820 0.840 0.860 0.880 0.900 0.920 Orsay, 1962 Stanford, 1963 Saskatoon, 1974 Mainz, 1980 Sick, 2003 Hydrogen Dispersion fit CODATA 2006 MAMI, 2010 JLab, 2011 Sick, 2011 CODATA 2010 year ! Protonradius(fm) Figure 1: Proton radius determinations over time. Electronic measurements seem to settle around rp=0.88 fm, whereas the muonic hydrogen value [1,2] is at 0.84 fm. Values are (from left to right): Orsay [10], Stanford [11], Saskatoon [12, 13], Mainz [14] (all in blue) are early electron scattering measurements. Recent new scattering measurements are from MAMI [4] and Jlab [15]. The green and cyan points denote various reanalyses of the world electron scattering data [16–21]. The red symbols originate from laser spectroscopy of atomic hydrogen and advances Pohl, Gilman, Miller, Pachucki review, arXiv:1301.0905, Novel beyond SM physics? Novel hadron physics? already excluded: missing atomic physics, structures in FF, anomalous 3rd Zemach radius Sunday, April 13, 2014

38. R. Pohl et al., Nature 466, (2010) 213 The Radius Puzzle Discrepancy is between muonic and electronic measurements New data are needed and they are coming ... Range of new experiment Belushkin (Dispersion Analysis 2007) Price (CEA 1971) Murphy (Saskatoon 1974) Borkowski (MAMI 1975) Simon (MAMI 1980) Bernauer (MAMI 2010) Four-Momentum Transfer Q2 / (GeV2 /c2 )ElectricFormFactorGp E/GDipole 0.010.0010.0001 1.02 1.01 1 0.99 0.98 0.97 0.96 Where should we determine the root-mean-square-radius? r2 E = −6 d dQ2 GE(Q2 ) Q2=0 Extrapolation to Q2 = 0, no absolute cross section! ...where should we determine the root-mean- square-radius? Extrapolation ! No absolute cross section Sunday, April 13, 2014

39. Possible experiments include: Redoing atomic hydrogen Light muonic atoms for radius comparison in heavier systems Electron scattering at lower Q2 (JLAB, MAMI) Muon scattering (MUSE@PSI) Improvements on Proton Radius Sunday, April 13, 2014

40. The Proton Radius Puzzle Sunday, April 13, 2014

41. Second constraint © Jens Rydén © Corgi Lane © ryandury It’s always just water Sunday, April 13, 2014

42. Second constraint © CERN © NASA It’s always just nuclear matter © SciencePhotoLibrary Sunday, April 13, 2014

43. Second constraint It’s always just nuclear matter Sunday, April 13, 2014

44. Second constraint Modern nuclear physics is about... !Unravelling the phases of nuclear matter LRP Nuclear Science Advisory Committee(2008) Sunday, April 13, 2014

45. Second constraint Modern nuclear physics is about... !Unravelling the phases of nuclear matter LRP Nuclear Science Advisory Committee(2008) Sunday, April 13, 2014

46. Second constraint Each PHASE can exist in a variety of states. Each STATE is characterized by defined properties Sunday, April 13, 2014

47. Second constraint Each PHASE can exist in a variety of states. Each STATE is characterized by defined properties The EOS summarizes the physically possible combination of states. PV = nRT Sunday, April 13, 2014

48. A heavy nucleus (like 208Pb) is 18 orders of magnitude smaller and 55 orders of magnitude lighter than a neutron star Yet bounded by the same EOS The Equation of State of Nuclear Matter © NASA © SciencePhotoLibrary Sunday, April 13, 2014

49. Strong Interactions Hadron Structure Hadron Spectroscopy High-Energy Physics Precision Physics Atomic Physics Astrophysics The Low Energy Frontier ...the Astrophysics frontier !#$% '()*+ !,-.(, Sunday, April 13, 2014

50. Where do the neutrons go? Pressure forces neutrons out against surface tension EOS Neutron Skin Measurements Sunday, April 13, 2014

51. Where do the neutrons go? Pressure forces neutrons out against surface tension EOS Neutron Skin Measurements Sunday, April 13, 2014

52. PV: the view in the mirror #) !*+,#-./0 1111/./././.1111 3456345634563456 78(358978(358978(358978(3589:#:#:#:#5%'5%'5%'5%' 7';7';7';7'; 9#9#9#9#5%'5%'5%'5%' 4484448444844484 #$%' (#)$$!%*'+, #-)'+! -!*#*$. /01!)2 #-)'+! /03)%*$. 2!)(4%! )(.22!$%., !!#$%*# #-)%+! 5 6 7!)8 #-)%+! !696: 5 Non-PV e-scattering Electron scattering γ exchange provides Rp through nucleus FFs Sunday, April 13, 2014

53. 1111/./././.1111 !*#*$. /01!)2 #-)'+! /03)%*$. 22!$%., !!#$%*# #-)%+! 5 6 7!)8 #-)%+! !696: 5 PV: the view in the mirror #) !*+,#-./0 1111/./././.1111 3456345634563456 78(358978(358978(358978(3589:#:#:#:#5%'5%'5%'5%' 7';7';7';7'; 9#9#9#9#5%'5%'5%'5%' 4484448444844484 #$%' (#)$$!%*'+, #-)'+! -!*#*$. /01!)2 #-)'+! /03)%*$. 2!)(4%! )(.22!$%., !!#$%*# #-)%+! 5 6 7!)8 #-)%+! !696: 5 Non-PV e-scattering Electron scattering γ exchange provides Rp through nucleus FFs PV e-scattering Electron also exchange Z, which is parity violating Primarily couples to neutron Sunday, April 13, 2014

54. PV: the view in the mirror #) !*+,#-./0 1111/./././.1111 3456345634563456 78(358978(358978(358978(3589:#:#:#:#5%'5%'5%'5%' 7';7';7';7'; 9#9#9#9#5%'5%'5%'5%' 4484448444844484 #$%' (#)$$!%*'+, #-)'+! -!*#*$. /01!)2 #-)'+! /03)%*$. 2!)(4%! )(.22!$%., !!#$%*# #-)%+! 5 6 7!)8 #-)%+! !696: 5 Non-PV e-scattering Electron scattering γ exchange provides Rp through nucleus FFs PV e-scattering Electron also exchange Z, which is parity violating Primarily couples to neutron Detectable in PV asymmetry of electrons with different helicity 23456234562345623456 78(358978(358978(358978(3589:#:#:#:#5%'5%'5%'5%' 7';7';7';7'; 9#9#9#9#5%'5%'5%'5%' 4484448444844484 !!#$%' (#)$$!%*'+, #-)'+! -!*#*$. /01!)2 #-)'+! /03)%*$. 2!)(4%! )(.22!$%., !!#$%*# #-)%+! 5 6 7!)8 #-)%+! !696: 5 Violating Electron Scattering − also exchange Z, which is parity olating rimarily couples to neutron: n ∝ 1 − 4 sin2 θW ≈ 0.076, Qneutron weak ∝ −1 e− Z Detectable in parity violating asymmetry of electrons with diﬀerent helicity In Born approximation, Q2 M2 Z , from γ − Z interference: APV = σ+ − σ− σ+ + σ− = GF Q2 4πα √ 2 1 − 4 sin2 θW − Fn(Q2) Fp(Q2) For ﬁxed target exp., typical APV ∼ 10−7 − 10−4 Sunday, April 13, 2014

55. Hard, harder, PV Experiments 3 Decades of Progess sub-part per billion statistical reach and systematic control sub-1% normalization control State-of-the-art: Sunday, April 13, 2014

56. Hard, harder, PV Experiments sub-part per billion statistical reach and systematic control sub-1% normalization control State-of-the-art: 3 Decades of Progess Roca-Maza et al ± 3% ± 0.06 fm PV Measurements@A1 (commissioning in Spring 2014 - 12C) Sunday, April 13, 2014

57. Diverse experiments but consistent results Too many model dependent observables Neutron skin Radii: Where are we? Precise determination of NSkin in 208Pb set a basic constraint on the nuclear symmetry energy does not. Then, we have to conclude that a 3% accuracy in APV sets modest constraints on L, implying that some of the expectations that this measurement will constrain L precisely may have to be revised to some extent. To narrow down L, though demanding more experimental effort, a 1% measurement of APV should be sought ultimately in PREX. Our approach can support it to yield a new accuracy near Árnp 0:02 fm and L 10 MeV, well below any previous constraint. Moreover, PREX is unique in that the and Grants No. FIS2008-01661 from MEC and FEDER, No. 2009SGR-1289 from Generalitat de Catalunya, and No. N N202 231137 from Polish MNiSW. [1] Special issue on The Fifth International Conference on Exotic Nuclei and Atomic Masses ENAM’08, edited by M. Pfu¨tzner [Eur. Phys. J. A 42, 299 (2009)]. [2] G. W. Hoffmann et al., Phys. Rev. C 21, 1488 (1980). [3] J. Zenihiro et al., Phys. Rev. C 82, 044611 (2010). [4] A. Krasznahorkay et al., Nucl. Phys. A731, 224 (2004). [5] B. Kłos et al., Phys. Rev. C 76, 014311 (2007). [6] E. Friedman, Hyperfine Interact. 193, 33 (2009). [7] T. W. Donnelly, J. Dubach, and Ingo Sick, Nucl. Phys. A503, 589 (1989). [8] D. Vretenar et al., Phys. Rev. C 61, 064307 (2000). [9] C. J. Horowitz, S. J. Pollock, P. A. Souder, and R. Michaels, Phys. Rev. C 63, 025501 (2001). [10] K. Kumar, P. A. Souder, R. Michaels, and G. M. Urciuoli, http://hallaweb.jlab.org/parity/prex (see section ‘‘Status and Plans’’ for latest updates). [11] M. Centelles, X. Roca-Maza, X. Vinãs, and M. Warda, Phys. Rev. C 82, 054314 (2010). [12] I. Angeli, At. Data Nucl. Data Tables 87, 185 (2004). [13] B. A. Brown, Phys. Rev. Lett. 85, 5296 (2000); S. Typel and B. A. Brown, Phys. Rev. C 64, 027302 (2001). [14] R. J. Furnstahl, Nucl. Phys. A706, 85 (2002). [15] A. W. Steiner, M. Prakash, J. M. Lattimer, and P. J. Ellis, Phys. Rep. 411, 325 (2005). [16] B. G. Todd-Rutel and J. Piekarewicz, Phys. Rev. Lett. 95, v090MSk7 HFB-8SkP HFB-17 SkM* Ska Sk-Rs Sk-T4 DD-ME2DD-ME1FSUGold DD-PC1PK1.s24 NL3.s25 G2 NL-SV2PK1NL3NL3* NL2 NL1 0 50 100 150 L (MeV) 0.1 0.15 0.2 0.25 0.3 ∆rnp (fm) Linear Fit, r = 0.979 Nonrelativistic models Relativistic models D1S D1N SGII Sk-T6SkX SLy5 SLy4 MSkAMSL0SIVSkSM*SkMP SkI2 SV G1 TM1 NL-SHNL-RA1 PC-F1 BCP RHF-PKO3Sk-Gs RHF-PKA1PC-PK1 SkI5 FIG. 3 (color online). Neutron skin of 208 Pb against slope of the symmetry energy. The linear fit is Árnp ¼ 0:101 þ 0:001 47L. A sample test constraint from a 3% accuracy in APV is drawn. PRL 106, 252501 (2011) P H Y S I C A L R E V I E W L E T T E R S week ending 24 JUNE 2011 X. Roca-Maza, at al. Phys. Rev. Lett. 106, 252501 (2011) Method 1 2 3 4 5 6 S(fm) 0.05 0.1 0.15 0.2 0.25 0.3 0.35 0.4 0.45 0.5 Pb Neutron Skin Radius 208 PREX Pb(p,p)208 Antiprotonic Atoms EDP PDR Pionic Atoms Sunday, April 13, 2014

58. ! Suggest what PV experiment can’t do: good quality skin thickness measurements of a wide range of nuclei: Do we need this systematics? Neutron skin Radii: Where are we? dy of neutron skins leadK ¼ À500þ125 À100 MeV. A value K ¼ À550 Æ 100 Mseems to be favored by the giant monopole resona(GMR) measured in Sn isotopes as is described in [Even if the present analyses may not be called deﬁnit 0 0.1 0.2 I = (N−Ζ) /Α -0.1 0 0.1 0.2 0.3 S(fm) 40 20Ca 58 28Ni 54 26Fe 60 28Ni 56 26Fe 59 27Co 57 26Fe 106 48Cd 112 50Sn 90 40Zr 64 28Ni 116 50Sn 122 52Te 124 52Te 48 20Ca 96 40Zr 120 50Sn 116 48Cd 126 52Te 128 52Te 124 50Sn 130 52Te 209 83Bi 208 82Pb 232 90Th 238 92U experiment linear average of experiment prediction Eq. (2) FSUGold SLy4 FIG. 2 (color online). Comparison of the ﬁt described in th text of Eq. (2) with the experimental neutron skins from anti protonic measurements and their linear average S ¼ ð0:9 Æ 0:15ÞI þ ðÀ0:03 Æ 0:02Þ fm [20]. Results of the modern Skyrme SLy4 and relativistic FSUGold forces are also shown. M. Centelles, et al Phys. Rev. Lett. 102, 122502 (2009) A. Trzcinska et al., Phys. Rev. Lett. 87, 082501 (2001); J. Jastrzebski et al., Int. J. Mod. Phys. E 13, 343 (2004). NSkin from antiprotonic-atoms: correlation between thickness and isospin Neutron radius is not directly measured ! strong dependence on theoretical models. Sunday, April 13, 2014

59. If YES then ... shine light on the nucleus! !#$%$'!#$%$'!#$%$'!#$%$' !!!!(((( )#')%*+!',)#')%*+!',)#')%*+!',)#')%*+!', -./0-./0-./0-./0 12.3#,$4.5 1678.0(9: ;;;;;;;; !!!!! #$%'(% )*+, (-./ #$0.0*/*+1 $2 #$+$23 .2%42(+#$23 5.++(#46$#746.'+$# ! #8783847.++(#4#.%*3 5$3+43*7/(49:;4.#$=*7.+*$2 !!!!! ?4- Sunday, April 13, 2014

60. If YES then ... shine light on the nucleus! !#$%$'!#$%$'!#$%$'!#$%$' !!!!(((( )#')%*+!',)#')%*+!',)#')%*+!',)#')%*+!', -./0-./0-./0-./0 12.3#,$4.5 1678.0(9: ;;;;;;;; !!!!! #$%'(% )*+, (-./ #$0.0*/*+1 $2 #$+$23 .2%42(+#$23 5.++(#46$#746.'+$# ! #8783847.++(#4#.%*3 5$3+43*7/(49:;4.#$=*7.+*$2 !!!!! ?4- Sunday, April 13, 2014

61. 208Pb neutron skin from Coherent π0 D. Watts, et al,EPJ Web of Conferences 37, 01027 (2012) Method 1 2 3 4 5 6 7 S(fm) 0.1 0.2 0.3 0.4 0.5 Pb Neutron Skin Radius 208 PREX Pb(p,p)208 Antiprotonic Atoms EDP PDR Pionic Atoms Coh.Ph.! Skin ~ 0.12 ±0.02(stat) fm Systematic error currently being finalised. expect ~0.05 fm p,d pickup PREX@JLAB Proton Scatt Antiproton@CERN Dipole MAMI-C q = 0 to 2 q =1st minima q=2nd minima q =3rd minima Eγγγγ=155±5 Eγγγγ=165±5 Eγγγγ=175±5 Eγγγγ=185±5 Eγγγγ=195±5 (fm-1) |q| = pγγγγ-pππππ0 (fm-1) PhD: Tarbert(Edinburgh) Skin ~ 0.12 ±0.02(stat) fm Systematic error currently being finalised. expect ~0.05 fm p,d pickup PREX@JLAB Proton Scatt Antiproton@CERN Dipole MAMI-C q = 0 to 2 q =1st minima q=2nd minima q =3rd minima Eγγγγ=155±5 Eγγγγ=165±5 Eγγγγ=175±5 Eγγγγ=185±5 Eγγγγ=195±5 |q| = pγγγγ-pππππ0 (fm-1) |q| = pγγγγ-pππππ0 (fm-1) Neutronskinthickness(fm) PhD: Tarbert(Edinburgh) New experimental campaign@A2 (October 2012) 116,120,124Sn, 58Ni, 208Pb (I = 0.03÷0.21) 208Pb Target Sunday, April 13, 2014

62. Concettina Sfienti Johannes Gutenberg-Universität - Institut für Kernphysik, Mainz ...perspective are excellent! Near future (2013-2015) .... Radius Puzzle: ISR and d-FF Neutron form factor: new neutron detector Nucleon polarizabilities with real photons High resolution pion spectroscopy of light hypernuclei PRECISION COMPLEXITY The Low Energy Frontier @ Mainz: Results and ... Sunday, April 13, 2014

63. Concettina Sfienti Johannes Gutenberg-Universität - Institut für Kernphysik, Mainz ...perspective are excellent! Near future (2013-2015) .... Radius Puzzle: ISR and d-FF Neutron form factor: new neutron detector Nucleon polarizabilities with real photons High resolution pion spectroscopy of light hypernuclei PRECISION COMPLEXITY The Low Energy Frontier @ Mainz: Results and ... Sunday, April 13, 2014

64. Strong Interactions Hadron Structure Hadron Spectroscopy High-Energy Physics Precision Physics Atomic Physics Astrophysics The Low Energy Frontier ...the discovery (HE, Precision, Astroparticle) frontier !#$%% '()(*% Sunday, April 13, 2014

65. Conventional strategies for DM searches ventional strategies for dark matter search in particle physics Direct Production: Tevatron, LHC Direct Search: CDMS, DAMA/LIBRA, XENON, CRESST, LUX, COUPP, KIMS, ... Indirect Search: PAMELA, Fermi, HESS, ATIC, WMAP, ... A bottom up approach: Looking for interacting particles Sunday, April 13, 2014

66. Conventional strategies for DM searches Assumptions: There is dark matter (SUSY or something else) Dark matter interacts with Standard Model matter (besides gravity) Dark matter interacts via a “dark force” Question: What is the character of this “dark force”? Scalar, pseudo-scalar, vector bosons? Massive or mass-less? Mass range? Size of the coupling constant? ventional strategies for dark matter search in particle physics Direct Production: Tevatron, LHC Direct Search: CDMS, DAMA/LIBRA, XENON, CRESST, LUX, COUPP, KIMS, ... Indirect Search: PAMELA, Fermi, HESS, ATIC, WMAP, ... A bottom up approach: Looking for interacting particles Sunday, April 13, 2014

67. A top down motivation ● Extra U(1) gauge bosons ubiquitous in well motivated extension of SM ● U(1) gauge bosons may be hidden (no interaction with SM) ● No reason for U(1) boson to be heavy ● Dark matter couples to U(1) bosons γ and γ’ ● Mixing parameter ε of γ/γ’ mixing ● Boson mass mγ’ 0 decay suppressed, macroscopic lifetime Look for χ at high energies OR for γ’ at low energies! B. Holdom Phys. Lett. B 166 (1986) 196 Kinetic mixing Dark matter couples to U(1) bosons γ and γ : e e γ ′γ∗ χ χ _ L ⊃ − 1 4 FSM µν Fµν SM − 1 4 Fhidden µν Fµν hidden + ε 2 FSM µν Fµν hidden + m2 γAhidden µ Aµ h Renormalization of charge: Sunday, April 13, 2014

68. Dark Photon Light weakly coupled U(1) gauge boson N. Arkani-Hamed, et al., Phys. Rev. D 79 (2009) 015014 Proton Radius Puzzle D. Tucker-Smith and I. Yavin Phys. Rev. D83 (2011) 101702 (g-2)µ anomaly M. Pospelov, Phys. Rev. D80 (2009) 095002 ...it explains ... terrestrial anomalies (DAMA, CDMS, XENON) satellite anomalies (PAMELA, FERMI) Probing Dark Forces @ GeV Scale Sunday, April 13, 2014

69. Probing Dark Forces @ GeV Scale Prediction are testable: Large cross section in leptons ' World wide effort (CERN, DESY, JLAB, MAMI, all e+e- colliders, ...)Proton Radius Puzzle D. Tucker-Smith and I. Yavin Phys. Rev. D83 (2011) 101702 (g-2)µ anomaly M. Pospelov, Phys. Rev. D80 (2009) 095002 ...it explains ... terrestrial anomalies (DAMA, CDMS, XENON) satellite anomalies (PAMELA, FERMI) Dark Photon Light weakly coupled U(1) gauge boson N. Arkani-Hamed, et al., Phys. Rev. D 79 (2009) 015014 Sunday, April 13, 2014

70. Search for the Dark Photon @ MAMI Bump Hunt: Quasi-photoproduction off 181Ta target H. Merkel et al., Phys. Rev. Lett. 106 (2011) 251802 Beam current:! 100µA Luminosity: L = 1.7·1035 (s·cm2)-1 Minimal angles for spectrometers Geometry as symmetric as possible (background reduction) Coincidence time resolution! ≈ 1 ns FWHM Almost no accidental background! ≈ 5% Above background: only coincident e+e− pairs! δme+e− 0.5MeV/c2 Sunday, April 13, 2014

71. MixingParameter 2 Dark Photon Mass m ’ (MeV/c2 ) 10 -7 10 -6 10-5 10 -4 10 100 (g-2)!(g-2)e vs. BaBar A1-2011 e e #! ! |(g-2)!| 2 E774 KLOE APEX Bump Hunt: Quasi-photoproduction off 181Ta target % Fight background .... ... with high intensity ... ... and resolution. Search for the Dark Photon @ MAMI H. Merkel et al., Phys. Rev. Lett. 106 (2011) 251802 Feasibility: Background (within 1%) First exclusion limits 10−3 New ε/mγ’ scan 4 days beam time!! APEX: S. Abrahamyan et al., Phys. Rev. Lett. 107 (2011) 191804 KLOE: F. Archilli et al., Phys. Lett. B. 706 (2012) 251 PRELIMINARY Future: Low mass region 50 MeV/c2 and small dark photon coupling ε2 Sunday, April 13, 2014

72. ... MESA beyond MAMI ... Harald Merkel, European Few Body 22, Krak´ow 09/2013 MESA: Mainz Energy recovering Superconducting Accelerator Superconducting LINAC Three recirculation arcs for external beam high external current for “next generation” parity violation experiments Energy recovery mode (half wave-length recirculation) for internal target experiments Current Energy Luminosity External Beam Mode: 150 µA 200 MeV 1039 cm−2 s−1 Energy Recovery Mode: 10 mA 150 MeV 1036 cm−2 s−1 Mainz Energy recovering Superconducting Accelerator Sunday, April 13, 2014

73. Concettina Sfienti Johannes Gutenberg-Universität - Institut für Kernphysik, Mainz ...perspective are excellent! Near future (2013-2015) .... Radius Puzzle: ISR and d-FF Neutron form factor: new neutron detector Nucleon polarizabilities with real photons High resolution pion spectroscopy of light hypernuclei PRECISION COMPLEXITY DISCOVERY POTENTIAL The Low Energy Frontier @ Mainz: Results and ... Sunday, April 13, 2014

The Low Energy Physics Frontier of the Standard Model at the MAMI accelerator

The Low Energy Physics Frontier of the Standard Model at the MAMI accelerator

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