ISMS 2015 Urbana-Champaign, 22 June 2015 Wim Ubachs VU University Amsterdam Physics beyond the Standard Model from Molecular Hydrogen Some approaches 1)Search for an electron-EDM Imperial College YbF Yale/Harvard - ThO Refute some of the SUSY models 2)Test of the symmetrization principle of quantum mechanics Spin statistics theorem; Boson-Fermion dichotomy CO 2 Mazotti, Cancio, Giusfredi, Inguscio, de Natale Phys. Rev. Lett. 86, 1919 (2001) O 2 Naus, de Lange, Ubachs Phys. Rev. A 56 (1997) Physics and the Universe What do we know ? What do we not know ? Problems - Dark Matter - Dark Energy - How does Gravity fit to SM ? -Why is Gravity so weak ? -Are there only 3+1 dimensions - Are there only 4 forces ? - Proton Size Puzzle an indicator ? Fine tuning and the constants - Variation on cosmological scale - Dependencies on fields as indicators ? Physics and the Universe What do we know ? What do we not know ? Problems - Dark Matter - Dark Energy - How does Gravity fit to SM ? -Why is Gravity so weak ? -Are there only 3+1 dimensions - Are there only 4 forces ? - Proton Size Puzzle an indicator ? Fine tuning and the constants - Variation on cosmological scale - Dependencies on fields as indicators ? Historical Inspiration Willis E Lamb Breakdown of the Dirac theory of electron The advent of Quantum Electro Dynamics Measurement of the tiny 2S 1/2 2P 1/2 splitting Varying Constants ? Bekenstein-Barrow Sandvik Mageijo Light scalar fields 1) Coupling to cosmology Variation on cosmological time scales Coupling constants are free parameters in Standard Model 2) Local effects Coupling to matter density -> chameleons Coupling to gravity Jacob Bekenstein Empirical search for a cosmological change in =M p /m e Compare H 2 spectra in different epochs QSO 12 Gyr ago Lab today nm ~ nm H 2 laboratory wavelengths The Amsterdam XUV-laser XUV-laser excitation P(3) C-X (1,0) R(0) B-X (9,0) line Ubachs, Phys. Rev. Lett. (2004) Reinhold et al, Phys. Rev. Lett. (2006) Salumbides et al, Phys. Rev. Lett. (2009) For HD Ivanov et al., Phys. Rev. Lett. (2008) >160 lines measured at ~ 5 x Some lines at < 1 x 10 -8 K sensitivity coefficients in H 2 Blue shifters Red shifters Anchor lines VLT UVES Paranal, Chili Keck HIRES Hawaii, VS Various systems observed H 2 and cosmological -variation 10 H 2 absorption systems towards quasars analyzed: 23 additional H 2 absorption systems towards quasars known Status = (3.5 1.6) x 10 -5 Cosmic Origins Spectrograph Hubble Space Telescope Spectrum of GD-133 and GD29-38 White Dwarf stars H 2 in VUV In search for the chameleon scenario (local conditions) Dependence of on gravitational field Dependence of on gravitational field GD133: = (-2.7 +/- 4.7) x GD29-38: = (-5.9 +/-3.8) x Invoke partition function Invoke intensities (1500 lines) Fit T and Bagdonaite et al., Phys. Rev. Lett. 113, (2014) Search for (quintessence) forces; grand picture Molecules Salumbides, Ubachs, Korobov J. Mol. Spectr. 300, 65 (2014) Molecules as a metrology test system Search for 5 th forces from molecular spectroscopy experiment Test of theory (QED) New Physics: Theory is needed only for calculable systems H 2 /H 2 + /HD + have become a calculable systems Benchmark: Dissociation energy H 2 D o (H 2 ) = E IP (H 2 ) + D o (H 2 + ) - E IP (H) D o (H 2 + ) = (50) cm -1 E IP (H) = (10) cm -1 E IP (H 2 ) D o (H 2 ) N + =2 N + =0 vibrational interlopers H 2 Dissociation energy; measurement of IP Herzberg and Jungen 1972 EF 1 g +, v=0, N=0,1 ~150 ns X 1 g +, v=0, N=0,1 H 2 + : X 2 g +, v + =0, N + =0,1 54p Measurement of IP in H 2 3 step approach ( Zrich-Amsterdam collaboration) E i (ortho) = (36) cm -1 E i (para) = (37) cm -1 QED Comparison Theory/Experiment (Theory: Pachucki, Komasa, et al.) Fundamental vibration in H 2 Features Narrowband UV sources Absolute frequency calibration 2-photon Doppler-free REMPI Sagnac alignment Delayed ionisation ac-Stark extrapolation E = (18) cm -1 E exp ~ 1.8 x cm -1 Dickenson, M. Niu, Salumbides, Komasa, Eikema, Pachucki, Ubachs, PRL 110, (2013). Collision-free measurement HD + ions in a trap; measurement of (8,0) 750 Be HD nm 782 nm nm Look for loss of HD + Signal detection involves excitation of the Coulomb crystal + photons from Be+ laser cooling cycle HD + spectrum J = 1 F = 0 F = 1 S = 1 S = 0 S = 1 S = 2 J = 4 J = 3 J = 2 J = 3 J = 4 J = 2 J = 3 J = 4 J = 5 J = 3 J = 0 F = 0 F = 1 S = 1 S = 0 S = 1 S = 2 J = 3 J = 2 J = 1 J = 2 J = 3 J = 1 J = 2 J = 3 J = 4 J = 2 v = 0, L =3 v = 8, L =2 782 nm Theory Experiment Experiment: 383,407,177.38(41) MHz Theory*:383,407, (15) MHz *Korobov, Hilico, Karr, Phys. Rev. A 89, (2014) Tests of QED in molecules Salumbides, Koelemeij, Komasa, Pachucki, Eikema, Ubachs, Phys Rev D 87, (2013). Fifth-force searches Yukawa potential (Phenomenological) Hideki Yukawa Extra hadron-hadron interaction strength: range: Insert in molecular wave function Fifth force constraints: The future molecular test systems for physics Lifetimes 10 6 seconds (!) Quadrupole transitions ~ Hz Possible precision 20-digit 1442 nm 1445 nm 532 nm H2H2 Two-photon Doppler-free Lamb-Dicke ion trap HD + Thanks & Acknowledgement Edcel Salumbides Kjeld Eikema Julija Bagdonaite Michael Murphy Frederic Merkt Krzysztof Pachucki Vladimir Korobov MingLi Niu Jeroen Koelemeij Jurriaan Biesheuvel Laurent Hilico Jean-Philippe Karr Detection Signal = fractional loss of ions (A f A i )/A i Signal = fractional loss of ions (A f A i )/A i B. Roth, JK, H. Daerr, S. Schiller, PRA 74, (R) (2006) During secular excitation, T Be+ rises to T max During secular excitation, T Be+ rises to T max A i T N HD+ for T max < 400 mK A i T N HD+ for T max < 400 mK BUT in practice T max 4 K BUT in practice T max 4 K 10 s REMPD detection cycle: Secular excitation REMPD HD+ /2 AiAi AfAf 313 nm detuning [MHz] Normalized scattering rate 10 mK 500 mK 1000 mK Spatial analysis Free fit (1 ): RA = 4.9 +/- 4.8 hrs; Dec = \- 30 degrees RA=17.5projection Dec = -58