Physics beyond the Standard Model from molecular hydrogen

Physics beyond the Standard Model from molecular hydrogen; Part I VLT HST Lasers Wim Ubachs Vrije Universiteit Amsterdam ALMA Effelsberg PSAS 2016 Jerusalem, 23 May 2016

Varying Constants of Nature ? Coupling constants are free parameters in Standard Model But cannot be varied at will Bekenstein – Barrow – Flambaum : consistent models 1) Coupling to matter Variation on cosmological time scales “Connection to Dark Energy scenarios” 2) Coupling to environment -> “chameleons” Dependence on local density Dependence on gravity

Empirical search for a change in m Compare H 2 in different epochs Lab QSO today 12 Gyr ago 90 -112 nm ~275 -350 nm Cosmological redshift Practical: atmospheric transmission only for z>2

H 2 molecule (1 s)2 - (1 s)(2 p); threefold 2 p orbitals 2 pp 2 ps H H 2 Blue-shifted from Lyman-a X 1 Sg+ - (2 ps) B 1 Su+ X 1 Sg+ - (2 pp) C 1 Pu Doubly degenerate

H 2 dipole-allowed spectrum Blue-shifted from Lyman-a 2 pp 2 ps H H 2, Lyman en Werner BANDS ~90 - 110 nm Extreme Ultraviolet Wavelengths Theodore Lyman

“Sensitivity” Perturbations

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)

Soleil VUV Fourier-Transform Spectrometer HD

>160 lines measured at ~ 5 x 10 -8 Some lines at < 1 x 10 -8

VLT – UVES Paranal, Chili Keck – HIRES Hawaii

Various systems observed

Analysis method: “comprehensive fitting” Produce molecular fingerprint li – set of accurate wavelengths fi – set of line oscillator strengths (from ab initio theory) Gi – set of damping coefficients (from ab initio theory) Astrophysical conditions b – Doppler width parameter z – red shift NJ – column densities Fit equation onto spectrum “Treat” HI and metal lines Multiple velocity components (? ) Ki – set of sensitivity coefficients

The best system: J 2123 -005 at zabs=2. 05 Unique spectrum from Keck; Resolution 110000 ; seeing 0. 3” Spectrum from VLT; R=54000; seeing 0. 8”; better SNR 37 panels, 3071 – 3421 Å ~100 H 2 + 7 HD lines Keck: Dm/m = (5. 6 ± 5. 5 stat ± 2. 9 syst) x 10 -6 VLT: Dm/m = (8. 5 ± 3. 6 stat ± 2. 2 syst) x 10 -6

Q 1441+272 ; the most distant zabs = 4. 22 ; 1. 5 Gyrs after the Big Bang Systematic analysis Phys. Rev. Lett. 114, 071301 (2015)

Status |Dm/m| = (3. 1 1. 6) x 10 -6 W. Ubachs, J. Bagdonaite, E. J. Salumbides, M. T. Murphy, L. Kaper Search for a drifting proton-electron mass ratio from H 2 Rev. Mod. Phys. 88, 021003 (2016)

Satelite-Based observations Dependence of m on gravitational field Cosmic Origins Spectrograph Spectrum of GD-133 and GD 29 -38 White Dwarf stars H 2 in VUV In search for the chameleon scenario (local conditions) Hubble Space Telescope

Contributions of many lines in the B-X Lyman system l ~ 130 -140 nm High temperatures High v populated Franck-Condon factors

Dependence of Dm/m on gravitational field Invoke partition function: Invoke intensities (1500 lines): Fit T and Dm/m GD 133: Dm/m = (-2. 7 +/- 4. 7) x 10 -5 GD 29 -38: Dm/m = (-5. 9 +/-3. 8) x 10 -5 Bagdonaite et al. , Phys. Rev. Lett. 113, 123002 (2014)

CO A 1 P-X 1 S+ electronic bands In J 1237+065 at z=2. 69 POSTER

What should you look at ? Search for higher sensitivity molecule Calculations Extreme shifters

Methanol: the extreme shifter 48372. 4558 MHz; K=-1 48376. 892 MHz; K=-1 12178. 597 MHz; K=-33 60531. 1489 MHz; K=-7

A Stringent Limit on a Drifting Proton-to-Electron Mass Ratio from Alcohol in the Early Universe Bagdonaite, Jansen, Henkel, Bethlem, Menten, Ubachs, Science 339 (2013) 46 K=-33 K=-1 K=-7 Effelsberg Radio Telescope PKS-1830 -211 “molecular factory” at z=0. 88582 (7. 5 Gyrs look-back)

PKS 1830 -211; lensing, blazar, time-varying Radio-loud quasar “Blazar” Intervening galaxy with cold methanol

Result from three telescopes Chajnantor, Chile 5 km altitude IRAM-30 m 261 GHz 160 GHz

HD+ ions in a trap; measurement of (8, 0) Look for loss of HD+ 750 Be+ 40 -85 HD+ 782 nm + 532 nm 313 nm Signal detection by REMPD

S=2 HD+ spectrum F=1 v = 8, L =2 S=1 S=0 Theory S=1 782 nm F=0 S=2 F=1 Experiment v = 0, L =3 S=0 F=0 Experiment: Theory*: Biesheuvel et al. (Nature Comm. 2016) S=1 J=4 J=3 J=2 J=1 J=0 J=3 J=2 J=1 J=2 J=3 J=5 J=4 J=3 J=2 J=1 J=4 J=3 J=2 J=3 J=4 383, 407, 177. 38(41) MHz 383, 407, 177. 150(15) MHz *Korobov, Hilico, Karr, Phys. Rev. A 89, 032511 (2014)

Thanks & Acknowledgement Julija Bagdonaite Mario Dapra Ming. Li Niu Edcel Salumbides Paul Jansen Isabelle Kleiner HD+ Michael Murphy Karl Menten Nissim Kanekar Jeroen Koelemeij Jurriaan Biesheuvel