Physics beyond the Standard Model from molecular hydrogen; Part I ALMA VLT HST Effelsberg Lasers Wim Ubachs Vrije Universiteit Amsterdam 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

Lab QSO Empirical search for a change in m Compare H2 in different epochs Lab today QSO 12 Gyr ago 90-112 nm ~275-350 nm Cosmological redshift Practical: atmospheric transmission only for z>2

H2 molecule 2pp 2ps H H2 Blue-shifted from Lyman-a (1s)2- (1s)(2p); threefold 2p orbitals 2pp 2ps H H2 X1Sg+ - (2ps) B1Su+ X1Sg+ - (2pp) C1Pu Blue-shifted from Lyman-a Doubly degenerate

H2 dipole-allowed spectrum Blue-shifted from Lyman-a 2pp 2ps H H2 Theodore Lyman H2, Lyman en Werner BANDS ~90 - 110 nm Extreme Ultraviolet Wavelengths

“Sensitivity” Perturbations

H2 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: J2123-005 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 H2 + 7 HD lines Keck: Dm/m = (5.6 ± 5.5stat ± 2.9syst) x 10-6 VLT: Dm/m = (8.5 ± 3.6stat ± 2.2syst) x 10-6

Q1441+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 H2 Rev. Mod. Phys. 88, 021003 (2016)

Satelite-Based observations Cosmic Origins Spectrograph Hubble Space Telescope Dependence of m on gravitational field Spectrum of GD-133 and GD29-38 White Dwarf stars H2 in VUV In search for the chameleon scenario (local conditions)

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 GD133: Dm/m = (-2.7 +/- 4.7) x 10-5 GD29-38: Dm/m = (-5.9 +/-3.8) x 10-5 Bagdonaite et al., Phys. Rev. Lett. 113, 123002 (2014)

CO A1P-X1S+ electronic bands POSTER CO A1P-X1S+ electronic bands In J1237+065 at z=2.69

Search for higher sensitivity molecule 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

PKS-1830-211 “molecular factory” A Stringent Limit on a Drifting Effelsberg Radio Telescope PKS-1830-211 “molecular factory” at z=0.88582 (7.5 Gyrs look-back) 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

PKS1830-211; lensing, blazar, time-varying Radio-loud quasar “Blazar” Intervening galaxy with cold methanol

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

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

HD+ spectrum Theory 782 nm Experiment J = 4 HD+ spectrum S = 2 J = 3 J = 2 J = 1 J = 0 F = 1 S = 1 J = 3 J = 2 J = 1 v = 8, L =2 Theory S = 0 J = 2 F = 0 S = 1 J = 1 J = 2 J = 3 782 nm J = 5 S = 2 J = 4 J = 3 J = 2 J = 1 F = 1 S = 1 J = 4 J = 3 v = 0, L =3 J = 2 Experiment S = 0 J = 3 F = 0 S = 1 J = 2 J = 3 J = 4 Experiment: 383,407,177.38(41) MHz Theory*: 383,407,177.150(15) MHz *Korobov, Hilico, Karr, Phys. Rev. A 89, 032511 (2014) Biesheuvel et al. (Nature Comm. 2016)

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