Evidence For Cosmological Evolution of the Fine Structure Constant?

1. Evidence For Cosmological Evolution of the Fine Structure Constant? Chris Churchill (Penn State) a = e2/hc Da = (az-a0)/a0

2. John Webb (UNSW) - Analysis; Fearless Leader Steve Curran (UNSW) - QSO (mm and radio) obs. Vladimir Dzuba (UNSW) - Computing atomic parameters Victor Flambaum (UNSW) - Atomic theory Michael Murphy (UNSW) - Spectral analysis John Barrow (Cambridge) - Interpretations Fredrik T Rantakyrö (ESO) - QSO (mm) observations Chris Churchill (Penn State) - QSO (optical) observations Jason Prochaska (Carnegie Obs.) - QSO (optical) observations Arthur Wolfe (UC San Diego) - QSO optical observations Wal Sargent (CalTech) - QSO (optical) observations Rob Simcoe (CalTech) - QSO (optical) observations Juliet Pickering (Imperial) - FT spectroscopy Anne Thorne (Imperial) - FT spectroscopy Ulf Greismann (NIST) - FT spectroscopy Rainer Kling(NIST) - FT spectroscopy Webb etal. 2001 (Phys Rev Lett 87, 091391)

3. QSO Spectra

4. Intrinisic QSO Emission/Absorption Lines

5. H I (Lyman-a) 1215.67

6. C IV 1548, 1550 & Mg II 2796, 2803

7. And, of course… The Beam Collector. Keck Twins 10-meter Mirrors

8. The High Resolution Echelle Spectrograph (HIRES)

9. 2-Dimensional Echelle Image of the Sun Dark features are absorption lines

10. We require high resolution spectra…

11. Interpreting cloud-cloud velocity splittings….

12. b (km/s) N (atoms/cm2) (1+z)lrest Parameters describing ONE absorption line 3 Cloud parameters: b, N, z “Known” physics parameters: lrest, f, G...

13. Cloud parameters describing TWO (or more) absorption lines from the same species… (eg. MgII 2796 + MgII 2803 A) N b b 3 cloud parameters (no assumptions), z

14. We decompose the complex profiles as multiple clouds, using Voigt profile fitting natural line broadening + Gaussian broadening Gaussian is line of sight thermal broadening gives “b”

15. The “alkali doublet method” Resonance absorption lines such as CIV, SiIV, MgII are commonly seen at high redshift in intervening gas clouds. Bethe & Salpeter 1977 showed that the l1, l2of alkali-like doublets, i.e transitions of the sort are related to a by which leads to Note, measured relative to same ground state l2 l1

16. But there is more than just The doublets… there are other transitions too!

17. Cloud parameters describing TWO absorption lines from different species (eg. MgII 2796 + FeII 2383 A) b(FeII) b(MgII) N(FeII) maximum of 6 cloud parameters, without assumptions N(MgII) z(FeII) z(MgII)

18. We reduce the number of cloud parameters describing TWO absorption lines from different species: b Kb N(FeII) 4 cloud parameters, with assumptions: no spatial or velocity segregation for different species N(MgII) z

19. Ei Ec Represents different FeII multiplets The “Many-Multiplet method” - using different multiplets and different species simultaneously - In addition to alkali-like doublets, many other more complex species are seen in quasar spectra. Now we measure relative to different ground states High mass nucleus Electron feels large potential and moves quickly: large relativistic correction Low mass nucleus Electron feels small potential and moves slowly: small relativistic correction

20. Procedure 1. Compare heavy (Z~30) and light (Z<10) atoms, OR 2. Compare s p and d p transitions in heavy atoms. Shifts can be of opposite sign. Illustrative formula: Ez=0 is the laboratory frequency. 2nd term is non-zero only if a has changed. q is derived from relativistic many-body calculations. Relativistic shift of the central line in the multiplet K is the spin-orbit splitting parameter. Numerical examples: Z=26 (s p) FeII 2383A: w0 = 38458.987(2) + 1449x Z=12 (s p) MgII 2796A: w0 = 35669.298(2) + 120x Z=24 (d p) CrII 2066A: w0 = 48398.666(2) - 1267x where x = (az/a0)2 - 1 MgII “anchor”

21. ZnII FeII SiIV FeII Positive MgI, MgII Mediocre Anchor Mediocre Negative CrII Low-z (0.5 – 1.8) High-z (1.8 – 3.5)

22. Da/a= -5×10-5 Low-z High-z Low-z vs. High-z constraints:

23. Current results:

24. Possible Systematic Errors • Laboratory wavelength errors • Heliocentric velocity variation • Differential isotopic saturation • Isotopic abundance variation (Mg and Si) • Hyperfine structure effects (Al II and Al III) • Magnetic fields • Kinematic Effects • Wavelength mis-calibration • Air-vacuum wavelength conversion (high-z sample) • Temperature changes during observations • Line blending • Atmospheric dispersion effects • Instrumental profile variations

25. 2-Dimensional Echelle Image of the Sun Dark features are absorption lines

26. Using the ThAr calibration spectrum to see if wavelength calibration errors could mimic a change ina ThAr lines Quasar spectrum Modify equations used on quasar data: quasar line:w = w0(quasar) + q1x ThAr line:w = w0(ThAr) + q1x w0(ThAr) is known to high precision (better than 0.002 cm-1)

27. ThAr calibration results:

28. Atmospheric dispersion effects:

29. Rotator

30. Isotopic ratio evolution:

31. Isotopic ratio evolution results: Isotope

32. Correcting for both systematics: Rotator + Isotope

33. Uncorrected: Quoted Results

34. Conclusions and the next step • ~100 Keck nights; QSO optical results are “clean”, i.e. constrain a directly, and give ~6s result. Undiscovered systematics? If interpreted as due to a, a was smaller in the past. • 3 independent samples from Keck telescope. Observations and data reduction carried out by different people. Analysis based on a RANGE of species which respond differently to a change in a: • Work for the immediate future: (a) 21cm/mm/optical analyses. (b) UVES/VLT, SUBARU data, to see if same effect is seen in independent instruments; (c) new experiments at Imperial College to verify/strengthen laboratory wavelengths;

35. CMB Behavior and Constraints Smaller a delays epoch of last scattering and results in first peak at larger scales (smaller l) and suppressed second peak due to larger baryon to photon density ratio. Last scattering vs. z CMB spectrum vs. l Solid (da=0); Dashed (da=-0.05); dotted (da=+0.05) (Battye etal 2000)

36. BBN Behavior and Constraints D, 3He, 4He, 7Li abundances depend upon baryon fraction, Wb. Changing a changes Wb by changing p-n mass difference and Coulomb barrier. Avelino etal claim no statistical significance for a changed a from neither the CMB nor BBN data. They refute the “cosmic concordance” results of Battye etal, who claim that da=-0.05 is favored by CMB data. (Avelino etal 2001)

37. 49 Systems ; 0.5 < z < 3.5 ; 28 QSOs Da/a = -0.72 +/- 0.18 x 10-5 (4.1s)

38. Numerical procedure: • Use minimum no. of free parameters to fit the data • Unconstrained optimisation (Gauss-Newton) non-linear least-squares method (modified version of VPFIT, Da/a explicitly included as a free parameter); • Uses 1st and 2nd derivates of c2with respect to each free parameter ( natural weighting for estimating Da/a); • All parameter errors (including those for Da/aderived from diagonal terms of covariance matrix (assumes uncorrelated variables but Monte Carlo verifies this works well)

39. However… T is the cloud temperature, m is the atomic mass So we understand the relation between (eg.) b(MgII) and b(FeII). The extremes are: A: totally thermal broadening, bulk motions negligible, B: thermal broadening negligible compared to bulk motions,

40. Line of sight to Earth FeII MgII How reasonable is the previous assumption? Cloud rotation or outflow or inflow clearly results in a systematic bias for a given cloud. However, this is a random effect over and ensemble of clouds. The reduction in the number of free parameters introduces no bias in the results

41. We model the complex profiles as multiple clouds, using Voigt profile fitting (Lorentzian + Gaussian convolved) Free parameters are redshift, z, and Da/a Lorentzian is natural line broadening Gaussian is thermal line broadening (line of sight)

42. Dependence of atomic transition frequencies on a Zero Approximation – calculate transition frequencies using complete set of Hartree-Fock energies and wave functions; Calculate all 2nd order corrections in the residual electron-electron interactions using many-body perturbation theory to calculate effective Hamiltonian for valence electrons including self-energy operator and screening; perturbation V = H-HHF. This procedure reproduces the MgII energy levels to 0.2% accuracy (Dzuba, Flambaum, Webb, Phys. Rev. Lett., 82, 888, 1999) Important points: (1) size of corrections are proportional to Z2, so effect is small in light atoms; (2) greatest precision will be achieved when considering all relativistic effects (ie. including ground state)

43. Wavelength precision and q values

44. Line removal checks:

45. Post-removal Removing MgII2796: Pre-removal Line Removal

46. Post-removal Removing MgII2796: Pre-removal Line Removal

47. Number of systems where transition(s) can be removed Pre-removal Post-removal Transition(s) removed

49. Thepositionof a potential interloper “X” Suppose some unidentified weak contaminant is present, mimicking a change in alpha. Parameterise its position and effect by dl, Dl: MgII line generated with N = 1012 atoms/cm2 b = 3 km/s Interloper strength can vary Position of fitted profile is measured