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THE LYMAN- a FOREST AS A PROBE OF FUNDAMENTAL PHYSICS

THE LYMAN- a FOREST AS A PROBE OF FUNDAMENTAL PHYSICS. MATTEO VIEL. Cosmological significance of the Lyman- a forest 2. LUQAS: The observational sample Hydro-dynamical simulations of the Lyman- a forest Cosmological parameters – Implications for: inflation,

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THE LYMAN- a FOREST AS A PROBE OF FUNDAMENTAL PHYSICS

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  1. THE LYMAN-a FOREST AS A PROBE OF FUNDAMENTAL PHYSICS MATTEO VIEL • Cosmological significance of the Lyman-a forest • 2. LUQAS: The observational sample • Hydro-dynamical simulations of the Lyman-a forest • Cosmological parameters – Implications for: inflation, • neutrinos, gravitinos, warm dark matter particles With M. Haehnelt, J. Lesgourgues, S. Matarrese, A. Riotto, V. Springel, J. Weller Shanghai, 16 March 2005

  2. GOAL: the primordial dark matter power spectrum CMB physics z = 1100 dynamics Continuum fitting Lya physics z < 6 dynamics + termodynamics Temperature, metals, noise Tegmark & Zaldarriaga 2002 CMB + Lyman a Long lever arm Relation: P FLUX (k) - P MATTER (k) ?? Constrain spectral index and shape

  3. the WMAP era before WMAP Croft et al. 2002 Tilt in the spectrum n<1 ? Running spectral index dn/dlnk < 0 ? WMAP Verde et al. 2003

  4. Wm = 0.26 WL = 0.74 Wb=0.0463 H = 72 km/sec/Mpc - 60 Mpc/h COSMOS computer – DAMTP (Cambridge) DM GAS STARS NEUTRAL HYDROGEN

  5. The LUQAS sample -I Large sample Uves Qso Absorption Spectra (LP-UVES program P.I. J. Bergeron) high resolution 0.05 Angstrom, high S/N > 50 low redshift, <z>=2.25, Dz = 13.75 Nr. spectra redshift Kim, MV, Haehnelt, Carswell, Cristiani, 2004, MNRAS, 347, 355

  6. The LUQAS sample –II systematic errors Effective optical depth Low resolution SDSS like spectra High resolution UVES like spectra <F> = exp (- t eff) Power spectrum of F/<F>

  7. Hydro-simulations: scalings P FLUX (k) = b2(k) P MATTER (k) T = T0 ( 1 + d) g-1 Effective optical depth Viel, Haehnelt, Springel, MNRAS, 2004, 354, 684

  8. Hydro-simulations: what have we learnt? Many uncertainties which contribute more or less equally (statistical error is not an issue!) ERRORS CONTRIBUTION TO FLUCT. AMPL.

  9. Cosmological implications: combining the forest data with CMB - I MV, Haehnelt, Springel 2004 SDSS Seljak et al. 2004 n = 1.01 ± 0.02 ± 0.06 s8 = 0.93 ± 0.03 ± 0.09 Systematic error Statistical error Note that the flux bispectrum analysis agrees with these values MV, Matarrese, Heavens, Haehnelt, Kim, Springel, Hernquist, 2004

  10. Cosmological implications: combining the forest data with CMB - II MV, Weller, Haehnelt, MNRAS, 2004, 355, L23 s8= 0.93 ± 0.07 n=0.99 ± 0.03 d ns/ d ln k SDSS Seljak et al. 2004 s8= 0.90 ± 0.03 n=0.98 ± 0.02 nrun = -0.003 ± 0.010 nrun=-0.033± 0.025

  11. Cosmological implications: constraints on slow-roll inflation - III MV, Weller, Haehnelt, MNRAS, 2004, 355, L23 V = inflaton potential T/S = r < 0.45 (95% lim.) r = 0.50 ± 0.30 No evidence for gravity waves SDSS Seljak et al. 2004 T/S

  12. Cosmological implications: Warm Dark Matter particles-I LCDM WDM 0.5 keV 30 comoving Mpc/h z=3 In general if light gravitinos k FS ~ 5 Tv/Tx (m x/1keV) Mpc-1 k FS ~ 1.5 (m x/100eV) h/Mpc Set by relativistic degrees of freedom at decoupling MV, Lesgourgues, Haehnelt, Matarrese, Riotto, PRD in press

  13. Cosmological implications: Warm Dark Matter particles-II LWDM LCWDM (gravitino like) Wgravitino/ WDM Scale of free streaming Set limits on the scale of Supersymmetry breaking L susy< 260 TeV m WDM > 550 eV > 2keV sterile neutrino < 16 eV gravitino

  14. Cosmological implications: constraints on neutrinos WMAP + 2dF + Lyman-a S mn (eV) = 0.33 ± 0.27

  15. HPM simulations of the forest Full hydro 200^3 part. HPM PMGRID=600 HPM PMGRID=400 FLUX POWER

  16. HIGH RESOLUTION HIGH S/N vs LOW RESOLUTION LOW S/N

  17. LUQAS vs SDSS

  18. SUMMARY • LUQAS: a unique high resolution view on the Universe at z=2.1 • 2. Hydro-dynamical simulations of the Lyman-a forest. Systematic • Errors? Differences between hydro codes? • Cosmological parameters: no fancy things going on • s8 = 0.93 n = 1 no running • substantial agreement between SDSS and LUQAS but SDSS has • smaller error bars not because of the larger sample but because of • the different theoretical modelling • Constraints on inflationary models, neutrinos and WDM

  19. HPM simulations of the forest-I equation of motion for gas element if T = T0 ( 1 + d) g-1 Gnedin & Hui 1998

  20. Feedback effects: Galactic winds No Feedback Feedback Density Temperature

  21. Feedback effects: Galactic winds-III Line widths distribution Column density distribution function

  22. Metal enrichment CIV systems at z=3 Strong Feedback e=1 ---- Role of the UV background Mori, Ferrara, Madau 2000; Rauch, Haehnelt, Steinmetz 1996; Schaye et al. 2003 Soft background ---- Role of different feedback e=0 e=1 e=0.1

  23. `

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