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Metals at Highish Redshift And Large Scale Structures

Metals at Highish Redshift And Large Scale Structures. From DLAs to Underdense Regions Patrick Petitjean Institut d’Astrophysique de Paris. B. Aracil R. Srianand C. Ledoux F. Stoehr C. Pichon

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Metals at Highish Redshift And Large Scale Structures

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  1. Metals at Highish RedshiftAnd Large Scale Structures From DLAs to Underdense Regions Patrick Petitjean Institut d’Astrophysique de Paris B. Aracil R. Srianand C. Ledoux F. Stoehr C. Pichon J. Bergeron E. Rollinde M. Longhetti F. Coppolani E. Scannapieco P. Richer P. Erni P. Noterdaeme

  2. Overall Picture • Where are the metals ? • Center of halos : which one ? • Expelled from the center of . Halos -> Winds • Along filaments • What about the Voids ? • Derive Metallicities • Correlations – Clustering Colombi et al. (2005)

  3. QSO (GRBs ? Galaxies ?) Absorption Lines Metals in the IGM Association with galaxies Metallicities and SF

  4. Damped Ly-α Systems HI : Metals : -> Metallicities -> Dust content -> Kinematics Molecules H2 : -> Density/Temperature -> UV flux Star- Formation ? Winds ?

  5. Redshift-Evolution and Depletion pattern Keck-ESI – X-shooter UVES Prochaska et al. (2003) Rodriguez et al. (2006) * Some evolution * Presence of dust * No system at Z<-3 * Gas not obviously cold

  6. Homogeneity Dispersion is small Pixel by pixel metal ratios => Associated objects probably small Rodriguez et al. 2005, A&A, 446, 791

  7. Abundance ratios in DLA Systems Sample of ~100 DLAs * [O/Fe] ~ +0.35 for -2.6<[O/H]<-1 * Depletion sequence from [Zn/Fe] * Phosphorus under-solar for [Zn/H]<-1 Ledoux et al., in prep.

  8. Peculiar Metallicities in DLAs 1. Z=2.19 towards HE0001-2340: [O/H]=-1.81 [C/H]=-1.76 [N/H]<-3.3 [Fe/H]=-2.12 [P/C] > 1 ? Richter et al., 2005, astro-ph/0505340 2. Z=2.62 towards Q0913+072: [O/H]=-2.45 [C/H]=-2.81 [N/H]=-3.83 [Fe/H]=-2.76 -> Metallicity as in the IGM ? -> IMF 10-50 Msun ?

  9. Molecular Hydrogen in DLA systems at z>2 75 DLAs ; 12 detections 15% of DLAs have H2 - Small H2/HI fraction Physical conditions : -> Different J levels -> CI* ; CII* T=100 K ; n=10 cm-3 -> Ambiant UV flux is several times that of the Galaxy Star formation : H2 ; CII* ; Lya emission Winds ? Ledoux et al. 2003, MNRAS, 346, 209 - Noterdaeme et al., in prep

  10. DLA at z=2.09 towards Q0458-02 logNHI = 21.7 - Ly-alpha in emission – CII* very strong [Zn/H]=-1.22 [Fe/Zn]=-0.65 DLA Lya Wind ? SFR : Ly-a emission : 1.6 Ms/yr Consistent with CII* No H2 : UVBG 10x+/Galaxy Winds are slow… Heinmüller et al. (2005) astro-ph

  11. PSS J1443+2724Molecules at z=4.224 CI – CI* Temperature of the Microwave Background

  12. Mass-Metallicity Relation [X/H] : metallicity - W1 : Absorption Width Ledoux et al. Astro-ph/0504402 Metal Rich = Massive Galaxy Evolution with z : For a given mass Z increases with time There is SF ; If winds : not very strong except for massive objects

  13. Summary DLAs • Mild evolution of [X/H] with z (<[X/H]>=-1.5) • Presence of dust : depletion a factor of 10 smaller than in our Galaxy • H2 detected in about 15% of DLAs ; amount much smaller than in the Galactic disk -> T larger ; dust amount smaller • Small variations of abundance ratios along the profiles -> small dimensions • Star-formation : N/O small -> massive stars Lya emission weak but CII* conspicuous Winds slow • Mass-metallicity relation ?

  14. Direct Correlation Galaxy-Absorber • MgII Systems (z ~ 1) • *Broad band imaging and spectroscopic follow-up -> 35 kpc • Bergeron & Boissé (1991, A&A 243, 344); Steidel (1993) • * Weak MgII systems ? Churchill et al. (2000) -> > 70 kpc • 2. CIV Systems -> Much larger Very few observations CIV z=1.334 > 150 kpc MgII z = 0.73 100 kpc

  15. CIV longitudinal correlation function Large Programme ESO – 643 CIV systems detected directly Observations : Correlation Function Column density distribution • SPH Simulation : • Bubbles (radius Rbubble) around haloes of mass Mhalo • Ionized by the UV background • Simulated los analyzed the same way as data

  16. Fitting the CIV longitudinal correlation function Fitting the column density distribution and the correlation function => Mhalo = 5x1011 Msun and Rbubble = 2.5 Mpc Filling factor : ~10% Scannapieco et al., 2006, MNRAS, 365, 615

  17. The Third Dimension • Where are the metals ? • Expelled from the center of . Halos -> Winds • Along filaments • What about the Voids ? • The IGM • Correlations • Along the los -> Big Sample • Transverse -> Pairs or groups

  18. Transverse Correlation in the Lyman-α forest and the metals Longitudinal : Large Programme ESO : 20 LOS UVES R=45000 S/N=40-100 Transverse : 33 pairs 1-3 arcmin observed with FORS - z ~ 2.1

  19. Correlation Functions for CIV All together Without a quartet of QSO Transverse Correlation Longitudinal Correlation Coppolani et al. (2006, submitted)

  20. A quartet of QSOs within 10 arcmin 10 arcmin 1.5 < z < 2.2 -> Tol 1037-27

  21. Correlation in the Lyman-α ForestLongitudinal correlation function Observed versus Simulated correlation functions UVES z=3 FORS z=2

  22. Simulated correlation functions • - Hydro simulations in a 100 Mpc simulation • Effect of temperature and peculiar velocities on longitudinal and • transverse correlation functions Longitudinal Transverse • Dark Matter only • Effect of T • Peculiar Velocities

  23. Transverse correlation functionAlcock & Paczynski test Correlation signal up to 5 arcmin -> Sample should be increased to derive Wl -> Very good prospect for further investigation -> Groups of QSOs

  24. Metals in Underdense Regions Large Programme ESO : R=45000 S/N>70 20 LOS OVI CIV 1. IGM is Very Inhomogeneous 2. Metallicity small : [C/H] < -2.5 Pixel analysis: <τ(CIV)> vs τ(HI) Aracil et al. 2004, A&A 419, 811

  25. Metals in Underdense Regions CIV and OVI are present for t(HI)>1 CIV OVI Log CIV/HI ~ -3 and log OVI/HI ~ -1.8 for τ(HI)>1 or δ~ 2 for z=2.5 Excess of OVI in the vicinity of overdensities -> Winds ? Simulations : [C/H]=-3 filling factor : 20% (Schaye & Aguirre) Aracil et al. 2004, A&A, 419, 811

  26. Conclusions Metals detected directly – CIV: => Mhalo = 5x1011 Msun and Rbubble = 2.5 Mpc Filling factor : ~10% There is SF in DLAs : * H2 in 15% of DLAs * Metallicity – Mass Relation => Metals come from the most massive objects * Difficult to estimate the SFR (Lyα emission and CII*) Winds are not fast ? Transverse Correlation: * No signal in strong CIV at 2 arcmin and z=2 * Strong signal in the Lyα forest up to 5 armin Metals in Underdense regions : * CIV is present in at least 20% of the volume * Excess of OVI within 300 km/s from overdensities -> Winds ? petitjean@iap.fr

  27. OVI in the IGM

  28. Molecular Hydrogen at High Redshift

  29. Ly-b Ly-a C IV Metals QSO Spectra

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