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Metals in the IGM

QSO (GRBs ?) Absorption Lines. Metals in the IGM. Association with galaxies. Metallicities and SF. Ly- b. Ly- a. C IV. Metals. Quasar Absorption Lines -> Diffuse IGM and dense ISM. ESO Blues…. H2. The ISM of high -z galaxies at intermediate Res.

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Metals in the IGM

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

  2. Ly-b Ly-a C IV Metals Quasar Absorption Lines -> Diffuse IGM and dense ISM ESO Blues… H2

  3. The ISM of high-z galaxies atintermediateRes SFR and DLA region very small: 1 kpc Lyα extended : Red and blue parts are not cospatial Out-In-Fall-Flows (OIFF) QSO SFR Size < 5 kpc

  4. Lyaemission in SDSS Q1135-0010 (Noterdaeme, Laursen, PPJ et al. 2011) Recent star-burst : 25 M¤/yr Hereit’s on the los – Couldbe off

  5. Damped Ly-α Systems : Searching for the ISM of high-z galaxies=> High Resolution – Full WR HI : Metals : -> Metallicities (high-res) -> Dust content -> Kinematics Molecules H2 + CI, CI* : -> Density/Temperature -> UV flux (excitation) Star- Formation ? Winds ?

  6. Heatingprocesses: Molecular excitation : High Res Two temperatures No velocity shift 5 Fluorescence ->UV flux 4 3 Collisions -> Tk, density CI+ CI* 2 1 J = 0 Doppler parameter increases with J nH=30-100 cm-3 (3-10pc) T=70-150 K UV flux 10xGal

  7. Search for molecules : High Res Selection H2: *** High dust content (depletion) 30% eff ** High metallicity * High NHI Othermolecules: CO + HD

  8. CO => Translucentclouds -> Blue

  9. CO and HD -> 6 detections z=2.42 ; [S/H]=-0.07; [Fe/S]=-1.33 Log(f) = -0.3 (highest in DLAs) ; CO/H2 = 3x10-6 HD/2H2 = 1.9x10-5 (>Galactic local D/H in ISM) -> 5x+ Gal ; Low astration Srianand et al. (2008) A&A, 482, L39 - Noterdaeme et al. (2010) A&A, 523, 80

  10. Excitation of CO: Redshift evolution of TCMB β = 0.007±0.027 (we’ve tried…)

  11. HD/H2 : toohighathigh z ? Could D/H after BBN be made higher (Li smaller) by decayingparticles. Scatter in QSOsis large ?

  12. Towards the science case for E-ELT HIRES, Cambridge UK, September 2012 KVA HIRES quasar spectrum (A.S.Cowie, Univ.ofHawaii) WAVELENGTH SHIFTS OF INTERGALACTIC ABSORPTION LINES Dainis Dravins – Lund Observatory, Sweden www.astro.lu.se/~dainis

  13. WHENEVER SPECTRAL LINES DO NOT ORIGINATE IN ISOTROPIC TURBULENCE, WAVELENGTH SHIFTS RESULT Observed solar granulation (Swedish Solar Telescope on La Palma; G.Scharmer& M.G.Löfdahl) SOLAR MODEL Synthetic line profiles showing convective wavelength shifts originating in granulation  = 620 nm;  = 1, 3, 5 eV; 5 line strengths Teff= 5700 K; log g [cgs] = 4.4; G2 V Solar disk center; µ = cos  = 1.0 (Models by Hans-Günter Ludwig, Landessternwarte Heidelberg)

  14. WHENEVER SPECTRAL LINES DO NOT ORIGINATE IN ISOTROPIC TURBULENCE, WAVELENGTH SHIFTS RESULT … AND THE SAME MUST APPLY TO ALSO INTERGALACTIC CONVECTION, DRIVEN BY HEATING BY AGNs NEAR CLUSTER CENTERS (Eveniftimescalesmight be 100 Myr, ratherthan solar 10 minutes) Perseus cluster core in X-rays (Chandra), overlaid with Hα (WYIN). Arc-shaped Hα filaments suggest vortex-like flows. Density slices at three times. Viscosity stabilizes the bubble, allowing a flattened buoyant “cap” to form. X-ray brightness and inferred velocity field in Per-A can be reproduced. (Reynolds et al.: Buoyant radio-lobes in a viscous intracluster medium, MNRAS 357, 242, 2005)

  15. INTERGALACTIC LINE ASYMMETRIES AND SHIFTS: ANALOGIES AND DIFFERENCES TO STELLAR CONVECTION: • Plausible amount: 1 % of “general” line broadening = 0.5 – 1 km/s ? • Mapping 3-D structure from different shifts in different lines ! • Need line synthesis from 3-D hydrodynamic models ! • Lines closer to cluster centers gravitationally more redshifted • Mapping depth structure from multiple line components ? • Probably useful to have resolving power approaching 1,000,000 ?? • Resolving lateral structure from secular time changes ???

  16. Large Scales: Direct reconstruction of the IGM atz=2.5 Correlation of HI Lyman-α Z=2.5 => 4200A + metals and galaxies

  17. Pichon et al. 2001, MNRAS, 326, 597 Pichon et al. 2001 900 400 150 . QSOs -> 100 / sqdeg not enough With LBGs => Density field will be recovered

  18. ELT-MOS Inversion methods tested : density of sources: LBGs: about 900 sources/sq degree at r=24.8 QSOs: only 100 sources/sq degree Topology of the IGM (cosmological parameters; growth of structures) Correlation IGM-galaxies: winds; metal enrichment; infall Caucci et al. 2008, MNRAS, 386, 211

  19. Reconstruction : R=10,000 3h at g=23.5 => 15h per spectrum Multiplex of 10 in 5 arcmin : 100 fields : 1500 hours for 1 sqdeg With a bit of optimisation: 700 h => OK What about correlations (IGM, metals) + transverse proximityeffect (combination of resolutions) 1 arcmin 5 arcmin m=19-24 m=17-22 . Groups of quasars Quasar and galaxies

  20. A new instrument The IGM : WR:The bluestRes: 20,000 Metals in the IGM : WR: CIV in the opticalRes: > 100,000 Association withgalaxies: WR: OpticalRes: 50,000 vs 5,000 Metallicities and SF (DLAs) : WR: OpticalRes: 50,000 Molecules in the ISM : WR: UV, OpticalRes: 100,000 Reconstruction/correlation: Mutiplexx15 in 5 arcminRes=8000 Possibility to combine bothresolutions Relative spectro-photometric calibration=> Continuum ? Multi-resolution : 100,000 and 8,000 Multi-object : x15 in a field of 1 to 10 arcmin Full wavelength range in the UV-optical - ? IR athighRes ?

  21. Variability And a lot of strange things ! The boomerang outflow

  22. In BOSS – DR10 (half of BOSS) 120,000 QSOswith z>2.15; density > 16 QSOs per sqdegreeat g=22 Mean distance between 2 and 4 arcmin: Group of 5: 185 Group of 6: 63 Group of 7: 14 Group of 8: 9

  23. Molecules: Why H2 ? • H2 isubiquitous in star-forminggiantclouds and in the diffuse interstellar medium in ourGalaxy • H2 isformed on the surface of dust-grains :Whatis the role of dust ? • Excitation of H2 in differentrotationallevels: Signature of the UV ambient flux + Physicalproperties of the gas • Tracer of cold gas in galaxies • Othermolecules ? CO, HD • By-products: variation of μ=me/mp Two steps : * Survey to learn about the H2-bearing DLA population * Derive selection criteria -> detailed observations

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