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Investigating Absorption Lines and Metallicities in the IGM: Insights from High-z Galaxies

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This study explores the absorption lines associated with quasars, particularly their relation to metallicities and star formation in high-redshift galaxies. We analyze damped Lyman-alpha systems (DLA) and molecular hydrogen (H2) presence within the intergalactic medium (IGM). Our findings highlight the intricate connections between galaxies, their star formation rates (SFR), and the surrounding diffuse IGM, characterized by varying metallicities and densities. These insights enhance our understanding of the cosmic web and the evolution of matter in the universe.

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Investigating Absorption Lines and Metallicities in the IGM: Insights from High-z Galaxies

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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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