Metals in the IGM

Association with galaxies

Metallicities and SF

QSO (GRBs ?) Absorption Lines

Quasar Absorption Lines -> Diffuse IGM and dense ISM

Ly-aLy-b C IV

Metals

H2

ESO Blues…

The ISM of high-z galaxies at intermediate Res

SFR and DLA region very small: 1 kpcLyα extended :Red and blue parts are not cospatial

Out-In-Fall-Flows (OIFF)

QSO

SFR

Size < 5 kpc

Lya emission in SDSS Q1135-0010

(Noterdaeme, Laursen, PPJ et al. 2011)

Recent star-burst : 25 M¤/yr

Here it’s on the los – Could be off

Damped Ly-α Systems : Searching for the ISM of high-z galaxies=> High Resolution – Full WR

Metals :

-> Metallicities (high-res)

-> Dust content

-> Kinematics

Molecules H2 + CI, CI* :

-> Density/Temperature

-> UV flux (excitation)

Star- Formation ?

Winds ?

HI :

Heating processes: Molecular excitation : High Res

Two temperatures

No velocity shift

Doppler parameter increases with J

J = 0

4 3

5

2 1

Fluorescence -> UV flux

Collisions -> Tk, density

CI+ CI*

nH=30-100 cm-3 (3-10pc) T=70-150 K UV flux 10xGal

Search for molecules : High Res

Selection H2: *** High dust content (depletion)

30% eff ** High metallicity

* High NHI

Other molecules: CO + HD

CO => Translucent clouds -> Blue

CO and HD -> 6 detections

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

z=2.42 ; [S/H]=-0.07; [Fe/S]=-1.33

Excitation of CO: Redshift evolution of TCMB

β = 0.007±0.027 (we’ve tried…)

HD/H2 : too high at high z ?

Could D/H after BBN be made higher (Li smaller) by decaying particles. Scatter in QSOs is large ?

WAVELENGTH SHIFTS OF INTERGALACTIC ABSORPTION

LINESDainis Dravins – Lund Observatory, Sweden

www.astro.lu.se/~dainis

KVA

Towards the science case for E-ELT HIRES, Cambridge UK, September 2012

HIRES quasar spectrum (A.S.Cowie, Univ.of Hawaii)

WHENEVER SPECTRAL LINES DO NOT ORIGINATE IN

ISOTROPIC TURBULENCE, WAVELENGTH SHIFTS RESULT

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)

Observed solar granulation (Swedish Solar Telescope on La Palma; G.Scharmer & M.G.Löfdahl)

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

(Even if timescales might be 100 Myr, rather than 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)

INTERGALACTIC LINE ASYMMETRIES AND SHIFTS:

• 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 ???

ANALOGIES AND DIFFERENCES TO STELLAR

CONVECTION:

Large Scales: Direct reconstruction of the IGM at z=2.5

Correlation of HI Lyman-α

Z=2.5 => 4200A

+ metals and galaxies

Pichon et al. 2001

QSOs -> 100 / sqdeg not enough

With LBGs => Density field will be recovered

. 150400900

Pichon et al. 2001, MNRAS, 326, 597

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

ELT-MOS

Caucci et al. 2008, MNRAS, 386, 211

.

Reconstruction : R=10,000 3h at g=23.5 => 15h per spectrum

Multiplex of 10 in 5 arcmin : 100 fields : 1500 hours for 1 sq deg

With a bit of optimisation: 700 h => OK

What about correlations (IGM, metals) + transverse proximity effect (combination of resolutions)

Groups of quasars Quasar and galaxies

5 arcmin 1 arcmin

m=17-22

m=19-24

Metals in the IGM : WR: CIV in the optical Res: > 100,000

Association with galaxies: WR: Optical Res: 50,000 vs 5,000

Metallicities and SF (DLAs) : WR: Optical Res: 50,000

Molecules in the ISM : WR: UV, Optical Res: 100,000

A new instrument

The IGM : WR: The bluest Res: 20,000

Multi-resolution : 100,000 and 8,000Multi-object : x15 in a field of 1 to 10 arcminFull wavelength range in the UV-optical - ? IR at high Res ?

Reconstruction/correlation: Mutiplex x15 in 5 arcmin Res=8000 Possibility to combine both resolutions

Relative spectro-photometric calibration => Continuum ?

Variability

And a lot of strange things !

The boomerang outflow

In BOSS – DR10 (half of BOSS)

120,000 QSOs with z>2.15; density > 16 QSOs per sq degree at 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

Molecules: Why H2 ?

• H2 is ubiquitous in star-forming giant clouds and in the diffuse interstellar medium in our Galaxy

• H2 is formed on the surface of dust-grains :What is the role of dust ?

• Excitation of H2 in different rotational levels: Signature of the UV ambient flux + Physical properties of the gas

• Tracer of cold gas in galaxies• Other molecules ? 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