QSO ABSORPTION LINE STUDIESwith the HUBBLE SPACE TELESCOPE

COLORADO GROUP: JOHN STOCKE, MIKE SHULL, JAMES GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY

Results thus far based on:

> 300 QSO ABSORBERS found by HST Spectrographs at z < 0.1 and at low

column densities (NH I = 1012.5—16.5 cm-2 ) AND

>1.35 Million galaxy locations and redshifts from the CfA galaxy redshift survey, 2DF/6DF, SLOAN Digital Sky Spectroscopic Survey (DR-6), FLASH & others, including our own pencil-beam Surveys in progress

DLA: @

cz=5250 km/s in HST & HI 21cm spectra of PKS 1327-206

QSO ABSORPTION LINE STUDIESwith the HUBBLE SPACE TELESCOPE

COLORADO GROUP: JOHN STOCKE, MIKE SHULL, JAMES GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY

Results thus far based on:

> 300 QSO ABSORBERS found by HST Spectrographs at z < 0.1 and at low

column densities (NH I = 1012.5—16.5 cm-2 ) AND

>1.35 Million galaxy locations and redshifts from the CfA galaxy redshift survey, 2DF/6DF, SLOAN Digital Sky Spectroscopic Survey (DR-6), FLASH & others, including our own pencil-beam Surveys in progress

H II regions in red in ESO G1327-2041

??

Absorption Studies with HST + GHRS/STIS/COS allows direct connections between gas and galaxies, filaments and cosmic voids to be explored in detail

SUMMARY OF STATISTICAL RESULTS• COSMIC BARYON CENSUS: Ly baryon = 29 4 % in warm ionized medium (most of the mass is in

NHI < 10 14 cm-2 absorbers)(WHIM)baryon < 10% from census

of O VI absorbing systems; space density of metal-free WHIM clouds from numbers of broad, shallow Lyα absorptions very uncertain (Richter et al.; Lehner et al.; Stocke & Danforth, in prep)

• ASSOCIATION WITH GALAXIES? 78% LOCATED IN SUPERCLUSTER FILAMENTS; 22% IN VOIDS. STRONGER absorbers at NH I > 1013 cm-2 are more closely ASSOCIATED WITH GALAXIES; WEAKER absorbers are more UNIFORMLY DISTRIBUTED in space.

• b(voids)/ b = 4.5 ±1.5% AS PREDICTED BY SIMULATIONS (Gottlober et al 2003). Metallicity < 1.5% Solar (Stocke et al. 2007, ApJ, 671, 146)

• At least 55% of all Ly α absorbers with NH I > 1013 cm-2 are METAL-BEARING at ~ 10% SOLAR. A typical galaxy filament is covered >50% by metal-enriched gas.

• Metal-bearing absorbers at ~10% Solar abundance (Danforth and Shull 2008) show spread around galaxies of:

150—800h-170 kpc from the nearest L* galaxy and

50—450 h-170 kpc from the nearest 0.1L* galaxy

based on OVI and CIII data from FUSE/HST

• For details see PENTON et al. (2000a,b, 2002, 2004) ApJ (Ly alpha absorbers w/ HST/STIS & GHRS) and STOCKE et al. (2006) ApJ 641, 217 . (OVI and C III absorbers with FUSE)

IGM Gas without feedback from Galactic Superwinds

YELLOW: T > 106.5 oK (OVII/OVIII WHIM) RED: T=105--6.5 oK (OVI WHIM) GREEN & BLUE: T=103.5--5 oK (Warm IGM: Lyα Forest)

IGM Gas WITH Galactic Superwind Feedback (prescription requires that feedback is proportional to the local star formation rate per pixel)

** Prescription may be too simplistic ??

Simulation finds ~50% of local IGM in WHIM gas

Cen & Ostriker 2006 ApJ 650, 560 and Cen & Fang 2006 ApJ 650, 573

30 h-170 Mpc

Space Density of

O VI Absorbing Systems broadly agrees with strong galactic superwind simulations

(but absorber metallicity an uncertain factor; here 10% Solar assumed)

Impact Parameters Required to reproduce the Observed OVI dN/dz(covering factor = 0.5; all galaxies of luminosity > L contribute)

Sample Sizes = 23 9

Mean distance = 1800 kpc 250 kpc prediction for COS: If dwarfs enrich IGM, filaments

(Between comparable L galaxies) will be FILLED w/ metal-enriched gas

Figure from

Tumlinson & Fang

2005 ApJL 623, L97

O VI maximum impact parameters from

Stocke et al. 2007

ApJ, 671, 146

Evaluation of nearest galaxies and covering factors for all available metal ions (Si II, CII, Si III, CIII, CIV, Si IV, NV, OVI now in progress(Danforth, Stocke, Shull and Keeney 2008)

Which Starburst Winds Escape ?(Brian Keeney, PhD dissertation 2007)

Dwarf galaxies may play a larger role in the chemical evolution of the intergalactic medium than their more massive counterparts.

Galaxy Luminosity Dgal-abs Wind

Milky Way ~0.8 L* 5-12 kpc Bound

NGC 3067 0.5 L* 11 kpc Bound

IC 691 0.06 L* 35 kpc Unbound

3C 273 Dwarf 0.004 L* 70 kpc Unbound

The Milky Way’s Nuclear Wind

Reproduced from Keeney et al. 2006, ApJ, 646, 951.

Milky Way Wind: Bound at 12 kpc

PKS 2005489 Absorbers

vlsr = 105±12 +168±10 km/svw = 250±20 +250±20 km/svesc = +560±90 +560±90 km/s

zobs = 4.9±0.2 5.8±0.2 kpczmax = 10.8±0.9 12.5±1.0 kpc

Mrk 1383 Absorbers

vlsr = +46±7 +95±11 km/svw = +30±10 +90±15 km/svesc = +530±90 +520±90 km/s

zobs = +11.7±0.2 +12.2±0.3 kpczmax = +12.6±0.1 +12.6±0.1 kpc

• All four absorbers reach comparable maximum heights (|zmax| 12.5 kpc) in the Galactic gravitational potential They were ejected from the Galactic center with comparable energies.

• These high-velocity absorbers have similar ionization states and metallicities as highly-ionized HVCs (although we need to look w/ CHANDRA).

SBS 1122+594 / IC 691ABSORBER/GALAXY CONNECTIONS

IC 691

SDSS J112625.97+591737.5

czgal = 1204 ± 3 km/s

czabs(CIV) = 1110 ± 30

km/s

NHI ~ 1015 cm-2

vesc(r>33kpc) ≤35 km/s

IC 691: H I 21 cm

czabs

from Keeney et al. 2006, AJ, 132, 2496

GASEOUS FILAMENT

VOIDVOID VOID

FILAMENT

Observational Goals Include:

** Massive Starburst Galaxy Winds(3 QSO/galaxy pairs)

** Dwarf and LSB Galaxy winds(6 QSO/galaxy pairs)

** Normal Luminous Galaxy Halos(3 QSOs around one L* galaxy)

** “Cosmic Tomography” of the Great Wall(6 QSO sightlines in 30 Mpc2 region

** BL Lac Targets to search for Broad Lyα(7 targets totaling Δz 1.5)

Bright, long pathlength targets(entire GTO target set yields Δz 15)

PI: James Green, U of Colorado

COSMIC ORIGINS SPECTROGRAPH: TO BE INSTALLED DURING SERVICING MISSION #4 IN OCTOBER 2008

WHAT WILL BE DONE WHEN THE ``COSMIC ORIGINS SPECTROGRAPH’’ IS INSTALLED THIS YEAR ON HST

he Extent, Metallicity and Kinematics of a Normal, Luminous (~L*) Spiral Galaxy Using multiple QSO sightlines

IGM: The InterGalactic Medium Explorertracing the Baryons from Cosmic Web to Galaxy Halo

Science Payloads:

#1: Long-Slit Diffuse Spectrograph Lyα and O VI 1031Å at Δλ/λ=2000Slit: 1 x 20 arcminutesSensitivity: 25 photon units in deep, multi-day pointings at z=0—0.1.

#2: NUV Camera: 2150-2350Å band33 arcmin FOV; 3 arcsec resolutionMAB = 30.8 arcsec-2 in deep pointingfor 6 arcsec sized object

#3: FUV Camera: 900-1000Å bandMAB = 27.6 arcsec-2 in deep pointingfor 6 arcsec sized objectStrong Mg II/Lyman Limit Systems as

HVC AnalogsDoes our Universe have the BLAs (Broad Lyα Absorbers)?(Lehner et al. 2007 ApJ 658, 680)

7 sightlines 341 Lyα absorbers with total pathlength Δz=2.06

# of BLAs # confirmed or # improbable # not (b > 40 km/s) probable BLAs as BLAs BLAs

121 32 28 61

It is well-known that b < b (Lyα) due to streaming and turbulent motions in absorbers (Shull et al. 2000, ApJL 538, L13; Danforth et al. 2006 ApJ, 640, 716). This is confirmed explictly for this sample using curve-of-growth (COG) b-values for which we find: < b(COG)/b(Lyα) >=0.61.

Further, due to their very small neutral fractions, BLAs with b > 60 km/s would contribute most of mass to cosmic baryon census. For this sub-population of 34 BLAs we find

34 16 11 8

BLAs do NOT add significantly to Cosmic Baryon census.Examples of a contentious and an uncontentous BLA in the

HE 0226-41110 spectrum

PI: James Green,

U of Colorado