QSO ABSORPTION LINE STUDIES with 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 (N H I = —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 cz=5250 km/s in HST & HI 21cm spectra of PKS

QSO ABSORPTION LINE STUDIES with 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 (N H I = —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 G

?? 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 N HI < 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 N H I > 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 N H I > 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 kpc from the nearest L* galaxy and 50—450 h 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 > o K (OVII/OVIII WHIM) RED: T= o K (OVI WHIM) GREEN & BLUE: T= o K (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, h 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 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 D gal-abs Wind Milky Way ~0.8 L* 5-12 kpc Bound NGC L*  11 kpc Bound IC L*  35 kpc Unbound 3C 273 Dwarf 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 2005  489 Absorbers v lsr =  105± ±10 km/s v w =  250± ±20 km/s v esc = +560± ±90 km/s z obs =  4.9±0.2  5.8±0.2 kpc z max =  10.8±0.9  12.5±1.0 kpc Mrk 1383 Absorbers v lsr = +46±7 +95±11 km/s v w = +30±10 +90±15 km/s v esc = +530± ±90 km/s z obs = +11.7± ±0.3 kpc z max = +12.6± ±0.1 kpc All four absorbers reach comparable maximum heights (|z max |  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 / IC 691 ABSORBER/GALAXY CONNECTIONS IC 691 SDSS J cz gal = 1204 ± 3 km/s cz abs(CIV) = 1110 ± 30 km/s N HI ~ cm -2 v esc (r>33kpc)  35 km/s IC 691: H I 21 cm cz abs from Keeney et al. 2006, AJ, 132, 2496

GASEOUS FILAMENT 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 Mpc 2 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 Explorer tracing the Baryons from Cosmic Web to Galaxy Halo Science Payloads: #1: Long-Slit Diffuse Spectrograph Lyα and O VI 1031Å at Δλ/λ=2000 Slit: 1 x 20 arcminutes Sensitivity: 25 photon units in deep, multi-day pointings at z=0—0.1. #2: NUV Camera: Å band 33 arcmin FOV; 3 arcsec resolution M AB = 30.8 arcsec -2 in deep pointing for 6 arcsec sized object #3: FUV Camera: Å band M AB = 27.6 arcsec -2 in deep pointing for 6 arcsec sized object Strong Mg II/Lyman Limit Systems as HVC Analogs Does our Universe have the BLAs (Broad Lyα Absorbers)? (Lehner et al 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 It is well-known that b =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  BLAs do NOT add significantly to Cosmic Baryon census. Examples of a contentious and an uncontentous BLA in the HE spectrum PI: James Green, U of Colorado