1. CONNECTING GALAXIES TO THE COSMIC WEB WITH HUBBLE AND EVLA 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 = 10 12.5—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 Strong Mg II, maybe DLA? @ cz=5250 km/s in HST & HI 21cm spectra of PKS 1327- 206

2. 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 = 10 12.5—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

3. VLA H I EMISSION & ABSORPTION IN PKS 1327-204 A typical galaxy disk ? SYSTEM #1 #2 FWHM ~ 17 km/s 44 km/s System #2 System #1 Log N H I = 19.3 for T~100K 20.1 for T~300K But no Lyα absorption available due to intervening Lyman limit system at higher z Radio continuum in green H I 21cm emission in blue Contours = 2.5, 5, 10, 15 x 10 20 cm -2

4. WF/PC2 Hα Image shows no plumes or wisps in direction of 3C232  not outflow? Greater obscuration of H II regions to bottom of NGC 3067 support “underside” view of NGC 3067  gas seen in H I absorption is infalling 3C 232 NGC 3067

5.  ``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067  OPTICAL IMAGE WITH HI 21cm CONTOURS (Carilli & van Gorkom 1992 ApJ 399, 373 )   C 232 z=0.533; Absorber has N HI = 1 x 10 20 cm -2 and T spin = 500 ± 200 K (Keeney et al. 2005 ApJ 622, 267)  NGC 3067 cz=1465 km/s 0.5L* edge-on Sb galaxy star formation rate = 1.4 Solar masses yr -1 HST GHRS NEAR-UV SPECTRA  (Tumlinson et al. 1999 AJ 118, 2148). Three distinct metal line systems @ cz = 1370 km/s 1420 km/s (H I 21cm Absorber) 1530 km/s Each system contains: NaI, CaII, MgI, MgII, FeII, MnII + CIV and SiIV.

6. 3C 232 / NGC 3067 Velocity field suggests H I 21 cm cloud to be infalling (v rad =  115 km/s) unless the halo gas is counter-rotating. HST image confirms Reproduced from Carilli & van Gorkom, 1992, ApJ, 399, 373. NGC 3067 3C 232 H I 21 cm velocity contours Metals from Na I D to C IV are observed with the same 3 velocity components, but H I is only detected in one. Reproduced from Tumlinson et al. 1999, AJ, 118, 2148. Reproduced from Keeney et al. 2005, ApJ, 622, 267. H I 21 cm

7. NGC 3067 H I Absorber N HI = 1.0 x 10 20 cm  2 T spin = 500 ± 200 K T kin = 380 ± 30 K R(Galactocentric)= 11 kpc Cloud Size = 5 kpc Z > 0.25 Z  UV f esc < 2% Galactic HVCs N HI > 2 x 10 18 cm  2 T spin > 200 K R(Galactocentric) < 40 kpc Cloud Size = 3  20 kpc Z = 0.08  0.35 Z  UV f esc = 1-2% Keeney et al (2005) Putman et al (2003) Tumlinson et al (1999) Akeson & Blitz (1999) Collins, Shull, & Giroux (2004) Hulsbosch & Wakker (1988) Strong Mg II/Lyman Limit Systems as HVC Analogs

8. SBS 1122+594 / IC 691 ABSORBER/GALAXY CONNECTIONS IC 691 SDSS J112625.97+591737.5 cz gal = 1202 ± 5 km/s cz abs(CIV) = 1110 ± 50 km/s N HI ~ 10 15 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

9. Which Starburst Winds Escape ? QSO Galaxy Pairs are new probe of Feedback to IGM (Brian Keeney, PhD dissertation 2007)  Dwarf galaxies play a larger role in the chemical evolution of the intergalactic medium than their more massive counterparts. Galaxy Luminosity D gal-abs Wind Is Milky Way ~0.8 L* 5-12 kpc Bound NGC 30670.5 L*  11 kpc Bound IC 691 0.06 L*  35 kpc Unbound 3C 273 Dwarf 0.004 L*  70 kpc Unbound

10. GASEOUS FILAMENT VOID  FILAMENT

11. Typical H I 21cm emitter (DLA) G = Galactic Disk & HVCs Lyα = feedback + pristine

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

13. IGM Gas without feedback from Galactic Superwinds YELLOW: T > 10 6.5 o K (OVII/OVIII WHIM) RED: T=10 5--6.5 o K (OVI WHIM) GREEN & BLUE: T=10 3.5--5 o K (Warm IGM: Lyα Forest) Simulation without GSW finds ~30% of local IGM in the WHIM IGM Gas WITH Galactic Superwind Feedback (prescription requires that feedback is proportional to the local star formation rate per pixel) GSW Simulation finds ~50% of local IGM in WHIM Cen & Ostriker 2006 ApJ 650, 560 and Cen & Fang 2006 ApJ 650, 573 30 h -1 70 Mpc

14. 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 MAY 2009

15. COS has 2 channels to provide low and medium resolution UV spectroscopy –FUV: 1150-1775Å, NUV: 1700-3200Å FUV gratings: G130M, G160M, G140L NUV gratings: G185M, G225M, G285M, G230L –M gratings have spectral resolution of R ~ 20,000 NUV MAMA Detector (STIS spare) Calibration Platform FUV XDL Detector OSM2: G185M, G225M, G285M, G230L, TA1 OSM1: G130M, G160M, G140L, NCM1 Aperture Mechanism: Primary Science Aperture, Bright Object Aperture Optical bench (not shown): re-use of GHRS bench COS OPTICAL LAYOUT: FUV PRIME SPECTROGRAPH NUV originally for STIS BACKUP

16. HST + COS SURVEYS THE GREAT WALL SIX SIGHTLINES OVER 30 Mpc 2

18. WHAT WILL BE DONE WHEN THE ``COSMIC ORIGINS SPECTROGRAPH’’ IS INSTALLED THIS YEAR NEXT ON HST  he Extent, Metallicity and Kinematics of a Normal, Luminous (~L*) Spiral Galaxy Halo Using Multiple QSO sightlines