1. QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS COLORADO GROUP: JOHN STOCKE, MIKE SHULL, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY EMERITUS: MARK GIROUX (ETSU), JASON TUMLINSON (CHICAGO), JESSICA ROSENBERG (CfA), MARY PUTMAN (MICHIGAN) ELSEWHERE: RAY WEYMANN (CARNEGIE), J. VAN GORKOM (COLUMBIA) Results based on: ƿ >200 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  > 900,000 galaxy locations and redshifts from the CfA galaxy redshift survey, 2DF/6DF, SLOAN Digital Sky Spectroscopic Survey (DR-3), FLASH & others, including our own pencil-beam surveys

4. SUMMARY OF STATISTICAL RESULTS COSMIC BARYON CENSUS:  Ly     baryon = 29  4 % (most of mass in low column density (N HI < 10 14 cm -2 ) absorbers) ASSOCIATION WITH GALAXIES? 78% LOCATED IN SUPERCLUSTER FILAMENTS; 22% IN VOIDS. ABSORBERS AT N H I > 10 13 cm -2 ARE MUCH MORE CLOSELY ASSOCIATED WITH GALAXIES; WEAKER ABSORBERS ARE NEARLY UNIFORMLY DISTRIBUTED IN SPACE  b (voids)  /  b = 4.5 ±1.5% as predicted by simulations (Gottlober et al 2003); At least 55% of all Ly α absorbers with N H I > 10 13 cm -2 are metal-bearing O VI-bearing absorbers indicate spread of metals from nearest L* galaxies: 150—800h -1 70 kpc For details see Penton et al. (2000a,b, 2002, 2004) ApJ and watch for Stocke et al. (in prep).

5. CUMULATIVE DISTRIBUTION FUNCTIONS (CDFs) FOR NEAREST L* GALAXY DISTANCES

6. MEDIAN DISTANCE TO L* GALAXIES Sample Distance in Sample Name h -1 70 kpc Size L* Galaxies : 170 thousands O VI Absorber Pairs : 170 10 O VI Absorbers : 250 23 Stronger half Ly  Sample : 240 69 Weaker half Ly  Sample : 1650 69 --------------------------------------------------------------------- Simulations of WHIM GAS : 200 Dave’ et al Simulations of Photo-ionized Gas: 1200 (1999)

7. Lyα LINE PROFILES FOR OVI ABSORBERS: A SAMPLING SINGLE: SINGLE SINGLE: SINGLE DOUBLE

8. TWO-POINT CORRELATION FUNCTION (TPCF) AMPLITUDE GALAXY-GALAXY TPCF SHOWS EVIDENCE FOR SUPERCLUSTER FILAMENTS AT Δ V < 600 km/s AND VOIDS AT Δ V > 1000 km/s Ly α ABSORBER-ABSORBER TPCF ALSO SHOWS EXCESS ( 7σ LEVEL) DUE TO FILAMENTS AT Δ V < 600 km/s. (UPPER- RIGHT) LOWER LEFT PANEL SHOWS THAT THIS EXCESS IS DUE ENTIRELY TO STRONGER Ly α LINES (N HI > 10 13 cm -2 ). LOWER LEFT PANEL ALSO SHOWS A HINT OF VOIDS (deficit at larger ΔV). O VI ABSORBERS WITH Ly α LINES IN PAIRS CAN ACCOUNT FOR THIS ENTIRE EXCESS. THE LOWER-RIGHT PANEL SHOWS THAT WEAKER Ly α ABSORBERS SHOW NO EVIDENCE FOR CLUSTERING IN SPACE

11.  SPECTRUM OF DWARF IS POST-STARBURST [Z]= -1±0.5; AGE=3.5±1.5 Gyrs

12. ABSORBER/GALAXY CONNECTIONS 3C273 ABSORBER cz= 1586 ± 5 km/s N HI = 7 x 10 15 cm -2 n = 1.4 x 10 -3 cm -3 Shell thickness = 70 pc Shell mass < 10 8 M sun (if centered on dwarf) [Fe/H] = -1.2 [Si/C] = +0.2 DWARF SPHEROIDAL GALAXY cz = 1635 ± 50 km/s b= 71 h -1 70 kpc m B = 17.9 M B = -13.9  6 x 10 7 L sun M HI < 3 x 10 6 M sun [Fe/H] = -1 Mean Stellar Age = 2—5 Gyrs  STARBURST(S) totalling > 0.3 M sun yr -1 for ˜ 10 8 yrs at a time 2— 5 Gyrs ago had sufficient SN energy to expel > 3 X 10 7 M sun of gas at 20—30 km s -1 to ~ 100 kpc and so create the 3C273 absorber

13.  ``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067  OPTICAL IMAGE WITH HI 21cm CONTOURS  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) 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). 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.

14. VELOCITY FIELD OBTAINED FROM VLA H I EMISSION MAP  (Carilli & van Gorkom 1992) REQUIRES CLOUD TO BE INFALLING (V RADIAL = -115 km/s) UNLESS THE HALO GAS IS COUNTER-ROTATING. EVEN IF THE HI 21cm ABSORBER IS OUTFLOWING, IT STILL LACKS THE ESCAPE SPEED. ARECIBO HI PROFILE OF NGC 3067: HI 21cm ABSORBER AT cz(cloud) – cz(galaxy)= 45 ± 5 km/s. ARROWS MARK OTHER METAL-LINE SYSTEMS WITH N HI < 1 X 10 19 cm -2. (Keeney et al. 2005)  LOWEST REDSHIFTS H I 21cm PROVIDES ESSENTIAL INFORMATION 3C 232 NGC 3067

15. LYMAN LIMIT SYSTEMS AS HVC ANALOGUES NGC 3067 H I ABSORBER N HI = 1.0 x 10 20 cm -2 T spin = 500 ± 200 K T kinetic = 380 ± 30 K R(galactocentric)= 11 kpc CLOUD SIZE = 5 kpc Z > 0.25 SOLAR f escape < 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 SOLAR f escape = 1—2% Keeney et al (2005) Putman et al (2003) Akeson & Blitz (1999) Collins, Shull & Giroux (2004) Hulsbosch & Wakker (1988)

16.  THE MILKY WAY’S NUCLEAR WIND: BOUND TO THE GALAXY AT 12.4 kpc (l,b)=(350,+55) (see Keeney poster this conference)

17. GASEOUS FILAMENT VOID  FILAMENT

18. WHAT COULD BE DONE IF THE ``COSMIC ORIGINS SPECTROGRAPH’’ CAN GET INTO ORBIT ( ONE WAY OR ANOTHER! )  he Extent, Metallicity and Kinematics of a Normal, Luminous (~L*) Spiral Galaxy Using multiple QSO sightlines

19. CUMULATIVE DISTRIBUTION FUNCTIONS (CDFs) OF NEAREST NEIGHBOR GALAXY DISTANCES TOP: > L * GALAXIES BOTTOM: > 0.1L * GALAXIES CHANGING LIMITING GALAXY LUMINOSITIES DOES NOT ALTER THE BASIC RESULT: ABSORBER- GALAXY DISTANCES ARE > GALAXY-GALAXY DISTANCES  IT IS DIFFICULT TO ASSOCIATE AN ABSORBER WITH ANY ONE GALAXY MEDIAN NEAREST NEIGHBOR DISTANCES FROM ABSORBERS TO 0.1L * GALAXIES ARE ~ ½ DISTANCES TO L* GALAXIES