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QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS

QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS. COLORADO GROUP: JOHN STOCKE, MIKE SHULL, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY

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QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS

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  1. QSO ABSORBER GALAXY ASSOCIATIONSFINDING 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 (NH I = 1012.5—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

  2. SUMMARY OF STATISTICAL RESULTS • COSMIC BARYON CENSUS: WLy a /Wbaryon = 29 ± 4 % (most of mass in low column density (NHI < 1014 cm-2) absorbers) • ASSOCIATION WITH GALAXIES? 78% LOCATED IN SUPERCLUSTER FILAMENTS; 22% IN VOIDS. ABSORBERS AT NH I > 1013 cm-2 ARE MUCH MORE CLOSELY ASSOCIATED WITH GALAXIES; WEAKER ABSORBERS ARE NEARLY UNIFORMLY DISTRIBUTED IN SPACE • Wb(voids)/ Wb = 4.5 ±1.5% as predicted by simulations (Gottlober et al 2003); • At least 55% of all Ly α absorbers with NH I > 1013 cm-2 are metal-bearing • O VI-bearing absorbers indicate spread of metals from nearest L* galaxies: 150—800h-170 kpc • For details see Penton et al. (2000a,b, 2002, 2004) ApJ and watch for Stocke et al. (in prep).

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

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

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

  6. 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 (NHI > 1013 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

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

  8. 3C273 ABSORBER cz= 1586 ± 5 km/s NHI = 7 x 1015 cm-2 n = 1.4 x 10-3 cm-3 Shell thickness = 70 pc Shell mass < 108 Msun (if centered on dwarf) [Fe/H] = -1.2 [Si/C] = +0.2 DWARF SPHEROIDAL GALAXY cz = 1635 ± 50 km/s b= 71 h-170 kpc mB = 17.9 MB = -13.9  6 x 107 Lsun MHI < 3 x 106 Msun [Fe/H] = -1 Mean Stellar Age = 2—5 Gyrs ABSORBER/GALAXY CONNECTIONS STARBURST(S) totalling > 0.3 Msun yr-1 for ˜ 108 yrs at a time 2—5 Gyrs ago had sufficient SN energy to expel > 3 X 107 Msun of gas at 20—30 km s-1 to ~ 100 kpc and so create the 3C273 absorber

  9. ``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067 • OPTICAL IMAGE WITH HI 21cm CONTOURS 3C 232 z=0.533; Absorber has NHI= 1 x 1020 cm-2 and Tspin = 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.

  10. AT LOWEST REDSHIFTS H I 21cm PROVIDES ESSENTIAL INFORMATION 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 NHI < 1 X 1019 cm-2. (Keeney et al. 2005) 3C 232 VELOCITY FIELD OBTAINED FROM VLA H I EMISSION MAP  (Carilli & van Gorkom 1992) REQUIRES CLOUD TO BE INFALLING (VRADIAL = -115 km/s) UNLESS THE HALO GAS IS COUNTER-ROTATING. EVEN IF THE HI 21cm ABSORBER IS OUTFLOWING, IT STILL LACKS THE ESCAPE SPEED. NGC 3067

  11. NGC 3067 H I ABSORBER NHI = 1.0 x 1020 cm-2 Tspin= 500 ± 200 K Tkinetic= 380 ± 30 K R(galactocentric)= 11 kpc CLOUD SIZE = 5 kpc Z > 0.25 SOLAR fescape < 2% GALACTIC HVCs NHI > 2 X 1018 cm-2 Tspin > 200 K R(Galactocentric) < 40 kpc CLOUD SIZE = 3—20 kpc Z = 0.08-0.35 SOLAR fescape= 1—2% LYMAN LIMIT SYSTEMS AS HVC ANALOGUES Keeney et al (2005) Putman et al (2003) Akeson & Blitz (1999) Collins, Shull & Giroux (2004) Hulsbosch & Wakker (1988)

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

  13. VOID VOID VOID FILAMENT GASEOUS FILAMENT

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

  15. 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

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