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QSO ABSORBER GALAXY ASSOCIATIONS FINDS THE KEYS AT THE LOWEST REDSHIFTS

QSO ABSORBER GALAXY ASSOCIATIONS FINDS 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 FINDS THE KEYS AT THE LOWEST REDSHIFTS

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  1. QSO ABSORBER GALAXY ASSOCIATIONSFINDS THE KEYS AT THE LOWEST REDSHIFTS COLORADO GROUP: JOHN STOCKE, MIKE SHULL, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY ALUMNI: MARK GIROUX (ETSU), JASON TUMLINSON (YALE), JESSICA ROSENBERG (George Mason), MARY PUTMAN (MICHIGAN), KEVIN McLIN (SonomaState) ELSEWHERE: RAY WEYMANN (NIRVANA), J. VAN GORKOM (COLUMBIA), CHRIS CARLLI ( NRAO) Results 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

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  3. SUMMARY OF STATISTICAL RESULTS • COSMIC BARYON CENSUS: WLy a /Wbaryon = 29 ± 4 % (most of the mass is in NHI < 10 13 cm-2 absorbers) • 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. • Wb(voids)/ Wb = 4.5 ±1.5% AS PREDICTED BY SIMULATIONS (Gottlober et al 2003). Metallicity < 1.5% Solar (Stocke et al. 2007, ApJ, in press; Dec 20 issue) • 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 show spread of metals of 150—800h-170 kpc from the nearest L* galaxy (23 absorbers in complete sample) and 50—450 h-170 kpc from the nearest 0.1L* galaxy (9 absorbers in complete sample) based on OVI and CIII (C IV, Si III accounting in progress) • For details see PENTON et al. (2000a,b, 2002, 2004) ApJ (Ly alpha absorbers) and STOCKE et al. (2006) ApJ 641, 217 . (OVI absorbers)

  4. Impact Parameters Required to reproduce the Observed OVI dN/dz(covering factor = 0.5; all galaxies of luminosity > L contribute) Figure from Tumlinson & Fang 2005 ApJL 623, L97 as added to by Shull, this conference Sample Sizes = 23 9 (of metal-enriched absorbers)

  5. GalaxyLuminosityDgal-absWind 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  Dwarf galaxies may play a larger role in the chemical evolution of the intergalactic medium than their more massive counterparts. Do Starburst Winds Escape ?(Brian Keeney, PhD dissertation)

  6. ``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067 • OPTICAL IMAGE WITH HI 21cm CONTOURS (Carilli & van Gorkom 1992 ApJ 399, 373) • 3C 232 z=0.533; Absorber has NHI= 1 x 1020 cm-2 and Tspin = 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.

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

  8. Lyman Limit Systems as HVC Analogs NGC 3067 H I Absorber NHI = 1.0 x 1020 cm-2 Tspin= 500 ± 200 K Tkin = 380 ± 30 K R(Galactocentric)= 11 kpc Cloud Size = 5 kpc Z > 0.25 Z8 UV fesc < 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 Z8 UV fesc= 1-2% Keeney et al (2005) Putman et al (2003) Tumlinson et al (1999) Akeson & Blitz (1999) Collins, Shull, & Giroux (2004) Hulsbosch & Wakker (1988)

  9. Reproduced from Keeney et al. 2006, ApJ, 646, 951. The Milky Way’s Nuclear Wind

  10. Mrk 1383 Absorbers vlsr = +46±7 +95±11 km/s vw = +30±10 +90±15 km/s vesc = +530±90 +520±90 km/s zobs = +11.7±0.2 +12.2±0.3 kpc zmax = +12.6±0.1 +12.6±0.1 kpc PKS 2005-489 Absorbers vlsr = -105±12 +168±10 km/s vw = -250±20 +250±20 km/s vesc = +560±90 +560±90 km/s zobs = -4.9±0.2 -5.8±0.2 kpc zmax = -10.8±0.9 -12.5±1.0 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). Milky Way Wind: Bound at 12 kpc

  11. Reproduced from Stocke et al. 2004, ApJ, 609, 94. Reproduced from Keeney et al. 2006, AJ, 132, 2496 3C 273 / 0.004 L* Dwarf SBS 1122+594 / IC 691 (0.06 L*) Dwarf galaxies produce unbound winds! Dwarf Galaxy Winds

  12. SPECTRUM OF DWARF IS POST-STARBURST Complete Blow Out then fading to become Dwarf Spheroidal? “Cheshire Cat Galaxy” (Charlton, 1995) [Z]= -1±0.5; AGE=3.5±1.5 Gyrs

  13. 3C 273 Absorber/Galaxy Connections 3C 273 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 M8 (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  L ~ 6 x 107 L8 ~ 0.004 L* MHI < 3 x 106 M8 [Fe/H] = -1 Mean Stellar Age = 2-5 Gyrs STARBURST(S) totaling > 0.3 M8 yr-1 for ~108 yrs at a time 2-5 Gyrs ago had sufficient SN energy to expel > 3 X 107 M8 of gas at 20-30 km s-1 to ~100 kpc and so create the 3C 273 absorber.

  14. IC 691: H I 21 cm SDSS J112625.97+591737.5 czgal = 1202 ± 5 km/s Czabs(CIV) = 1110 ± 50 km/s MHI = (4.1 ± 0.1) x 107 M8 vesc(D > 33 kpc) ≤ 35 km/s IC 691 SBS 1122+594 / IC 691ABSORBER/GALAXY CONNECTIONS

  15. VOID VOID VOID FILAMENT GASEOUS FILAMENT

  16. COSMIC ORIGINS SPECTROGRAPH: TO BE INSTALLED DURING SERVICING MISSION #4 IN AUGUST 2008 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)

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

  18. Does 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 # confirmed but not confirmed (b > 40 km/s) as BLAs narrower as absorbers 99 52 30 17 But: 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) For Lehner et al. sample we have curve-of-growth b-values for 20 absorbers with b(Lyα) > 40 and find < b(COG)/b(Lyα) >=0.61, so that for absorbers truly at T > 105 : b (Lyα) > 65 km/s, for which, the Lehner et al. absorber numbers become: 26 6 13 7 • BLAs do NOT add significantly to Cosmic Baryon census.

  19. Examples of a contentious and an uncontentous BLA in theHE 0226-41110 spectrum

  20. MEDIAN DISTANCE TO NEAREST > 0.1L* GALAXY Sample Distance in Sample Name h-170 kpc Size • L* Galaxies : 350 500 • O VI Absorbers : 290 23 • Stronger half Ly a Sample : 450 69 • Weaker half Ly a Sample : 1850 69 ----------------------------------------------------------------------------- • Simulations of WHIM GAS : 200 Dave’ et al • Simulations of Photo-ionized Gas: 1200 (1999) • Data from Stocke et al. 2006 ApJ 641, 217

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