QSO ABSORPTION LINE STUDIES with the HUBBLE SPACE TELESCOPE

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1 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 = 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 UV and H I 21cm spectra of PKS

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 = cm -2 ) AND H II regions in red in ESO G >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

3

4 Ly reveals H I not redshifted 21cm emission or absorption lines??

5 SUMMARY OF STATISTICAL RESULTS COSMIC BARYON CENSUS: Ly / baryon = 29 ± 4 % (most of the mass is in N HI < cm -2 absorbers) 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 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 show spread of metals of h kpc from the nearest L* galaxy (23 absorbers in complete sample) and h kpc from the nearest 0.1L* galaxy (9 absorbers in complete sample) based on OVI and CIII (C IV, Si III accounting and covering factor measurements 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 and C III absorbers with FUSE)

6 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 O VI maximum impact parameters from Stocke et al Apj, 671, 146 Sample Sizes = 23 9 (of metal-enriched absorbers)

7 EXAMPLES of ABSORBER..DWARF GALAXY PAIRS KEENEY et al In prep. Dwarf Galaxy Winds May Be the largest contributor to IGM metal enrichment

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

9 SBS / IC 691ABSORBER/GALAXY CONNECTIONS SDSS J IC 691: H I 21 cm cz abs IC 691 cz gal = 1204 ± 3 km/s cz abs(civ) = 1110 ± 30 km/s N HI ~ cm -2 v esc (r>33kpc) 35 km/s from Keeney et al. 2006, AJ, 132, 2496

10 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

11 3C 273 Absorber/Galaxy Connections 3C 273 Absorber Dwarf Spheroidal Galaxy cz= 1586 ± 5 km/s N HI = 7 x cm 2 n = 1.4 x 10 3 cm 3 Shell thickness = 70 pc Shell mass < 10 8 M (if centered on dwarf) [Fe/H] = 1.2 [Si/C] = +0.2 cz = 1635 ± 50 km/s b= 71 h 1 70 kpc m B = 17.9 M B = 13.9 L ~ 6 x 10 7 L ~ L* M HI < 3 x 10 6 M [Fe/H] = 1 Mean Stellar Age = 2-5 Gyrs STARBURST(S) totaling > 0.3 M yr 1 for ~10 8 yrs at a time 2-5 Gyrs ago had sufficient SN energy to expel > 3 X 10 7 M of gas at km s 1 to ~100 kpc and so create the 3C 273 absorber.

12 VOID VOID VOID FILAMENT GASEOUS FILAMENT

13 COSMIC ORIGINS SPECTROGRAPH: TO BE INSTALLED DURING SERVICING MISSION #4 IN SEPTEMBER 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 Mpc 2 region BL Lac Targets to search for Broad Ly (7 targets totaling z 1.5) Bright, long pathlength targets (entire GTO target set yields z 15) PI: James Green, U of Colorado

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

15 IGM: The InterGalactic Medium Explorer tracing the Baryons from Cosmic Web to Galaxy Halo Science Payloads: #1: Long-Slit Diffuse Spectrograph Ly and O VI 1031Å at / =2000 Slit: 1 x 20 arcminutes Sensitivity: 25 photon units in deep, multi-day pointings at z= #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 PI: James Green, U of Colorado

16 MEDIAN DISTANCE TO NEAREST > 0.1L* GALAXY Sample Distance in Sample Name h kpc Size L* Galaxies : O VI Absorbers : Stronger half Ly Sample : Weaker half Ly Sample : Simulations of WHIM GAS : 200 Dave et al Simulations of Photo-ionized Gas: 1200 (1999) Data from Stocke et al ApJ 641, 217

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