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QSO ABSORPTION LINE STUDIES with the HUBBLE SPACE TELESCOPE

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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: DLA @ > 300 QSO ABSORBERS found by HST cz=5250 Spectrographs at z < 0.1 and at low km/s in UV and H I 12.5—16.5 -2 column densities (NH I = 10 cm ) 21cm AND spectra of PKS 1327- 206 >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 QSO ABSORPTION LINE STUDIES with the HUBBLE SPACE TELESCOPE COLORADO GROUP: JOHN STOCKE, MIKE SHULL, JAMES GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY H II Results thus far based on: regions in red > 300 QSO ABSORBERS found by HST in ESO Spectrographs at z < 0.1 and at low G1327- 2041 12.5—16.5 -2 column densities (NH I = 10 cm ) 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 Ly reveals H I not visible @ redshifted 21cm emission or absorption lines ?? SUMMARY OF STATISTICAL RESULTS 13 • COSMIC BARYON CENSUS: Ly / baryon = 29 ± 4 % (most of the mass is in NHI < 10 cm-2 absorbers) • ASSOCIATION WITH GALAXIES? 78% LOCATED IN SUPERCLUSTER FILAMENTS; 13 -2 22% IN VOIDS. STRONGER absorbers at NH I > 10 cm 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) 13 -2 • At least 55% of all Ly absorbers with NH I > 10 cm are METAL-BEARING at ~ 10% SOLAR. A typical galaxy filament is covered >50% by metal-enriched gas -1 • Metal-bearing absorbers show spread of metals of 150—800h 70 kpc from the nearest -1 L* galaxy (23 absorbers in complete sample) and 50—450 h 70 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) 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. 2007 Apj, 671, 146 Sample Sizes = 23 9 (of metal-enriched absorbers) EXAMPLES of ABSORBER ..DWARF GALAXY PAIRS KEENEY et al In prep. Dwarf Galaxy Winds May Be the largest contributor to IGM metal enrichment Dwarf Galaxy Winds Reproduced from Keeney et al. 2006, AJ, 132, Reproduced from Stocke et al. 2004, ApJ, 609, 94. 2496 3C 273 / 0.004 L* Dwarf SBS 1122+594 / IC 691 (0.06 L*) Dwarf galaxies produce unbound winds! SBS 1122+594 / IC 691ABSORBER/GALAXY CONNECTIONS IC 691: H I 21 cm SDSS J112625.97+591737.5 czabs czgal = 1204 ± 3 km/s IC 691 czabs(CIV) = 1110 ± 30 km/s 15 -2 NHI ~ 10 cm vesc(r>33kpc) 35 km/s from Keeney et al. 2006, AJ, 132, 2496 SPECTRUM OF DWARF IS POST-STARBURST Complete Blow Out then fading to [Z]= -1±0.5; AGE=3.5±1.5 Gyrs become Dwarf Spheroidal? “Cheshire Cat Galaxy” (Charlton, 1995) 3C 273 Absorber/Galaxy Connections 3C 273 Absorber Dwarf Spheroidal Galaxy cz= 1586 ± 5 km/s cz = 1635 ± 50 km/s 15 2 1 NHI = 7 x 10 cm b= 71 h 70 kpc 3 3 n = 1.4 x 10 cm mB = 17.9 MB = 13.9 7 Shell thickness = 70 pc L ~ 6 x 10 L ~ 0.004 L* 8 6 Shell mass < 10 M MHI < 3 x 10 M (if centered on dwarf) [Fe/H] = 1.2 [Fe/H] = 1 [Si/C] = +0.2 Mean Stellar Age = 2-5 Gyrs 1 8 STARBURST(S) totaling > 0.3 M yr for ~10 yrs at a time 2-5 7 Gyrs ago had sufficient SN energy to expel > 3 X 10 M of gas at 20-30 km s1 to ~100 kpc and so create the 3C 273 absorber. VOID VOID VOID FILAMENT GASEOUS FILAMENT 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 Mpc2 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 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 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=0—0.1. #2: NUV Camera: 2150-2350Å band 33 arcmin FOV; 3 arcsec resolution -2 MAB = 30.8 arcsec in deep pointing for 6 arcsec sized object #3: FUV Camera: 900-1000Å band PI: James Green, -2 MAB = 27.6 arcsec in deep pointing for 6 arcsec sized object U of Colorado MEDIAN DISTANCE TO NEAREST > 0.1L* GALAXY Sample Distance in Sample -1 Name h 70 kpc Size • L* Galaxies : 350 500 • O VI Absorbers : 290 23 • Stronger half Ly Sample : 450 69 • Weaker half Ly 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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