QSO ABSORBER GALAXY ASSOCIATIONSFINDS THE KEYS AT THE LOWEST

REDSHIFTSCOLORADO GROUP: JOHN STOCKE, MIKE SHULL, STEVE PENTON,

CHARLES DANFORTH, BRIAN KEENEYALUMNI: MARK GIROUX (ETSU), JASON TUMLINSON (YALE),

JESSICA ROSENBERG (George Mason), MARY PUTMAN (MICHIGAN), KEVIN McLIN (Sonoma State)

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

??

SUMMARY OF STATISTICAL RESULTS• COSMIC BARYON CENSUS: Ly baryon = 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.

• b(voids)/ b = 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)

Impact Parameters Required to reproduce the Observed OVI dN/dz(covering factor = 0.5; all galaxies of luminosity > L contribute)

Sample Sizes = 23 9 (of metal-enriched absorbers)

Figure from

Tumlinson & Fang

2005 ApJL 623, L97 as added to by Shull, this conference

Do Starburst Winds Escape ?(Brian Keeney, PhD dissertation)

Dwarf galaxies may play a larger role in the chemical evolution of the intergalactic medium than their more massive counterparts.

Galaxy Luminosity Dgal-abs Wind

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

``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067OPTICAL IMAGE WITH HI 21cm CONTOURS (Carilli & van Gorkom  1992 ApJ 399, 373)

C 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.

3C 232 / NGC 3067

Velocity field suggests H I 21 cm cloud to be infalling (vrad = 115 km/s) unless the halo gas is counter-rotating.

Reproduced from Carilli & van Gorkom, 1992, ApJ, 399, 373.

NGC 3067

3C 232

H I 21 cm velocity contours

Metals from Na I D to C IV are observed with the same 3 velocity components, but H I is only detected in one.

Reproduced from Tumlinson et al. 1999, AJ, 118, 2148.

Reproduced from Keeney et al. 2005, ApJ, 622, 267.

H I 21 cm

NGC 3067 H I Absorber

NHI = 1.0 x 1020 cm2

Tspin= 500 ± 200 K

Tkin = 380 ± 30 K

R(Galactocentric)= 11 kpc

Cloud Size = 5 kpc

Z > 0.25 Z

UV fesc < 2%

Galactic HVCs

NHI > 2 x 1018 cm2

Tspin > 200 K

R(Galactocentric) < 40 kpc

Cloud Size = 320 kpc

Z = 0.080.35 Z

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)

Lyman Limit Systems as HVC Analogs

The Milky Way’s Nuclear Wind

Reproduced from Keeney et al. 2006, ApJ, 646, 951.

Milky Way Wind: Bound at 12 kpc

PKS 2005489 Absorbers

vlsr = 105±12 +168±10 km/svw = 250±20 +250±20 km/svesc = +560±90 +560±90 km/s

zobs = 4.9±0.2 5.8±0.2 kpczmax = 10.8±0.9 12.5±1.0 kpc

Mrk 1383 Absorbers

vlsr = +46±7 +95±11 km/svw = +30±10 +90±15 km/svesc = +530±90 +520±90 km/s

zobs = +11.7±0.2 +12.2±0.3 kpczmax = +12.6±0.1 +12.6±0.1 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).

Dwarf Galaxy Winds

3C 273 / 0.004 L* Dwarf SBS 1122+594 / IC 691 (0.06 L*)

Dwarf galaxies produce unbound winds!

Reproduced from Stocke et al. 2004, ApJ, 609, 94.Reproduced from Keeney et al. 2006, AJ, 132, 2496

SPECTRUM OF DWARF IS POST-STARBURST

[Z]= -1±0.5; AGE=3.5±1.5 GyrsComplete Blow Out then fading to become Dwarf Spheroidal? “Cheshire Cat Galaxy” (Charlton, 1995)

3C 273 Absorber

cz= 1586 ± 5 km/s

NHI = 7 x 1015 cm2

n = 1.4 x 103 cm3

Shell thickness = 70 pc

Shell mass < 108 M

(if centered on dwarf)

[Fe/H] = 1.2

[Si/C] = +0.2

Dwarf Spheroidal Galaxy

cz = 1635 ± 50 km/s

b= 71 h70 kpc

mB = 17.9 MB = 13.9

L ~ 6 x 107 L ~ 0.004 L*

MHI < 3 x 106 M

[Fe/H] = 1Mean Stellar Age = 2-5 Gyrs

STARBURST(S) totaling > 0.3 M yr for ~108 yrs at a time 2-5 Gyrs ago had sufficient SN energy to expel > 3 X 107 M of gas at 20-30 km s to ~100 kpc and so create the 3C 273 absorber.

3C 273 Absorber/Galaxy Connections

SBS 1122+594 / IC 691ABSORBER/GALAXY CONNECTIONS

IC 691

SDSS J112625.97+591737.5

czgal = 1202 ± 5 km/s

Czabs(CIV) = 1110 ± 50

km/s

MHI = (4.1 ± 0.1) x 107 M

vesc(D > 33 kpc) ≤

35 km/s

IC 691: H I 21 cm

GASEOUS FILAMENT

VOIDVOID VOID

FILAMENT

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)

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

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

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.

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

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 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