QSO ABSORBER GALAXY ASSOCIATIONSFINDING THE KEYS AT THE LOWEST

REDSHIFTSCOLORADO 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

SUMMARY OF STATISTICAL RESULTS

• COSMIC BARYON CENSUS: Ly baryon = 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

• b(voids)/ b = 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-1

70 kpc

• For details see Penton et al. (2000a,b, 2002, 2004) ApJ and watch for Stocke et al. (in prep).

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

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 Sample : 240 69• Weaker half Ly Sample : 1650 69---------------------------------------------------------------------• Simulations of WHIM GAS : 200 Dave’ et al• Simulations of Photo-ionized Gas: 1200 (1999)

Lyα LINE PROFILES FOR OVI ABSORBERS: A SAMPLING

SINGLE:

SINGLE

SINGLE

SINGLE

SINGLE: SINGLE

DOUBLE

DOUBLE DOUBLE

DOUBLE

DOUBLE

DOUBLE

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

SPECTRUM OF DWARF IS POST-STARBURST

[Z]= -1±0.5; AGE=3.5±1.5 Gyrs

ABSORBER/GALAXY CONNECTIONS

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

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

``CLOSE-UP’’ OF A LYMAN LIMIT SYSTEM: 3C232/NGC 3067

OPTICAL IMAGE WITH HI 21cm CONTOURS

C 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.

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.

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)

LOWEST REDSHIFTS H I 21cm PROVIDES ESSENTIAL INFORMATION

3C 232

NGC 3067

LYMAN LIMIT SYSTEMS AS HVC ANALOGUES

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%

Keeney et al (2005) Putman et al (2003)

Akeson & Blitz (1999)

Collins, Shull & Giroux (2004)

Hulsbosch & Wakker (1988)

THE MILKY WAY’S NUCLEAR WIND: BOUND TO THE GALAXY AT 12.4 kpc

(l,b)=(350,+55) (see Keeney poster this conference)

GASEOUS FILAMENT

VOIDVOID VOID

FILAMENT

WHAT COULD BE DONE IF THE ``COSMIC ORIGINS SPECTROGRAPH’’

CAN GET INTO ORBIT ( ONE WAY OR ANOTHER! )

he Extent, Metallicity and Kinematics of a Normal, Luminous (~L*) Spiral Galaxy Using multiple QSO sightlines

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