QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS COLORADO 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 (N H I = 10 12.5—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
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QSO ABSORBER GALAXY ASSOCIATIONS FINDING THE KEYS AT THE LOWEST REDSHIFTS COLORADO GROUP: JOHN STOCKE, MIKE SHULL, STEVE PENTON, CHARLES DANFORTH, BRIAN.
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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