Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/~astro/hiconference/hiconf_pdfs/aohi08_stocke.pdf Дата изменения: Fri Feb 8 00:27:31 2008 Дата индексирования: Sun Apr 13 03:53:33 2008 Кодировка: Поисковые слова: arp 220

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 (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 in progress

DLA @
cz=5250 km/s in UV and H I 21cm spectra of PKS 1327206


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 (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 in progress

H II regions in red in ESO G13272041



Ly

reveals H I not visible @ redshifted 21cm emission or absorption lines

??


SUMMARY OF STATISTICAL RESULTS
· COSMIC BARYON CENSUS: cm-2 absorbers)
Ly

/

baryon

= 29 ± 4 % (most of the mass is in NHI < 10

13

·

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. 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 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 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)
b(

·

·

·

·


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 (of metal-enriched absorbers)

9


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 Stocke et al. 2004, ApJ, 609, 94.

Reproduced from Keeney et al. 2006, AJ, 132, 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

cz
IC 691

gal

= 1204 ± 3 km/s = 1110 ± 30 km/s

cz

abs(CIV)

NHI ~ 1015 cm-2 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 become Dwarf Spheroidal? "Cheshire Cat Galaxy" (Charlton, 1995)

[Z]= -1±0.5; AGE=3.5±1.5 Gyrs


3C 273 Absorber/Galaxy Connections
3C 273 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 M (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 L ~ 6 x 107 L ~ 0.004 L* MHI < 3 x 106 M [Fe/H] = 1 Mean Stellar Age = 2-5 Gyrs

STARBURST(S) totaling > 0.3 M yr 1 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 1 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 PI: James Green, U of Colorado

15)


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:
Science Payloads:

The InterGalactic Medium Explorer

tracing the Baryons from Cosmic Web to Galaxy Halo

#1: Long-Slit Diffuse Spectrograph Ly and O VI 1031е at / =2000 Slit: 1 x 20 arcminutes Sensitivity: 25 photon units in deep, multi-day pointings at z=0--0.1. #2: NUV Camera: 2150-2350е band 33 arcmin FOV; 3 arcsec resolution MAB = 30.8 arcsec-2 in deep pointing for 6 arcsec sized object #3: FUV Camera: 900-1000е band MAB = 27.6 arcsec-2 in deep pointing for 6 arcsec sized object PI: James Green, U of Colorado


MEDIAN DISTANCE TO NEAREST > 0.1L* GALAXY
Sample Name Distance in h-170 kpc Sample 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