CONNECTING GALAXIES TO THE COSMIC WEB WITH HUBBLE AND EVLA

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CONNECTING GALAXIES TO THE COSMIC WEBWITH HUBBLE
AND EVLA
COLORADO GROUP JOHN STOCKE, MIKE SHULL, JAMES
GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN
KEENEY Results thus far based on gt 300 QSO
ABSORBERS found by HST Spectrographs at z lt 0.1
and at low column densities (NH I 1012.516.5
cm-2 ) AND gt1.35 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
Strong Mg II, maybe DLA? _at_ cz5250 km/s in HST
HI 21cm spectra of PKS 1327-206
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QSO ABSORPTION LINE STUDIESwith the HUBBLE SPACE
TELESCOPE
COLORADO GROUP JOHN STOCKE, MIKE SHULL, JAMES
GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN
KEENEY Results thus far based on gt 300 QSO
ABSORBERS found by HST Spectrographs at z lt 0.1
and at low column densities (NH I 1012.516.5
cm-2 ) AND gt1.35 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 G1327-2041
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VLA H I EMISSION ABSORPTION INPKS 1327-204A
typical galaxy disk ?
System 2
System 1
Log N H I 19.3 for T100K 20.1 for
T300K But no Lya absorption available due
to intervening Lyman limit system at higher z
SYSTEM 1 2
Radio continuum in green H I 21cm emission in
blue Contours 2.5, 5, 10, 15 x 1020 cm-2
FWHM 17 km/s 44 km/s
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WF/PC2 Ha Image shows no plumes or wisps in
direction of 3C232 ? not outflow? Greater
obscuration of H II regions to bottom of NGC 3067
support underside view of NGC 3067 ? gas seen
in H I absorption is infalling
3C 232
NGC 3067
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CLOSE-UP OF A LYMAN LIMIT SYSTEM
3C232/NGC 3067

• OPTICAL IMAGE WITH HI 21cm CONTOURS (Carilli
  van Gorkom  1992 ApJ 399, 373)
• 3C 232 z0.533 Absorber has NHI 1 x 1020 cm-2
  and Tspin 500
  200 K (Keeney et al. 2005 ApJ 622, 267)
• NGC 3067 cz1465 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 _at_ 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.
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3C 232 / NGC 3067
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Strong Mg II/Lyman Limit Systems as HVC Analogs
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SBS 1122594 / IC 691ABSORBER/GALAXY CONNECTIONS
czabs
from Keeney et al. 2006, AJ, 132, 2496
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Which Starburst Winds Escape ?QSO Galaxy Pairs
are new probe of Feedback to IGM(Brian Keeney,
PhD dissertation 2007)
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VOID
VOID
VOID
FILAMENT
GASEOUS FILAMENT
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Typical H I 21cm emitter (DLA)
G Galactic Disk HVCs
Lya feedback pristine
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Absorption Studies with HST GHRS/STIS/COS
allows direct connections between gas and
galaxies, filaments and cosmic voids to be
explored in detail
??
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IGM Gas without feedback from Galactic
Superwinds YELLOW T gt 106.5 oK (OVII/OVIII
WHIM)
RED T105--6.5 oK (OVI WHIM)
GREEN BLUE T103.5--5 oK
(Warm
IGM Lya Forest) Simulation without GSW finds
30 of local IGM in the WHIM IGM Gas WITH
Galactic Superwind Feedback (prescription
requires that feedback is proportional to the
local star formation rate per pixel) GSW
Simulation finds 50 of local IGM in WHIM Cen
Ostriker 2006 ApJ 650, 560 and
Cen Fang 2006 ApJ 650, 573
30 h-170 Mpc
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COSMIC ORIGINS SPECTROGRAPH TO BE INSTALLED
DURING SERVICING MISSION 4 IN MAY 2009

• 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 Lya
• (7 targets totaling ?z ? 1.5)
• Bright, long pathlength targets
• (entire GTO target set yields ?z ? 15)

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COS OPTICAL LAYOUT FUV PRIME SPECTROGRAPH
NUV originally
for STIS BACKUP
NUV MAMA Detector (STIS spare)
Calibration Platform
OSM2 G185M, G225M, G285M, G230L, TA1
FUV XDL Detector
Aperture Mechanism Primary Science
Aperture, Bright Object Aperture
OSM1 G130M, G160M, G140L, NCM1

• COS has 2 channels to provide low and medium
• resolution UV spectroscopy
• FUV 1150-1775Å, NUV 1700-3200Å
• FUV gratings G130M, G160M, G140L
• NUV gratings G185M, G225M, G285M, G230L
• M gratings have spectral resolution of R 20,000

Optical bench (not shown) re-use of GHRS bench
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HST COS SURVEYS THE GREAT WALLSIX SIGHTLINES
OVER 30 Mpc2
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WHAT WILL BE DONE WHEN THE
COSMIC ORIGINS
SPECTROGRAPH IS INSTALLED THIS YEAR NEXT ON HST
The Extent, Metallicity and Kinematics of a
Normal, Luminous (L) Spiral Galaxy Halo Using
Multiple QSO sightlines
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