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CONNECTING GALAXIES TO THE COSMIC WEB WITH HUBBLE AND EVLA. 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

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slide1

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:

> 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

Strong Mg II, maybe DLA? @

cz=5250 km/s in HST & HI 21cm spectra of PKS 1327-206

slide2

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:

> 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 G1327-2041

vla h i emission absorption in pks 1327 204 a typical galaxy disk
VLA H I EMISSION & ABSORPTION INPKS 1327-204A typical galaxy disk ?

System #2

System #1

Log N H I = 19.3 for T~100K 20.1 for T~300K

But no Lyα 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

slide4

WF/PC2 Hα 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

slide5

``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 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

H I 21 cm velocity contours

3C 232

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

H I 21 cm

NGC 3067

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

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

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

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

3C 232 / NGC 3067
strong mg ii lyman limit systems as hvc analogs
Strong Mg II/Lyman Limit Systems as HVC Analogs

NGC 3067 H I Absorber

NHI = 1.0 x 1020 cm-2

Tspin= 500 ± 200 K

Tkin = 380 ± 30 K

R(Galactocentric)= 11 kpc

Cloud Size = 5 kpc

Z > 0.25 Z8

UV fesc < 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 Z8

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)

sbs 1122 594 ic 691 absorber galaxy connections

IC 691: H I 21 cm

SDSS J112625.97+591737.5

czgal = 1202 ± 5 km/s

czabs(CIV) = 1110 ± 50

km/s

NHI~ 1015 cm-2

vesc(r>33kpc) ≤35 km/s

IC 691

SBS 1122+594 / IC 691ABSORBER/GALAXY CONNECTIONS

czabs

from Keeney et al. 2006, AJ, 132, 2496

slide9

GalaxyLuminosityDgal-absWind Is

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

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

Which Starburst Winds Escape ?QSO Galaxy Pairs are new probe of Feedback to IGM(Brian Keeney, PhD dissertation 2007)
slide10

VOID

VOID

VOID

FILAMENT

GASEOUS FILAMENT

slide11

Typical H I 21cm emitter (DLA)

G = Galactic Disk & HVCs

Lyα = feedback + pristine

slide12

Absorption Studies with HST + GHRS/STIS/COS allows direct connections between gas and galaxies, filaments and cosmic voids to be explored in detail

??

slide13

IGM Gas without feedback from Galactic Superwinds

YELLOW: T > 106.5 oK (OVII/OVIII WHIM) RED: T=105--6.5 oK (OVI WHIM) GREEN & BLUE: T=103.5--5 oK (Warm IGM: Lyα 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

slide14

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 Lyα

(7 targets totaling Δz  1.5)

Bright, long pathlength targets

(entire GTO target set yields Δz  15)

PI: James Green, U of Colorado

slide15

COS OPTICAL LAYOUT: FUV PRIME SPECTROGRAPH

NUV originally for STIS BACKUP

NUV MAMA

Detector

(STIS spare)

Calibration

Platform

OSM2: G185M, G225M,

G285M, G230L, TA1

  • 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

FUV XDL

Detector

Aperture Mechanism:

Primary Science Aperture,

Bright Object Aperture

OSM1: G130M,

G160M, G140L,

NCM1

Optical bench

(not shown):

re-use of GHRS

bench

slide18

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