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CONNECTING GALAXIES TO THE COSMIC WEB WITH HUBBLE AND EVLA

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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CONNECTING GALAXIES TO THE COSMIC WEB WITH HUBBLE AND EVLA

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  1. 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

  2. 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

  3. 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

  4. 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

  5. ``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.

  6. 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

  7. 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)

  8. 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

  9. 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)

  10. VOID VOID VOID FILAMENT GASEOUS FILAMENT

  11. Typical H I 21cm emitter (DLA) G = Galactic Disk & HVCs Lyα = feedback + pristine

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

  13. 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

  14. 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

  15. 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

  16. HST + COS SURVEYS THE GREAT WALLSIX SIGHTLINES OVER 30 Mpc2

  17. 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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