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Gaseous Halos Around z=0.1 Galaxies. Glenn G. Kacprzak (Swinburne). E. Barton (UC Irvine) J. Cooke (UC Irvine) C. Churchill (NMSU) D. Ceverino (HUJ) J. Evans (NMSU) A. Klypin (NMSU) M. Murphy (Swinburne) C. Steidel (Caltech). Chynoweth et al. 2008. MgII doublet. 2796. 2803.

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2796

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  1. Gaseous Halos Around z=0.1 Galaxies Glenn G. Kacprzak (Swinburne) E. Barton (UC Irvine) J. Cooke (UC Irvine) C. Churchill (NMSU) D. Ceverino (HUJ) J. Evans (NMSU) A. Klypin (NMSU) M. Murphy (Swinburne) C. Steidel (Caltech) Chynoweth et al. 2008 MgII doublet 2796 2803

  2. Galaxy/Halo Gas Kinematics - MgII Absorption Selected Galaxies z~0.5 Q0454-220 zgal= 0.48382 D= 107 kpc Foreground galaxy QSO • 12/16 cases, all the absorbing gas resides on one side of the systemic velocity of the galaxy. • However, the a lagging halo model cannot reproduce the observed velocity spread in the gas. • 4/16 span both sides of the galaxy velocity. At least 3/4 are likely caused by winds. Gas velocities at 107 kpc are consistent with that of the galaxy Kacprzak et al. submitted Steidel et al. 2002, Ellison et al. 2003

  3. Kinematics: Simulated Galaxy and Simulated QSO LOS • 900 sightlines, sampling at 7.5 kpc intertervals. • Galaxy: vrot = 180 km/s, L = 0.4 LB* Kacprzak et al. submitted Probability Distribution vr/vT 220 kpc

  4. Galaxy Sample Selection z~0.1 Barton & Cooke 2009 • Identifying galaxy sample first, then identifying subset with background quasars. • Mr + 5 log h < -20.5 • Volume-limited sample of quasar-galaxy pairs at z ~0.11.

  5. Absorbing Galaxies at z~0.1 125 kpc Late-type absorbers Early-type absorbers

  6. Early-type Galaxy Example: - 20 kpc QSO + • Gas to one side of galaxy systemic velocity, similar to z~0.5 galaxies. Kacprzak et al. In prep

  7. Late-type Galaxy Example: - 50 kpc + QSO • All galaxies have absorption to one side of systemic velocity. • Three exhibit “counter rotating” gas. • Rotation does not account for all the velocity spread. • Gas must either be infalling or outflowing. Kacprzak et al. In prep

  8. Resolution Effects Mlow= 9.4x104 M Mmed= 0.5Mlow=4.7x104 M Mhigh= 0.1Mlow=9.4x103 M Mhigh= 0.02Mlow=1.9x103 M Low Medium High High+ N(HI) Column Density (cm-2) 110 kpc 1022 1021 1020 1019 1018 1017 1016 1015 1014 • SFR=0.3 M/yr • M*=1.3E9 M¤ • SFR=0.2 M/yr • M*=0.5E9 M¤ • SFR=0.2 M/yr • M*=1.0E9 M¤ • SFR=1.9 M/yr • M*=1.9E9 M¤ Spatial and line of sight velocity (relative to galaxy systemic) distribution of MgII gas Low Medium High vLOS vLOS vLOS vLOS MgII Covering fraction: 6% 8% 12% 8% CIV Covering fraction: 15% 21% 17% 21%

  9. Low Medium High High+ 106 Hydrogen Density 105 600 kpc 105 104 103 102 101 1 10-1 10-2 Temperature 106 103 104 Metallicity (SNII) 1 10-1 10-2 10-3 10-4 10-5 10-6

  10. Resolution Effects Mlow= 9.4x104 M Mmed= 0.5Mlow=4.7x104 M Mhigh= 0.1Mlow=9.4x103 M Mhigh= 0.02Mlow=1.9x103 M Low Medium High High+ N(HI) Column Density (cm-2) 110 kpc 1022 1021 1020 1019 1018 1017 1016 1015 1014 MgII absorption gas Velocity Distribution MgII absorption Profile Velocity Width Distribution Frequency Frequency Low Low 0.2 0.2 Medium Medium High High High+ High+ 0.1 0.1 MgII Absorption Profile Velocity Width (km/s)

  11. Summary : • Absorbing Gas at z~0.1 resides to one side of galaxy systemic velocity. • Some gas is on the opposite side, if originating from disk rotation. • Source of gas still unknown (likely combination of infall and outflow). • One way to figure this out is by with multiphase absorbing gas studies. Keck II ESI in Jan 2010 - HI, OVI, CIV absorber/galaxy connection. • MgII is sensitive to resolution effects. Although large scale structures producing the absorption are consistent. • Resolution tests may be converging for MgII, but still unsure what is causing the slight variations. Most likely scaling of feedback.

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