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Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1

Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1. Glenn Kacprzak. NMSU. Collaborators:. Chris Churchill. NMSU. Chuck Steidel. Caltech. Method & Goals.

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Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1

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  1. Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1 Glenn Kacprzak NMSU Collaborators: Chris Churchill NMSU Chuck Steidel Caltech

  2. Method & Goals • Study Mg II quasar absorption line systems in order to understand the kinematics of halos probing distances out to 70 kpcs from the galaxies. • Therefore the galaxies in our sample are selected by the known presence of Mg II absorption • Determine whether the galaxy kinematics and/or morphologies are coupled to the halo kinematics • Our main goal is to determine how early epoch galaxy halos are built and sustained.

  3. Quasar Spectra & Intervening Galaxies Mg II 2796, 2803

  4. High Resolution Spectra 2796 2803 Mg II 2796, 2803

  5. Quasar Spectra of Intervening Galaxies Velocity km s-1 Sample includes absorbers with W(2796) < 1

  6. UnderStanding Galaxies is the Key Selected 5 edge-on galaxies 4 of the 5 showed the trend for the halo gas kinematics follows that of the galaxies What is needed is a larger sample which represents a broad range of orientations with respect to the quasar line of sight Steidel et al. (2002)

  7. HST WFPC-2 5” z = 0.374 z = 0.298 z = 0.346 z = 0.368 z = 0.317 Orientated such that the QSO is down 5” z = 0.418 z = 0.442 z = 0.472 z = 0.494 z = 0.437 z = 0.525 z = 0.550 z = 0.551 z = 0.553 z = 0.591 z = 0.640 z = 0.656 z = 0.661 z = 0.729 z = 0.787 z = 0.797 z = 0.851 z = 0.888 z = 0.888 z = 0.891

  8. Halo Gas Absorption Strength Correlated to Oriention of Galaxies? PA = 45o i = 0o PA = 45o i = 30o PA = 0o i = 0o PA = N/A i = 90o cos(PA)cos(i) = 0.61 cos(PA)cos(i) = 1.0 cos(PA)cos(i) = 0.0 QSO Intensity Velocity

  9. Co-rotating Disk Gas & Oriention of Galaxies “Normal” Absorbers Wind Dominate & DLA Systems

  10. Impact Parameter & Absorption

  11. z = 0.374 z = 0.298 z = 0.346 z = 0.368 z = 0.317 z = 0.418 z = 0.442 z = 0.472 z = 0.494 z = 0.437 z = 0.525 z = 0.550 z = 0.551 z = 0.553 z = 0.591 z = 0.640 z = 0.656 z = 0.661 z = 0.729 z = 0.787 z = 0.797 z = 0.851 z = 0.888 z = 0.888 z = 0.891

  12. Galaxy Models: GIM2D Simard et al. (2002) N E HST Galaxies Model Images Residual Images

  13. GIM2D: Galaxy Asymmetry HST Image Model Model Residual RA32 RT > 0.05 Barred Spiral Structure! If more than 5% of the galaxies total residual flux is due to asymmetries then these galaxies are considered to not be “normal”; they are “asymmetric”. Schade et al. (1995)

  14. Asymmetry & Absorption Strength Asymmetric Galaxies “Normal” Galaxies “Normal” Absorbers Wind Dominate & DLA Systems

  15. Summary • Halo gas is “aware” of the kinematics of the galaxy (pilot study 5 galaxies). • There are no clear trends between absorption strength and orientation of the galaxy. More detailed models are needed. • Minor morphological perturbations are correlated to absorption strength. This may suggest that most Mg II absorption selected galaxies have had some previous minor interactions or harassments. Future Work • 21 of 25 Keck HIRES spectra are in hand and are currently being analyzed. The remaining quasar spectra will be obtained in the near future. • Obtain redshifts of remaining candidates in order to increase sample size to over 50. • Obtain rotation curves of the galaxy using Gemini and Keck.

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