1. UNM 29-Oct04 Galaxy-Halo Gas Kinematic Connection at 0.3 < z < 1 Collaborators: Chris Churchill (NMSU) Chuck Steidel (Caltech) Alice Shapley (Princeton) Wal Sargent (Caltech) Michael Murphy (IoA) Glenn Kacprzak (New Mexico State University)

2. UNM 29-Oct04 How do the kinematics of the stellar component reflect that of the halo kinematics? Do absorption properties depend on the orientation of the host galaxy? Is there a connection between absorption properties and host galaxy morphology? Toward Establishing Kinematic Detailed Connections… Our ultimate goal is to better understand how early epoch galaxy halos are built and sustained: Mg II absorbers provide excellent laboratory.

3. UNM 29-Oct04 Steidel et al. (2002) Pilot Study of Mg II Galaxy Halo & Stellar Kinematics In 4/4 strong systems, the Mg II gas co- rotates with the galaxy In one weak system the absorption is at the systemic velocity of the galaxy. RESULTS Need a sample of galaxies that have a wide range of morphologies and orientations.

4. UNM 29-Oct04 Velocity km s -1 Mg II 2796 Absorber/Galaxy Selection

5. UNM 29-Oct04 z = 0.550z = 0.551 z = 0.640z = 0.661 z = 0.374 z = 0.525 z = 0.787 z = 0.346 z = 0.442 z = 0.553 z = 0.888 z = 0.729 z = 0.418 z = 0.494 z = 0.591 z = 0.298 z = 0.888 z = 0.472 z = 0.368 z = 0.317 z = 0.437 z = 0.891 z = 0.798 z = 0.656 z = 0.851 5” z = 0.534 z = 0.524 z = 0.312 z = 0.313 z = 0.393 z = 0.948 z = 0.430 z = 0.752 z = 0.383 z = 0.702 Quasar is oriented downward

6. UNM 29-Oct04 Simard et al. (2002) N E Galaxy Models: GIM2D HST Galaxies Model Images Residual Images

7. UNM 29-Oct04 Luminosity Impact parameter Disk inclination PA wrt QSO Bulge to Total ratio Bulge effective radius Disk scale length Half light radius Morphological asymmetries Toward Establishing Kinematic Detailed Connections… Equivalent width Doublet ratio Velocity spread Velocity asymmetry Number of clouds Total column density Galaxy Properties Absorption Properties

8. UNM 29-Oct04 QSO Velocity Intensity PA = 45 o i = 90 o PA = 45 o i = 60 o PA = 0 o i = 90 o PA = N/A i = 0 o cos(PA)sin(i) = 0.61cos(PA)sin(i) = 1.0cos(PA)sin(i) = 0.0 Testing a Simple Model of Orientation and Position Angle

9. UNM 29-Oct04 No Orientation Correlation! More detailed models are needed

10. UNM 29-Oct04 Barred Spiral Structure! GIM2D: Galaxy Asymmetry HST ImageModel Model Residual

11. UNM 29-Oct04 Asymmetry & Absorption Strength Galaxy asymmetry and Impact parameter are both important factors in determining the absorption strength. 3.2 σ correlation. This suggests past minor mergers or interactions influence the quantity and/or velocity dispersion of halo gas.

12. UNM 29-Oct04 3C.336 Field Absorbers & Non-Absorbers

13. UNM 29-Oct04 Absorbers vs. Non-Absorbers within 25΄΄ Possible techniques for finding absorbers in a galaxy rich field. We will obtain photo-z this summer.

14. UNM 29-Oct04 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. Some indication that absorbers and non-absorbers may differ in their luminosity weighted morphological perturbations. Incorporate C IV and other ionization species into the analysis. Obtain redshifts of remaining candidates in order to increase sample size to over 50. Obtain rotation curves of the galaxy using Gemini and Keck. Obtain photometric redshifts of all HST fields to 200+kpc and fixed limiting absolute magnitude. Conclusions … Future …

15. UNM 29-Oct04 Forbidden GasLagging Halo Ellison et al. (2003) Swaters et al. (1997) Schaap et al. (2000) Sancisi et al. (2001) Fraternali et al. (2002) CAUTIONARY TAIL: A counter example!! MC 1331+170; z abs =0.7446; Edge on spiral that does not align with disk kinematics! Because of the symmetric velocity splittings, this has been interpreted as superbubbles (Bond+ 2001; Ellison+ 2003).

16. UNM 29-Oct04 Observed spectra contain an admixture of both models Asymmetric Blended Line Morphology Symmetric Resolved Line Morphology

17. UNM 29-Oct04 Swaters et al. (1997) Halo gas appears to rotate 25 to 100 km s -1 more slowly than the gas in the plane. Disk gas Halo gas D = 9.5 Mpc Neutral hydrogen map from WSRT Presence of an H I halo extending up to at least 5 kpc from the plane 21-cm Mapping of Rotations Curves in Lower Halos…