Mathematics – Logic
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.8401k&link_type=abstract
American Astronomical Society, AAS Meeting #211, #84.01; Bulletin of the American Astronomical Society, Vol. 39, p.875
Mathematics
Logic
Scientific paper
Our research is focused on understanding the formation and evolution of galaxies via their extended gaseous halos using the methods of quasar absorption line systems. Galaxy-absorber pairs provide direct observational constraints on competing scenarios aimed at establishing the role of gas in galaxy formation and evolution. Our sample consists of 37 intermediate redshift galaxy-absorber pairs, which have been imaged with HST. The absorption line data are VLT/UVES and Keck/HIRES high resolution quasar spectra. Rotation curves are measured from Keck/ESI spectra for a subset of 10 galaxies.
We present new results on the kinematics and morphological connections between MgII absorption selected galaxies and their halo gas. We also analyze mock quasar absorption line observations of galaxies and their gaseous halos in ΛCDM cosmological simulations in order constrain the dynamic interaction of the galaxy/halo/cosmic web environment and the distribution of gas within halos. We find previous results suggesting spherical halos with a uniform distribution of gas are not consistent with our data nor with the simulations. Statistically, gaseous halos have sizes of 43-88 kpc with a gas covering fraction of around 60%. Previous observational results from six edge-on galaxies suggest that halo gas velocities are consistent with extended disk-like rotation at galactocentric distances of 25-72 kpc. We demonstrate that the gas velocities are by and large not consistent with being kinematically coupled to the galaxy over galactocentric distances of 25-105 kpc. Our sample contains two pairs of interacting galaxies and, in one case, the gas velocities are both retrograde to the disk rotations and the angular momentum of the galaxies.
The simulations and our new observations support the picture in which gaseous halos are chemically enriched by outflowing shock-heated supernovae winds while low metallicity gas inflowing along filaments produces an inhomogeneous temperature, velocity and metallicity distributions with a non-unity gas covering fraction.
Churchill Christopher W.
Kacprzak Glenn G.
Klypin Anatoly
Murphy Michael T.
Rodriguez David
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