'Galaxy density' presentation slideshows

HI Gas as Function of Environment

HI Gas as Function of Environment. When and where do galaxies stop accreting cool gas? How do they loose the cool gas? When do they stop forming stars?. Jen Donovan poster. The lore.. if halos get too big, gas does not cool But.. at least some dry mergers are wet, and forming stars

462 views • 35 slides

Observations of the evolution of HI in galaxies across different environments.

Observations of the evolution of HI in galaxies across different environments. D.J. Pisano (West Virginia University). Why study galaxy environment?. Nature vs. Nurture Can they be distinguished? What does the environment do to a galaxy?

422 views • 32 slides

H OPCAT , 6dFGS & Star Formation Rates

317 views • 20 slides

H OPCAT , 6dFGS & Star Formation Rates

327 views • 20 slides

H OPCAT , 6dFGS & Star Formation Rates

207 views • 20 slides

H OPCAT , 6dF & Star Formation Rates

279 views • 17 slides

H OPCAT , 6dF & Star Formation Rates

295 views • 17 slides

Star Formation & the Morphology-Density Relation in the Local Universe

291 views • 15 slides

Robust identification of distant Compton-thick AGNs

1Ms simulated XEUS spectrum. Optical AGN. Robust identification of distant Compton-thick AGNs. IR AGN. Alexander et al. (2008). Need for deep optical-mid-IR spectroscopy: multiple lines of evidence for intrinsic AGN luminosity can make a case for distant Compton-thick absorption. X-rays.

334 views • 15 slides

Robust identification of distant Compton-thick AGNs

1Ms simulated XEUS spectrum. Optical AGN. Robust identification of distant Compton-thick AGNs. IR AGN. Alexander et al. (2008). Need for deep optical-mid-IR spectroscopy: multiple lines of evidence for intrinsic AGN luminosity can make a case for distant Compton-thick absorption. X-rays.

151 views • 15 slides

Star Formation Efficiency and Environment

58 views • 1 slides