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Seminarium im. Bohdana Paczyńskiego

The lecture by Jeremiah P. Ostriker will be held on May 19th 2014, at 3 pm in the lecture hall of the Nicolaus Copernicus Astronomical Center, Warsaw, ul. Bartycka 18.

 

"On the formation of massive galaxies"

 Jeremiah P. Ostriker (Dept. of Astrophysical  Sciences,  Princeton University)

 

Abstract: Looking backwards we have been able to reconstruct from the detailed structure of our own Galaxy and from the fossil evidence derived from the study of nearby galaxies a plausible history of how galaxies formed over the last several billion years. In addition, now that we have a quite definite cosmological model, providing us with a quantitative picture of how perturbations grew from very low amplitude Gaussian fluctuations, we can perform the forward modeling of representative pieces of the universe using standard physical processes to see how well we match our local knowledge and the time-reversed modeling based on the fossil evidence. Finally, we can employ large ground and space based telescopes to use the universe as a time-machine – directly observing the past history of our light-cone.  While none of these approaches can give us at the present time results accurate to more than roughly the 5% -> 10% level, a coherent and plausible picture is emerging.  Massive galaxies form in two phases. In the first phase, which peaks at redshift z = 6 and ends by redshift z = 2, cold gas streams in, making stars in a small (<1kpc) region, but as the stellar mass approaches 1011 Msolar, a hot bubble forms which suppresses further inflow of cold gas. But from redshift z = 3 to the present time, small stellar satellite systems are accreted at typically 10kpc from the center and the size of the total system grows by about a factor of three as the mass doubles. Energy release from gravitational infall in various forms will greatly reduce star-formation even in the absence of feedback from SN or MBHs. And, output from massive black holes at the centers of these systems significantly helps to terminate or “quench” star formation. This physical picture seems naturally to lead to the mass, size, scale and epoch of galaxy formation and, increasingly, to a first understanding of the detailed internal structure of these systems.

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