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A major fraction of star formation in the universe occurs in starbursts. These regions of particularly rapid star formation are often located towards the centers of host galaxies. Studies of this kind of star formation at high redshift have produced astonishing results over recent years that were only possible with the latest generation of large ground-based and space telescopes. The papers collected in this volume present these results in the context of the much firmer foundation of star formation in the local universe, and they emphasize all the important topics, from star formation in different environments to the cosmic star formation history.
Using information and scale as central themes, this comprehensive survey explains how to handle real problems in astronomical data analysis through a modern arsenal of powerful techniques. The coverage includes chapters or appendices on: detection and filtering; image compression; multichannel, multiscale, and catalog data analytical methods; wavelets transforms, Picard iteration, and software tools.
Studying massive star formation is hard, both observationally and theoretically. Many basic questions concerning the formation and early evolution of massive stars remain unclear. Based on a series of spectral lines and mapping surveys on a large sample of massive star-forming cores, we have been able to study the dynamics and physical properties of massive star-forming regions. The HCN 3-2 survey has revealed a large fraction of line asymmetry that indicates the global existence of infall in massive cores. Using the spectra and maps of multiple HCN and CS transitions, as well as of their isotopes, we have started to model the massive star-forming cores with a 1D Monte Carlo simulation. The surveys of dense gas tracers in Galactic cores revealed a linear correlation between the star formation rate, as indicated by the infrared luminosity, and the amount of the dense gas, as traced by the line luminosity of dense gas tracer like HCN 1-0. The linear LIR-L' HCN1-0 correlation was found to extend over 8 orders of magnitude, from distant starburst and normal galaxies to Galactic massive cores, with a lower cutoff in luminosity. It suggests that star formation may follow a simple relationship when the appropriate tracers are used, and we may understand distant star formation in terms of the known properties of local star-forming regions. To explain this linear correlation, we propose the existence of a basic unit for the clustered star formation in galaxies, with the basic units similar to the massive dense cores studied in the Galaxy.
Theideatocelebrate50yearsoftheSalpeterIMFoccurredduringtherecent IAU General Assembly in Sydney, Australia. Indeed, it was from Australia that in July 1954 Ed Salpeter submitted his famous paper "The Luminosity Function and Stellar Evolution" with the rst derivation of the empirical stellar IMF. This contribution was to become one of the most famous astrophysics papers of the last 50 years. Here, Ed Salpeter introduced the terms "original mass function" and "original luminosity function", and estimated the pro- bility for the creation of stars of given mass at a particular time, now known as the "Salpeter Initial Mass Function", or IMF. The paper was written at the Australian National University in Canberra on leave of absence from Cornell University (USA) and was published in 1955 as 7 page note in the Astroph- ical Journal Vol. 121, page 161. To celabrate the 50th anniversary of the IMF, along with Ed Salpeter’s 80th birthday, we have organized a special meeting that brought together scientists involved in the empirical determination of this fundamental quantity in a va- ety of astrophysical contexts and other scientists fascinated by the deep imp- cations of the IMF on star formation theories, on the physical conditions of the gas before and after star formation, and on galactic evolution and cosmology. The meeting took place in one of the most beautiful spots of the Tuscan countryside, far from the noise and haste of everyday life.
The most massive stars in the galaxy - those with more than 15 to 20 solar masses - are lilkely to ionize their surroundings before they reach their final mass. How can they accrete in spite of the presence of over-pressurized gas? This thesis presents results of Submillimeter Array (SMA) and Very Large Array (VLA) studies of massive star formation regions in the early stages of ionization, as well as an analysis of numerical simulations of the evolution of these young HII regions. The results favor a picture in which very massive stars form in accretion flows that are partially ionized and that keep accreting material from their environment.