The Formation and Evolution of High-Redshift Submillimeter Galaxies
Desika Narayanan (CfA)
Submillimeter galaxies at z~2 are the most luminous, heavily star-forming galaxies in the Universe. While observers have been rapidly amassing clues regarding this enigmatic population, the mere existence of these galaxies has remained a sticking point for theoretical models. In explaining their observed properties, theorists have required varied physical deviancies from local Universe phenomena. I will argue that extraordinary physics is unnecessary to explain this population. In this talk, I will present a merger-driven model that describes the formation and evolution of SMGs which accurately reproduces the observed UV-mm wave SED, the inferred physical properties of the population, and the observed number counts. This model provides a natural connection between SMGs, 24 micron sources, and BzK galaxies, thus providing some synthesis to the zoo of galaxies being detected at high-z. Finally, I will describe model distinguishing tests which will be feasible with the next generation of telescopes (Herschel, JWST and ALMA).
Contact: Juna Kollmeier
Desika Narayanan (CfA)
Submillimeter galaxies at z~2 are the most luminous, heavily star-forming galaxies in the Universe. While observers have been rapidly amassing clues regarding this enigmatic population, the mere existence of these galaxies has remained a sticking point for theoretical models. In explaining their observed properties, theorists have required varied physical deviancies from local Universe phenomena. I will argue that extraordinary physics is unnecessary to explain this population. In this talk, I will present a merger-driven model that describes the formation and evolution of SMGs which accurately reproduces the observed UV-mm wave SED, the inferred physical properties of the population, and the observed number counts. This model provides a natural connection between SMGs, 24 micron sources, and BzK galaxies, thus providing some synthesis to the zoo of galaxies being detected at high-z. Finally, I will describe model distinguishing tests which will be feasible with the next generation of telescopes (Herschel, JWST and ALMA).
Contact: Juna Kollmeier