Lessons on galactic nuclear activity from voids.
Anca Constantin (Harvard-Smithsonian CfA)
Galaxies in the most underdense regions of the universe, the voids, must have different evolutionary histories than those in denser regions, the walls,. This is mainly because of the expected huge difference in their rate of interactions, which is believed to affect the nuclear activity, and thus the growth process. It is thus important to determine the degree to which the void galactic nuclear activity compares to its counterpart in denser environments. I will present a comparison of void and wall systems based on a variety of physical properties and near neighbor statistics, together with spatial clustering calculations, which provides empirical evidence that both small and large scale environment influence the interplay between AGN and nuclear stellar activity, and thus the optically dominant power source. I will present these ideas in the context of a potential H II -> Seyfert/Transition Object -> LINER evolutionary sequence, and show support for this scenario with new Chandra X-ray measurements.
contact: J. Rigby
Anca Constantin (Harvard-Smithsonian CfA)
Galaxies in the most underdense regions of the universe, the voids, must have different evolutionary histories than those in denser regions, the walls,. This is mainly because of the expected huge difference in their rate of interactions, which is believed to affect the nuclear activity, and thus the growth process. It is thus important to determine the degree to which the void galactic nuclear activity compares to its counterpart in denser environments. I will present a comparison of void and wall systems based on a variety of physical properties and near neighbor statistics, together with spatial clustering calculations, which provides empirical evidence that both small and large scale environment influence the interplay between AGN and nuclear stellar activity, and thus the optically dominant power source. I will present these ideas in the context of a potential H II -> Seyfert/Transition Object -> LINER evolutionary sequence, and show support for this scenario with new Chandra X-ray measurements.
contact: J. Rigby