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Full-Text Articles in Physical Sciences and Mathematics
The Aimss Project – Iii. The Stellar Populations Of Compact Stellar Systems, Joachim Janz, Mark Norris, Duncan Forbes, Avon Huxor, Aaron Romanowsky, Matthias Frank, Carlos Escudero, Favio Faifer, Juan Forte, Sheila Kannappan, Claudia Maraston, Jean Brodie, Jay Strader, Bradley Thompson
The Aimss Project – Iii. The Stellar Populations Of Compact Stellar Systems, Joachim Janz, Mark Norris, Duncan Forbes, Avon Huxor, Aaron Romanowsky, Matthias Frank, Carlos Escudero, Favio Faifer, Juan Forte, Sheila Kannappan, Claudia Maraston, Jean Brodie, Jay Strader, Bradley Thompson
Faculty Publications
In recent years, a growing zoo of compact stellar systems (CSSs) have been found whose physical properties (mass, size, velocity dispersion) place them between classical globular clusters (GCs) and true galaxies, leading to debates about their nature. Here we present results using a so far underutilized discriminant, their stellar population properties. Based on new spectroscopy from 8–10m telescopes, we derive ages, metallicities, and [α/Fe] of 29 CSSs. These range from GCs with sizes of merely a few parsec to compact ellipticals (cEs) larger than M32. Together with a literature compilation, this provides a panoramic view of the stellar population characteristics …
Stellar Populations Across The Black Hole Mass–Velocity Dispersion Relation, Ignacio Martín-Navarro, Jean Brodie, Remco Van Den Bosch, Aaron Romanowsky, Duncan Forbes
Stellar Populations Across The Black Hole Mass–Velocity Dispersion Relation, Ignacio Martín-Navarro, Jean Brodie, Remco Van Den Bosch, Aaron Romanowsky, Duncan Forbes
Faculty Publications
Coevolution between supermassive black holes (BH) and their host galaxies is universally adopted in models for galaxy formation. In the absence of feedback from active galactic nuclei (AGNs), simulated massive galaxies keep forming stars in the local universe. From an observational point of view, however, such coevolution remains unclear. We present a stellar population analysis of galaxies with direct BH mass measurements and the BH mass–σ relation as a working framework. We find that over-massive BH galaxies, i.e., galaxies lying above the best-fitting BH mass–σ line, tend to be older and more α-element-enhanced than under-massive BH galaxies. The scatter in …