We investigate the mass-to-light ratios of stellar populations as predicted by stellar population synthesis codes and compare those to dynamical/gravitational measurements. In Bell & de Jong (2001) we showed that population synthesis models predict a tight relation between the color and mass-to-light ratio of a stellar population. The normalization of this relation depends critically on the sha...

Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as Ultra Comp...

Dependence of other stellar parameters on mass The Russell–Vogt theorem states that, if we know a star’s mass and its CHEMICAL COMPOSITION, we can use the laws of physics to determine all of its other properties: its luminosity, its radius, its temperature and density profiles, and how these properties change with time. (We know that this is a slight simplification; for instance, the amount of ...

We use published optical spectral and IR excess data from nine young clusters and associations to study the stellar mass dependent dispersal of circumstellar disks. All clusters older than ∼3Myr show a decrease in disk fraction with increasing stellar mass for Solar to higher mass stars. This result is significant at about the 1σ level in each cluster. For the complete set of clusters we reject...

We use a complete and uniform sample of almost half a million galaxies from the Sloan Digital Sky Survey to characterise the distribution of stellar mass in the lowredshift Universe. Galaxy abundances are well determined over almost four orders of magnitude in stellar mass, and are reasonably but not perfectly fit by a Schechter function with characteristic stellar mass m∗ = 6.7× 10 10M⊙ and wi...

Galactic dynamical structures are fossil records of the assembly histories galaxies. By analyzing cosmological hydrodynamical simulation TNG50, we find that a structure call "hot inner stellar halo," defined by stars on dynamically hot orbits with circularity $\lambda_z < 0.5$ at $3.5\,{\rm kpc}<r \lesssim 2\,R_e$, is strong indicator mass accreted satellite We correlation between this halo and...

The current status of both the observational evidence and the theory of the stellar initial mass function (IMF) is reviewed, with particular attention to the two basic, apparently universal features shown by all observations of nearby stellar systems: (1) a characteristic stellar mass of the order of one solar mass, and (2) a power-law decline of the IMF at large masses similar to the original ...

We develop a theoretical framework that combines measurements of galaxy-galaxy lensing, galaxy clustering, and the galaxy stellar mass function in a self-consistent manner. While considerable effort has been invested in exploring each of these probes individually, attempts to combine them are still in their infancy. These combinations have the potential to elucidate the galaxy-dark matter conne...

We present N-body simulations of elliptical galaxy encounters into dry mergers to study the resulting unbound intergalactic stellar population, in particular that of the post-Main Sequence stars. The systems studied are pairs of spherical galaxies without dark halos. The stellar content of the model galaxies is distributed into mass-bins representing lowand intermediate-mass stars (0.85 – 8 M⊙)...