Simulations of Galaxy Formation in a Lambda CDM Universe II: The Fine Structure of Simulated Galactic Disks

Abstract

We present a detailed analysis of the dynamical properties of a simulated disk galaxy assembled hierarchically in the Lambda CDM cosmogony. At z=0, two distinct dynamical components are identified on the basis of the orbital parameters of stars in the galaxy: a slowly rotating, centrally concentrated spheroid and a disk-like component largely supported by rotation. These components are also recognized in the surface brightness profile of the galaxy, which can be very well approximated by the superposition of an R^{1/4} spheroid and an exponential disk. However, neither does the dynamically-identified spheroid follow de Vaucouleurs' law nor is the disk purely exponential, a resultwhich calls for caution when estimating the importance of the disk from traditional photometric decomposition techniques. The disk may be further decomposed into a thin, dynamically cold component with stars on nearly circularorbits and a hotter, thicker component with orbital parameters transitional between the thin disk and the spheroid. The spheroid is old, and has essentiallyno stars younger than the time elapsed since the last major accretion event ~8 Gyr ago. The majority of thin disk stars, form after the merging activity is over, although a significant fraction ~15% of thin-disk stars are old enough to predate the last major merger event. This unexpected population of old disk stars consists mainly of the tidal debris of satellites whose orbital plane was coincident with the disk and whose orbits were circularized by dynamical friction prior to full disruption. Our results highlight the role of satellite accretion events in shaping the disk and the spheroidal component and reveal some of the clues to the assembly process of a galaxy preserved in the detailed dynamics of old stellar populations.