摘要：ESO 243-49 is a high-mass
(circular velocity vc ≈ 200 km s-1), edge-on S0
galaxy in the Abell 2877 cluster at a distance of
~95 Mpc. To elucidate
the origin of the thick disc of this S0 galaxy, we use Multi Unit Spectroscopic Explorer
(MUSE) science verification data to study its kinematics and stellar populations. The
thick disc emits ~80% of
the light at heights in excess of \hbox{$3\farcs5$} (1.6 kpc). The rotation velocities of its stars lag by
30−40 km s-1
compared to those in the thin disc, which is compatible with the asymmetric drift. The
thick disc is found to be more metal-poor than the thin disc, but both discs have old
ages. We suggest an internal origin for the thick disc stars in high-mass galaxies. We
propose that the thick disc formed either a) first in a turbulent phase with a high star
formation rate and that a thin disc formed shortly afterwards, or b) because of the
dynamical heating of a thin pre-existing component. Either way, the star formation in ESO
243-49 was quenched just a
few Gyr after the galaxy was born and the formation of a thin and a thick disc must have
occurred before the galaxy stopped forming stars. The formation of the discs was so fast
that it could be described as a monolithic collapse where several generations of stars
formed in rapid succession.
关键词：galaxies: individual: ESO243-49;galaxies: kinematics and dynamics;galaxies: structure;galaxies: evolution;galaxies: formation
