Strangulation in galaxy groups.
ASTROPHYS J LETT
L103 - L106.
We use a cosmological chemodynamical simulation to study how the group environment impacts the star formation ( SF) properties of disk galaxies. The simulated group has a total mass of M similar to 8 x 10(12) M-circle dot and a total X-ray, luminosity of L-x similar to 10(41) erg s(-1). Our simulation suggests that ram pressure is not sufficient in this group to remove the cold disk gas from a V-rot similar to 150 km s galaxy. However, the majority of the hot gas in the galaxy is stripped over a timescale of approximately 1 Gyr. Since the cooling of the hot-gas component provides a source for new cold gas, the stripping of the hot component effectively cuts off the supply of cold gas. This in turn leads to a quenching of SF. The galaxy maintains the disk component after the cold gas is consumed, which may lead to a galaxy similar to an S0. Our self-consistent simulation suggests that this strangulation mechanism works even in low-mass groups, providing an explanation for the lower SF rates in group galaxies relative to galaxies in the field.
|Title:||Strangulation in galaxy groups|
|Keywords:||galaxies : evolution, galaxies : kinematics and dynamics, galaxies : stellar content, methods : numerical, DIGITAL SKY SURVEY, RAM-PRESSURE, STAR-FORMATION, DISK GALAXIES, S0 GALAXIES, COSMOLOGICAL SIMULATIONS, STATISTICAL PROPERTIES, INTRACLUSTER MEDIUM, ELLIPTIC GALAXIES, CLUSTER GALAXIES|
|UCL classification:||UCL > School of BEAMS
UCL > School of BEAMS > Faculty of Maths and Physical Sciences
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