#RAM PRESSURE STRIPPING OCTOPUS FULL#
#RAM PRESSURE STRIPPING OCTOPUS CODE#
#RAM PRESSURE STRIPPING OCTOPUS FREE#

It hence is plausible that the evolution of a galaxy strongly depends on the strength of ram pressure (RP) it experiences. Furthermore, starvation cannot modify the colours of galaxies on sufficiently short timescales, unlike RPS ( Boselli et al. 2009) observed in many systems, which cannot be easily reproduced by pure “starvation” scenarios (the removal of the extended gas reservoir that refuels the disk with gas available for star formation (SF) e.g. Indirect evidence for RPS in action are asymmetries and truncated radial density profiles (e.g.

Gunn & Gott 1972), the removal and possible compression of parts of the gas disk due to interaction with the intracluster medium (ICM), remains one of the main candidates responsible for environmental quenching of disk galaxies. Since the density of the environment seems to play an important role, and the merger cross section is small in galaxy clusters owing to the high relative velocity dispersion, classic ram-pressure stripping (RPS, e.g. However, the question of the physical mechanisms behind quenching still persists, and especially the environmental dependence, which also gives rise to phenomena such as “galaxy conformity” ( Weinmann et al. Galaxy surveys have shown that the quenching of disk galaxies mainly depends on their mass and environment ( Peng et al. Key words: galaxies: evolution / galaxies: clusters: general / methods: numerical / galaxies: interactions / galaxies: star formation

#RAM PRESSURE STRIPPING OCTOPUS FREE#

Stripped gas in the wake is mixed efficiently with intracluster gas already a few tens of kpc behind the disk, and this gas is free of residual star formation. On the other hand, galaxies experiencing only mild ram pressure actually show an enhanced star formation rate that is consistent with observations. Depending on the inclination angle, this can light up a galaxy for a few hundred Myrs until all of the gas is stripped or consumed and star formation drops to almost zero, suggesting a typical quenching timescale of ~200 Myr.

#RAM PRESSURE STRIPPING OCTOPUS FULL#

The cold gas disk is only stripped completely in extreme cases, leading to full quenching and significant reddening on a very short timescale. Star formation in our model galaxies is quenched mainly because the hot gas halo is stripped, depriving the galaxy of its gas supply. As long as the disk is not completely stripped in peaks of RPS during pericentre passage, some gas that remains bound to the galaxies is redistributed to the outer parts of disks as soon as the ram pressure becomes weaker again, an effect that is not captured in simplified treatements of RPS. In most cases, the actual stripping radius of the simulated disk galaxies is larger than assumed in the SAMs, corresponding to an over prediction of the mass loss in SAMs. We find that the stripping models employed in current SAMs often differ substantially from our direct simulations.

#RAM PRESSURE STRIPPING OCTOPUS CODE#

Stellar light maps and the evolution of galaxy colours are computed with the stellar synthesis code FSPS to draw conclusions about quenching timescales of our model galaxies. Cooling, star formation, and stellar feedback are included according to a simple sub-resolution model. We use the moving-mesh code AREPO, augmented with a special refinement strategy to yield high resolution around the galaxy on its way through the cluster in a computationally efficient way. Our set-up employs a live model of a galaxy cluster that interacts with infalling disk galaxies on different orbits. We also analyse the gaseous wake of the galaxy, focusing on gas mixing and metal enrichment of the intracluster medium (ICM). In particular, we compare our findings for the mass loss and evolution of the star formation rate in our simulations with prescriptions commonly employed in SAMs. In this work, we use hydrodynamical simulations to investigate the quenching of disk galaxies through ram-pressure stripping (RPS) as they fall into galaxy clusters with the goal of characterising the importance of this effect for the reddening of disk galaxies. The exact cause of the environmental dependence is still poorly understood, yet semi-analytic models (SAMs) of galaxy formation need to parameterise it to reproduce observations of galaxy properties.Īims. Observationally, the quenching of star-forming galaxies appears to depend both on their mass and environment. Zentrum für Astronomie der Universität Heidelberg,Īstronomisches Recheninstitut, Mönchhofstr.Ĭontext. Technikerstrasse Institut für Theoretische Studien, Institut für Astro- und Teilchenphysik Universität Innsbruck,

Astronomical objects: linking to databasesĭominik Steinhauser 1, Sabine Schindler 1 and Volker Springel 2 ,3.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes

Ram pressure stripping octopus