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• Ram pressure stripping octopus code#

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 This effectively halts star formation in the galaxy, supporting the belief that ram pressure stripping could be one of the processes responsible for the morphology density relation. The result of ram pressure stripping is a galaxy which contains very little cold gas. This has revealed bright blue stars along the leading edge of the galaxy (bottom of the galaxy in the image). At the same time, the ‘wind’ has pushed the dust and gas that would normally be found ahead of the motion of the galaxy up into the galaxy itself. Streamers of dust and gas can be seen trailing behind the motion of the galaxy, obscuring and reddening the stars behind (top of the galaxy in the image).This observation suggests that the loosely bound dust and gas in the outer regions of the disk has been stripped from the galaxy after the formation of these stars. The stellar disk (blue) appears to extend well beyond the star forming disk of dust and gas.This indicates that the galaxy is having trouble holding onto the loosely bound dust and gas in the outer regions of the disk against the pressure of the ‘wind’. The disk of dust and gas appears bowed.For example, NGC 4402 (right), which is currently falling into the Virgo cluster, shows several clear indicators that ram pressure stripping is at work: ‘Ram pressure stripping’ occurs if this wind is strong enough to overcome the gravitational potential of the galaxy to remove the gas contained within it.Įvidence for ram pressure stripping can be found in many galaxy clusters. As individual galaxies move within such clusters, they experience this intra-cluster gas as a ‘wind’ – much like the wind experienced by a moving bicyclist, even on a still day.

Galaxy clusters are permeated by hot, X-ray emitting gas known as the intra-cluster medium.

Crowl (Yale University) and WIYN/NOAO/AURA/NSF The bowed and truncated disk, and the concentration of dust and gas to one side of the galaxy are all indicators that ram pressure stripping is forcing gas out of the galaxy. The spiral galaxy, NGC4402, is currently falling towards the centre of the Virgo cluster (downwards in this image).