11/27/2022 0 Comments Ram pressure stripping equation![]() ![]() We discuss physical mechanisms across a range of epochs and environments that could explain our results. ![]() By $z$ = 2, only 3.3 Gyr after the big bang, the universe has quenched ∼25 per cent of M⋆ = 1011 M⊙ galaxies and ∼45 per cent of M⋆ = 1012 M⊙ galaxies. At redshifts 1.5 < $z$ < 3.0, the quiescent fraction increases as a function of stellar mass. All three methods give similar values at 1.5 < $z$ < 2.0, however the results differ by up to a factor of 2 at 2.0 < $z$ < 3.0. We derive the quiescent fraction using three methods: specific star formation rate, distance from the main sequence, and UVJ colour–colour selection. We explore the buildup of quiescent galaxies using a sample of 28,469 massive ($M_\star \ge 10^)\ge 11.5$ than previous studies. Finally, we discuss the implications for star formation in galaxies during infall into haloes. We comment on the limitations of our model, and we look at and illustrate a situation where a significant amount of gas may be retained in the galaxy disc. as a result of a greater retention of baryons). Galaxies in cluster haloes are stripped of gas more efficiently compared with group and galaxy haloes, because they have a higher infall speed and a higher density of gas in the intra-cluster medium (i.e. We find that gas discs in galaxies with a higher spin parameter are stripped sooner than galaxies with a smaller spin parameter. We show that the worst-case scenario is not affected greatly by changes in redshift. the maximum effect resulting from ram pressure). In each case, we model the worst-case scenario (i.e. We also study variations in galaxy properties and redshift. We take an analytical approach to study ram pressure stripping, using simple models for discs and the distribution of halo gas to look at this phenomenon in cluster, group and galaxy haloes. ![]()
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