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Ram pressure stripping octopus5/6/2023 ![]() ![]() Differences in the efficiency of ram pressure stripping in groups versus clusters likely contribute to the positive trend between the quenched fraction and host halo mass observed in the local Universe. On the whole, there is clear evidence for ongoing ram pressure stripping in galaxy groups (down to very low group masses), though the frequency of jellyfish galaxies and the strength of ram pressure stripping appear lower in groups than in clusters. Finally, we find that the star formation rates of jellyfish galaxies in groups are consistent with ‘normal’ star-forming group galaxies, which is in contrast to cluster jellyfish galaxies that have clearly enhanced star formation rates. Both the orientation of observed radio continuum tails and the positions of group jellyfish galaxies in phase space suggest that galaxies are stripped more slowly in groups relative to clusters. We find that jellyfish galaxies are most commonly found in clusters, with the frequency decreasing towards the lowest-mass groups. We compare the group jellyfish galaxies identified in this work with the LoTSS jellyfish galaxies in clusters presented in a recent work, allowing us to compare the effects of ram pressure stripping across three decades in group and cluster mass. We identify 60 jellyfish galaxies in groups with extended, asymmetric radio continuum tails, which are found across the entire range of group mass from 10 12.5 < M group < 10 14 h −1 M ⊙. In this work we use the LOFAR Two-metre Sky Survey (LoTSS) to search for jellyfish galaxies (i.e., galaxies with ram pressure stripped tails extending beyond the optical disk) in ∼500 SDSS groups ( z < 0.05), making this the most comprehensive search for ram pressure stripping in groups to date. Numerous examples of ram pressure stripping in galaxy clusters are present in literature however, substantially less work has been focused on ram pressure stripping in lower-mass groups, the most common galaxy environment in the local Universe. Ram pressure stripping is a frequently cited mechanism for quenching galaxy star formation in dense environments. INAF – Osservatorio astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The NetherlandsĮ-mail: of Birmingham School of Physics and Astronomy, Edgbaston, Birmingham, UK Astronomical objects: linking to databases.Including author names using non-Roman alphabets.As galaxies fall toward the center of a cluster, more and more of their gas is stripped out, including the cool, denser gas that is the source of continued star formation. ![]() 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. Suggested resources for more tips on language editing in the sciences Ram pressure stripping is thought to have profound effects on the evolution of galaxies. The result of ram pressure stripping is a galaxy which contains very little cold gas. Punctuation and style concerns regarding equations, figures, tables, and footnotes By comparing simulations with the observed sample, we find that a combination of face-on and edge-on 'unwinding' effects is likely to be occurring in our galaxies as they experience stripping with different inclinations with respect to the ICM. The pattern is fairly short-lived (<0.5 Gyr) in the stripping process, occurring during first infall and eventually washed out by the ICM wind into the tail of the jellyfish galaxy. In face-on cases, gas removed from the outer edges falls to higher orbits, appearing to 'unwind'. We compare the morphology and kinematics with simulated ram-pressure stripping galaxies, taking into account the estimated inclination with respect to the intracluster medium (ICM) and find that in edge-on stripping, unwinding can occur due to differential ram pressure caused by the disc rotation, causing stripped material to slow and 'pile up'. We find only younger stars in the unwound component, while older stars in the disc remain undisturbed. We first confirm the unwinding nature, finding that the spiral arm pitch angle increases radially in 10 stripped galaxies and also simulated face-on and edge-on stripped galaxies. Gravitational influence from neighbours is ruled out and we compare the sample with a control group of undisturbed spiral galaxies and simulated stripped galaxies. For dwarf galaxies (DGs) within a cluster, the transformation from gaseous to gas-poor systems by RPS is not easily observed and must happen in the outskirts of clusters. We study 11 ram-pressure stripped galaxies from GASP (GAs Stripping Phenomena in galaxies) in which, in addition to more commonly observed 'jellyfish' features, dislodged material also appears to retain the original structure of the spiral arms. Ram-pressure stripping (RPS) is a well observed phenomenon of massive spiral galaxies passing through the hot intra-cluster medium (ICM) of galaxy clusters. We present the first study of the effect of ram pressure 'unwinding' the spiral arms of cluster galaxies. ![]()
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