![]() ![]() arXiv:astro-ph/0004078īalogh ML, McGee SL, Mok A, Wilman DJ, Finoguenov A, Bower RG, Mulchaey JS, Parker LC, Tanaka M (2014) The GEEC2 spectroscopic survey of Galaxy groups at \(0.8 < z < 1\). arXiv:1210.8407īalogh ML, Navarro JF, Morris SL (2000) The origin of star formation gradients in rich galaxy clusters. arXiv:1410.8161īahé YM, McCarthy IG, Balogh ML, Font AS (2013) Why does the environmental influence on group and cluster galaxies extend beyond the virial radius? MNRAS 430:3017–3031. arXiv:2011.05336 īahé YM, McCarthy IG (2015) Star formation quenching in simulated group and cluster galaxies: when, how, and why? MNRAS 447:969–992. arXiv:0909.0948 Īyromlou M, Kauffmann G, Yates RM, Nelson D, White SDM (2021) Galaxy formation with L-GALAXIES: modelling the environmental dependency of galaxy evolution and comparing with observations. ![]() arXiv:1901.05969 Īsplund M, Grevesse N, Sauval AJ, Scott P (2009) The chemical composition of the Sun. arXiv:1205.3095 Īrthur J, Pearce FR, Gray ME, Knebe A, Cui W, Elahi PJ, Power C, Yepes G, Arth A, De Petris M, Dolag K, Garratt-Smithson L, Old LJ, Rasia E, Stevens ARH (2019) THETHREEHUNDRED Project: ram pressure and gas content of haloes and subhaloes in the phase-space plane. arXiv:1708.00508 Īrrigoni Battaia F, Gavazzi G, Fumagalli M, Boselli A, Boissier S, Cortese L, Heinis S, Ferrarese L, Côté P, Mihos JC, Cuillandre JC, Duc PA, Durrell P, Gwyn S, Jordán A, Liu C, Peng E, Mei S (2012) Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS. arXiv:1311.4361 Īrmitage TJ, Barnes DJ, Kay ST, Bahé YM, Dalla Vecchia C, Crain RA, Theuns T (2018) The Cluster-EAGLE project: velocity bias and the velocity dispersion-mass relation of cluster galaxies. arXiv:1506.01703 Īndreon S, Newman AB, Trinchieri G, Raichoor A, Ellis RS, Treu T (2014) JKCS 041: a Coma cluster progenitor at \(z = 1.803\). Īnderson ME, Sunyaev R (2016) Searching for FUV line emission from 10 \(^\) K gas in massive elliptical galaxies and galaxy clusters as a tracer of turbulent velocities. Īndersen V, Owen FN (1995) The far-infrared-radio relation in cluster spiral galaxies. arXiv:1604.01883 Īhad SL, Bahé YM, Hoekstra H, van der Burg RFJ, Muzzin A (2021) The stellar mass function and evolution of the density profile of galaxy clusters from the Hydrangea simulations at \(0 < z< 1.5\). arXiv:1101.4066Ībramson A, Kenney J, Crowl H, Tal T (2016) HST imaging of dust structures and stars in the ram pressure stripped Virgo spirals NGC 4402 and NGC 4522: stripped from the outside in with dense cloud decoupling. arXiv:1401.0023Ībramson A, Kenney JDP, Crowl HH, Chung A, van Gorkom JH, Vollmer B, Schiminovich D (2011) Caught in the act: strong, active ram pressure stripping in Virgo Cluster spiral NGC 4330. arXiv:astro-ph/9903436Ībramson A, Kenney JDP (2014) Hubble Space Telescope imaging of decoupled dust clouds in the ram pressure stripped Virgo spirals NGC 4402 and NGC 4522. ![]() Finally, combining the results of local and high-redshift observations with the prediction of tuned models and simulations, we try to quantify the importance of this process on the evolution of galaxies of different mass, from dwarfs to giants, in various environments and at different epochs.Ībadi MG, Moore B, Bower RG (1999) Ram pressure stripping of spiral galaxies in clusters. We also discuss on the possible fate of the stripped material once removed from the perturbed galaxies and mixed with the ICM, and we try to estimate its contribution to the pollution of the surrounding environment. We summarise the effects of this perturbing process on the baryonic components of galaxies, from the different gas phases (cold atomic and molecular, ionised, hot) to magnetic fields and cosmic rays, and describe their induced effects on the different stellar populations, with a particular attention to its role in the quenching episode generally observed in high-density environments. This review is aimed at describing this physical mechanism in different environments, from rich clusters of galaxies to loose and compact groups. the pressure exerted by the hot and dense intracluster medium (ICM) on galaxies moving at high velocity within the cluster gravitational potential well, is a key process able to remove their interstellar medium (ISM) and quench their activity of star formation. Among these, ram pressure stripping, i.e. Galaxies living in rich environments are suffering different perturbations able to drastically affect their evolution. ![]()
0 Comments
Leave a Reply. |