Theyconclude that the amount of gas suppression cannot bebecause of a slow process like starvation or strangulation(Larson, Tinsley & Caldwell 1980) and a fast process likeram pressure stripping is needed to explain the observation.Recently Treyer et al. They observe that gas suppression in ahigh-density environment begins at the group level. (2017) per-formed a multi-wavelength study taking data from SloanDigital Sky-Survey (SDSS) and Arecibo Legacy Fast ALFA(ALFALFA) survey. 2011), a phenomenonknown as ’galactic conformity’. Interestingly one finds apositive correlation between the star formation of the centralgalaxy and its satellite for the regions extending far beyondvirial radius (Weinmann, van den Bosch, Yang & Mo 2006 Ann, Park & Choi 2008 Guo et al. An undisturbed optical disc with anextraplanar gas component in these galaxies indicates in-teraction of galaxy with the ICM. Kenney, Crowl, van Gorkom & Vollmer (2004) ob-serve IC3392, NGC4402, NGC4388 and NGC4419 to have © Singh, Gulati and Bagla a truncated HI disc. 2003 Goto, Stecklum, Linz, Feldt, Henning, Pascucci & Usuda2006 Verdugo, Ziegler & Gerken2008 Park & Hwang 2009 von der Linden, Wild, Kauffmann, White & Weinmann ⋆ E-Mail: † E-Mail: ‡ E-Mail: α and HI, but the stellar disc is undis-turbed. Thiscondition, on putting numbers for spirals galaxies, led themto conclude that a spiral galaxy should lose its gas disc whilepassing through the centre of a cluster.It is observed (G´omez, et al. (1)Here, the right-hand side is a gravitational restoring pres-sure with Σ s being the surface density of stars and Σ g isthe surface density of the gas, the density of ICM is ρ ICM ,and the in-fall velocity of the galaxy is given by V in.
Key words: galaxies: clusters: intracluster medium πG Σ s Σ g. Lastly, we discussimplications for star formation in galaxies as these fall into halos. We commenton the limitations of our model and situations where a significant amount of gas maybe retained in galaxy disc and also give an illustration for the same. Galaxies in cluster halos get stripped of gas more efficientlyas compared to group and galaxy halos: this is due to the higher infall speed and ahigher density of gas in the ICM due to a greater retention of baryons. We find that gasdiscs in galaxies with a higher spin parameter get stripped sooner than galaxies witha smaller spin parameter. We showthat there is little variation in the worst case scenario with redshift. In each case wemodel the worst case scenario (i.e., maximum effect due to ram pressure). We also study variations with galaxy properties and redshift. We use an analytical approach to study ram pressure stripping with simple models fordiscs and halo gas distribution to study the phenomena in cluster, group and galaxyhalos. Bagla ‡ Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, Sahibzada Ajit Singh Nagar, Punjab 140306, India School of Mathematics, Thapar Institute of Engineering and Technology, Patiala, Punjab 147004, India
Ram pressure stripping: An analytical approachĪnkit Singh ⋆, Mamta Gulati † and Jasjeet S. Lastly, we discuss implications for star formation in galaxies as these fall into halos.Īa r X i v. We comment on the limitations of our model and situations where a signiffcant amount of gas may be retained in galaxy disc and also give an illustration for the same. Galaxies in cluster halos get stripped of gas more effciently as compared to group and galaxy halos: this is due to the higher infall speed and a higher density of gas in the ICM due to a greater retention of baryons. We find that gas discs in galaxies with a higher spin parameter get stripped sooner than galaxies with a smaller spin parameter. We show that there is little variation in the worst case scenario with redshift. In each case we model the worst case scenario (i.e., maximum effect due to ram pressure). We use an analytical approach to study ram pressure stripping with simple models for discs and halo gas distribution to study the phenomena in cluster, group and galaxy halos.
0 kommentar(er)
