(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). RPS relation works reasonably well in a broad sense when RPS is the mostĭominant process and the galaxy is located where the surrounding environmentĬan be well defined.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. Signs of environmental impacts other than RPS such as tidal interaction or Hand, galaxies likely in the early or later RPS stage and/or the ones with Predictions and observations within a measurement uncertainty. Observation with the predicted gas truncation radii for the given conditions.įor the sample undergoing active RPS, we generally find good agreements between Of Virgo cluster galaxies in different stages of RPS measured from the HI In order to verify how well the observed signatures of the RPS processĬan be understood as simple momentum transfer, we compare the stripping radii Such as compression and geometrical self-shielding as well as cooling and Stripping process can be more complicated due to the complexity of gas physics (ISM) by the gravitational potential of a galaxy. Intracluster medium (ICM) and the anchoring pressure on the interstellar medium The RPS process isĬommonly described as a competition between the ram pressure by the #RAM PRESSURE STRIPING PDF#Authors: Seona Lee, Yun-Kyeong Sheen, Hyein Yoon, Yara Jaffé, Aeree Chung Download PDF Abstract: Ram pressure stripping (RPS) is known to be a key environmental effect thatĬan remove interstellar gas from galaxies in a cluster.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |