Detailed kinematics and morphological features in tidally heated disks

Abstract

Abstract. The recent discovery of hidden non-axysimmetric and disk-like structures in bright Virgo dwarf elliptical and lenticular galaxies (dE/dSph/dS0) indicates that they may have latetype progenitors. Using N-body simulations we follow the evolution of disk galaxies within a ΛCDM cluster simulated with 10 7 particles, where the hierarchical growth and galaxy harassment are modeled self-consistently. Most of the galaxies undergo significant morphological transformation, even at the outskirts of the cluster, and move through the Hubble sequence from late type disks to dwarf spheroidals. The time evolution of the simulated galaxies is compared with unsharp-masked images obtained from VLT data and the projected kinematics of our models with the latest high resolution spectroscopic studies from the Keck and Palomar telescopes.

On the accretion of a new group of galaxies on to Virgo: I. Internal kinematics of nine in-falling dEs

“…Lisker et al (2006aLisker et al ( , 2009 reported the existence of two rather faint spiral arms for VCC1896 and a bar aligned with the outer photometric minor axis of this galaxy. Mastropietro et al (2005a) showed that, due to tidal interactions, asymmetric features and open spiral arms can be formed in those dEs which are located in the outskirts of cluster. In addition to that and as shown by Kwak et al (2019), the cluster tidal field can trigger the formation of weak spiral arms in disk dEs.…”

“…The bar in the central region of VCC1896 can either be a pristine structure that formed and developed through standard processes or a tidal feature that formed as a result of interactions with the environment (e.g., see Mastropietro et al 2005a). Tidal interactions are known as one of the most dominant mechanisms that can induce instabilities in the stellar disk of galaxies and form bars, particularly in central regions of galaxy clusters and groups .…”

The no-spin zone: rotation versus dispersion support in observed and simulated dwarf galaxies

“…While tidal stirring simulations have been successful at producing systems with v rot /σ 1 (Mayer et al 2001a(Mayer et al ,b, 2006Klimentowski et al 2009;Mayer 2010;Łokas, Kazantzidis & Mayer 2011;Kazantzidis et al 2011a;Kazantzidis, Łokas & Mayer 2013;Łokas et al 2015;Tomozeiu, Mayer & Quinn 2016), historically it has been difficult to reduce v rot /σ to values < 0.5 found for many observed dwarf satellites (Mastropietro et al 2005). The most complete transformations occur for highly eccentric orbits (Mayer et al 2001a,b), at low inclination, and that are mildly prograde (Kazantzidis et al 2011a;Łokas et al 2015, but see Mayer et al 2006).…”