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      Ring Galaxies Through Off-Center Minor Collisions by Tuning Bulge-to-Disk Mass Ratio of Progenitors

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          Abstract

          Collisional ring galaxies (CRGs) are formed through off-center collisions between a target galaxy and an intruder dwarf galaxy. We study the mass distribution and kinematics of the CRGs by tuning the bulge-to-disk mass ratio (\(B/D\)) for the progenitor, i.e., the target galaxy. We find that the lifetime of the ring correlates with the initial impact velocity vertical to the disk plane (i.e., \(v_{\rm z0}\)). Three orbits for the collisional galaxy pair, on which clear and asymmetric rings form after collisions, are selected to perform the N-body simulations at different values of \(B/D\) for the progenitor. It is found that, the ring structures are the strongest for the CRGs with small values of \(B/D\). The S\'{e}rsic index, \(n\), of the central remnant in the target galaxy becomes larger after collision. Moreover, the S\'{e}rsic index of a central remnant strongly correlates with the initial value of \(B/D\) for the progenitor. A bulge-less progenitor results in a late-type object in the center of the ring galaxy, whereas a bulge-dominated progenitor leads to an early-type central remnant. Progenitors with \(B/D\in [0.1,~0.3]\), i.e., minor bulges, leave central remnants with \(n\approx 4\). These results provide a possible explanation for the formation of a recently observed CRG with an early-type central nucleus, SDSS J1634+2049. In addition, we find that the radial and azimuthal velocity profiles for a ring galaxy are more sensitive to the \(B/D\) than the initial relative velocity of the progenitor.

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          On a Cluster of Nebulae in Hydra

          F Zwicky (1941)
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            Numerical experiments in spiral structure

            Results of an n -body calculation, containing about 120000 particles, were shown as a motion picture. Some of the particles are treated as ‘gas’, obeying a special dissipative dynamics, the rest as ‘stars’. The system was started as pure ‘gas’, and ‘stars’ were made out of the ‘gas’ in a manner closely mimicking real galaxies. Spiral density wave patterns appear in the ‘gas’, and last for about 3 ‘galactic rotations’ without substantial change of form. Various experiments are described that have been undertaken in an attempt to learn the roles of various parts of the system in the maintenance of spiral patterns.
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              Author and article information

              Journal
              17 July 2018
              Article
              1807.06598
              c76d84cf-9cdf-4556-8c2f-d1660dc7da02

              http://arxiv.org/licenses/nonexclusive-distrib/1.0/

              History
              Custom metadata
              21 pages, 17 figures, accepted for publication in ApJ
              astro-ph.GA

              Galaxy astrophysics
              Galaxy astrophysics

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