English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We study the formation of early-type galaxies (ETGs) through mergers with asample of 70 high-resolution numerical simulations of binary mergers of discgalaxies. These simulations encompass various mass ratios, initial conditionsand orbital parameters. We find that binary mergers of disc galaxies with massratios of 3:1 and 6:1 are nearly always classified as Fast Rotators accordingto the Atlas3D criterion: they preserve the structure of the input fastrotating spiral progenitors. Major disc mergers (mass ratios of 2:1 and 1:1)lead to both Fast and Slow Rotators. Most of the Slow Rotators hold a stellarKinematically Distinct Core (KDC) in their 1-3 central kilo-parsec: these KDCsare built from the stellar components of the progenitors. The mass ratio of theprogenitors is a fundamental parameter for the formation of Slow Rotators inbinary mergers, but it also requires a retrograde spin for the progenitorgalaxies with respect to the orbital angular momentum. The importance of theinitial spin of the progenitors is also investigated in the library of galaxymergers of the GalMer project.

Simulations of binary galaxy mergers and the link with Fast Rotators, Slow Rotators, and Kinematically Distinct Cores