Numerical hydrodynamic simulations based on semi-analytic galaxy merger trees: method and Milky-Way like galaxies

TL;DR

This paper introduces a novel hybrid simulation method combining merger trees and hydrodynamic models to study galaxy evolution, focusing on Milky Way-like galaxies and their merger histories.

Contribution

The paper presents a new integrated approach that combines semi-analytic models with hydrodynamic simulations for efficient, high-resolution galaxy evolution studies.

Findings

Multiple mergers are more common than isolated ones.

Simulations match observed stellar masses and gas properties.

Method reduces computational time significantly.

Abstract

We present a new approach to study galaxy evolution in a cosmological context. We combine cosmological merger trees and semi-analytic models of galaxy formation to provide the initial conditions for multi-merger hydrodynamic simulations. In this way we exploit the advantages of merger simulations (high resolution and inclusion of the gas physics) and semi-analytic models (cosmological background and low computational cost), and integrate them to create a novel tool. This approach allows us to study the evolution of various galaxy properties, including the treatment of the hot gaseous halo from which gas cools and accretes onto the central disc, which has been neglected in many previous studies. This method shows several advantages over other methods. As only the particles in the regions of interest are included, the run time is much shorter than in traditional cosmological simulations, leading to greater computational efficiency. Using cosmological simulations, we show that multiple mergers are expected to be more common than sequences of isolated mergers, and therefore studies of galaxy mergers should take this into account. In this pilot study, we present our method and illustrate the results of simulating ten Milky Way-like galaxies since z=1. We find good agreement with observations for the total stellar masses, star formation rates, cold gas fractions and disc scale length parameters. We expect that this novel numerical approach will be very useful for pursuing a number of questions pertaining to the transformation of galaxy internal structure through cosmic time.