Exploring the evolution of a dwarf spheroidal galaxy with SPH simulations: I. Stellar feedback
arXiv:2404.18701 · doi:10.3847/1538-4357/ad4700
Abstract
A fundamental question regarding the evolution of dwarf spheroidal galaxies is the identification of the key physical mechanisms responsible for gas depletion. Here, we focus on the study of stellar feedback in isolated dwarf spheroidal galaxies, by performing numerical simulations using a modified version of the SPH code GADGET-3. The Milky Way satellite Leo II (PGC 34176) in the Local Group was considered as our default model dwarf galaxy. The parameter space for the stellar feedback models was explored to match observational constraints of Leo II, such as residual gas mass, total mass within the tidal radius, star formation history, final stellar mass, stellar ages and metallicity. Additionally, we examined the impact of the binary fraction of stars, initial mass function, dark matter halo mass and initial gas reservoir. Many simulations revealed recent star formation quenching due to stellar feedback. In general, the gas depletion, expected star formation history, total mass of stars and total mass within the tidal radius were adequately reproduced in the simulations when compared to observational estimates. However, there were discrepancies in the distribution of stellar ages and metallicities, which suggested that the cosmic gas infall would play a more complex role in our dwarf spheroidal galaxy than captured by a monolithic infall scenario. Our results suggest that currently quenched dwarf galaxies may not necessarily need to evolve within clusters or groups, and that stellar feedback alone could be a sufficient factor in shaping at least some of these galaxies as we observe them today.
To be published in The Astrophysical Journal. 33 pages, 20 figures
References in corpus (23)
- Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
- Properties of galaxies reproduced by a hydrodynamic simulation
- The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
- A common mass scale for satellite galaxies of the Milky Way
- Velocity Dispersion Profiles of Seven Dwarf Spheroidal Galaxies
- Population III stars: hidden or disappeared ?
- Scaling Relations and the Fundamental Line of the Local Group Dwarf Galaxies
- Gaia early DR3 systemic motions of Local Group dwarf galaxies and orbital properties with a massive Large Magellanic Cloud
- Delving Deeper into the Tumultuous Lives of Galactic Dwarfs: Modeling Star Formation Histories
- Complexity on Small Scales II: Metallicities and Ages in the Leo II Dwarf Spheroidal Galaxy
- Simulations of the formation and evolution of isolated dwarf galaxies
- Observational constraints on stellar feedback in dwarf galaxies
- Quasar outflows at : the impact on the host galaxies
- The binary fraction of stars in dwarf galaxies: the case of Leo II
- The role of faint population III supernovae in forming CEMP stars in ultra-faint dwarf galaxies
- A multi-epoch kinematic study of the remote dwarf spheroidal galaxy Leo II
- A Wide-Field View of Leo II -- A Structural Analysis Using the SDSS
- Galactic outflow and diffuse gas properties at z>=1 using different baryonic feedback models
- How much metals did the first stars provide to the ultra-faint dwarfs?
- Three-dimensional hydrodynamical simulations of the supernovae-driven gas loss in the dwarf spheroidal galaxy Ursa Minor
- Extended Schmidt law holds for faint dwarf irregular galaxies
- Wide-field Survey around Local Group Dwarf Spheroidal Galaxy Leo II: Spatial Distribution of Stellar Content
- Solo dwarfs IV: Comparing and contrasting satellite and isolated dwarf galaxies in the Local Group