Exploring simulated early star formation in the context of the ultrafaint dwarf galaxies

  title={Exploring simulated early star formation in the context of the ultrafaint dwarf galaxies},
  author={Lauren Corlies and Kathryn V. Johnston and John H. Wise},
  journal={Monthly Notices of the Royal Astronomical Society},
Ultrafaint dwarf galaxies (UFDs) are typically assumed to have simple, stellar populations with star formation ending at reionization. Yet as the observations of these galaxies continue to improve, their star formation histories (SFHs) are revealed to be more complicated than previously thought. In this paper, we study how star formation, chemical enrichment, and mixing proceed in small, dark matter halos at early times using a high-resolution, cosmological, hydrodynamical simulation. The goals… 

Dancing in the Dark: Uncertainty in Ultrafaint Dwarf Galaxy Predictions from Cosmological Simulations

The existence of ultrafaint dwarf (UFD) galaxies highlights the need to push our theoretical understanding of galaxies to extremely low mass. We examine the formation of UFDs by twice running a fully

High-resolution three-dimensional simulations of gas removal from ultrafaint dwarf galaxies

Context. The faintest Local Group galaxies found lurking in and around the Milky Way halo provide a unique test bed for theories of structure formation and evolution on small scales. Deep Subaru and

Probing the Assembly of Dwarf Galaxies through Cosmic Time with Damped Lyα Absorption Spectroscopy

We investigate the absorption features associated with a gas-rich dwarf galaxy, using cosmological hydrodynamics simulations. Our goal is to explore whether the progenitors of the lowest-mass dwarf

Simulating an isolated dwarf galaxy with multichannel feedback and chemical yields from individual stars

In order to better understand the relationship between feedback and galactic chemical evolution, we have developed a new model for stellar feedback at grid resolutions of only a few parsecs in global

The little things matter: relating the abundance of ultrafaint satellites to the hosts’ assembly history

Ultrafaint dwarf galaxies ($M_\star \le 10^{5}\, {\rm M}_\odot$) are relics of an early phase of galaxy formation. They contain some of the oldest and most metal-poor stars in the Universe which

Exploring chemical homogeneity in dwarf galaxies: a VLT-MUSE study of JKB 18

Deciphering the distribution of metals throughout galaxies is fundamental in our understanding of galaxy evolution. Nearby, low-metallicity, star-forming dwarf galaxies, in particular, can offer

Metal Mixing and Ejection in Dwarf Galaxies Are Dependent on Nucleosynthetic Source

Using a high-resolution simulation of an isolated dwarf galaxy, accounting for multichannel stellar feedback and chemical evolution on a star-by-star basis, we investigate how each of 15 metal

The formation times and building blocks of Milky Way-mass galaxies in the FIRE simulations

Surveys of the Milky Way (MW) and M31 enable detailed studies of stellar populations across ages and metallicities, with the goal of reconstructing formation histories across cosmic time. These

Simulating Metal Mixing of Both Common and Rare Enrichment Sources in a Low-mass Dwarf Galaxy

One-zone models constructed to match observed stellar abundance patterns have been used extensively to constrain the sites of nucleosynthesis with sophisticated libraries of stellar evolution and

Minimum star-forming halo mass in axion cosmology

Elucidating the particle physics nature of dark matter (DM) is one of the great challenges in modern science. The current lack of any direct DM detections in the laboratory heightens the need for



Connecting the First Galaxies with Ultrafaint Dwarfs in the Local Group: Chemical Signatures of Population III Stars

We investigate the star formation history (SFH) and chemical evolution of isolated analogs of Local Group (LG) ultrafaint dwarf galaxies (UFDs; stellar mass range of ) and gas-rich, low-mass dwarfs

The effect of feedback and reionization on star formation in low-mass dwarf galaxy haloes

We simulate the evolution of a 10^9 Msun dark matter halo in a cosmological setting with an adaptive-mesh refinement code as an analogue to local low luminosity dwarf irregular and dwarf spheroidal

Metal Enrichment of the Intergalactic Medium in Cosmological Simulations

Observations have established that the diffuse intergalactic medium (IGM) at z ~ 3 is enriched to ~10-2.5 solar metallicity and that the hot gas in large clusters of galaxies (ICM) is enriched to -

Scaling Relations for Galaxies Prior to Reionization

The first galaxies in the universe are the building blocks of all observed galaxies. We present scaling relations for galaxies forming at redshifts z ⩾ 15 when reionization is just beginning. We

Star-Formation Histories, Abundances, and Kinematics of Dwarf Galaxies in the Local Group

Within the Local Universe galaxies can be studied in great detail star by star, and here we review the results of quantitative studies in nearby dwarf galaxies. The color-magnitude diagram synthesis

Resolving the Formation of Protogalaxies. III. Feedback from the First Stars

The first stars form in dark matter halos of masses ~106 M☉ as suggested by an increasing number of numerical simulations. Radiation feedback from these stars expels most of the gas from the shallow


We utilize metal-poor stars in the local, ultra-faint dwarf galaxies (UFDs; Ltot ⩽ 105 L☉) to empirically constrain the formation process of the first galaxies. Since UFDs have much simpler star

Formation of isolated dwarf galaxies with feedback

We present results of high resolution hydrodynamical simulations of the formation and evolution of dwarf galaxies. Our simulations start from cosmological initial conditions at high redshift. They


This paper presents the first results from a model for chemical evolution that can be applied to N-body cosmological simulations and quantitatively compared to measured stellar abundances from large

The effects of photoionization on galaxy formation - II. Satellite galaxies in the Local Group

We use a self-consistent model of galaxy formation and the evolution of the intergalactic medium to study the effects of the reionization of the Universe at high redshift on the properties of