THE FIRST GALAXIES: CHEMICAL ENRICHMENT, MIXING, AND STAR FORMATION

By Thomas Greif, S. Glover, Volker Bromm, Ralf Klessen. 2010

178 citations recorded by the source corpus.

Using three-dimensional cosmological simulations, we study the assembly process of one of the first galaxies, with a total mass of ∼108 M☉, collapsing at z ≃ 10. Our main goal is to trace the transport of the heavy chemical elements produced and dispersed by a pair-instability supernova exploding in one of the minihalo progenitors. To this extent, we incorporate an efficient algorithm into our smoothed particle hydrodynamics code that approximately models turbulent mixing as a diffusion process. We study this mixing with and without the radiative feedback from Population III (Pop III) stars that subsequently form in neighboring minihalos. Our simulations allow us to constrain the initial conditions for second-generation star formation, within the first galaxy itself, and inside of minihalos that virialize after the supernova explosion. We find that most minihalos remain unscathed by ionizing radiation or the supernova remnant, while some are substantially photoheated and enriched to supercritical levels, likely resulting in the formation of low-mass Pop III or even Population II (Pop II) stars. At the center of the newly formed galaxy, ∼105 M☉ of cold, dense gas uniformly enriched to ∼10−3 Z☉ is in a state of collapse, suggesting that a cluster of Pop II stars will form. The first galaxies, as may be detected by the James Webb Space Telescope, would therefore already contain stellar populations familiar from lower redshifts.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3c351317042d448442c58a134bda04a607aab960

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Citations in the corpus

Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionization (2016, result): “We find that the typical metallicity of the halo gas after the explosion of Pop III stars is ∼ 10−3 − 10−2Z , consistent with previous studies (Greif et al. 2010; Ritter et al. 2012).”
THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I. JAMES WEBB SPACE TELESCOPE DETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES (2011, background): “Since the first generation of galaxies is predicted to form in high-density regions that have been pre-enriched by pop III stars in minihalos, these galaxies are not expected to be metal-free, and are most likely dominated by chemically enriched stars (e.g. Greif et al. 2010).”
Evolution and fate of very massive stars (2013, methodology): “…Note, however, that the most recent star formation simulations find lower mass stars forming in groups, similarly to present-day star formation (Greif et al. 2010; Stacy, Greif & Bromm 2010). metallicities using the GENEVA stellar evolution code (Eggenberger et al. 2008) including the…”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, background): “470 million years old (Wise & Abel 2007; Wise et al. 2008; Greif et al. 2008, 2010; and for recent reviews, see Bromm & Yoshida 2011 and Dunlop 2012).”
Ubiquitous seeding of supermassive black holes by direct collapse (2012, background): “The second generation of stars, Pop II, is also expected to exist at high redshifts within metal-enriched regions (e.g. Wise& Abel 2008; Greif et al. 2010).”
The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, background): “In addition, some are directly affected by radiative and SN feedback from Pop III stars (Johnson & Bromm 2006; Wise & Abel 2008b; Greif et al. 2010; Maio et al. 2010; Wise et al. 2012b; Muratov et al. 2013; Pawlik, Milosavljević & Bromm 2013).”
Production of dust by massive stars at high redshift (2011, background): “Greif et al (2010) showed in a cosmological simulation that one single PISN (at z ≃ 30) can enrich the mini halo in which it forms uniformly up toZ = 10−3 Z⊙ and induce Pop II star formation (atz≃ 10).”
Evolution of the atomic and molecular gas content of galaxies (2013, unknown): “This gas can then form “Pop III” stars which can enrich the surrounding ISM to ZIII ∼ 10−3 Z⊙ (Schneider et al. 2002; Greif et al. 2010; Wise et al. 2012).”
GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS (2016, background): “…halo (Kitayama et al. 2004; Whalen et al. 2004, 2008; Kitayama & Yoshida 2005; Abel et al. 2007), leaving behind a gas-poor halo that only recovers by cosmological accretion after tens of megayears (Wise & Abel 2008b; Greif et al. 2010; Wise et al. 2012b; Muratov et al. 2013; Jeon et al. 2014).”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “Metal mixing, however, occurs in a rather inhomogeneous fashion resulting in large abundance spreads of several dex across the system (Greif et al. 2010,Wise et al. 2012).”
Formation of Supermassive Black Hole Seeds (2016, background): “…background temperature (TCMB) by dust and metal line cooling at z=15 even in the presence of UV flux (Tornatore et al. 2007; Smith et al. 2009; Greif et al. 2010; Wise et al. 2012; Whalen et al. 2013; Johnson et al. 2013a; Safranek-Shrader et al. 2014a; Bovino et al. 2014; Pallottini et al.…”
Photodissociation of H2 in protogalaxies: modelling self‐shielding in three‐dimensional simulations (2011, methodology): “…either adopted the optically–thin dissociation rate throughout (Machacek et al. 2001, 2003; Mesinger et al. 2006, 2009; Wise & Abel 2007, 2008a,b; Greif et al. 2010), relied upon estimating NH2 from local properties of the gas (Bromm & Loeb 2003; Johnson et al. 2008; Gnedin et al. 2009; Shang…”
Formation and evolution of primordial protostellar systems (2012, background): “…Yoshida et al. 2007; Whalen et al. 2008; Greif et al. 2009), and the violent supernova explosions that marked their deaths enriched the primordial gas with the first heavy elements (e.g. Heger et al. 2003; Umeda & Nomoto 2003; Wise & E-mail: tgreif@mpa-garching.mpg.de Abel 2008; Greif et al. 2010).”
The First Stars (2012, background): “III star is significantly larger than the volume that is enriched by the metals produced in the supernova occurring at the end of the massive star’s life (see e.g. the recent treatment by Greif et al. 2010, or Ciardi & Ferrara (2005) for a summary of earlier work).”
Building up the Population III initial mass function from cosmological initial conditions (2016, background): “…same massive Pop III stars also left behind the first metal-enriched SN remnants (e.g. Mori et al. 2002; Bromm et al. 2003; Wada & Venkatesan 2003; Norman et al. 2004; Tornatore et al. 2007; Greif et al. 2007, 2010; Wise et al. 2012; Maio et al. 2011; recently reviewed in Karlsson et al. 2013).”
Star formation in semi-analytic galaxy formation models with multiphase gas (2015, unknown): “This gas can then form “Pop III” stars which can enrich the surrounding ISM to ZIII ∼ 10 −3 Z⊙ (Schneider et al. 2002; Greif et al. 2010; Wise et al. 2012).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, background): “…from cosmological simulations of early SNe feedback and metal enrichment (e.g. Tornatore et al. 2007; Wise & Abel 2008; Wiersma et al. 2009a; Greif et al. 2010; Maio et al. 2011; Wise et al. 2012) and of the build-up of the global background (e.g. Yoshida et al. 2003; Wise & Abel 2005;…”
THE BIRTH OF A GALAXY: PRIMORDIAL METAL ENRICHMENT AND STELLAR POPULATIONS (2010, background): “These features and a well-mixed ISM (cf. Wise & Abel 2008; Greif et al. 2010) are apparent in the metallicity projections in Figure 2.”