The First Cosmic Structures and Their Effects

By Benedetta Ciardi, A. Ferrara. 2004

305 citations recorded by the source corpus.

Despite much recent theoretical and observational progress in our knowledge of the early universe, many fundamental questions remain only partially answered. Here, we review the latest achievements and persisting problems in the understanding of first cosmic structure formation.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/74e8e1e61b874fc22c5f0d544a4c5924029a6d10

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Citations in the corpus

Formation and evolution of primordial protostellar systems (2012, background): “…T RO D U C T I O N The formation of the first stars, also termed Population III (Pop III), heralded an end to the physical simplicity of the Universe at the end of the cosmic dark ages (e.g. Barkana & Loeb 2001; Bromm & Larson 2004; Ciardi & Ferrara 2005; Glover 2005; Bromm et al. 2009; Loeb 2010).”
The cooling of shock-compressed primordial gas (2005, background): “…hierarchical structure formation, shocks in the primordial gas arise naturally, both through the merging of dark matter (DM) haloes in the formation of galaxies and through the supernovae (SNe) that marked the deaths of the first generation stars (e.g. Barkana & Loeb 2001; Ciardi & Ferrara 2005).”
A case study of hurdle and generalized additive models in astronomy: the escape of ionizing radiation (2018, result): “While previous works (see e.g. Ciardi & Ferrara 2005) determined a strong dependence of the escape fraction on the gas distribution (fesc increasing with the clumping factor), here we find only a mild dependence, possibly because of the relatively small values of C obtained due to the limited…”
Improved upper limits on the 21 cm signal power spectrum of neutral hydrogen at z ≈ 9.1 from LOFAR (2020, background): “…of their formation, as well as the impact on the physics of the interstellar medium (ISM) and intergalactic medium (IGM) of the radiation emitted by these first light sources (see, e.g. Ciardi & Ferrara 2005; Morales & Wyithe 2010; Pritchard & Loeb 2012; Furlanetto 2016, for extensive reviews).”
Population III stars: hidden or disappeared? (2007, background): “This condition can be met for newly formed halos that either (i) gain their gas from regions not yet polluted by outflows from nearby star forming galaxies, or (ii) have progenitors in which star formation has not occurred or was suppressed (Ciardi & Ferrara 2005).”
The first stars: formation of binaries and small multiple systems (2009, background): “How did the cosmic dark ages end, and how was the homogeneous early Universe transformed into the highly complex state that we observe today (e.g. Barkana & Loeb 2001; Miralda-Escudé 2003; Ciardi & Ferrara 2005)?”
The transition from population III to population II-I star formation (2010, background): “The determination of the properties of early stars and their effects on the following baryonic-structure formation episodes is still a problem under debate (for a complete review see e.g. Ciardi & Ferrara 2005).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, background): “Concurrent with the build-up of the LW background radiation field is the onset of reionization, the process by which the intergalactic medium becomes heated and ionized at z > ∼ 6 (e.g. Ciardi & Ferrara 2005).”
The First Stars: Mass Growth Under Protostellar Feedback (2011, background): “Also known as Population III (Pop III) stars, they are the early drivers of cosmic evolution (e.g. Barkana & Loeb 2001; Bromm & Larson 2004; Ciardi & Ferrara 2005; Glover 2005; Bromm et al. 2009; Loeb 2010).”
Constraining the Evolution of the Ionizing Background and the Epoch of Reionization with z ∼ 6 Quasars. II. A Sample of 19 Quasars (2005, background): “When and how the universe reionized remains one of the fundamental questions of modern cosmology (for reviews of theoretical models, see Barkana & Loeb 2001, Loeb & Barkana 2001, and Ciardi & Ferrara 2005).”
The global 21-centimeter background from high redshifts (2006, background): “This has been a subject of extensive study over the past three decades (see e.g. Barkana & Loeb 2001; Haiman 2004; Ciardi & Ferrara 2005 for recent reviews).”
Reionization and the Cosmic Dawn with the Square Kilometre Array (2012, background): “Because of the large uncertainties in the nature and intensity of high-z feedback effects (for a review see Ciardi & Ferrara 2005 and its updated version ArXiv:astro-ph/0409018), it is not straightforward to estimate the relative importance of the absorption signals from the diffuse IGM and from…”
The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “Understanding the formation of the first stars and galaxies at the end of the cosmic dark ages is one of the most important challenges in modern cosmology (Barkana & Loeb 2001; Bromm & Larson 2004; Ciardi & Ferrara 2005; Glover 2005).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…amenable to simulation than tracking subsequent generations of stars (Abel, Bryan & Norman 2002; see also Bromm & Larson 2004; Yoshida et al. 2003; Ciardi & Ferrara 2005): (i) The gravitational potential wells most likely to host the first sites of star formation can be identified given a power…”
Cosmological radiative transfer codes comparison project – I. The static density field tests (2006, unknown): “…e.g. modelling and understanding of the Lyα forest, absorption lines in spectra of high-z quasars, radiative feedback effects, the reionization of the intergalactic medium (IGM) and star formation, just to mention a few (see e.g. Ciardi & Ferrara 2005, for a recent review on C© 2006 The Authors.”
Science with a lunar low-frequency array: From the dark ages of the Universe to nearby exoplanets (2009, background): “…HI line emission A fundamental question of current cosmological research is on the nature of structure formation in the Universe (for a review, see Ciardi and Ferrara, 2005): how is the observed distribution of visible matter created from the initial conditions just after the big bang, when…”