Cosmological Inflation and Large-Scale Structure: Preface

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The Mass of a halo (2000, methodology): “We begin by recalling some background about the spherical top-hat collapse model (see e.g. Peebles 1993; Peacock 1999; Liddle & Lyth 2000, and references therein) from which much of the language in this field has been borrowed.”
THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, background): “5.3. owCDM : Constant Equation of State in a Curved Universe Inflation models generally predict that the curvature of the Universe,Ωk, is ∼ 10−5 (Guth 1981; Liddle & Lyth 2000).”
Bounds on slow roll and the de Sitter Swampland (2018, background): “6 This is partly justified by the fact that inflation is of interest typically around attractor solutions, where the two conditions are indeed also sufficient [21].”
Non-Gaussianities in two-field inflation (2006, background): “(13) The first equality follows from taking k at Hubble crossing, k = aH ∝ H expN , while the second is a consequence of the definition of N , Eq.”