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## Observational signatures and non-gaussianities of general single field inflation

Citations: | 157 - 10 self |

### Citations

894 |
Supergravity and a confining gauge theory: Duality cascades and chi SB resolution of naked singularities,
- Klebanov, Strassler
- 2000
(Show Context)
Citation Context ...tors, can arise when there are fluxes supported on cycles localized in small regions of the compactified space. A prototypical example of such a strongly warped throat is the warped deformed conifold =-=[50,51]-=-. The effective field theory of compact models containing such throats [48,49] has been explored in detail in [52]. In the slow-roll paradigm, inflation can happen when a brane is approaching anti-bra... |

715 | Hierarchies from fluxes in string compactifications,
- Giddings, Kachru, et al.
- 2001
(Show Context)
Citation Context ...egions of the compactified space. A prototypical example of such a strongly warped throat is the warped deformed conifold [50,51]. The effective field theory of compact models containing such throats =-=[48,49]-=- has been explored in detail in [52]. In the slow-roll paradigm, inflation can happen when a brane is approaching anti-branes in a throat if the potential is flat enough. However, this is non-generic ... |

499 |
De Sitter vacua in string theory,” Phys
- Kachru, Kallosh, et al.
- 2003
(Show Context)
Citation Context ...egions of the compactified space. A prototypical example of such a strongly warped throat is the warped deformed conifold [50,51]. The effective field theory of compact models containing such throats =-=[48,49]-=- has been explored in detail in [52]. In the slow-roll paradigm, inflation can happen when a brane is approaching anti-branes in a throat if the potential is flat enough. However, this is non-generic ... |

402 | Non-Gaussian features of primordial fluctuations in single field inflationary models,
- Maldacena
- 2003
(Show Context)
Citation Context ...ations is characterized by a three-point function which is, a priori, a nontrivial function of three variables (momentum magnitude and ratios) on the sky. Furthermore, as demonstrated conclusively in =-=[7,8]-=-, slow-roll models where the density perturbations are produced by fluctuations of the inflaton itself, predict negligible non-Gaussianity. A detection of non-Gaussianity by the next generation of exp... |

274 | CFT’s from Calabi-Yau four-folds, - Gukov, Vafa, et al. - 2000 |

256 |
Gravity Duals of Supersymmetric SU(N) x SU(N+M) Gauge Theories," Nucl.Phys. B578
- Klebanov, Tseytlin
- 2000
(Show Context)
Citation Context ...tors, can arise when there are fluxes supported on cycles localized in small regions of the compactified space. A prototypical example of such a strongly warped throat is the warped deformed conifold =-=[50,51]-=-. The effective field theory of compact models containing such throats [48,49] has been explored in detail in [52]. In the slow-roll paradigm, inflation can happen when a brane is approaching anti-bra... |

166 | Scalar speed limits and cosmology: acceleration from D-cceleration, Phys - Silverstein, Tong - 2004 |

163 | Particle physics models of inflation and the cosmological density perturbation,”
- Lyth, Riotto
- 1999
(Show Context)
Citation Context ... . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 45 11 Introduction Inflation has been a very successful paradigm for understanding otherwise puzzling aspects of big bang cosmology =-=[1,2]-=-. It can naturally solve the flatness, homogeneity and monopole problems that otherwise seem to require a very high degree of fine tuning for the initial state of our universe. Furthermore, inflation ... |

149 |
Theory of cosmological perturbations. Part 1. Classical perturbations. Part 2. Quantum theory of perturbations.
- Mukhanov, Feldman, et al.
- 1992
(Show Context)
Citation Context ...at otherwise seem to require a very high degree of fine tuning for the initial state of our universe. Furthermore, inflation generically predicts almost scale invariant Gaussian density perturbations =-=[3]-=-, consistent with experimental observations of the Cosmic Microwave Background. Future experiments can constrain and distinguish between inflationary models in several ways. In the next few years, we ... |

141 | D term inflation,” Phys - Binetruy, Dvali - 1996 |

93 |
The Shape of non-Gaussianities,
- Babich, Creminelli, et al.
- 2004
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Citation Context ... term.) It is very interesting to construct such models, and we will show an example in this section. The most significant non-Gaussianities come from Aλ and Ac when cs ≪ 1 and/or λ/Σ ≫ 1. As in Ref. =-=[20]-=-, to show the shape of A(k1, k2, k3), we present the 3-d plot x −1 2 x−1 3 A(1, x2, x3) as a function of x2 = k2/k1 and x3 = k3/k1. The shapes of −Aλ/k1k2k3 and Ac/k1k2k3 are 23shown in Fig. 1 and 2.... |

91 | The inflationary brane-antibrane universe - Burgess, Majumdar, et al. |

83 |
Primordial non-Gaussianities in single field inflation,
- Seery, Lidsey
- 2005
(Show Context)
Citation Context ...te theory, appears in [18]. This model does not belong to the general class that we will study in Einstein gravity.) Our results build on these papers and further significant work by Seery and Lidsey =-=[19]-=-, who found the fluctuation Lagrangian to cubic order for a general class of Lagrangians, and of Babich, Creminelli and Zaldarriaga [20], who emphasized the importance of analyzing the full shape of n... |

67 | Spergel et al., First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters - Collaboration, D |

58 | Second-order cosmological perturbations from inflation,” Nucl. Phys. B667 - Acquaviva, Bartolo, et al. - 2003 |

41 |
Mukhanov, “Perturbations in k-inflation,” Phys
- Garriga, F
- 1999
(Show Context)
Citation Context ...ass, can confine her attention to sections §2 and §4 (which are more or less self-contained). 2 Inflation models with a general Lagrangian To set up our notation, let us first review the formalism in =-=[37]-=- where a general Lagrangian for the inflaton field is considered. The Lagrangian is of the general form S = 1 ∫ d 2 4 x √ −g [ M 2 plR + 2P(X, φ)] , (2.1) where φ is the inflaton field and X = −1 2gµν... |

38 | Inflation from warped space
- Chen
(Show Context)
Citation Context ...h the standard AdS/CFT relation between gsN and the compactification volume), it seems very likely that model building could significantly reduce the apparent tune. For discussions of this issue, see =-=[13,16,17]-=-. 3.3 Kinetically driven inflation One simple class of models which can give rise to large non-Gaussianities is the models of K-inflation, where the dynamics of inflation is governed by (non-standard)... |

37 |
et al.: Wilkinson Microwave Anisotropy Probe (WMAP) three year results: implications for cosmology. Astrophys
- Spergel
- 2007
(Show Context)
Citation Context ...the non-Gaussianity is not diluted by the inflationary expansion itself, as happens in some models [11]). However, this 1 Already, there are strong hints that models with a red spectrum are preferred =-=[4]-=-. Moreover, if the spectral index runs from blue to red, then there should be an approximate coincidence [5] between the length scale k at which n(k) − 1 = 0 and the length scale at which the tensor t... |

33 |
Multi-throat brane inflation,” Phys
- Chen
- 2005
(Show Context)
Citation Context ...the work of Alishahiha, Silverstein and Tong [13], who found that a fairly concrete string construction [14] could yield substantially larger fNL >> 1. Different models in this class were constructed =-=[15,16]-=- in the context of warped compactification. The large non-Gaussianities in these models are compatible with the current observational bound, but potentially observable in future experiments [13,17]. (... |

29 |
On non-Gaussianities in single-field inflation,”
- Creminelli
- 2003
(Show Context)
Citation Context ...reaches a minimum. Such a coincidence of scales, if observed, can put constraints on inflationary model building. 2effect can only reach fNL ∼ O(1) in the regime where effective field theory applies =-=[12]-=-. A proof of principle that significantly larger fNL can occur in sensible models was provided by the work of Alishahiha, Silverstein and Tong [13], who found that a fairly concrete string constructio... |

23 | D-brane inflation,” arXiv:hep-th/0105203 - Dvali, Shafi, et al. - 2001 |

19 | Some aspects of brane inflation - Shiu, Tye |

19 | theory, orientifolds and G-flux, - Dasgupta, Rajesh, et al. - 1999 |

11 | Running non-Gaussianities in DBI inflation,” Phys - Chen - 2005 |

11 |
Non-Gaussian Inflationary Perturbations from the dS/CFT Correspondence,
- Seery, Lidsey
- 2006
(Show Context)
Citation Context ...e is no exact relation between the dS gravity theory and a dual field theory, since the useful aspects of the duality for this purpose are purely kinematical. Recent work in this direction appears in =-=[34,35]-=-. Our work on this connection will eventually appear in a companion paper [36]. The organization of this paper is as follows. In §2, we present the general class of Lagrangians that we will analyze (t... |

8 |
Inflation from string theory,” [arXiv:hep-th/0501179
- Cline
(Show Context)
Citation Context ...lnP h k d lnk = −M2 V pl ′2 . (3.9) V 2 There has been significant effort invested in developing slow-roll models of inflation in string theory. Some fairly recent reviews with further references are =-=[38,39]-=-. 63.2 DBI inflation DBI inflation [13–16] is motivated by brane inflationary models [21,40–43] in warped compactifications [44–49]. In particular, strongly warped regions or “warped throats” with ex... |

7 | Cosmological rescaling through warped space,” Phys
- Chen
- 2005
(Show Context)
Citation Context ... field theory). This scenario can naturally arise in warped string compactifications [15]. The inflaton φ is the position of a D-brane moving in a warped throat. In the region where the back-reaction =-=[14,16,60]-=- and stringy physics [16,17] can be ignored, the effective action has the following form S = M2 pl 2 ∫ d 4 x √ ∫ −gR − d 4 x √ −g [f(φ) −1 √ 1 + f(φ)g µν∂µφ∂νφ −f(φ) −1 +V (φ)] . (3.10) The above expr... |

4 |
Consistency relation for single scalar inflation,” Phys
- Gruzinov
- 2005
(Show Context)
Citation Context ...um. 4 Non-Gaussian Perturbations Now in the general setup of Sec. 2, we consider the non-Gaussian perturbations in the primordial power spectrum. There is a large literature on this subject, see e.g. =-=[7, 8, 13, 17,19,64,69,70]-=-. However, most of the literature has been focused on the case where the speed of sound cs is very close to one, where the primordial non-Gaussianities are generally too small to be detected in future... |

3 | eConf C041213 - Greene, Schalm, et al. - 2004 |

2 | Inflation and string cosmology,” [arXiv:hep-th/0503195 - Linde |

2 |
Acoustic signatures in the primary microwave background bispectrum,” Phys
- Creminelli, Nicolis, et al.
(Show Context)
Citation Context .... (5.3) The bound on the parameter fNL from data analysis depends on the shape of the nonGaussianities which we will discuss shortly. The current bound is roughly |fNL| < 300 for the first two shapes =-=[65]-=-, and |fNL| < 100 for the rest [4]. A non-Gaussianity is potentially observable in future experiments if |fNL| > 5 [66–68]. The magnitudes of Aǫ, Aη and As are unobservably small, of order O(ǫ). The s... |