#### DMCA

## A Consistency Relation for the CMB B-mode Polarization in the Squeezed Limit

### Citations

398 | Non-gaussian features of primordial fluctuations in single field inflationary models - Maldacena |

84 | Single field consistency relation for the 3-point function, JCAP 0410 - Creminelli, Zaldarriaga - 2004 |

29 | Conformal consistency relations for single-field inflation - Creminelli, Norena, et al. |

27 |
et al. Detection of B-Mode Polarization at Degree Angular Scales by BICEP2
- Ade
(Show Context)
Citation Context ...om that induced by inter-stellar dust. 1 Introduction The recent detection of B-mode polarization pattern in the Cosmic Microwave Background (CMB) on degree-angular scales by the BICEP2 collaboration =-=[1]-=-, has generated a great deal of excitement in the field. The range of scales and the shape of the spectrum suggest that it has primordial origin and an outburst of work has followed up focusing on the... |

26 |
Toward an Understanding of Foreground Emission
- Flauger, Hill, et al.
(Show Context)
Citation Context ...it will be a strong argument in favor of inflation. However, it has been shown that this observation is also consistent with the polarized radiation emitted by the poorly-understood interstellar dust =-=[2, 3]-=-. Nevertheless, these results open the possibility that a detailed observational study of B-mode polarization is not too far from our technological reach. One may wonder whether measuring the three-po... |

24 |
The Cosmic Linear Anisotropy Solving
- Lesgourgues
(Show Context)
Citation Context ...the long-wavelength mode to be in the range 20 ≤ l3 ≤ 300 and the two short-wavelength modes to be equal and in the range 10 l3 ≤ l1 ≤ lmax. The power spectra are computed by the numerical code CLASS =-=[38]-=-. The signal-to-noise of the TBB and TEE bispectra in the squeezed limit for these three experiments and a zero noise experiment are given in table [1]. We quote two cases: considering only the rescal... |

22 |
A joint analysis of Planck and BICEP2 B modes including dust polarization uncertainty (2014
- Mortonson, Seljak
(Show Context)
Citation Context ...it will be a strong argument in favor of inflation. However, it has been shown that this observation is also consistent with the polarized radiation emitted by the poorly-understood interstellar dust =-=[2, 3]-=-. Nevertheless, these results open the possibility that a detailed observational study of B-mode polarization is not too far from our technological reach. One may wonder whether measuring the three-po... |

21 | Galilean invariance and the consistency relation for the nonlinear squeezed bispectrum of large scale structure - Peloso, Pietroni |

19 | The (not so) squeezed limit of the primordial 3-point function, JCAP 1111 - Creminelli, D’Amico, et al. - 2011 |

19 | Operator Product Expansion of Inflationary Correlators and Conformal Symmetry of de Sitter, Nucl.Phys. B864 - Kehagias, Riotto - 2012 |

18 | An Infinite Set of Ward Identities for Adiabatic Modes - Hinterbichler, Hui, et al. |

18 |
Introduction to the Theory of the Early Universe: Cosmological Perturbations and Inflationary Theory (World Scientific,
- Gorbunov, Rubokov
- 2011
(Show Context)
Citation Context ...on, the effect of the long-wavelength mode corresponds to a rescaling of the wave vector ~k and the time coordinate η given by ~k 7−→ ~k e5ΦL/3, η 7−→ η eΦL/3. (A.2) The BB power spectrum is given by =-=[40]-=- CBBl = 4pi 25 ∆η2rec ∫ ∞ 0 d ln k PT (k)h ′2(k, ηrec) [ l + 2 2l + 1 jl−1(kηobs)− l − 1 2l + 1 jj+1(kηobs) ]2 (A.3) 10 with primordial tensor power spectrum given by PT (k) = AT ( k k∗ )nT , (A.4) an... |

14 |
Sachs-Wolfe at second order: the CMB bispectrum on large angular scales,”
- Boubekeur, Creminelli, et al.
- 2009
(Show Context)
Citation Context ...omes from the lensing induced by the long-wavelength mode, and we estimate this signal to be observable for a futuristic experiment. This is similar to what happens for the CMB temperature bispectrum =-=[14, 26]-=-. An interesting feature of this result is that for the case of B-mode polarization we obtain a relation that connects the squeezed limit of the TBB three-point function with the primordial tensor pow... |

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

7 |
The full squeezed CMB bispectrum from inflation
- Lewis
- 2012
(Show Context)
Citation Context ...omes from the lensing induced by the long-wavelength mode, and we estimate this signal to be observable for a futuristic experiment. This is similar to what happens for the CMB temperature bispectrum =-=[14, 26]-=-. An interesting feature of this result is that for the case of B-mode polarization we obtain a relation that connects the squeezed limit of the TBB three-point function with the primordial tensor pow... |

7 |
Weak lensing of the CMB: A harmonic approach
- Hu
(Show Context)
Citation Context ...sor power spectrum nT . However, as we will see in the next section it is difficult, to say the least, to observe this contribution. 4 Signal-to-noise estimation Similar to the temperature bispectrum =-=[33]-=-, for the TBB and TEE bispectra given in Eq. (3.8), the signal-to-noise is given by( S N )2 = fsky pi 1 (2pi)2 ∫∫ d2l1 d 2l3 ( BTXXl1l2l3 )2 Var , (4.1) where again X can be either E or B. Assuming l3... |

5 |
Adiabatic modes
- Weinberg
(Show Context)
Citation Context ... for the short modes. We take the long mode to be constant at the scale of the short modes at recombination such that its effect is equivalent to a coordinate transformation (i.e. it is what Weinberg =-=[29]-=- calls an adiabatic 2 mode) η̃ = η + (η) , x̃i = xi(1− λ) , (2.1) where is an arbitrary function of time and λ is an arbitrary constant. In the limit of instantaneous recombination and considering ... |

5 |
An all sky analysis of polarization
- Zaldarriaga, Seljak
- 1997
(Show Context)
Citation Context ...re of the sphere and consider it as a plane normal to ez the spin raising and lowering operators reduce to L± = Lx ± iLy = ∂x ± i∂y. (2.12) Therefore the spin-0 quantities Ẽ and B̃ can be defined as =-=[32]-=- Ẽ = −1 2 ( L2+(Q− iU) + L2−(Q+ iU) ) , (2.13) B̃ = 1 2i ( L2+(Q− iU)− L2−(Q+ iU) ) , (2.14) and under a Fourier transform aẼ( ~l) = ∫ d~m l2(Q cos 2φl + U sin 2φl)e −i~l·~m, (2.15) aB̃( ~l) = ∫ d~m... |

5 |
Bouchet et al., “COrE (Cosmic Origins Explorer) A White Paper
- Collaboration, F
(Show Context)
Citation Context ...uncorrelated. In our signal-to-noise estimation we use the values of θfwhm and σY for three frequency channels of the Planck 14-month mission [35], seven frequency channels of the COrE 4-year mission =-=[36]-=-, five frequency channels of the PRISM 4-year mission [37] as given in Tables [2-4] of the Appendix and an ideal noiseless experiment with lmax = 3000. For all four cases we take the sky fraction to b... |

5 |
et al., “PRISM (Polarized Radiation Imaging and Spectroscopy Mission): A White Paper on the Ultimate Polarimetric Spectro-Imaging of the Microwave and Far-Infrared Sky
- Collaboration, Andre
(Show Context)
Citation Context ... values of θfwhm and σY for three frequency channels of the Planck 14-month mission [35], seven frequency channels of the COrE 4-year mission [36], five frequency channels of the PRISM 4-year mission =-=[37]-=- as given in Tables [2-4] of the Appendix and an ideal noiseless experiment with lmax = 3000. For all four cases we take the sky fraction to be fsky = 0.65. For the fiducial model, we consider a 6 par... |

4 | Soft-Pion Theorems for Large Scale Structure - Horn, Hui, et al. |

3 | Angular averaged consistency relations of large-scale structures - Valageas - 2014 |

3 |
The full CMB temperature bispectrum from single-field inflation
- Huang, Vernizzi
(Show Context)
Citation Context ...en for a very futuristic experiment. It is noteworthy that the full calculation of the temperature bispectrum in the absence of primordial non-Gaussianity can now be carried out numerically (see e.g. =-=[27]-=-). While this note was being prepared, an analytical and numerical study of the correlation function involving E-mode polarization appeared [28] and our results seem to agree with theirs. We begin in ... |

3 |
et al. Scientific optimization of a ground - based CMB polarization experiment
- Bowden
(Show Context)
Citation Context ...heoretical power spectra plus the instrumental noise C̃Y Yl = C Y Y l +N Y Y l , (4.3) where Y can be T, E or B mode. The noise power spectrum for a multi-frequency experiment like Planck is given by =-=[34]-=- NY Yl = (∑ c 1 NY Yl,c )−1 . (4.4) The noise in each channel is given by NY Yl,c = θ 2 fwhmσ 2 Y exp [ l(l + 1) θ2fwhm 8ln2 ] , (4.5) 8 Modes long-mode lensing Planck COrE PRISM Ideal TBB no 6.7× 10−... |

2 | Single-Field Consistency Relations of Large Scale Structure - Creminelli, Gleyzes, et al. |

2 | Testing the equal-time angular-averaged consistency relation of the gravitational dynamics in N-body simulations - Nishimichi, Valageas |

2 |
et al., “The Scientific programme of Planck”, arXiv:astro-ph/0604069
- Collaboration, Tauber
(Show Context)
Citation Context ...nish since the noise contribution from different maps are uncorrelated. In our signal-to-noise estimation we use the values of θfwhm and σY for three frequency channels of the Planck 14-month mission =-=[35]-=-, seven frequency channels of the COrE 4-year mission [36], five frequency channels of the PRISM 4-year mission [37] as given in Tables [2-4] of the Appendix and an ideal noiseless experiment with lma... |

1 | Consistency relations of large-scale structures - Valageas |

1 |
et al., “Impact of polarisation on the intrinsic CMB bispectrum
- Pettinari, Fidler, et al.
(Show Context)
Citation Context ...aussianity can now be carried out numerically (see e.g. [27]). While this note was being prepared, an analytical and numerical study of the correlation function involving E-mode polarization appeared =-=[28]-=- and our results seem to agree with theirs. We begin in Section 2 by computing the effect of a long-wavelength metric perturbation on the polarization power spectrum; we do this by closely following t... |

1 |
Position-dependent power spectrum of the large-scale structure: a novel method to measure the squeezed-limit bispectrum”, JCAP 1405
- Chiang, Wagner, et al.
- 2014
(Show Context)
Citation Context ...of the B-mode power spectrum among different small patches in the sky and correlate this with the average temperature of each patch, similar to what was proposed for the large scale structure in ref. =-=[39]-=-. One could then attempt to subtract the lensing in each patch using lensing potential maps in order to reduce the lensing variance. We leave a detailed analysis of such a technique as future work if ... |