Locally compact (2, 2)‐transformation groups

Bartolo, Alfonso Di; Falcone, Giovanni; Strambach, Karl

doi:10.1002/mana.200910244

Cited by 3 publications

(1 citation statement)

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“…inflation predict slightly different deviations from Gaussian primordial fluctuations (see e.g. Bartolo et al 2004Bartolo et al , 2010Yadav & Wandelt 2010;Liguori et al 2010;Martínez-González & Planck Collaboration 2012). The latest constraints by the Planck 1 satellite put strong constraints on the amount of primordial NG that is present in the data (Planck 2013results XXIV 2014.…”

Section: Introductionmentioning

confidence: 99%

The CIB-lensing bispectrum: impact on primordial non-Gaussianity and detectability for the Planck mission

Curto

Tucci

Kunz

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We characterize the Cosmic Infrared Background (CIB)-lensing bispectrum which is one of the contributions to the three-point functions of Cosmic Microwave Background (CMB) maps in harmonic space. We show that the CIB-lensing bispectrum has a considerable strength and that it can be detected with high significance in the Planck high-frequency maps. We also present forecasts of the contamination on different shapes of the primordial non-Gaussianity f nl parameter produced by the CIB-lensing bispectrum and by the extragalactic point sources bispectrum in the Planck high-resolution CMB anisotropy maps. The local, equilateral and orthogonal shapes are considered for 'raw' single-frequency (i.e., without applying any component separation technique) and foreground-reduced Planck temperature maps. The CIB-lensing correlation seems to mainly affect orthogonal shapes of the bispectrum -with ∆f (ort) nl = −21 and −88 for the 143 and 217 GHz bands respectively -while point sources mostly impact equilateral shapes, with ∆f (eq) nl = 160, 54 and 60 at 100, 143 and 217 GHz. However, the results indicate that these contaminants do not induce any relevant bias on Planck f nl estimates when foreground-reduced maps are considered: using SEVEM for the component separation we obtain ∆f (ort) nl = 10.5 due to the CIB-lensing and ∆f (eq) nl = 30.4 due to point sources, corresponding to 0.3σ and 0.45σ in terms of the Planck 2013 f nl uncertainty. The component separation technique is, in fact, able to partially clean the extragalactic source contamination and the bias is reduced for all the shapes. We have further developed single-and multiple-frequency estimators based on the Komatsu, Spergel & Wandelt (2005) formalism that can be implemented to efficiently detect this signal.

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Section: Introductionmentioning

confidence: 99%