Multitracing anisotropic non-Gaussianity with galaxy shapes

Chisari, Nora Elisa; Dvorkin, Cora; Schmidt, Fabian; Spergel, David N.

doi:10.1103/physrevd.94.123507

Cited by 68 publications

(86 citation statements)

References 64 publications

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“…Notice that, as long as we are constraining non-Gaussianity using the halo power spectrum only, any information on the angle between k s and k is lost. One needs to look at the bispectrum [272][273][274][275][276][277][278][279][280][281][282][283][284][285][286][287] or, alternatively, to galaxy shapes [20,21] and intrinsic alignments [22] to be sensitive to it.…”

Section: The Squeezed Limit Of the Primordial Bispectrummentioning

confidence: 99%

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

Biagetti

2019

Galaxies

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The understanding of the primordial mechanism that seeded the cosmic structures we observe today in the sky is one of the major goals in cosmology. The leading paradigm for such a mechanism is provided by the inflationary scenario, a period of violent accelerated expansion in the very early stages of evolution of the universe. While our current knowledge of the physics of inflation is limited to phenomenological models which fit observations, an exquisite understanding of the particle content and interactions taking place during inflation would provide breakthroughs in our understanding of fundamental physics at high energies. In this review, we summarize recent theoretical progress in the modeling of the imprint of primordial interactions in the large-scale structures of the universe. We focus specifically on the effects of such interactions on the statistical distribution of dark-matter halos, providing a consistent treatment of the steps required to connect the correlations generated among fields during inflation all the way to the late-time correlations of halos.

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Section: The Squeezed Limit Of the Primordial Bispectrummentioning

confidence: 99%

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

Biagetti

2019

Galaxies

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“…This is typically known as the "GI" contamination [9]. Second, it has been shown that intrinsic alignments encode information from phenomena such as primordial non-Gaussianity and gravitational waves from inflation in complementary manner to other probes of the large-scale structure [22][23][24][25]. Accurate extraction of this information requires a reliable alignment model.…”

Section: Introductionmentioning

confidence: 99%

An EFT description of galaxy intrinsic alignments

Vlah

Chisari

Schmidt

2020

J. Cosmol. Astropart. Phys.

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146

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We present a general perturbative effective field theory (EFT) description of galaxy shape correlations, which are commonly known as intrinsic alignments. This rigorous approach extends current analytical modelling strategies in that it only relies on the equivalence principle. We present our results in terms of three-dimensional statistics for two-and three-point functions of both galaxy shapes and number counts. In case of the two-point function, we recover the well-known linear alignment result at leading order, but also present the full next-to-leading order expressions. In case of the three-point function we present leading order results for all the auto-and cross-correlations of galaxy shapes and densities. We use a spherical tensor basis to decompose the tensor perturbations in different helicity modes, which allows us to make use of isotropy and parity properties in the correlators. Combined with the results on projection presented in a forthcoming companion paper, our framework is directly applicable to accounting for intrinsic alignment contamination in weak lensing surveys, and to extracting cosmological information from intrinsic alignments. 42A.1 Two-point functions 44 A.2 Three-point functions 47 B Fields in Fourier space 50 B.1 Bias expansion and renormalisation of the one-loop power spectrum 55 B.2 Degeneracy of the bias operators 62 B.3 Bias expansion of the tree-level bispectrum 63 C Bias renormalisation for tensor fields 65 1 Explicitly, we writewhere the Dirac delta function ensures the total momentum conservation, and is a consequence of the statistical translation invariance.

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“…We do not consider spin here, and leave this for a future study. See e.g [42] for a recent attempt to constrain the effects of anisotropic non-Gaussianity on galaxy shapes.…”

Section: Adding Spinmentioning

confidence: 99%

Prospects for cosmological collider physics

Meerburg

Münchmeyer

Muñoz

et al. 2017

J. Cosmol. Astropart. Phys.

112

120

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It is generally expected that heavy fields are present during inflation, which can leave their imprint in late-time cosmological observables. The main signature of these fields is a small amount of distinctly shaped non-Gaussianity, which if detected, would provide a wealth of information about the particle spectrum of the inflationary Universe. Here we investigate to what extent these signatures can be detected or constrained using futuristic 21-cm surveys. We construct model-independent templates that extract the squeezed-limit behavior of the bispectrum, and examine their overlap with standard inflationary shapes and secondary non-Gaussianities. We then use these templates to forecast detection thresholds for different masses and couplings using a 3D reconstruction of modes during the dark ages (z ∼ 30 − 100). We consider interactions of several broad classes of models and quantify their detectability as a function of the baseline of a dark ages interferometer. Our analysis shows that there exists the tantalizing possibility of discovering new particles with different masses and interactions with future 21-cm surveys. Contents

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Multitracing anisotropic non-Gaussianity with galaxy shapes

Cited by 68 publications

References 64 publications

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

The Hunt for Primordial Interactions in the Large-Scale Structures of the Universe

An EFT description of galaxy intrinsic alignments

Prospects for cosmological collider physics

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