The integrated perturbation theory for cosmological tensor fields I: Basic formulation

Matsubara, Takahiko

doi:10.48550/arxiv.2210.10435

“…In this paper we worked with a simple extension of the NLA model to include partly the FoG effect (T. Okumura et al 2023, in preparation). However, more sophisticated nonlinear models of IA statistics have been proposed recently (Blazek et al 2019;Vlah et al 2020;Akitsu et al 2021;Matsubara 2022). These models enable us to use the measured IA correlation functions down to smaller scales, which will enhance the science return from IA of galaxies.…”

Section: Discussionmentioning

confidence: 99%

First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70

Okumura

¹

,

Taruya

²

2023

ApJL

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We report the first constraints on the growth rate of the universe, f(z)σ 8(z), with intrinsic alignments (IAs) of galaxies. We measure the galaxy density-intrinsic ellipticity cross-correlation and intrinsic ellipticity autocorrelation functions over 0.16 < z < 0.7 from luminous red galaxies (LRGs) and LOWZ and CMASS galaxy samples in the Sloan Digital Sky Survey (SDSS) and SDSS-III BOSS survey. We detect clear anisotropic signals of IA due to redshift-space distortions. By combining measured IA statistics with the conventional galaxy clustering statistics, we obtain tighter constraints on the growth rate. The improvement is particularly prominent for the LRG, which is the brightest galaxy sample and known to be strongly aligned with underlying dark matter distribution; using the measurements on scales above 10 h −1 Mpc, we obtain f σ 8 = 0.5196 − 0.0354 + 0.0352 (68% confidence level) from the clustering-only analysis and f σ 8 = 0.5322 − 0.0291 + 0.0293 with clustering and IA, meaning 19% improvement. The constraint is in good agreement with the prediction of general relativity, f σ 8 = 0.4937 at z = 0.34. For LOWZ and CMASS samples, the improvement of constraints on f σ 8 is found to be 10% and 3.5%, respectively. Our results indicate that the contribution from IA statistics for cosmological constraints can be further enhanced by carefully selecting galaxies for a shape sample.

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“…In this paper we worked with a simple extension of the NLA model to include partly the FoG effect. However, more sophisticated nonlinear models of IA statistics have been proposed recently (Blazek et al 2019;Vlah et al 2020;Akitsu et al 2021;Matsubara 2022). These models enable us to use the measured IA correlation functions down to smaller scales, which will enhance the science return from IA of galaxies.…”

Section: Discussionmentioning

confidence: 99%

First Constraints on Growth Rate from Redshift-Space Ellipticity Correlations of SDSS Galaxies at $0.16 < z < 0.70$

Okumura¹,

Taruya²

2023

Preprint

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We report the first constraints on the growth rate of the universe, f (z)σ 8 (z), with intrinsic alignments (IA) of galaxies. We measure the galaxy density-intrinsic ellipticity cross-correlation and intrinsic ellipticity auto-correlation functions over 0.16 < z < 0.7 from luminous red galaxies (LRG) and LOWZ and CMASS galaxy samples in the Sloan Digital Sky Survey (SDSS) and SDSS-III BOSS survey. We detect clear anisotropic signals of IA due to redshift-space distortions. By combining measured IA statistics with the conventional galaxy clustering statistics, we obtain tighter constraints on the growth rate. The improvement is particularly prominent for the LRG, which is the brightest galaxy sample and known to be strongly aligned with underlying dark matter distribution; we obtain f σ 8 = 0.5297 +0.0310 −0.0316 (68% C.L.) from the clustering-only analysis and f σ 8 = 0.4871 +0.0218 −0.0222 with clustering and IA, meaning 24% improvement. The constraint is in good agreement with the prediction of general relativity, f σ 8 = 0.4937 at z = 0.34. For LOWZ and CMASS samples, the improvement by adding the IA statistics is found to be 9% and 2%, respectively. Our results indicate that the contribution from IA statistics for cosmological constraints can be further enhanced by carefully selecting galaxies for a shape sample.

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“…[34] in the context of super-sample responses and, while this work was in the early stages of preparation, refs. [35][36][37] appeared which detailed the formal construction of a Lagrangian theory of shapes within the Lagrangian integrated perturbation theory (iPT) -however to our knowledge we are the first to explicitly construct the necessary bias expansion of shapes up to 1-loop in perturbation theory, including effective-theory corrections, and compute summary statistics within a resummation scheme that respects Galilean invariance. The paper is structured as follows: in section 2 we formulate the bias expasion of shapes in terms of Lagrangian displacements, describe their behavior under advection, and relate the resulting contributions to previous results in the literature.…”

Section: Jcap01(2024)027mentioning

confidence: 99%

“…is the pairwise distortion in redshift space. Calculating the power spectrum in redshift space is then equivalent to boosting the pairwise-displacement and bias operator correlators we have already computed at each order n with the matrix R (n) ij , though we caution that the resulting angular integrals will be slightly more complicated than in this work [29,56] -the resulting power spectra will now only be symmetric about rotations about the line-of-sight and thus require a different tensor basis [35][36][37]. Alternatively the displacements can be perturbatively expanded to yield a moment expansion in the velocities, also known as the distribution function approach to redshift-space distortions [38,56,57].…”

Section: Jcap01(2024)027mentioning

confidence: 99%

A Lagrangian theory for galaxy shape statistics

Chen,

Kokron

2024

J. Cosmol. Astropart. Phys.

6

0

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We formulate the Lagrangian perturbation theory of galaxy intrinsic alignments and compute the resulting auto and cross power spectra of galaxy shapes, densities and matter to 1-loop order. Our model represents a consistent effective-theory description of galaxy shape including the resummation of long-wavelength displacements which damp baryon acoustic oscillations, and includes one linear, three quadratic and two cubic dimensionless bias coefficients at this order, along with counterterms and stochastic contributions whose structure we derive. We compare this Lagrangian model against the three-dimensional helicity spectra of halo shapes measured in N-body simulations by ref. [1] and find excellent agreement on perturbative scales while testing a number of more restrictive bias parametrizations. The calculations presented are immediately relevant to analyses of both cosmic shear surveys and spectroscopic shape measurements, and we make a fast FFTLog-based code spinosaurus publicly available at https://github.com/sfschen/spinosaurus.

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The integrated perturbation theory for cosmological tensor fields I: Basic formulation

Cited by 4 publications

References 62 publications

First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70

First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70

First Constraints on Growth Rate from Redshift-Space Ellipticity Correlations of SDSS Galaxies at $0.16 < z < 0.70$

A Lagrangian theory for galaxy shape statistics

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