Anisotropies of galaxy ellipticity correlations in real and redshift space: angular dependence in linear tidal alignment model

Okumura, Teppei; Taruya, Atsushi

doi:10.1093/mnrasl/slaa024

Cited by 34 publications

(35 citation statements)

References 38 publications

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“…When a Fisher matrix is calculated for multiple model parameters, the inverse of this matrix gives the covariance matrix for these parameters. The Fisher matrix for cosmological parameters is given by [20]…”

Section: Fisher Forecast and Resultsmentioning

confidence: 99%

“…In this article, the aim is to show that measuring the correlation between shapes of galaxies and the underlying velocity field of the large scale structure is within the reach of upcoming galaxy surveys. To this end, we predict this correlation relying on the linear alignment model as described in [18,20,21]. Our prediction gives significant results for measuring the signal of the velocity-shape correlation in the data and therefore, we also describe two possible applications of the velocity-shape correlation.…”

Section: Introductionmentioning

confidence: 97%

“…5]. Recently, it has been proposed that there also exists a correlation between the shapes of galaxies and the cosmic velocity field [18,20,21]. This correlation could add information on top of the already measured galaxy density-shape correlation because of the relation between velocity v and the dark matter over-density δ , expressed in Fourier space as…”

Section: Introductionmentioning

confidence: 99%

“…It is furthermore expected that the velocityshape correlation signal is enlarged relative to the densityshape signal on large scales because of the k/k 2 term, in which a small wavenumber k indicates large real space distances. Nbody simulations show that this amplification of the signal is indeed present [18,20,21] and the next step would be to determine whether the velocity-shape correlation signal could be measured with real data. In this article, the aim is to show that measuring the correlation between shapes of galaxies and the underlying velocity field of the large scale structure is within the reach of upcoming galaxy surveys.…”

Section: Introductionmentioning

confidence: 99%

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Prospects for detection and application of the alignment of galaxies with the large-scale velocity field

Gemeren

Chisari

2020

Phys. Rev. D

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Studies of intrinsic alignment effects mostly focus on the correlations between shapes of galaxies with each other, or with the underlying density field of the large scale structure of the universe. Lately, the correlation between shapes of galaxies and the large-scale velocity field has been proposed as an additional probe of the large scale structure. We use a Fisher forecast to make a prediction for the detectability of this velocity-shape correlation with a combination of redshifts and shapes from the 4MOST+LSST surveys, and radial velocity reconstruction from the Simons Observatory. The signal-to-noise ratio for the velocity-shape (dipole) correlation is 23, relative to 44 for the galaxy density-shape (monopole) correlation and for a maximum wavenumber of 0.2 Mpc −1. Increasing signal-to-noise for higher values of the maximum wavenumbers (respectively, 56 and 69, for a maximum wavenumber of 1 Mpc −1) indicate potential gains in the nonlinear regime. Encouraged by these predictions, we discuss two possible applications for the velocity-shape correlation. Measuring the velocity-shape correlation could improve the mitigation of selection effects induced by intrinsic alignments on galaxy clustering. We also find that velocity-shape measurements could potentially aid in determining the scale-dependence of intrinsic alignments when multiple shape measurements of the same galaxies are provided.

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Section: Fisher Forecast and Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Prospects for detection and application of the alignment of galaxies with the large-scale velocity field

Gemeren

Chisari

2020

Phys. Rev. D

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“…Following the convention, we introduce another parameter, A LA , as A LA = C 1 ρ cr /0.0134, where ρ cr is the critical density. The Hankel transform converts the power spectrum into the 3-D GI correlation function Okumura et al 2020):…”

Section: Linear Alignment Modelmentioning

confidence: 99%

First Evidence of Intrinsic Alignments of Red Galaxies at $z > 1$: Cross-correlation between CFHTLenS and FastSound Samples

Tonegawa,

Okumura

2021

Preprint

Self Cite

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We report the first evidence of intrinsic alignment (IA) of red galaxies at z > 1. We measure the gravitational shear-intrinsic ellipticity (GI) cross-correlation function at z ∼ 1.3 using galaxy positions from the FastSound spectroscopic survey and galaxy shapes from Canada-Hawaii-France telescope lensing survey data. Adopting the non-linear alignment model, we obtain a 2.4σ level detection of the IA amplitude, A LA = 27.48 +11.53 −11.54 , larger than the value extrapolated from the constraints obtained at lower redshifts. Our measured IA is translated into a ∼ 20% contamination to the weak lensing power spectrum for the red galaxies. This marginal detection of IA for red galaxies at z > 1 motivates the continuing investigation of the nature of IA for weak lensing studies. Furthermore, our result provides the first step to utilize IA measurements in future high-z surveys as a cosmological probe, complementary to galaxy clustering and lensing.

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Evidence for baryon acoustic oscillations from galaxy–ellipticity correlations

Xu¹,

Jing²,

Zhao³

et al. 2023

Nat Astron

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The baryon acoustic oscillation feature in the clustering of galaxies or quasars provides a ‘standard ruler’ for distance measurements in cosmology. In this work, we report a 2–3σ signal of the baryon acoustic oscillation dip feature in the galaxy density–ellipticity cross-correlation functions using the spectroscopic sample of the Baryon Oscillation Spectroscopic Survey CMASS, combined with the deep Dark Energy Spectroscopic Instrument Legacy Imaging Surveys for precise galaxy shape measurements. We measure the galaxy–ellipticity correlation functions and model them using the linear alignment model. We constrain the distance DV/rd to redshift 0.57 to a precision of 3–5%, depending on the details of modelling. The galaxy–ellipticity measurement reduces the uncertainty of distance measurement by ~10% on top of that derived from the galaxy–galaxy correlation. More importantly, for future large and deep galaxy surveys, the independent galaxy–ellipticity measurements can help sort out the systematics in the baryon acoustic oscillation studies.

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Anisotropies of galaxy ellipticity correlations in real and redshift space: angular dependence in linear tidal alignment model

Cited by 34 publications

References 38 publications

Prospects for detection and application of the alignment of galaxies with the large-scale velocity field

Prospects for detection and application of the alignment of galaxies with the large-scale velocity field

First Evidence of Intrinsic Alignments of Red Galaxies at $z > 1$: Cross-correlation between CFHTLenS and FastSound Samples

Evidence for baryon acoustic oscillations from galaxy–ellipticity correlations

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