Anisotropic halo assembly bias and redshift-space distortions

Obuljen, Andrej; Dalal, Neal; Percival, Will J.

doi:10.1088/1475-7516/2019/10/020

Cited by 27 publications

(21 citation statements)

References 64 publications

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“…We do not find a degeneracy with 𝑓 𝜎 8 , so the lack of constraint on 𝜎 log 𝑀 and 𝑓 max is not expected to bias our measurement. Numerical simulations have shown that the clustering of dark matter halos can depend on properties other than halo mass, a.k.a halo assembly bias (Sheth & Tormen 2004;Gao et al 2005;Harker et al 2006;Wechsler et al 2006;Obuljen et al 2019). This bias can propagate into the distribution of galaxies that live in these halos and thus introduce additional bias in the clustering measurement.…”

Section: Galaxy-halo Connection Parametersmentioning

confidence: 99%

The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the growth rate of structure from the small-scale clustering of the luminous red galaxy sample

Chapman¹,

Mohammad²,

Zhai³

et al. 2021

Preprint

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We measure the small-scale clustering of the Data Release 16 extended Baryon Oscillation Spectroscopic Survey Luminous Red Galaxy sample, corrected for fibre-collisions using Pairwise Inverse Probability weights, which give unbiased clustering measurements on all scales. We fit to the monopole and quadrupole moments and to the projected correlation function over the separation range 7 − 60 ℎ −1 Mpc with a model based on the cosmological emulator to measure the growth rate of cosmic structure, parameterized by 𝑓 𝜎 8 . We obtain a measurement of 𝑓 𝜎 8 (𝑧 = 0.737) = 0.408 ± 0.038, which is 1.4𝜎 lower than the value expected from 2018 Planck data for a flat ΛCDM model, and is more consistent with recent weak-lensing measurements. The level of precision achieved is 1.7 times better than more standard measurements made using only the large-scale modes of the same sample. We also fit to the data using the full range of scales 0.1 − 60 ℎ −1 Mpc modelled by the cosmological emulator and find a 4.5𝜎 tension in the amplitude of the halo velocity field with the Planck+ΛCDM model, driven by a mismatch on the non-linear scales. This may not be cosmological in origin, and could be due to a breakdown in the Halo Occupation Distribution model used in the emulator. Finally, we perform a robust analysis of possible sources of systematics, including the effects of redshift uncertainty and incompleteness due to target selection that were not included in previous analyses fitting to clustering measurements on small scales.

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Section: Galaxy-halo Connection Parametersmentioning

confidence: 99%

The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the growth rate of structure from the small-scale clustering of the luminous red galaxy sample

Chapman¹,

Mohammad²,

Zhai³

et al. 2021

Preprint

Self Cite

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“…A realistic selection function will smooth the triangle configuration dependence and degrade the constraining power of the bispectrum (Sefusatti & Scoccimarro 2005). Furthermore, galaxy samples selected based on photometric properties can also be impacted by, for instance, the alignment of galaxies to the large-scale tidal fields (Hirata 2009;Krause & Hirata 2011;Martens et al 2018;Obuljen et al 2019). If unaccounted for, this effect can significantly bias the inferred cosmological parameters (Agarwal et al 2020).…”

Section: Forecast Caveatsmentioning

confidence: 99%

Constraining $M_ν$ with the Bispectrum II: The Total Information Content of the Galaxy Bispectrum

Hahn,

Villaescusa-Navarro

2020

Preprint

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Massive neutrinos suppress the growth of structure on small scales and leave an imprint on large-scale structure that can be measured to constrain their total mass, M ν . With standard analyses of two-point clustering statistics, M ν constraints are severely limited by parameter degeneracies. demonstrated that the bispectrum, the next higher-order statistic, can break these degeneracies and dramatically improve constraints on M ν and other cosmological parameters. In this paper, we present the constraining power of the redshift-space galaxy bispectrum, B g 0 . We construct the Molino suite of 75, 000 mock galaxy catalogs from the Quijote N -body simulations using the halo occupation distribution (HOD) model, which provides a galaxy bias framework well-suited for simulation-based approaches. Using these mocks, we present Fisher matrix forecasts for {Ω m , Ω b , h, n s , σ 8 , M ν } and quantify, for the first time, the total information content of the B g 0 down to nonlinear scales. For k max =0.5 h/Mpc, B g 0 improves constraints on Ω m , Ω b , h, n s , σ 8 , and M ν by 2.8, 3.1, 3.8, 4.2, 4.2, and 4.6× over the power spectrum, after marginalizing over HOD parameters. Even with priors from Planck, B g 0 improves all of the cosmological constraints by 2×. In fact, for P g 0 +P g 2 and B g 0 out to k max =0.5 h/Mpc with Planck priors, we achieve a 1σ M ν constraint of 0.048 eV, which is tighter than the current best cosmological constraint. While effects such as survey geometry and assembly bias will have an impact, these constraints are derived for (1 h −1 Gpc) 3 , a substantially smaller volume than upcoming surveys. Therefore, we conclude that the galaxy bispectrum will significantly improve cosmological constraints for upcoming galaxy surveys -especially for M ν .

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“…In [41][42][43][44][45], it is shown that the intrinsic alignments of galaxies induce a selection effect in spectroscopic surveys. Galaxies aligned along the line of sight are more likely to be observed than galaxies aligned perpendicularly to the line of sight.…”

Section: A Mitigating Selection Effects Induced By Intrinsic Alignmementioning

confidence: 99%

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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Anisotropic halo assembly bias and redshift-space distortions

Cited by 27 publications

References 64 publications

The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the growth rate of structure from the small-scale clustering of the luminous red galaxy sample

The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the growth rate of structure from the small-scale clustering of the luminous red galaxy sample

Constraining $M_ν$ with the Bispectrum II: The Total Information Content of the Galaxy Bispectrum

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

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