The effective field theory of large-scale structure and multi-tracer

We present a formalism for jointly fitting pre- and post-reconstruction redshift-space clustering (RSD) and baryon acoustic oscillations (BAO) plus gravitational lensing (of the CMB) that works directly with the observed 2-point statistics. The formalism is based upon (effective) Lagrangian perturbation theory and a Lagrangian bias expansion, which models RSD, BAO and galaxy-lensing cross correlations within a consistent dynamical framework. As an example we present an analysis of clustering measured by the Baryon Oscillation Spectroscopic Survey in combination with CMB lensing measured by Planck. The post-reconstruction BAO strongly constrains the distance-redshift relation, the full-shape redshift-space clustering constrains the matter density and growth rate, and CMB lensing constrains the clustering amplitude. Using only the redshift space data we obtain Ωm = 0.303 ± 0.008, H 0 = 69.21 ± 0.78 and σ 8 = 0.743 ± 0.043. The addition of lensing information, even when restricted to the Northern Galactic Cap, improves constraints to Ωm = 0.303 ± 0.008, H 0 = 69.21 ± 0.77 and σ 8 = 0.707 ± 0.035, in tension with CMB and cosmic shear constraints. The combination of Ωm and H 0 are consistent with Planck, though their constraints derive mostly from redshift-space clustering. The low σ 8 value are driven by cross correlations with CMB lensing in the low redshift bin (z ≃ 0.38) and at large angular scales, which show a 20% deficit compared to expectations from galaxy clustering alone. We conduct several systematics tests on the data and find none that could fully explain these tensions.

Section: Emulatorsmentioning

confidence: 99%

Cosmological analysis of three-dimensional BOSS galaxy clustering and Planck CMB lensing cross correlations via Lagrangian perturbation theory

Chen

White

DeRose

et al. 2022

“…When having two tracers A and B, their auto-spectra will be the same as those defined in the previous section. Nevertheless, the cross-power spectrum will have a different form [47]:…”

Section: Multi-tracer (Mt)mentioning

confidence: 99%

“…As we have motivated in [47], the gains of doing multi-tracer go beyond cosmic variance cancellation in linear scales. We have shown that a real-space FS analysis of MT combined with EFTofLSS outperforms the usual single-tracer (ST) approach, improving the constraints on cosmological parameters with error bars approximately 60% smaller relative to ST.…”

Section: Introductionmentioning

confidence: 99%

“…We also perform a tracer split into two populations following the galaxy's star formation rate (SFR) provided by SHAMe, which is very similar to dividing galaxies by their color [51]. This improvement makes the comparison to galaxy surveys more reliable compared to our previous analysis [47], which focused mainly on halos split by their masses. Moreover, we analyze the dependence of the MT method on the shot noise of the sample and the volume of the box considered, providing projections for MT performance for ongoing and future galaxy surveys.…”

Section: Introductionmentioning

confidence: 99%

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The effective field theory of large-scale structure and multi-tracer II: redshift space and realistic tracers

Mergulhão,

Rubira,

Voivodic

2024

Self Cite

We extend the multi-tracer (MT) formalism of the effective field theory of large-scale structure to redshift space, comparing the results of MT to a single-tracer analysis when extracting cosmological parameters from simulations. We used a sub-halo abundance matching method to obtain more realistic multi-tracer galaxy catalogs constructed from N-body simulations. Considering different values for the sample shot noise and volume, we show that the MT error bars on A s, ω cdm, and h in a full-shape analysis are approximately 50% smaller relative to ST. We find that cosmological and bias coefficients from MT are less degenerate, indicating that the MT parameter basis is more orthogonal. We conclude that using MT combined with perturbation theory is a robust and competitive way to accommodate the information present in the mildly non-linear scales.

“…For a full expression for [35]. For a generalization of the largescale bias expansion to more tracers, see [54]. The two last terms correspond respectively to a term proportional to ∇ 2 δδ ∼ k 2 P lin and the stochastic contribution proportional to k 0 and k 2 .…”

Section: The Large-scale Bias Expansionmentioning

confidence: 99%

Full-shape BOSS constraints on dark matter interacting with dark radiation and lifting the S₈ tension

Rubira

Asmaa

Garny

2023

Self Cite

In this work we derive constraints on interacting dark matter-dark radiation models from a full-shape analysis of BOSS-DR12 galaxy clustering data, combined with Planck legacy cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) measurements. We consider a set of models parameterized within the effective theory of structure formation (ETHOS), quantifying the lifting of the S8 tension in view of KiDS weak-lensing results. The most favorable scenarios point to a fraction f ∼ 10-100% of interacting dark matter as well as a dark radiation temperature that is smaller by a factor ξ ∼ 0.1-0.15 compared to the CMB, leading to a reduction of the tension to the ∼ 1σ level. The temperature dependence of the interaction rate favored by relaxing the S8 tension is realized for a weakly coupled unbroken non-Abelian SU(N) gauge interaction in the dark sector. To map our results onto this SU(N) model, we compute higher-order corrections due to Debye screening. We find a lower bound αd ≡ gd 2/(4π) ≳ 10-8 (10-9) for dark matter mass 1000 (1) GeV for relaxing the S8 tension, consistent with upper bounds from galaxy ellipticities and compatible with self-interactions relevant for small-scale structure formation.