Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing

White, Martin; Zhou, Rongpu; DeRose, Joseph; Ferraro, Simone; Chen, Shi-Fan; Kokron, Nickolas; Bailey, Stephen; Brooks, David; Garcia-Bellido, Juan; Guy, Julien; Honscheid, Klaus; Kehoe, Robert; Kremin, Anthony; Levi, Michael; Palanque-Delabrouille, Nathalie; Poppett, Claire; Schlegel, David; Tarle, Gregory

doi:10.48550/arxiv.2111.09898

Cited by 13 publications

(20 citation statements)

References 78 publications

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“…This is consistent with the underprediction of 𝑓𝜎 8 between 0 < 𝑧 < 0.75 we discussed in the previous section. A lower value of 𝑆 8 would also be consistent with the most recent measurements by large scale structure experiments (Heymans et al 2021;DES Collaboration et al 2021b;García-García et al 2021;White et al 2021;Krolewski et al 2021), the origin of which could lie on a lower value of Ω 𝑚 (Hang et al 2021).…”

Section: Cosmological Parameterssupporting

confidence: 86%

“…This result is lower than, but statically compatible with, the Planck 2018 (Planck Collaboration et al 2020) cosmology. We also find 𝑆 8 = 0.788 ± 0.029, an intermediate value, statistically compatible with both the Planck 2018 cosmology (Planck Collaboration et al 2020) and recent local measurements from weak lensing and galaxy clustering(DES Collaboration et al 2021b;Heymans et al 2021;García-García et al 2021;Krolewski et al 2021;White et al 2021). …”

supporting

confidence: 88%

“…Riess et al 2021;Freedman et al 2020;Pesce et al 2020) or the density-weighted amplitude of fluctuations, 𝑆 8 ≡ 𝜎 8 (Ω 𝑚 /0.3) 0.5 (e.g. Asgari et al 2021;DES Collaboration et al 2021a;Alsing et al 2017;Nunes & Vagnozzi 2021;Heymans et al 2021;Ruiz-Zapatero et al 2021;García-García et al 2021;White et al 2021), where 𝜎 8 is the variance of 𝛿, in spheres of radius 8 ℎ −1 Mpc.…”

Section: Introductionmentioning

confidence: 99%

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Model-independent constraints on $Ω_m$ and $H(z)$ from the link between geometry and growth

Ruiz-Zapatero,

García-García,

Alonso

et al. 2022

Preprint

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We constrain the expansion history of the Universe and the cosmological matter density fraction in a model-independent way by exclusively making use of the relationship between background and perturbations under a minimal set of assumptions. We do so by employing a Gaussian process to model the expansion history of the Universe from present time to the recombination era. The expansion history and the cosmological matter density are then constrained using recent measurements from cosmic chronometers, Type-Ia supernovae, baryon acoustic oscillations, and redshift-space distortion data. Our results show that the evolution in the reconstructed expansion history is compatible with the Planck 2018 prediction at all redshifts. The current data considered in this study can constrain a Gaussian process on 𝐻 (𝑧) to an average 9.4% precision across redshift. We find Ω 𝑚 = 0.224 ± 0.066, lower but statistically compatible with the Planck 2018 cosmology. Finally, the combination of future DESI measurements with the CMB measurement considered in this work holds the promise of 8% average constraints on a model-independent expansion history as well as a five-fold tighter Ω 𝑚 constraint using the methodology developed in this work.

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Section: Cosmological Parameterssupporting

confidence: 86%

supporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

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Model-independent constraints on $Ω_m$ and $H(z)$ from the link between geometry and growth

Ruiz-Zapatero,

García-García,

Alonso

et al. 2022

Preprint

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“…The use of emulators is becoming commonplace in many forms of cosmological analysis (Chapman et al 2021;Kobayashi et al 2021;Zürcher et al 2021;White et al 2021;. These emulators can be thought of as sophisticated interpolation schemes that aim to approximate a computationally expensive model given a set of example outputs.…”

Section: Introductionmentioning

confidence: 99%

$\texttt{matryoshka}$ II: Accelerating Effective Field Theory Analyses of the Galaxy Power Spectrum

Donald-McCann¹,

Koyama²,

Beutler³

2022

Preprint

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In this paper we present an extension to the matryoshka suite of neural network based emulators. The new editions have been developed to accelerate EFTofLSS analyses of galaxy power spectrum multipoles in redshift space. They are collectively referred to as the EFTEMU. We test the EFTEMU at the power spectrum level and achieve a prediction accuracy of better than 1% with BOSS-like bias parameters and counterterms on scales 0.001 ℎ Mpc −1 𝑘 0.19 ℎ Mpc −1 . We also run a series of mock full shape analyses to test the EFTEMU at the inference level. Through these mock analyses we verify that the EFTEMU recovers the true cosmology within 1𝜎 at several redshifts (𝑧 = [0.38, 0.51, 0.61]), and with several noise levels (the most stringent of which being a Gaussian covariance associated with a volume of 5000 3 Mpc 3 ℎ −3 ). We compare mock inference results from the EFTEMU to those obtained with a fully analytic EFTofLSS model and again find no significant bias, whilst speeding up the inference by three orders of magnitude. The EFTEMU is publicly available as part of the matryoshka Python package https://github.com/JDonaldM/Matryoshka.

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“…Moreover, it is a powerful tool to break degeneracies between cosmological parameters, such as the one between the matter fraction Ω m and the amplitude of galaxy clustering measured on spheres of comoving radius R = 8/h Mpc, namely σ 8 , and also bypass the cosmic variance limited by the survey volume [8]. Already at the power spectrum level, cross-correlation analyses are expected to boost constraints on new physics such as neutrino mass, primordial non-Gaussianity and shed light on existing cosmological tensions, such as the clustering of the LSS and the value of the Hubble parameter [9][10][11][12][13][14][15].…”

Section: Introductionmentioning

confidence: 99%

Skewing the CMB$\times$LSS: a Fast Method for Bispectrum Analysis

Chakraborty,

Chen,

Dvorkin

2022

Preprint

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Upcoming cosmic microwave background (CMB) lensing measurements and tomographic galaxy surveys are expected to provide us with high-precision data sets in the coming years, thus paving the way for fruitful cross-correlation analyses. In this paper we study the information content of the weighted skew-spectrum, a nearly-optimal estimator of the angular bispectrum amplitude, as a means to extract non-Gaussian information on both bias and cosmological parameters from the bispectra of galaxies cross-correlated with CMB lensing, while gaining significantly on speed. Our results suggest that for the combination of Planck satellite and the Dark Energy Spectroscopic Instrument (DESI), the skew-spectrum achieves almost equivalent information for both bias and cosmological parameters as the bispectrum, where the difference in the constraints is at most 17%. We further compare and find agreement between our theoretical skew-spectra and those estimated from N-body simulations, and show that it is crucial to include gravitational non-linearities beyond perturbation theory and the post-Born effect for CMB lensing. We define an algorithm to apply the skew-spectrum estimator to the data and, as a preliminary step, we use the skew-spectra to constrain bias parameters and the amplitude of shot noise from the simulations through a Markov chain Monte Carlo likelihood analysis, finding that it may be possible to reach percent-level estimates for the linear bias parameter b 1 .

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Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing

Cited by 13 publications

References 78 publications

Model-independent constraints on $Ω_m$ and $H(z)$ from the link between geometry and growth

Model-independent constraints on $Ω_m$ and $H(z)$ from the link between geometry and growth

$\texttt{matryoshka}$ II: Accelerating Effective Field Theory Analyses of the Galaxy Power Spectrum

Skewing the CMB$\times$LSS: a Fast Method for Bispectrum Analysis

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