BOSS Correlation Function Analysis from the Effective Field Theory of Large-Scale Structure

Zhang, Pierre; D'Amico, Guido; Senatore, Leonardo; Zhao, Cheng; Cai, Yifu

doi:10.48550/arxiv.2110.07539

Cited by 8 publications

(19 citation statements)

References 89 publications

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“…This will allow us to reduce our dependence upon external datasets while retaining tight constraints. Recent constraints [20] from the BOSS correlation function, plus a range of external data, give Ω m = 0.306 ± 0.011 and σ 8 = 0.766 ± 0.055; again in good agreement with our results (and also in agreement with Planck). Finally an analysis of BOSS using an N-body based emulator [18] finds Ω m = 0.300 ± 0.011 and σ 8 = 0.742 ± 0.035; very close to our result.…”

Section: Comparisonsupporting

confidence: 91%

“…[3] for discussion), while other inferences from the thermal Sunyaev-Zeldovich (tSZ; [4]) power spectrum suggest values in good agreement with CMB [5]. Surveys measuring cosmic shear tend to find lower values than high redshift inferences [6][7][8][9][10][11][12] while studies of velocities of galaxies via redshift-space distortions find "low" [13][14][15][16][17][18], "intermediate" [19,20] and "high" [21] results. Earlier analyses of galaxies, clusters and quasars in combination with Planck lensing [22][23][24] found either consistent [22] or lower [25][26][27][28][29][30] clustering amplitudes than expected from CMB, though with low statistical significance.…”

Section: Introductionmentioning

confidence: 99%

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

White,

Zhou,

DeRose

et al. 2021

Preprint

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We use luminous red galaxies selected from the imaging surveys that are being used for targeting by the Dark Energy Spectroscopic Instrument (DESI) in combination with CMB lensing maps from the Planck collaboration to probe the amplitude of large-scale structure over 0.4 ≤ z ≤ 1. Our galaxy sample, with an angular number density of approximately 500 deg −2 over 18,000 sq.deg., is divided into 4 tomographic bins by photometric redshift and the redshift distributions are calibrated using spectroscopy from DESI. We fit the galaxy autospectra and galaxy-convergence cross-spectra using models based on cosmological perturbation theory, restricting to large scales that are expected to be well described by such models. Within the context of ΛCDM, combining all 4 samples and using priors on the background cosmology from supernova and baryon acoustic oscillation measurements, we find S 8 = σ 8 (Ω m /0.3) 0.5 = 0.73 ± 0.03. This result is lower than the prediction of the ΛCDM model conditioned on the Planck data. Our data prefer a slower growth of structure at low redshift than the model predictions, though at only modest significance.

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Section: Comparisonsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

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

White,

Zhou,

DeRose

et al. 2021

Preprint

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“…IV these two models to a compilation of Planck TTTEEE and lensing power spectra, BAO data from BOSS and eBOSS (including Ly-α data), uncalibrated luminosity distance to SN1a from the Pantheon catalogue [154], as well as measurements of the monopole and quadrupole of the galaxy power spectrum for three different sky-cut of BOSS-DR12 (see Ref. [139]), namely LOWZ NGC, CMASS NGC and CMASS SGC [136]. We compared the use of either the BAO/f σ 8 from that same release, or the full shape of the galaxy power spectrum.…”

Section: Discussionmentioning

confidence: 99%

“…LOWZ corresponds to the the BOSS DR12 data including the BAO post-reconstruction for 0.2 < z < 0.43 and has an effective redshift z ef f,LOWZ = 0.32, while CMASS corresponds to the the BOSS DR12 data also including the BAO post-reconstruction for 0.43 < z < 0.7 and has an effective redshift z ef f,CMASS = 0.57 (see Ref. [139]). This data set will be called, in the following, 'EFTofBOSS data'.…”

Section: The Galaxy Power Spectrum From the Eftoflss Formalismmentioning

confidence: 99%

Constraining decaying dark matter with BOSS data and the effective field theory of large-scale structures

Simon,

Abellán,

et al. 2022

Preprint

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We update cosmological constraints on two decaying dark matter models in light of BOSS-DR12 data analyzed under the Effective Field Theory of Large-Scale Structures (EFTofLSS) formalism, together with Planck, Pantheon and other BOSS measurements of the baryonic acoustic oscillation (BAO). In the first model, a fraction f dcdm of cold dark matter (CDM) decays into dark radiation (DR) with a lifetime τ . In the second model (recently suggested as a potential resolution to the S8 tension), all the CDM decays with a lifetime τ into DR and a massive warm dark matter (WDM) particle, with a fraction ε of the CDM rest mass energy transferred to the DR. Using numerical codes from the recent literature, we perform the first calculation of the mildly non-linear (matter and galaxy) power spectra with the EFTofLSS for these two models. In the case of DR products, we obtain the constraints f dcdm 0.022 (95% C.L.) for lifetimes shorter than the age of the universe, and τ /f dcdm 250 Gyr in the long-lived regime assuming f dcdm → 1. We show that Planck data contributes the most to these constraints, with EFTofBOSS providing a marginal improvement over conventional BAO and redshift space distortions (f σ8) data. In the case of DR and WDM decay products, we find that EFTofBOSS data significantly improves the constraints at 68% C.L. on the CDM lifetime with a S8 prior from KiDS-1000. We show that, in order to fit EFTofBOSS data while lowering S8 to match KiDS-1000, the best-fit model has a longer lifetime τ = 120 Gyr, with a larger kick velocity v kick /c ε 1.2%, than that without EFTofBOSS (τ = 43 Gyr, ε = 0.6%). We anticipate that future surveys will provide exquisite constraints on such models.1 More precisely, there even exists a 'lensing is low' anomaly when comparing galaxy clustering and weak lensing data within the ΛCDM cosmology [4][5][6].

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“…The first approach was to use the CMB lensing power spectrum [22]; since this observable is given by a projection of the matter power spectrum, the BAO oscillations average out such that only equality scale information remains. Later approaches [23,24] improved upon these constraints with novel analyses of the full 3D galaxy power spectrum, building on recent advances in modeling and analyzing the galaxy power spectrum, beyond just its oscillatory component [e.g., [25][26][27][28][29][30][31][32][33]. Whilst constraints from standard full-shape analyses remain BAOdominated, [24] successfully removed sound horizon information with a suitable choice of priors (omitting the baryonic information usually provided by Big Bang Nucleosynthesis (BBN) constraints [e.g., 13,28,34,35]); subsequently, [23] proposed and validated a new method to "integrate out" the sound horizon even with BBN priors, resulting in the tightest equality scale H 0 constraints to date.…”

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confidence: 99%

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae

Philcox¹,

Farren²,

Sherwin³

et al. 2022

Preprint

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Many theoretical resolutions to the so-called "Hubble tension" rely on modifying the sound horizon at recombination, rs, and thus the acoustic scale used as a standard ruler in the cosmic microwave background (CMB) and large scale structure (LSS) datasets. As shown in a number of recent works, these observables can also be used to compute rs-independent constraints on H0 by making use of the horizon scale at matter-radiation equality, keq, which has different sensitivity to high redshift physics than rs. In this work, we present the tightest keq-based constraints on the expansion rate from current data, finding H0 = 64.8 +2.2 −2.5 km s −1 Mpc −1 at 68% CL from a combination of BOSS galaxy power spectra, Planck CMB lensing, and the newly released Pantheon+ supernova constraints, as well as physical priors on the baryon density, neutrino mass, and spectral index. The BOSS and Planck measurements have different degeneracy directions, leading to the improved combined constraints, with a bound of H0 = 67.1 +2.5 −2.9 (63.6 +2.9 −3.6 ) from BOSS (Planck ) alone in km s −1 Mpc −1 units. The results show some dependence on the neutrino mass bounds, with the constraint broadening to H0 = 68.0 +2.9 −3.2 km s −1 Mpc −1 if we instead impose a weak prior on mν from terrestrial experiments rather than assuming mν < 0.26 eV, or shifting to H0 = 64.6 ± 2.4 km s −1 Mpc −1 if the neutrino mass is fixed to its minimal value. Even without any dependence on the sound horizon, our results are in ≈ 3σ tension with those obtained from the Cepheid-calibrated distance ladder, providing evidence against new physics models that vary H0 by changing acoustic physics or the expansion history immediately prior to recombination.

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BOSS Correlation Function Analysis from the Effective Field Theory of Large-Scale Structure

Cited by 8 publications

References 89 publications

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

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

Constraining decaying dark matter with BOSS data and the effective field theory of large-scale structures

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae

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