Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 1901.06854

Extracting the BAO scale from BOSS DR12 dataset

Eugenio Noda·Marco Peloso·Massimo Pietroni
View original source ↗Read source document ↗Export metadata ↓

Abstract

We present the first application to real data from the BOSS DR12 dataset of the Extractor procedure to determine the acoustic scale imprinted on Baryonic Acoustic Oscillations (BAO). We show that, being largely insensitive to the broadband shape of the Power Spectrum, this procedure requires a lower number of nuisance parameters than those used by the BOSS collaboration, For non-reconstructed data our analysis improves the accuracy on the acoustic scale by about 20 %, while for reconstructed ones we get essentially the same level of accuracy as the BOSS analysis.

Explore related subjects

astro-ph.CO

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Eugenio Noda, Marco Peloso, Massimo Pietroni. 2020-05-01. Extracting the BAO scale from BOSS DR12 dataset. https://arxiv.org/abs/1901.06854

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Cosmological Constraints from Full-Scale Clustering and Galaxy-Galaxy Lensing with DESI DR1

We present constraints on cosmic structure growth from the analysis of galaxy clustering and galaxy--galaxy lensing with galaxies from the Dark Energy Spectroscopic Instrument (DESI) Data Release 1. Our analysis includes four samples drawn from the Bright Galaxy Survey (BGS) and the Luminous Red Galaxy (LRG) target classes. Projected galaxy clustering measurements from DESI are supplemented with lensing data from the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and the Hyper Suprime-Cam (HSC) survey around the same targets. Our method relies on a simulation-based modeling framework using the AbacusSummit simulations and a complex halo occupation distribution model that incorporates assembly bias. We analyze scales down to $0.4 \, h^{-1} \, \mathrm{Mpc}$ for clustering and $2.5 \, h^{-1} \, \mathrm{Mpc}$ for lensing, leading to stringent constraints on $S_8 = σ_8 \sqrt{Ω_\mathrm{m} / 0.3}$ and $Ω_\mathrm{m}$ when fixing other cosmological parameters to those preferred by the CMB. We find $S_8 = 0.797_{-0.024}^{+0.023}$ and $Ω_\mathrm{m} = 0.292 \pm 0.011$ when using lensing measurements from DES and KiDS. Similarly, for HSC, we find $S_8 = 0.791_{-0.021}^{+0.020}$ and $Ω_\mathrm{m} = 0.300 \pm 0.009$ when assuming the best-fit photometric redshift offset suggested by the HSC collaboration. Overall, our results are in good agreement with other results in the literature while continuing to highlight the constraining power of non-linear scales.

astro-ph.CO↗
arXiv2026

The FLAMINGO Project: Exploring the X-ray--cosmic-shear cross-correlation as a probe of large-scale structure

Baryonic feedback processes associated with galaxy formation directly influence the large-scale structure by redistributing gas. Recent measurements of the kinetic Sunyaev-Zel'dovich (kSZ) effect and eROSITA stacks of X-ray emission from optically-selected galaxy clusters suggest that feedback from Active Galactic Nuclei (AGN) is more efficient at expelling gas from low-mass clusters than previously thought. The measurement of the cross-correlation between cosmic shear and diffuse X-ray emission provides a new probe of the distribution of gas in groups and clusters. We use the FLAMINGO cosmological, hydrodynamical simulations to examine the X-ray--cosmic-shear cross-correlation. The cross-correlation is most sensitive to the distribution of gas in haloes with masses $10^{14}\leq M_{200\mathrm{c}}/\mathrm{M}_{\odot}\leq10^{15}$. It is sensitive to the strength of feedback, but the effects of variations in cosmology and baryonic physics are largely degenerate. We compare the FLAMINGO predictions with the cross-correlation between cosmic shear from the Dark Energy Survey and the ROSAT all-sky X-ray map. We account for AGN that would remain unresolved by ROSAT using either the direct FLAMINGO predictions or by abundance matching to the observed (extrapolated) AGN luminosity function. We find that the fiducial FLAMINGO model is in excellent agreement with the ROSAT--DES-Y3 cross-correlation, while models assuming weaker feedback and models with the significantly stronger feedback suggested by kSZ and eROSITA stacks are both incompatible with the observed X-ray--cosmic-shear cross-correlation.

astro-ph.CO↗
arXiv2026

Parameterizations of the Hubble Constant from the Binned Type Ia Supernova Master Sample: Logarithmic versus Power-law Forms

Motivated by the Hubble tension and the increasing debate about the redshift-dependency in the inferred Hubble constant, we investigate its dependence within the flat $Λ$CDM framework using a 20-bin analysis of the Master Supernovae type Ia (SNe Ia) Sample, considering cases with and without very low-redshift data. The main quantity studied is $H_0(z)/H_0$, where $H_0$ is the Hubble constant today, and $H_0(z)$ is the binned data-driven estimate of the value of $H_0$ inferred from the SNe Ia data within redshift intervals at $z > 0$, such that $H_0(0) = H_0$. From the binned analyses, we obtain best-fitting values of $H_0$ and $Ω_{m0}$, and employ logarithmic and power-law parameterizations, which are statistically consistent within uncertainties over the redshift range considered. To assess their behavior at earlier epochs, we extrapolate both forms to the Cosmic Microwave Background radiation (CMB) era ($z\simeq1100$), Big Bang Nucleosynthesis (BBN, $z\sim10^{9}$), and inflationary scales ($z\sim10^{20}$). The reconstructed Hubble constant remains nearly indistinguishable up to the CMB scale, diverges at the few-to-ten percent level around BBN, and differs more substantially when extrapolated to inflationary redshifts, though these two regimes lie beyond the direct observational constraints. A distinct asymptotic behavior emerges at very-high redshift: the logarithmic form exhibits a vanishing behaviour of $H_0$ at finite $z$, while the power-law form approaches zero asymptotically as $z \rightarrow \infty$. In future studies, independent high-redshift observations and extensions beyond $Λ$CDM, such as $f(R)$ modified gravity, could allow a comparative study of the two parameterizations beyond the SNe Ia regime and their high-$z$ physical implications.

astro-ph.CO↗