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The growth rate of cosmic structures in the local Universe with the ALFALFA survey

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arxiv 2105.10583 v1 pith:W75E7FIJ submitted 2021-05-21 astro-ph.CO

F. Avila , A. Bernui , E. de Carvalho , C. P. Novaes This is my paper · ORCID
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keywords alfalfagrowthlocalratesigmastructuresvelocitymeasurement
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abstract

We investigate the growth rate of structures in the local Universe. For this, we use as a cosmological tracer the HI line extra-galactic sources from the Arecibo Legacy Fast ALFA (ALFALFA) survey to obtain a measurement of the normalized growth rate parameter, $f \sigma_{8}$, considered a powerful tool to constrain alternative models of gravity. For these analyses, we calculate the Local Group velocity due to the matter structures distribution in the ALFALFA catalogue and compare it with the Local Group velocity relative to the Cosmic Microwave Background frame to obtain the velocity scale parameter, $\beta$. Using Monte Carlo realizations and log-normal simulations, our methodology quantifies the errors introduced by shot-noise and partial sky coverage of the analysed data. The measurement of the velocity scale parameter $\beta$, and the calculation of the matter fluctuation of the cosmological tracer, $\sigma_{8}^{\text{tr}}$, lead us to $f \sigma_{8} = 0.46 \pm 0.06$ at $\bar{z} = 0.013$, in good agreement (at $1 \sigma$ level) with the value expected in the $\Lambda$CDM concordance model. In addition, our analyses of the ALFALFA sample also provide a measurement of the growth rate of structures $f \,=\, 0.56 \pm 0.07$, at $\bar{z} = 0.013$.

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Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Testing Scale-Dependent Suppression of Structure Growth in the Linear Regime

    astro-ph.CO 2026-08 conditional novelty 5.0 of 10

    A combined fit of galaxy-growth, supernova, and CMB data finds at most a weak 2.2σ hint for scale-dependent suppression of structure growth, with an inconclusive Bayes factor.

  2. Signatures of Modified Gravity on Linear Scales in a Dynamical Dark Energy Background

    astro-ph.CO 2026-05 unverdicted novelty 5.0 of 10

    Using Planck, DESI, supernovae, and redshift-space distortions, the authors infer that modified gravity, if present, must act only below ~30 Mpc and cannot modify the large scales previously considered.

  3. Illustrating the consequences of a misuse of $\sigma_8$ in cosmology

    astro-ph.CO 2025-01 accept novelty 5.0 of 10

    Cosmologists should compare clustering amplitude with the h-independent statistic sigma_12 instead of sigma_8, because sigma_8's smoothing scale shifts with H0 and artificially worsens the growth tension in high-H0 models.

  4. Composite Dark Energy and the Cosmological Tensions

    astro-ph.CO 2024-12 conditional novelty 5.0 of 10

    A composite dark energy with negative-energy phantom matter before z≈1.5 and quintessence afterward improves the fit over ΛCDM by ΔAIC≈60 and resolves both tensions with BAO 2D, but not with BAO 3D.

  5. Is $\omega_0 \omega_a$CDM a good model for the clumpy Universe?

    astro-ph.CO 2025-07 reject novelty 4.0 of 10

    Against a Gaussian-process reconstruction of 15 sigma8(z) measurements, the DESI w0waCDM model fits slightly better than LambdaCDM, but the difference is tiny and the comparison metric is biased.

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