Constraints on CDM cosmology from galaxy power spectrum,  CMB and SNIa evolution

Ferramacho, L.; Blanchard, Alain; Zolnierowski, Y.

doi:10.1051/0004-6361/200810693

Cited by 26 publications

(37 citation statements)

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“…This value is in quite good agreement with that provided by a variety of different methods; for example, an analysis based on cluster abundances gave the degenerate combination: σ 8,Λ = (0.83 ± 0.03) (Ω 0 m /0.25) −0.41 [69]. The weak-lensing analysis of Fu et al [70] provided σ 8,Λ = (0.837 ± 0.084) (Ω 0 m /0.25) −0.53 , while two recent studies based on a joint analysis of the large-scale clustering of red SDSS galaxies, CMB, SNIa and BAO data resulted in: σ 8,Λ ≃ 0.8 ± 0.02 (for Ω 0 m ≃ 0.26) [71,72]. The only method that provides discrepant results is that based on galaxy or cluster peculiar velocities [73,74].…”

Section: Collapse Threshold and Mass Variance Of The Running Vacuum Mmentioning

confidence: 99%

Hubble expansion and structure formation in the ``running FLRW model'' of the cosmic evolution

Grande

Solà

Basilakos

et al. 2011

J. Cosmol. Astropart. Phys.

111

159

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A new class of Friedmann-Lemaître-Robertson-Walker (FLRW) cosmological models with time-evolving fundamental parameters should emerge naturally from a description of the expansion of the universe based on the first principles of quantum field theory and string theory. Within this general paradigm, one expects that both the gravitational Newton's coupling G and the cosmological term Λ should not be strictly constant but appear rather as smooth functions of the Hubble rate H(t). This scenario ("running FLRW model") predicts, in a natural way, the existence of dynamical dark energy without invoking the participation of extraneous scalar fields. In this paper, we perform a detailed study of some of these models in the light of the latest cosmological data, which serves to illustrate the phenomenological viability of the new dark energy paradigm as a serious alternative to the traditional scalar field approaches. By performing a joint likelihood analysis of the recent supernovae type Ia data (SNIa), the Cosmic Microwave Background (CMB) shift parameter, and the Baryonic Acoustic Oscillations (BAOs) traced by the Sloan Digital Sky Survey (SDSS), we put tight constraints on the main cosmological parameters. Furthermore, we derive the theoretically predicted dark-matter halo mass function and the corresponding redshift distribution of cluster-size halos for the "running" models studied. Despite the fact that these models closely reproduce the standard ΛCDM Hubble expansion, their normalization of the perturbation's power-spectrum varies, imposing, in many cases, a significantly different cluster-size halo redshift distribution. This fact indicates that it should be relatively easy to distinguish between the "running" models and the ΛCDM using realistic future X-ray and Sunyaev-Zeldovich cluster surveys.

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Section: Collapse Threshold and Mass Variance Of The Running Vacuum Mmentioning

confidence: 99%

Hubble expansion and structure formation in the ``running FLRW model'' of the cosmic evolution

Grande

Solà

Basilakos

et al. 2011

J. Cosmol. Astropart. Phys.

111

159

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“…Obviously, SN progenitors in host galaxies are getting younger with redshift, and several investigators had some doubts on the assumption of no luminosity evolution in SN cosmology although they were not based on observational evidence (e.g., Drell et al 2000;Ferramacho et al 2009; Linden et al…”

Section: Introductionmentioning

confidence: 99%

Early-type Host Galaxies of Type Ia Supernovae. II. Evidence for Luminosity Evolution in Supernova Cosmology

Kang

Lee

Kim

et al. 2020

ApJ

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The most direct and strongest evidence for the presence of dark energy is provided by the measurement of galaxy distances using SNe Ia. This result is based on the assumption that the corrected brightness of SN Ia through the empirical standardization would not evolve with look-back time. Recent studies have shown, however, that the standardized brightness of SN Ia is correlated with host morphology, host mass, and local star formation rate (SFR), suggesting a possible correlation with stellar population property. To understand the origin of these correlations, we have continued our spectroscopic observations to cover most of the reported nearby early-type host galaxies. From high-quality (signal-to-noise ratio ∼175) spectra, we obtained the most direct and reliable estimates of population age and metallicity for these host galaxies.We find a significant correlation between SN luminosity (after the standardization) and stellar population age at a 99.5% confidence level. As such, this is the most direct and stringent test ever made for the luminosity evolution of SN Ia. Based on this result, we further show that the previously reported correlations with host morphology, host mass, and local SFR are most likely originated from the difference in population age.This indicates that the light-curve fitters used by the SNe Ia community are not quite capable of correcting for the population age effect, which would inevitably cause a serious systematic bias with look-back time. Notably, taken at face values, most of the Hubble residual used in the discovery of the dark energy appears to be affected by the luminosity evolution. ). According to the analysis by Childress et al. (2014), the difference in the mean age of SN progenitors between z = 0 and 1.0 is predicted to be ∼5.3 Gyr (see also Section 4 below). It is therefore possible that SNe at high redshift are fainter (after the standardization) than the value expected from the model without the dark energy, not because of the dark energy, but mostly because of the luminosity evolution. Careful investigation of this possible systematic bias with redshift is particularly important because the dimming of SNe is only ∼0.2 mag (∼20% in brightness) with respect to a cosmological model without dark energy (Ω M = 0.27, Ω Λ = 0.00; Hicken et al. 2009).Nevertheless, to test the effect of luminosity evolution, in the discovery papers, Riess et al. (1998), Schmidt et al. (1998), and Perlmutter et al. (1999 only used morphological classification of host galaxies in the local universe as a proxy for stellar population age. Because of apparently very small difference in the standardized brightness between SNe Ia in the early-type and late-type host galaxies, they concluded that the luminosity evolution is negligible in SN cosmology. Later analysis based on a larger sample by Hicken et al. (2009), however, found a systematic difference of ∼0.14 mag between the very early-and very late-type galaxies (see also Suzuki et al. 2012). Recent investigations of host galaxies further found a co...

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“…Different phenomenological models for ∆m evo (z) can be found in the literature (see for example Drell et al 2000;Linder 2006;Nordin et al 2008;Ferramacho et al 2009;Linden et al 2009). …”

Section: Type Ia Supernovaementioning

confidence: 99%

Is cosmic acceleration proven by local cosmological probes?

Tutusaus

Lamine

Dupays

et al. 2017

A&A

Self Cite

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Context. The cosmological concordance model (ΛCDM) matches the cosmological observations exceedingly well. This model has become the standard cosmological model with the evidence for an accelerated expansion provided by the type Ia supernovae (SNIa) Hubble diagram. However, the robustness of this evidence has been addressed recently with somewhat diverging conclusions. Aims. The purpose of this paper is to assess the robustness of the conclusion that the Universe is indeed accelerating if we rely only on low-redshift (z 2) observations, that is to say with SNIa, baryonic acoustic oscillations, measurements of the Hubble parameter at different redshifts, and measurements of the growth of matter perturbations. Methods. We used the standard statistical procedure of minimizing the χ 2 function for the different probes to quantify the goodness of fit of a model for both ΛCDM and a simple nonaccelerated low-redshift power law model. In this analysis, we do not assume that supernovae intrinsic luminosity is independent of the redshift, which has been a fundamental assumption in most previous studies that cannot be tested. Results. We have found that, when SNIa intrinsic luminosity is not assumed to be redshift independent, a nonaccelerated low-redshift power law model is able to fit the low-redshift background data as well as, or even slightly better, than ΛCDM. When measurements of the growth of structures are added, a nonaccelerated low-redshift power law model still provides an excellent fit to the data for all the luminosity evolution models considered. Conclusions. Without the standard assumption that supernovae intrinsic luminosity is independent of the redshift, low-redshift probes are consistent with a nonaccelerated universe.

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Constraints on CDM cosmology from galaxy power spectrum, CMB and SNIa evolution

Cited by 26 publications

References 50 publications

Hubble expansion and structure formation in the ``running FLRW model'' of the cosmic evolution

Hubble expansion and structure formation in the ``running FLRW model'' of the cosmic evolution

Early-type Host Galaxies of Type Ia Supernovae. II. Evidence for Luminosity Evolution in Supernova Cosmology

Is cosmic acceleration proven by local cosmological probes?

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