Cosmological constraints on the gas depletion factor in galaxy clusters

Holanda, R. F. L.; Busti, V. C.; González, Javier Elvira; Andrade-Santos, Felipe; Alcaniz, J. S.

doi:10.1088/1475-7516/2017/12/016

Cited by 23 publications

(37 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The parameter γ(z) corresponds to the depletion factor, i.e., the rate by which the hot gas fraction measured in a galaxy cluster is depleted with respect to the baryon fraction universal mean. A self-consistent observational estimate of γ(z) was recently obtained in [37], i.e., γ = 0.84±0.084 (1σ), where no evidence for redshift evolution was found, in agreement with the results of simulations reported in [38]. We adopt this value of γ in our analysis.…”

Section: Methodssupporting

confidence: 84%

An estimate of the dark matter density from galaxy clusters and supernovae data

Holanda

Gonçalves

González

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

View full text Add to dashboard Cite

Model-independent estimates of cosmological quantities are a challenge for observational cosmology. In this paper, we discuss a model-independent way to obtain the present dark matter density parameter (Ωc,0) by combining gas mass fraction measurements in galaxy clusters (fgas), type Ia supernovae (SNe Ia) observations and measurements of the cosmic baryon abundance from observations of absorption systems at high redshifts. Our estimate is Ωc,0 = 0.241 ± 0.012 (1σ). By considering the latest local measurement of the Hubble constant, H0 = 74.03 ± 1.42 (1σ), we obtain ΩM,0 = 0.282 ± 0.012 (1σ) for the total matter density parameter. We also investigate departures of the evolution of the dark matter density with respect to the usual a −3 scaling, as usual in interacting models of dark matter and dark energy. As the current data cannot confirm or rule out such an interaction, we perform a forecast analysis to estimate the necessary improvements in number and accuracy of upcoming fgas and SNe Ia observations to detect a possible non-minimal coupling in the cosmological dark sector. 95.36.+x, 98.80.Es

show abstract

Section: Methodssupporting

confidence: 84%

An estimate of the dark matter density from galaxy clusters and supernovae data

Holanda

Gonçalves

González

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

View full text Add to dashboard Cite

show abstract

“…This mathematical approach has been successfully used as a nonparametric reconstruction method in cosmology since the pioneering works of [46,47]. For instance, it has been applied to different datasets in order to calculate the dark energy equation of state [46][47][48][49], the Hubble constant [39,[50][51][52], the cosmological matter perturbations [53][54][55], and the gas deplection factor in galaxy clusters [56], among others.…”

Section: Gaussian Processesmentioning

confidence: 99%

Null test for interactions in the dark sector

et al. 2019

View full text Add to dashboard Cite

Since there is no known symmetry in Nature that prevents a non-minimal coupling between the dark energy (DE) and cold dark matter (CDM) components, such a possibility constitutes an alternative to standard cosmology, with its theoretical and observational consequences being of great interest. In this paper we propose a new null test on the standard evolution of the dark sector based on the time dependence of the ratio between the CDM and DE energy densities which, in the standard ΛCDM scenario, scales necessarily as a −3 . We use the latest measurements of type Ia supernovae, cosmic chronometers and angular baryonic acoustic oscillations to reconstruct the expansion history using model-independent Machine Learning techniques, namely, the Linear Model formalism and Gaussian Processes. We find that while the standard evolution is consistent with the data at 3σ level, some deviations from the ΛCDM model are found at low redshifts, which may be associated with the current tension between local and global determinations of H0.

show abstract

“…Type Ia SNe (from Union 2.1 and JLA compilation) and CDM model. They obtained γ 0 = 0.86 ± 0.04 and γ 1 = −0.04 ± 0.12 [18]. Therefore, their analysis showed no evolution of the gas depletion factor with redshift.…”

Section: Introductionmentioning

confidence: 92%

“…So the study of gas depletion factor and it's evolution with redshift play a pivotal role in the robustness of the f gas test. As argued in [18], the results for the gas depletion factor obtained using only the data could then be used as a prior for any cosmology studies with f gas .…”

Section: Introductionmentioning

confidence: 99%

“…We note that all these aforementioned simulations assumed CDM as the base cosmological model. Holanda et al [18] made the first attempt to study the gas depletion factor using only observations. They carried out an analysis using 40 f gas measurements [16] observed by the Chandra X-ray telescope spanning the redshift range 0.078 z 1.063 characterized as massive, morphologically relaxed systems and with kT 5 keV.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A model-independent test of the evolution of gas depletion factor for SPT-SZ and Planck ESZ clusters

Bora

Desai

2021

Eur. Phys. J. C

View full text Add to dashboard Cite

The gas mass fraction in galaxy clusters has been widely used to determine cosmological parameters. This method assumes that the ratio of the cluster gas mass fraction to the cosmic baryon fraction ($$\gamma (z)$$ γ ( z ) ) is constant as a function of redshift. In this work, we look for a time evolution of $$\gamma (z)$$ γ ( z ) at $$R_{500}$$ R 500 by using both the SPT-SZ and Planck Early SZ (ESZ) cluster data, in a model-independent fashion without any explicit dependence on the underlying cosmology. For this calculation, we use a non-parametric functional form for the Hubble parameter obtained from Gaussian Process regression using cosmic chronometers. We parameterize $$\gamma (z)$$ γ ( z ) as: $$\gamma (z)= \gamma _0(1+\gamma _1 z)$$ γ ( z ) = γ 0 ( 1 + γ 1 z ) to constrain the redshift evolution. We find contradictory results between both the samples. For SPT-SZ, $$\gamma (z)$$ γ ( z ) decreases as a function of redshift (at more than 5$$\sigma $$ σ ), whereas a positive trend with redshift is found for Planck ESZ data (at more than 4$$\sigma $$ σ ). We however find that the $$\gamma _1$$ γ 1 values for a subset of SPT-SZ and Planck ESZ clusters between the same redshift interval agree to within $$1\sigma $$ 1 σ . When we allow for a dependence on the halo mass in the evolution of the gas depletion factor, the $$4-5\sigma $$ 4 - 5 σ discrepancy reduces to $$2\sigma $$ 2 σ .

show abstract

Cosmological constraints on the gas depletion factor in galaxy clusters

Cited by 23 publications

References 44 publications

An estimate of the dark matter density from galaxy clusters and supernovae data

An estimate of the dark matter density from galaxy clusters and supernovae data

Null test for interactions in the dark sector

A model-independent test of the evolution of gas depletion factor for SPT-SZ and Planck ESZ clusters

Contact Info

Product

Resources

About