REVIEW 8 cited by
Toward a Better Understanding of Cosmic Chronometers: A new measurement of H(z) at z~0.7
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
We analyze the stellar ages obtained from a combination of Lick indices in Borghi et al. for 140 massive and passive galaxies selected in the LEGA-C survey at $0.6<z<0.9$. From their median age--redshift relation, we derive a new direct measurement of $H(z)$ without any cosmological model assumption using the cosmic chronometer approach. We thoroughly study the main systematics involved in this analysis: the choice of the Lick indices combination, the binning method, the assumed stellar population model, and the adopted star formation history; these effects are included in the total error budget. We obtain $H(z=0.75)= 98.8\pm33.6~\mathrm{km\,s^{-1}\,Mpc^{-1}}$. In parallel, we also propose a simple framework based on a cosmological model to describe the age--redshift relations in the context of galaxy downsizing. This allows us to derive constraints on the Hubble constant $H_0$ and the typical galaxy formation time. This new $H(z)$ measurement, whose accuracy is currently limited by the scarcity of the sample analyzed, paves the road for the joint study of the stellar populations of individual passive galaxies and the expansion history of the Universe in light of future spectroscopic surveys.
Forward citations
Cited by 8 Pith papers
-
Do we really need alternatives to the $\omega_0\omega_a$CDM parameterization after the DESI DR2?
In a common physically motivated pivot basis, the standard CPL parameterization is mildly preferred over the fafbCDM density expansion and reproduces quintessence backgrounds at least as well.
-
Cosmic CORALS: Timing the Universe with high-z star clusters
Star clusters at z=9.6 combined with local globular cluster ages give H0=70(+27,-16) km/s/Mpc and Omega_m=0.33(+0.37,-0.21), with a forecast that ~300 clusters could reach 4% precision.
-
Model-independent late-universe measurements of $H_0$ and $\Omega_K$ with the parametrization based on cosmic age-improved inverse distance ladder
A cosmic-age-based inverse distance ladder with DESI DR2, DESY5, SGL, CC and GRB data gives H0=71.59±0.94 km/s/Mpc and ΩK=0.001±0.038.
-
Investigating the cosmic distance duality relation with gamma-ray bursts
Combined gamma-ray burst and multi-probe data show no significant violation of the cosmic distance duality relation and prefer a Planck-like Hubble constant.
-
Is Dark Energy an Effective Manifestation of Non-equilibrium Thermodynamics? -- Insights from DESI
Two phenomenological dark matter creation rates can reproduce the accelerated expansion of the universe and fit current background data as well as or slightly better than LambdaCDM for some DESI-based data combinations.
-
Late-Time Alleviation of the Hubble Tension in CPL Cosmology with Massive Neutrinos via Bayesian Physics-Informed Neural Networks
A Bayesian PINN fit to late-time distance probes finds that CPL dark energy with free neutrino mass shifts H0 to ~70-71.6 km/s/Mpc and lowers the Hubble tension to ~1-2σ, but the tension measure is partly built in by ...
-
Constraints on Dark Energy Models Using Late Universe Probes
Using late-universe probes only, the authors find all dark energy models remain within 1-2 sigma of Lambda CDM, which wins the Bayesian model comparison, and confirm that DESI's LRG1 and LRG2 points drive the dynamica...
-
A Bayesian PINN Framework for Barrow-Tsallis Holographic Dark Energy with Neutrinos: Toward a Resolution of the Hubble Tension
The fitted Barrow-Tsallis holographic dark energy model gives H0 around 70.5 km/s/Mpc and neutrino mass bounds below 0.114 eV, but the model equation is not actually derived from the claimed entropy, so the central th...
Discussion (0). Sign in to comment.