Testing a Sign-Switch Cosmological Model with Curvature through Latest Planck 2018, DESI DR2 and PantheonPlus\&SH0ES Observational Data

Abstract

We investigate the spatial geometry of the Universe within the framework of a sign-switch dark energy scenario by extending the recently proposed ${\Lambda }_{\mathrm{s}}$CDM model to include a free curvature parameter ${\Omega }_k$.In this framework, the effective cosmological constant undergoes a transition from a negative to a positive value at a characteristic redshift $z_{†}$. Using the latest Planck 2018 cosmic microwave background (CMB) data, DESI DR2 baryon acoustic oscillation (BAO) measurements, and the PantheonPlus\&SH0ES Type Ia supernova sample, we derive joint constraints on the spatial curvature parameter ${\Omega }_k$ and other cosmological parameters. We find that Planck data itself slightly favors a closed universe within both the ${\Lambda }_{\mathrm{s}}$CDM$+{\Omega }_k$ and $\Lambda$CDM$+{\Omega }_k$ frameworks, although spatial flatness remains well within the allowed uncertainties. When low-redshift probes were included, the curvature constraints were significantly tightened. In particular, the full Pk18+DR2+PP\&SH0ES dataset yields ${\Omega }_k=0.0001\pm 0.0014$ for the ${\Lambda }_{\mathrm{s}}$CDM model, indicating a universe that is remarkably consistent with spatial flatness. We further analyzed the correlations between ${\Omega }_k$, $H_0$, and $S_8$, finding that the inclusion of curvature and a sign-switch dark energy component helps stabilize cosmological parameter estimates while remaining compatible with current observational constraints. Model comparison using AIC and Bayesian evidence shows that the ${\Lambda }_{\mathrm{s}}$CDM model receives inconclusive/weak observational support relative to $\Lambda$CDM.

12 pages, 4 figures, 1 table

References in corpus (2)

• Constraints on Spatial Curvature and Dark Energy Dynamics in the $w$CDM Model from DESI DR1 and DR2
• Dynamical Oscillations in Dark Energy: Joint Constraints on the $w_{sin}$CDM Model from DESI, OHD, and Supernova Samples