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5σ tension between Planck cosmic microwave background and eBOSS Lyman-alpha forest and constraints on physics beyond ΛCDM
Published 2025-01-01“…Model extensions can alleviate this tension: running in the tilt of the primordial power spectrum (α_{s}∼−0.01); a fraction ∼(1−5)% of ultralight axion dark matter (DM) with particle mass ∼10^{−25} eV or warm DM with mass ∼10 eV. The new Dark Energy Spectroscopic Instrument survey, coupled with high-accuracy modeling, will help distinguish the source of this discrepancy.…”
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42
Cosmology in the Universe with Distance Dependent Lorentz-Violating Background
Published 2017-01-01“…We also show that the regime of dark energy at large distances (low redshifts) is essentially dominated by the presence of the Lorentz-violating background.…”
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43
A Cosmological Scaling Relation for Describing the Late Time Dynamics
Published 2013-01-01“…Under this hypothesis, the scaling relation is interpreted as a thermodynamic modification able to describe the cosmological dynamics at late times. In this scheme, dark energy emerges, as a consequence of assuming the validity of our scale relation. …”
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44
Spinor Quintom Cosmology with Intrinsic Spin
Published 2016-01-01“…We consider a spinor quintom dark energy model with intrinsic spin, in the framework of Einstein-Cartan-Sciama-Kibble theory. …”
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45
Toy Models of Universe with an Effective Varying Λ-Term in Lyra Manifold
Published 2015-01-01“…Research on the accelerated expansion of our Universe captures a lot of attention. The dark energy (DE) is a way to explain it. In this paper we will consider scalar field quintessence DE with ωDE>-1 EoS, where the dynamics of the DE models related to the dynamics of the scalar field. …”
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46
Constraints on the Dark Side of the Universe and Observational Hubble Parameter Data
Published 2010-01-01“…This paper is a review on the observational Hubble parameter data that have gained increasing attention in recent years for their illuminating power on the dark side of the universe: the dark matter, dark energy, and the dark age. Currently, there are two major methods of independent observational H(z) measurement, which we summarize as the “differential age method” and the “radial BAO size method.” …”
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47
The Other Side of Gravity and Geometry: Antigravity and Anticurvature
Published 2012-01-01“…Also, it may throw some light on the mystery of physical nature of “Dark Energy.”…”
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48
Astronomical Signatures of Dark Matter
Published 2014-01-01“…The unambiguous detection of dark matter and more recently evidence for dark energy has positioned astronomy at the frontier of fundamental physics as it was in the 17th century.…”
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49
Constraining the Parameters of Modified Chaplygin Gas in Einstein-Aether Gravity
Published 2014-01-01“…We have assumed FRW model of the universe in Einstein-Aether gravity filled with dark matter and modified Chaplygin gas (MCG) type dark energy. We present the Hubble parameter in terms of some unknown parameters and observational parameters with the redshift z. …”
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50
Phenomenology of MaVaN’s Models in Reactor Neutrino Data
Published 2013-01-01“…Mass Varying Neutrinos (MaVaN’s) mechanisms were proposed to link the neutrino mass scale with the dark energy density, addressing the coincidence problem. …”
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51
Dynamical system analysis for extended f(P) gravity coupled with scalar field
Published 2025-01-01“…$$f(P)=\alpha P +\beta P^2$$ f ( P ) = α P + β P 2 , where $$\alpha $$ α and $$\beta $$ β are constant parameters. As an additional dark energy component, we take a canonical scalar field $$\phi $$ ϕ , and several types of interaction between the dark components are considered. …”
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52
Exploring the evolution of structure growth in the universe with field-fluid interactions through dynamical stability analysis
Published 2025-02-01“…Abstract We investigate an interacting quintessence dark energy – dark matter scenario and its impact on structure formation by analyzing the evolution of scalar perturbations. …”
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53
Extensive composable entropy for the analysis of cosmological data
Published 2025-02-01“…In recent decades, an intensive worldwide research activity is focusing both black holes and cosmos (e.g. the dark-energy phenomenon) on the basis of entropic approaches. …”
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54
Testing General Relativity Using Large-scale Structure Photometric Redshift Surveys and the Cosmic Microwave Background Lensing Effect
Published 2025-01-01“…In this study, we constrain the E _G statistic using photometric redshift data from the Dark Energy Survey (DES) MagLim sample in combination with the Planck 2018 cosmic microwave background (CMB) lensing map. …”
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55
Scalar Field Kantowski–Sachs Solutions in Teleparallel <i>F</i>(<i>T</i>) Gravity
Published 2025-01-01“…Some new <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>F</mi><mo>(</mo><mi>T</mi><mo>)</mo></mrow></semantics></math></inline-formula> solution classes may be relevant for future cosmological applications, especially concerning dark matter, dark energy quintessence, phantom energy leading to the Big Rip event, and quintom models of physical processes.…”
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56
Master Robotic Net
Published 2010-01-01“…Such a survey will make it possible to address a number of fundamental problems: search for dark energy via the discovery and photometry of supernovae (including SNIa), search for exoplanets, microlensing effects, discovery of minor bodies in the Solar System, and space-junk monitoring. …”
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57
COOL-LAMPS. VII. Quantifying Strong-lens Scaling Relations with 177 Cluster-scale Strong Gravitational Lenses in DECaLS
Published 2025-01-01“…We constrain the Einstein-radius-enclosed luminosity and stellar mass by fitting parametric spectral energy distributions to aperture photometry from the Dark Energy Camera Legacy Survey (DECaLS) in the g -, r -, and z -band Dark Energy Camera filters. …”
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58
GD-1 Stellar Stream and Cocoon in the DESI Early Data Release
Published 2025-01-01“…We present ∼115 new spectroscopically identified members of the GD-1 tidal stream observed with the 5000-fiber Dark Energy Spectroscopic Instrument (DESI). We confirm the existence of a “cocoon,” which is a broad (FWHM ∼ 2 $\mathop{.}…”
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