Improved Lemaitre-Tolman model and the mass and turn-around radius in group of galaxies II: the role of dark energy

Abstract

In this paper, we extend our previous study \cite{DelPopolo2021} on the Lemaitre-Tolman (LT) model showing how the prediction of the model changes when the equation of state parameter ($w$) of dark energy is modified. In the previous study, it was considered that dark energy was merely constituted by the cosmological constant. In this paper, as in the previous study, we also took into account the effect of angular momentum and dynamical friction ($J\eta$ LT model) that modifies the evolution of a perturbation, initially moving with the Hubble flow. As a first step, solving the equation of motion, we calculated the relationship between mass, $M$, and the turn-around radius, $R_0$. If one knows the value of the turn-around radius $R_0$, it is possible to obtain the mass of the studied objects. As a second step, we build up, as in the previous paper, a relationship between the velocity, $v$, and radius, $R$. The relation was fitted to data of groups and clusters. Since the relationship $v-R$ depends on the Hubble constant and the mass of the object, we obtained optimized values of the two parameters of the objects studied. The mass decreases of a factor of maximum 25\% comparing the $J\eta$ LT results (for which $w=-1$) and the case $w=-1/3$, while the Hubble constant increases going from $w=-1$ to $w=-1/3$. Finally, the obtained values of the mass, $M$, and $R_0$ of the studied objects can put constraints to the dark energy equation of state parameter, $w$.

arXiv comment12 pages, 6 figures

References in corpus (61)

• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Planck 2015 results. XIII. Cosmological parameters
• The Cosmological Constant and Dark Energy
• The Cosmological Constant
• Discovery of a Supernova Explosion at Half the Age of the Universe and its Cosmological Implications
• Profiles of dark haloes: evolution, scatter, and environment
• The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch
• On the spherical collapse model in dark energy cosmologies
• Distances to Nearby Galaxies in Sculptor
• The Local Group and other neighboring galaxy groups
• The Hubble flow around the CenA / M83 galaxy complex
• The BAO+BBN take on the Hubble tension
• Skewness and Kurtosis in Large-Scale Cosmic Fields
• The secondary infall model of galactic halo formation and the spectrum of cold dark matter particles on Earth
• Structure formation in the presence of dark energy perturbations
• ACS imaging of 25 galaxies in nearby groups and in the field
• On the physical origin of dark matter density profiles
• Structure Formation in Inhomogeneous Dark Energy Models
• The very local Hubble flow
• The Cusp/Core problem and the Secondary Infall Model
• Spherical collapse in quintessence models with zero speed of sound
• Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model
• Investigating the Origins of Dark Matter Halo Density Profiles
• Physical approximations for the nonlinear evolution of perturbations in dark energy scenarios
• Halo properties in models with dynamical Dark Energy
• Self-similar spherical collapse with non-radial motions
• Structure formation in inhomogeneous Early Dark Energy models
• Spherical collapse model in dark energy cosmologies
• Spherical collapse model with shear and angular momentum in dark energy cosmologies
• New low surface brightness dwarf galaxies in the Centaurus group
• Where the world stands still: turnaround as a strong test of ΛCDM cosmology
• Effects of shear and rotation on the spherical collapse model for clustering dark energy
• Shear and rotation in Chaplygin cosmology
• Turnaround radius in an accelerated universe with quasi-local mass
• Non-radial motion and the NFW profile
• Density profiles in a spherical infall model with non-radial motions
• Extended Spherical Collapse and the Accelerating Universe
• Spherical collapse of dark energy with an arbitrary sound speed
• Cosmological Density Distribution Function from the Ellipsoidal Collapse Model in Real Space
• Dynamics of Nearby Groups of Galaxies: the role of the cosmological constant
• Constraining Dark Energy through the Stability of Cosmic Structures
• Evolution of Cosmological Density Distribution Function from the Local Collapse Model
• The spherical collapse model in time varying vacuum cosmologies
• Dynamical Mutation of Dark Energy
• A high precision semi-analytic mass function
• Cosmological implications and structure formation from a time varying vacuum
• The signature of dark energy perturbations in galaxy cluster surveys
• Mass Determination of Groups of Galaxies: Effects of the Cosmological Constant
• The maximum sizes of large scale structures in alternative theories of gravity
• Self-Similar Spherical Collapse with Tidal Torque
• Turnaround radius in $f(R)$ model
• Some improvements to the spherical collapse model
• Constraints on shear and rotation with massive galaxy clusters
• Relation between the Turnaround radius and virial mass in $f(R)$ model
• Mass-Temperature relation in $\Lambda$CDM and modified gravity
• Are the nearby groups of galaxies gravitationally bound objects?
• Halo collapse: virialization by shear and rotation in dynamical dark-energy models. Effects on weak-lensing peaks
• Evolution of the cosmological mass function in a moving barrier model
• The radius, at which a galaxy group stops the Hubble stream, and the group mass: an exact analytical solution
• The Hubble stream near a massive object: the exact analytical solution for the spherically-symmetric case
• Improved Lemaitre-Tolman model and the mass and turn-around radius in group of galaxies

Cited by in corpus (5)

• The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics
• Weighing Milky Way and Andromeda in an expanding $\Lambda$CDM Universe: Decreasing the Local Group mass
• Galaxy groups in the presence of Cosmological Constant: Increasing the Masses of Groups
• Multiscale Cosmic Curvature: from Local Structures to Cosmology
• Islands in Simulated Cosmos: Probing the Hubble Flow around Groups and Clusters