Observational Constraints on Dynamical Dark Energy Models

1. Introduction

The accelerated expansion of our universe was first discovered in 1998 on the basis of measurements of the type Ia supernovae (SNe Ia) apparent magnitudes [1,2,3]. This fact was later confirmed by other cosmological observations, in particular, by measurements of the temperature anisotropy and the polarization in the cosmic microwave background (CMB) radiation [4,5,6,7,8,9,10,11,12,13], by studies of the large-scale structure (LSS) of the universe [14,15,16,17,18,19], by measurements of baryon acoustic oscillations (BAO) peak length scale [20,21,22,23,24,25,26], and by measurements of Hubble parameter [27,28,29,30,31,32,33,34,35].

One possible explanation for this empirical fact is that the energy density of the universe is dominated by dark energy or dark fluid, an energy component with an effective negative pressure (see Refs. [36,37,38,39,40,41,42,43] for reviews). The presence of dark matter in the universe, first discovered through the anomalously high rotation velocity of the outer regions of galaxies [44], is another major mystery of modern cosmology. Different models for dark matter have been proposed including cold dark matter (CDM), consisting of heavy particles with mass $m_{\mathrm{CDM}}\ge 100$ KeV, warm dark matter (WDM), composing of particles with a mass of $m_{\mathrm{WDM}}\approx 3-30$ KeV, and hot dark matter (HTM) consisting of ultrarelativistic particles [45]. Assuming general relativity is the correct description of gravity on cosmological scales, about $95\%$ of the energy in the universe has to be in the “dark” form, i.e., in the form of dark energy and dark matter, to explain available observations. According to the last Planck data release (PR4), our universe consists of $4.86\%$ of ordinary matter, $25.95\%$ of dark matter, and $70.39\%$ of dark energy [46].

The true nature and origin of dark energy and dark matter are still unresolved issues of modern cosmology. The simplest description of dark energy is the vacuum energy or the cosmological constant $\mathsf{\Lambda }$ (see Refs. [36,39,47] for reviews). The cosmological model based on such a description of dark energy in the spatially flat universe is called the Lambda Cold Dark Matter ($\mathsf{\Lambda }$CDM) model, which established itself as the standard or concordance model of the universe in the last two decades (see Ref. [36] for a pioneering work and Refs. [48] for recent review and discussion). In this model, dark matter is presented in the form of non-relativistic cold weakly interacting particles which either never been in the equilibrium with the primordial plasma or decoupled from it after becoming non-relativistic at an early stage. A good pedagogical overview of the $\mathsf{\Lambda }$CDM model is available in many recent books [49,50,51,52,53], and reviews [54,55,56,57,58,59].

Despite explaining various observations of our universe to a remarkable degree of accuracy, the $\mathsf{\Lambda }$CDM model has several unsolved problems and tensions [58,60,61,62,63,64,65], including the fine-tuning or cosmological constant problem, the coincidence problem, the Hubble and $S_8$ tensions, and the problem of the shape of the universe. A large number of cosmological models that go beyond the standard $\mathsf{\Lambda }$CDM scenario with modified dynamics of the expansion of the universe at late times have been considered in order to resolve these tensions, for a review [66,67,68,69,70,71,72,73,74,75].

The value of the energy density of cosmological constant ${\rho }_{\mathsf{\Lambda }}$ following from the quantum field theory estimates, is [61] ${\rho }_{\mathsf{\Lambda }}\sim \hslash M_{\mathrm{pl}}^4\sim {10}^{72}{\mathrm{Gev}}^4\sim 2·{10}^{110}\mathrm{erg}/{\mathrm{cm}}^3$, where $M_{\mathrm{pl}}\sim {10}^{18}$ Gev is a Planck mass scale, ℏ is a reduced Planck constant. While cosmological observations of the cosmological constant (like dark energy) show a very different result [61] ${\rho }_{\mathsf{\Lambda }}^{\mathrm{obs}}\sim {10}^{-48}{\mathrm{Gev}}^4\sim 2·{10}^{-10}\mathrm{erg}/{\mathrm{cm}}^3.$ This discrepancy in 120 orders of magnitude between the predicted and observed values of the energy scale of the cosmological constant is called the cosmological constant problem or the fine turning problem [54,55,57].

The coincidence or why now problem is that, based on precise cosmological observations [76], the energy density in dark energy ($68.7\%$) is comparable (within an order of magnitude) to that of nonrelativistic matter ($31.3\%$) at the present time. This fact is an enigma, because in the $\mathsf{\Lambda }$CDM model, the energy density of the cosmological constant does not depend on time, ${\rho }_{\mathsf{\Lambda }}=\mathrm{const}$, while the energy density of matter varies over time as ${\rho }_{\mathrm{DM}}\sim a^{-3}\left(t\right)$ ($a\left(t\right)$ and t are the scale factor and cosmic time, respectively), so the ratio of these quantities is time-dependent, ${\rho }_{\mathrm{DM}}/{\rho }_{\mathsf{\Lambda }}\propto a^{-3}\left(t\right)$.

The Hubble tension problem is that there is a discrepancy between the value of the Hubble parameter at present epoch $H_0=100h\mathrm{km}{\mathrm{c}}^{-1}{\mathrm{Mpc}}^{-1}$, with h is a dimensionless normalized Hubble constant, obtained by the local measurements and CMB temperature anisotropy data [13,77,78,79,80,81,82].

The $S_8$ tension problem is that there is a discrepancy at the $2\sigma$ to $3\sigma$ confidence level between the primary CMB temperature anisotropy measurements by the Planck satellite [13] in the strength of matter clustering compared to lower redshift measurements such as the weak gravitational lensing and galaxy clustering [66,68,83,84,85].

This tension is quantified using the weighted amplitude of matter fluctuation parameter $S_8={\sigma }_8{({\mathsf{\Omega }}_{\mathrm{m}}/0.3)}^{0.5}$, which modulates the amplitude of weak lensing measurements, here ${\sigma }_8$ is an amplitude of mass fluctuations on scales of $8h^{-1}\mathrm{Mpc}$; ${\mathsf{\Omega }}_{\mathrm{m}}={\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}/E^2\left(a\right)$ is a fractional matter density parameter; $E\left(a\right)=H\left(a\right)/H_0$ is a normalized Hubble parameter; $H\left(a\right)=\dot{a}/a$ is a Hubble parameter, $\dot{a}$ is a derivative of the scale factor a with respect to cosmic time.

The problem with the shape of the universe is that the CMB anisotropies power spectra measured by the Planck space telescope show a preference for a spatially-closed universe at more than $3\sigma$ confidence level [13,86]. This fact contradicts expectations from the inflation theory [64,66,87], and is interpreted by the cosmological community as a possible crisis of modern cosmology [87,88,89].

The main alternative to the $\mathsf{\Lambda }$CDM model, during the period of time when the accelerated expansion of the universe is governed by the cosmological constant $\mathsf{\Lambda }$, are dynamical dark energy scalar field $\varphi$CDM models [90,91,92,93,94,95,96,97,98]. In these models, dark energy is described through the equation of state (EoS) parameter, $w_{\varphi }\left(t\right)$, which depends on time: $w_{\varphi }\left(t\right)\equiv p_{Œ}/{\rho }_{Œ}$, $p_{Œ}$ - a scalar field pressure, ${\rho }_{Œ}$ - a scalar field energy density; whereas in the $\mathsf{\Lambda }$CDM model, the EoS parameter is a constant, $w_{\mathsf{\Lambda }}=-1$. At the same time, at the present epoch, the value of the time-dependent EoS parameter in scalar field models becomes approximately equal to minus one $w_{\varphi }\approx -1$, thus dynamical dark energy mimics the cosmological constant and becomes almost indistinguishable from it.

Depending on the value of the EoS parameter at the present epoch, $\varphi$CDM scalar field models are divided into: quintessence models, with $-1<w_{\varphi }\left(t\right)<-1/3$ [99,100,101], (see e.g., Refs. [36,43] [for a review) and phantom models, with $w_{\varphi }\left(t\right)<-1$ Refs. [102,103,104,105,106,107,108]. Quintessence models are divided into two classes: tracker (freezing) models, in which the scalar field evolves slower than the Hubble expansion rate, and thawing models, in which the scalar field evolves faster than the Hubble expansion rate [100,105,109,110,111]. In quintessence tracker models, the energy density of the scalar field first tracks the radiation energy density and then the matter energy density, while it remains subdominant [112]. Only recently does the scalar field become dominant and begins to behave as a component with the negative pressure, which leads to the accelerated expansion of the universe [101,113,114]. For certain forms of potentials, the quintessence tracker models have an attractor solution that is insensitive to initial conditions [112].

In the standard $\mathsf{\Lambda }$CDM cosmological scenario, one assumes the existence of two epochs of accelerated expansion in the universe. The first, i.e., inflation [115,116,117,118,119,120,121,122,123], which happens in the very early universe, and the second is the dark energy dominated epoch observed today, [50,51,124,125]. Inflation is a theory of the exponential expansion of space in the early universe, which is believed to have lasted approximately from ${10}^{-36}$ to ${10}^{-33}$-${10}^{-32}$ seconds after the Big Bang, the exact times being dependent on the microphysics of the model describing inflation. The inflationary models explain the origin of tiny primordial density fluctuations in the universe, which must have been present at very early epochs, as the seeds for structure formation in the later evolution of the universe. The exponential expansion during inflation comes to an end when a phase transition transforms the vacuum energy into radiation and matter, after which the radiation dominated epoch begins. This phase transition is called the reheating, and its governing dynamics is still debated. A successful inflationary model requires a smooth transition to the decelerated epoch (in which inflation rules the universe as if it were dominated by non-relativistic matter) because otherwise, the homogeneity of the universe would be violated [126,127]. Inflation resolves several problems in cosmology, namely, the horizon problem, associated with the lack of causal relationship between different regions in the early universe before recombination epoch (it’s an epoch of forming the electrically neutral hydrogen atoms, which began at $t_{\mathrm{rec}}\approx 350000$ years after the Big Bang), and the flatness problem, related to the fine-tuning of the spatial flatness of the universe in the early epoch so that the spatial flatness of the universe is preserved at present epoch.) The evolution of the universe from the inflationary epoch to the present dark energy epoch are investigated in quintessential inflation models too [128,129,130,131,132,133]. In these models, a single scalar field plays a role of both the inflaton field at the inflationary epoch, and of the quintessence scalar field at the present epoch, thereby the origin of dark energy at the present epoch is also explained within the same model.

The interaction between dark energy and dark matter, namely their transformation into each other, is considered in the interacting dark energy (IDE) models [134,135,136,137,138]. In these models, the coincidence problem of the standard $\mathsf{\Lambda }$CDM model as well as the Hubble constant $H_0$ tension can be alleviated [67,70,73,139,140,141].

In this review, we considered the most significant studies devoted to the observational constraints on dynamical dark energy models over the past twenty years, in particular, scalar field $\varphi$CDM models, quintessential inflation scalar field $\varphi$CDM models, IDE models both in the spatially flat and non-flat hypersurfaces. It can be seen from this review that the complication, refinement of cosmological data, and the increase in the variety of methods for studying dynamical dark energy models lead to more accurate constraints on the values of cosmological parameters in these models. Despite the refinement of various observational data and the complication of methods for studying dark energy in the universe, current observational data still favor the standard spatially flat $\mathsf{\Lambda }$CDM model, while not excluding dynamical dark energy models and spatially-closed hyperspaces [142,143,144,145,146,147,148,149,150,151,152,153,154,155,156]. At the same time, recent studies showed that the currently available observational datasets favor the IDE model at more than $2\sigma$ confidence level [67,139,139,140,157,158].

This paper is organized as follows: the different cosmological dynamical dark energy models are described in Section 2, observational constraints on dynamical dark energy models by various observational data are considered in Section 3, conclusions and discussions are presented in Section 4. In this paper, we used the natural system of units: $c=\hslash =k_B=1$.

2. Cosmological Dark Energy Models

2.1. $\mathsf{\Lambda }$CDM Model

As highlighted in the Introduction, the Lambda Cold Dark Matter ($\mathsf{\Lambda }$CDM) model is the standard or concordance model of a spatially flat universe. In this model, dark energy is represented by the cosmological constant $\mathsf{\Lambda }$, which is assumed to be associated with the vacuum energy density of quantum fields, and its energy density is a constant

$${\rho }_{\mathsf{\Lambda }}=\frac{\mathsf{\Lambda }{M}_{\mathrm{pl}}^2}{8\pi }={\rho }_{\mathrm{vac}}=\mathrm{const},$$

(1)

here $\mathsf{\Lambda }=4.33·{10}^{-66}{\mathrm{eV}}^2$. The pressure and the energy density in the $\mathsf{\Lambda }$CDM model are related as

$$p_{\mathsf{\Lambda }}=-{\rho }_{\mathsf{\Lambda }}=\mathrm{const},$$

(2)

leading to the constant EoS parameter

$$w_{\mathsf{\Lambda }}=-1.$$

(3)

The action describing the cosmological constant $\mathsf{\Lambda }$ is [43]

$$S=-\frac{M_{\mathrm{pl}}^2}{16\pi }\int d^{4}x\sqrt{-g}(R+2\mathsf{\Lambda })+S_{\mathrm{M}},$$

(4)

where $g\equiv \det \left(g_{\mu \nu }\right)$ is the determinant of the metric tensor $g_{\mu \nu }$, R is the Ricci scalar, and $S_{\mathrm{M}}$ is the action describing matter. The spatially flat $\mathsf{\Lambda }$CDM model is typically characterized by six independent parameters [159]: the physical baryon density parameter, ${\mathsf{\Omega }}_{\mathrm{b}}{h}^2$; the dark matter physical density parameter, ${\mathsf{\Omega }}_{\mathrm{c}}{h}^2$; the age of the universe, $t_0$; the scalar spectral index, $n_{\mathrm{s}}$; the amplitude of the curvature fluctuations, ${\Delta }_{\mathrm{R}}^2$; and the optical depth during the reionization period for $z\in (6,20)$, $\tau$. In addition to these parameters, the $\mathsf{\Lambda }$CDM model is described by six extended fixed parameters: the total density parameter, ${\mathsf{\Omega }}_{\mathrm{tot}}$; the EoS parameter, $w_{\mathsf{\Lambda }}$; the total mass of three types of neutrinos, $\sum m_{\nu }$; the effective number of the relativistic degrees of freedom, $N_{\mathrm{eff}}$; the tensor/scalar ratio, r; the scalar spectral index running, $a_s$.

The extension of the spatially flat $\mathsf{\Lambda }$CDM model to spatially non-flat hypersurfaces is the oCDM model. The first Friedmann equations describing the evolution of the universe for the spatially non-flat oCDM model and for the spatially flat $\mathsf{\Lambda }$CDM model are defined, respectively, as

$$E\left(a\right)={({\mathsf{\Omega }}_{\mathrm{r}0}{a}^{-4}+{\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}+{\mathsf{\Omega }}_{\mathrm{k}0}{a}^{-2}+{\mathsf{\Omega }}_{\mathsf{\Lambda }})}^{1/2},$$

(5)

,

$$E\left(a\right)={({\mathsf{\Omega }}_{\mathrm{r}0}{a}^{-4}+{\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}+{\mathsf{\Omega }}_{\mathsf{\Lambda }})}^{1/2},$$

(6)

here ${\mathsf{\Omega }}_{\mathrm{r}0}={\rho }_{\mathrm{r}0}/{\rho }_{\mathrm{cr}}$, ${\mathsf{\Omega }}_{\mathrm{m}0}={\rho }_{\mathrm{m}0}/{\rho }_{\mathrm{cr}}$, ${\mathsf{\Omega }}_{\mathsf{\Lambda }}={\rho }_{\mathsf{\Lambda }}/{\rho }_{\mathrm{cr}}$ are density parameters at present epoch for radiation, matter and vacuum, respectively, with ${\rho }_{\mathrm{r}0}$ and ${\rho }_{\mathrm{m}0}$ are energy densities for radiation and matter at present epoch, respectively. The value of the critical energy density at present epoch is equal to ${\rho }_{\mathrm{cr}}=3M_{\mathrm{pl}}^2{H}_0^2/8\pi =1.8791h^2·{10}^{-29}{\mathrm{g}\mathrm{cm}}^{-3}$; ${\mathsf{\Omega }}_{\mathrm{k}0}=-\mathrm{k}/H_0^2$ is a spatial curvature density parameter at present epoch, ${\rho }_{\mathrm{k}0}=-3\mathrm{k}{M}_{\mathrm{pl}}^2/8\pi$ is a spatial curvature density, $\mathrm{k}$ is a curvature parameter, and $E\left(a\right)\equiv H\left(a\right)/H_0$ is a normalized Hubble parameter.

Observational constraints on cosmological parameters ${\mathsf{\Omega }}_{m0}$ and ${\mathsf{\Omega }}_{\mathsf{\Lambda }}$, obtained from different cosmological datasets for the $\mathsf{\Lambda }$CDM model and for the oCDM model, are represented in Figure 1.

As we mentioned above, the $\mathsf{\Lambda }$CDM model is the fiducial model against which all alternative models are compared regarding their fit to observational data. Its predictions agree with the observational data pertaining to the accelerated expansion of the universe, the statistical distribution of LSS, the CMB temperature and polarization anisotropies, and the abundance of light elements in the universe [76,160].

2.2. Dynamical Dark Energy Scalar Field $\varphi$CDM Models

There are numerous physically motivated alternative models for the $\mathsf{\Lambda }$CDM model [43,56,164,165,166,167,168,169,170,171,172,173,174]. One of the prominent alternatives to the $\mathsf{\Lambda }$CDM model are dynamical scalar field $\varphi$CDM models [36,91,92]. In these models, the role of dark energy is played by a slowly varying uniform self-interacting scalar field $\varphi$, minimally interacting with gravity. These $\varphi$CDM models involving a dynamical scalar field do not suffer from the fine tuning problem of the $\mathsf{\Lambda }$CDM model, and have a more natural explanation for the observed low-energy scale of dark energy. In addition, the EoS parameter time dependent in the $\varphi$CDM model, as opposed to it being a constant $w=-1$ in the $\mathsf{\Lambda }$CDM model. When the energy density of the scalar field begins to dominate over the energy density of both radiation and matter, the universe begins the stage of the accelerated expansion. At early times during the evolution of the universe, the behavior of the dynamical scalar field is different from that of the cosmological constant $\mathsf{\Lambda }$, but is almost indistinguishable from that of the cosmological constant during later times.

Dynamical scalar field $\varphi$CDM models are divided into two classes: the quintessence models [112] and phantom models [102,175]. These two classes of models differ from each other by the following attributes:

(i) 

The EoS parameter – For quintessence fields, $-1<w_{\varphi }<-1/3$, while for phantom fields, $w_{\varphi }<-1$.

(ii) 

The sign of the kinetic term – For quintessence fields, the kinetic term in the Lagrangian has a positive sign, while it is negative for phantom fields.

(iii) 

The dynamics of the scalar field – The quintessence field rolls gradually to the minimum of its potential, while the phantom field rolls to the maximum of its potential.

(iv) 

Temporal evolution of dark energy – For quintessence fields, the dark energy density remains almost unchanging with time, while it increases for phantom fields.

(v) 

Forecasting the future of the universe – The quintessence models predict either an eternal expansion of the universe, or a repeated collapse, depending on the spatial curvature of the universe. On the other hand, the phantom models predict the destruction of any gravitationally-related structures in the universe. Depending on the asymptotic behavior of the Hubble parameter $H\left(t\right)$, the future scenarios of the universe are divided into: a big rip for which $H\left(t\right)\to \infty$ for a finite future time $t=\mathrm{const}$; a little rip for which $H\left(t\right)\to \infty$ at an infinite future time $t\to \infty$, and a pseudo rip for which $H\left(t\right)\to \mathrm{const}$ for an infinite future time $t\to \infty$.

The action describing a scalar field in the presence of matter is given by

$$S=\int d^{4}x\sqrt{-g}(-\frac{M_{\mathrm{pl}}^2}{16\pi }R+{\mathcal{L}}_{\varphi })+S_{\mathrm{M}},$$

(7)

where ${\mathcal{L}}_{\varphi }$ is the Lagrangian density of the scalar field, the form of which depends on the type of the chosen model, and as mentioned above, R is the Ricci scalar, and $S_{\mathrm{M}}$ is the action describing matter. We describe the form of ${\mathcal{L}}_{\varphi }$ for the quintessence and the phantom fields below.

2.2.1. Quintessence Scalar Field

The dynamics of the quintessence scalar field is described by the Lagrangian density

$${\mathcal{L}}_{\varphi }=\frac{1}{2}{g}^{\mu \nu }{\partial }_{\mu }\varphi {\partial }_{\nu }\varphi -V\left(\varphi \right),$$

(8)

where $V\left(\varphi \right)$ is a scalar field potential. There are various quintessence potentials discussed in the literature, but there are currently no observational constraint to prefer one of these over the others. A list of some of the quintessence potentials are presented in Table 1.

The EoS parameter for the quintessence scalar field is given by

$$w_{\varphi }\equiv {\displaystyle \frac{p_{\varphi }}{{\rho }_{\varphi }}}={\displaystyle \frac{{\dot{\varphi }}^2/2-V\left(\varphi \right)}{{\dot{\varphi }}^2/2+V\left(\varphi \right)}},$$

(9)

where $p_{\varphi }=\frac{1}{2}{\dot{\varphi }}^2-V\left(\varphi \right)$ and ${\rho }_{\varphi }=\frac{1}{2}{\dot{\varphi }}^2+V\left(\varphi \right)$ are respectively the pressure and energy density of the quintessence field. Here, overdots denoting derivatives with respect to the cosmic time t. The equation of motion for the quintessence scalar field can be obtained by varying the action in Equation (7), along with the Lagrangian in Equation (8),

$$\ddot{\varphi }+3H\dot{\varphi }+V^{\prime }\left(\varphi \right)=0,$$

(10)

with the prime denoting a derivative with respect to the scalar field $\varphi$. The first Friedmann’s equation for a $\varphi$CDM model in a spatially non-flat spacetime has the form

$$E\left(a\right)={({\mathsf{\Omega }}_{\mathrm{r}0}{a}^{-4}+{\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}+{\mathsf{\Omega }}_{\mathrm{k}0}{a}^{-2}+{\mathsf{\Omega }}_{Œ}\left(a\right))}^{1/2},$$

(11)

where ${\mathsf{\Omega }}_{Œ}\left(a\right)$ is the dark energy (scalar field) density parameter.

Depending on the shape of potentials, quintessence models are further subdivided into thawing models and freezing (tracking) models [43,100]

a) 

In the thawing models, the scalar field is too suppressed by the retarding effect of the Hubble expansion, represented by the term $3H\dot{\varphi }$ in Equation (10), until recently. This results in a much slower evolution of the scalar field compared to the Hubble expansion, and the thawing scalar field manifests itself as the vacuum energy, with the EoS parameter $w_{\varphi }\sim -1$. The Hubble expansion rate $H\left(t\right)$ decreases with time, and after it falls below $\sqrt{V^{″}\left(\varphi \right)}$, the scalar field begins to roll to the minimum of its potential. The value of the EoS parameter for the scalar field thus increases over time and becomes $w_{\varphi }>-1$.

b) 

In the freezing models, the scalar field is always suppressed (it is damped), i.e., $H\left(t\right)>\sqrt{V^{″}\left(\varphi \right)}$. Freezing scalar field models have so-called tracking solutions. According to tracking solutions, the quintessence component tracks the background EoS parameter (radiation in the radiation-dominated epoch and matter in the matter-dominated epoch) and eventually only recently grows to dominate the energy density in the universe. This leads to the accelerated expansion of the universe at late times, since the scalar field has a negative effective pressure. The tracker behavior allows the quintessence model to be insensitive to initial conditions. But this requires fine tuning of the potential energy, since $\sqrt{V^{″}\left(\varphi \right)}\sim H_0\sim {10}^{-33}\mathrm{eV}$.

Figure 2. (Left panel) The location of thawing and freezing scalar fields in the $w_{\varphi }-d{w}_{\varphi }/dlna$ plane. (The figure is adapted from [100]). (Right panel) Regimes of the quick rolling down and slow rolling down of the freezing scalar field to the minimum of its potential.

Figure 2. (Left panel) The location of thawing and freezing scalar fields in the $w_{\varphi }-d{w}_{\varphi }/dlna$ plane. (The figure is adapted from [100]). (Right panel) Regimes of the quick rolling down and slow rolling down of the freezing scalar field to the minimum of its potential.

In 1988, Ratra and Peebles introduced a tracker $\varphi$CDM model comprising of a scalar field with an inverse power-law potential of the form $V\left(\varphi \right)=\kappa /2M_{\mathrm{pl}}^2{\varphi }^{-\alpha }$, for a model parameter $\alpha >0$ [90,91]. For $\alpha =0$, this $\varphi$CDM Ratra-Peebles (RP) model reduces to the $\mathsf{\Lambda }$CDM model. The positive parameter $\kappa$ relates to the mass scale of the particles, $M_{\varphi }$, as $M_{\varphi }\sim {(\kappa M_{\mathrm{pl}}^2/2)}^{\frac{1}{\alpha +4}}$. The RP $\varphi$CDM model is a typical representative of the behavior of tracker quintessence scalar field $\varphi$CDM models.

2.2.2. Phantom Scalar Field

The Lagrangian density describing a phantom scalar field has the form

$${\mathcal{L}}_{\varphi }=-\frac{1}{2}{g}^{\mu \nu }{\partial }_{\mu }\varphi {\partial }_{\nu }\varphi -V\left(\varphi \right),$$

(12)

where the negative sign of the kinetic energy term is required to ensure the dark energy EoS parameter is less than -1, i.e., $w_{\varphi }<-1$, and the energy density increases over time [107]. The incomplete list of phantom potentials is given in Table 2.

Analogous to Equation (9), the EoS parameter for the phantom scalar field is given by

$$w_{\varphi }\equiv {\displaystyle \frac{p_{\varphi }}{{\rho }_{\varphi }}}={\displaystyle \frac{-{\dot{\varphi }}^2/2-V\left(\varphi \right)}{-{\dot{\varphi }}^2/2+V\left(\varphi \right)}},$$

(13)

where $p_{\varphi }=-\frac{1}{2}{\dot{\varphi }}^2-V\left(\varphi \right)$ and ${\rho }_{\varphi }=-\frac{1}{2}{\dot{\varphi }}^2+V\left(\varphi \right)$ are respectively the pressure and energy density of the phantom field. The equation of motion for the phantom scalar field has the form

$$\ddot{\varphi }+3H\dot{\varphi }-V^{\prime }\left(\varphi \right)=0.$$

(14)

2.3. Parameterized Dark Energy Models

2.3.1. wCDM Parameterization

In dynamical dark energy models, one can use the wCDM parameterization where the EoS parameter can be expressed as $p=w\left(a\right)\rho$. Dark energy models are sometimes characterized only by the EoS parameter, and corresponding cosmological models are called wCDM models [184]. This parameterization has no physical motivation, but is commonly used as an ansatz in data analysis to quantify different and distinguish between dark energy models. The wCDM parameterization in particular makes it possible to differentiate, at present epoch, the $\mathsf{\Lambda }$CDM model from other dark energy models.

The time-dependent EoS parameter in wCDM models is often characterized by the Chevallier-Polarsky-Linder (CPL) $w_0-w_a$ parameterization [185,186]

$$w\left(a\right)=w_0+w_a(1-a),$$

(15)

where $w_0=w\left(a_0\right)$ and $w_a=(dw/dz){{|}_{z=1}=-a^{-2}(dw/da)|}_{a=1/2}$, with z being the cosmological redshift defined as $z=1/a-1$, and $a_0$ is the scale factor at present time, conventionally normalized as $a_0=1$. Although the CPL parameterization is simple and flexible enough to accurately describe EoS parameters in most dark energy models, it cannot describe arbitrary dark energy models with good accuracy (up to a few percent) over a wide redshift range [186]. The dynamical dark energy models where the EoS parameter is expressed through the CPL parameterization are called the $w_0{w}_a$CDM models.

The normalized Hubble parameter for $w_0{w}_a$CDM model for the spatially flat universe has the form

$$E\left(a\right)={\left[{\mathsf{\Omega }}_{\mathrm{r}0}{a}^{-4}+{\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}+(1-{\mathsf{\Omega }}_{\mathrm{m}0})a^{-3(1+w_0+w_a)}{e}^{-3w_a(1-a)}\right]}^{1/2}.$$

(16)

1$\sigma$, 2$\sigma$ confidence level contours constraints on cosmological parameters $w_0$ and $w_a$ in the $w_0{w}_a$CDM model from different combinations of datasets: SNe Ia apparent magnitude (including measurenments of the Hubble Space Telescope (HST)), CMB temperature anisotropy, BAO peak length scale are presented in Figure 3 (Left panel).

2.3.2. XCDM Models

Cosmological dark energy models with a constant value of the EoS parameter are called XCDM models. These models are defined both in the spatially flat and spatially non-flat hyperspaces. The normalized Hubble parameter expressed through the dark energy EoS parameter $w_X$ has the form

$$E\left(a\right)={\left[{\mathsf{\Omega }}_{\mathrm{r}0}{a}^{-4}+{\mathsf{\Omega }}_{\mathrm{m}0}{a}^{-3}+{\mathsf{\Omega }}_{\mathrm{k}0}{a}^{-2}+(1-{\mathsf{\Omega }}_{\mathrm{m}0})a^{-3(1+w_X)}\right]}^{1/2}.$$

(17)

The case $w_X=-1$ is equivalent to the standard spatially flat $\mathsf{\Lambda }$CDM model with the same matter energy density parameter ${\mathsf{\Omega }}_{\mathrm{m}0}$ and zero spatial curvature, ${\mathsf{\Omega }}_{\mathrm{k}0}=0$, at present epoch.

1$\sigma$, 2$\sigma$ confidence level contours constraints on cosmological parameters $w_X$ in the XCDM model from different combinations of datasets: SNe Ia apparent magnitude, CMB temperature anisotropy, BAO peak length scale are presented in Figure 3 (Right panel).

2.4. Quintessential Inflation Models

The action for quintessential inflation models has the general form

$$S=\int d^{4}x\sqrt{-g}(-\frac{M_{\mathrm{pl}}^2}{16\pi }R+\frac{1}{2}{g}^{\mu \nu }{\partial }_{\mu }\varphi {\partial }_{\nu }\varphi -V\left(\varphi \right))+S_{\mathrm{M}}+S_{\mathrm{R}}+S_{\mathrm{I}}(g_{\mu \nu },\varphi ,\psi ,\chi ,B_{\mu }),$$

(18)

where $S_{\mathrm{R}}$ is the action describing radiation, $S_{\mathrm{I}}$ is the action describing the interactions of the inflaton field with the fermion ($\psi$), scalar ($\chi$), vector ($B_{\mu }$) degrees of freedom in the Standard Model and beyond.

To maintain inflation over a long period of time, it is necessary that the acceleration caused by the inflaton field be sufficiently small compared to its velocity over the Hubble time. Under these conditions, the first Friedmann’s and Klein-Gordon’s equations for the inflaton field in the spatially flat universe take the form [122,187,188]

$$\rho ={\dot{\varphi }}^2/2+V\left(\varphi \right)\stackrel{{\dot{\varphi }}^2/2\ll V\left(\varphi \right)}{\to }\rho =\frac{3M_{\mathrm{Pl}}^2}{8\pi }{H}^2\simeq V\left(\varphi \right),\ddot{\varphi }+3H\dot{\varphi }+V^{\prime }\left(\varphi \right)=0\stackrel{|\ddot{\varphi }|\ll 3H|\dot{\varphi }|}{\to }-V^{\prime }\left(\varphi \right)\simeq 3H\dot{\varphi }.$$

(19)

The slow-roll regime of the inflaton field is provided by potential of the inflaton field $V\left(\varphi \right)$ with certain shapes: exponential [131], power-law [128,129], and plateau-like [132,133]. The slow-roll parameters, which determine the curvature and slope of the potential of the inflaton field, should remain small for some period of time to sustain the inflationary behavior

$$ϵ=\frac{M_{\mathrm{pl}}^2}{2}{\left(\frac{V^{\prime }\left(\varphi \right)}{V\left(\varphi \right)}\right)}^2\ll 1,\eta =M_{\mathrm{pl}}^2\frac{V^{″}\left(\varphi \right)}{V\left(\varphi \right)}\ll 1,\xi =M_{\mathrm{pl}}^2\frac{V^{\prime }\left(\varphi \right)V^{‴}\left(\varphi \right)}{V{\left(\varphi \right)}^2}\ll 1.$$

(20)

The condition $ϵ\ll 1$ is necessary for the accelerated expansion of the universe to take place, while the condition $ϵ\simeq 1$ defines the end of inflation. In the case of $ϵ\approx 0$, the expansion rate of the universe is approximately constant, i.e., the scale factor grows exponentially with time, $a\propto e^{Ht}$, resulting in an almost de Sitter expansion of the universe.

The scalar spectral index ($n_s$), tensor spectral index ($n_t$), scalar spectral index running ($a_s$), and tensor-to-scalar ratio (r) are defined, respectively, as [131]

$$n_s-1=-6ϵ+2\eta ,n_t=-2ϵ,a_s\equiv \mathrm{d}{n}_s/\mathrm{d}lnk=16ϵ\eta -24{ϵ}^2-2\xi ,r=16ϵ.$$

(21)

During the inflationary epoch of the universe, scalar and tensor perturbations are created from quantum vacuum fluctuations and are spatially stretched to superhorizon scales, where they become classical, and the almost scale-invariant tilted primordial power spectrum is formed [189]. The tilted primordial scalar ${\mathcal{P}}_s\left(k\right)$ and tensor ${\mathcal{P}}_t\left(k\right)$ power spectra for spatially flat tilted quintessential inflation models are defined in terms of the wave number k as [122,187,188]

$${\mathcal{P}}_s\left(k\right)=A_s{\left(\frac{k}{k_0}\right)}^{n_s-1},{\mathcal{P}}_t\left(k\right)=A_t{\left(\frac{k}{k_0}\right)}^{n_t},$$

(22)

where $A_s$ and $A_t$ are the curvature perturbations amplitude and tensor amplitude at the pivot scale $k_0=0.05{\mathrm{Mpc}}^{-1}$ [51].

The untilted primordial power spectrum for untilted spatially non-flat quintessential inflation models is defined as [130,190]

$$P\left(q\right)\propto \frac{{(q^2-4K)}^2}{q(q^2-K)},$$

(23)

here $q=\sqrt{k^2+K}$ is the wavenumber for scalar perturbations. In the spatially flat limit $K=0$, $P\left(q\right)$ reduces to the $n_s=1$ spectrum.

2.5. Interacting Dark Energy Models

As mentioned above, one of the major unresolved problems of modern cosmology is the so called coincidence problem in the $\mathsf{\Lambda }$CDM model, in which the energy densities of dark energy and dark matter are of the same order of magnitude at the present epoch. One way to resolve this problem is to assume that these components somehow interact with each other. IDE models consider the transformation of dark energy and dark matter into each other, with their interaction between described by the following modified continuity equations for dark energy and matter, respectively

$$\begin{array}{c}\hfill {\dot{\rho }}_{\mathrm{m}}+3H{\rho }_{\mathrm{m}}={\delta }_{\mathrm{couple}},\end{array}$$

(24)

$$\begin{array}{c}\hfill {\dot{\rho }}_{Œ}+3H({\rho }_{Œ}+p_{Œ})=-{\delta }_{\mathrm{couple}},\end{array}$$

(25)

where ${\rho }_{\mathrm{m}}$ is the matter energy density, ${\rho }_{Œ}$ and $p_{Œ}$ are respectively the energy density and pressure of the scalar field, and ${\delta }_{\mathrm{couple}}$ is the coupling coefficient between dark energy and matter. In IDE models, the following forms of the coupling coefficient ${\delta }_{\mathrm{couple}}$ are typically used [136,137]

$$\begin{array}{c}\hfill {\delta }_{\mathrm{couple}}=nQ{\rho }_{\mathrm{m}}\dot{\varphi },\end{array}$$

(26)

$$\begin{array}{c}\hfill {\delta }_{\mathrm{couple}}=\beta H({\rho }_{\mathrm{m}}+{\rho }_{Œ}),\end{array}$$

(27)

where $n=\sqrt{8\pi /M_{\mathrm{pl}}^2}$, and $\beta$ and Q are dimensionless constants. The IDE models are subdivided into two types, as described below [88,136,137].

2.5.1. Coupling of the First Type

The IDE models of the first type are characterized by the exponential potential for the scalar $\varphi$ and the linear interaction determined by the coupling coefficient given by Equation (26), as discussed in [136]. The coupled quintessence scalar field equation is given as

$$\ddot{\varphi }+3H\dot{\varphi }+V^{\prime }\left(\varphi \right)=-nQ{\rho }_{\mathrm{m}}\dot{\varphi },$$

(28)

where $V\left(\varphi \right)=V_0{e}^{-n\lambda \varphi }$ is the scalar field potential and $\lambda$ is a model parameter. The coupled continuity equation for dark energy is

$${\dot{\rho }}_{Œ}+3H({\rho }_{Œ}+p_{Œ})=-nQ{\rho }_{\mathrm{m}}\dot{\varphi }.$$

(29)

The matter energy density evolves according to

$${\dot{\rho }}_{\mathrm{m}}+3H{\rho }_{\mathrm{m}}=nQ{\rho }_{\mathrm{m}},$$

(30)

leading to

$${\rho }_{\mathrm{m}}={\rho }_{\mathrm{m}0}{a}^{-3}{e}^{nQ\varphi }.$$

(31)

2.5.2. Coupling of the Second Type

For the second type of IDE models, the scalar potential, and hence the dynamics of the interaction between dark energy and matter, is constructed with the requirement that the coincidence parameter $r={\rho }_{\mathrm{m}}/{\rho }_{\varphi }$ takes an analytic expression and for $z\to 0$ becomes a constant, thereby alleviating the coincidences problem of the $\mathsf{\Lambda }$CDM model [88,137].

The equation of motion for $\varphi$, Equation (25), can be written as

$$\dot{\varphi }[\ddot{\varphi }+3H\dot{\varphi }+V^{\prime }\left(\varphi \right)]=-{\delta }_{\mathrm{couple}}.$$

(32)

The coupling coefficient ${\delta }_{\mathrm{couple}}$ is constrained by the requirement that the solution to Eqs. (25) be compatible with a constant relationship between ${\rho }_{\mathrm{m}}$ and ${\rho }_{\varphi }$ energy densities. It is convenient to introduce the quantities ${\Pi }_{\mathrm{m}}$ and ${\Pi }_{\varphi }$ by

$${\delta }_{\mathrm{couple}}=-3H{\Pi }_{\mathrm{m}}=3H{\Pi }_{\varphi },$$

(33)

by introducing these quantities, the continuity equations for dark energy and matter Eqs. (25) will have a form

$$\begin{array}{c}\hfill {\dot{\rho }}_{\mathrm{m}}+3H({\rho }_{\mathrm{m}}+{\Pi }_{\mathrm{m}})=0,{\dot{\rho }}_{Œ}+3H({\rho }_{Œ}+p_{Œ}+{\Pi }_{\varphi })=0.\end{array}$$

(34)

The quantities ${\Pi }_{\mathrm{m}}$ and ${\Pi }_{\varphi }$ are interconnected as

$${\Pi }_{\mathrm{m}}=-{\Pi }_{\varphi }={\displaystyle \frac{{\rho }_{\mathrm{m}}{\rho }_{\varphi }}{\rho }}({\gamma }_{\varphi }-1),$$

(35)

$${\gamma }_{\varphi }=\frac{p_{Œ}+{\rho }_{\varphi }}{{\rho }_{\varphi }}=\frac{{\dot{\varphi }}^2}{{\rho }_{\varphi }}$$

(36)

where $\rho ={\rho }_{\mathrm{m}}+{\rho }_{\varphi }$.

Assuming ${\gamma }_{\varphi }$ is a constant, the value of which ${\gamma }_{\varphi }\in (0,2)$, it can be found

$${\rho }_{\mathrm{m}}\propto {\rho }_{\varphi }\propto \rho \propto a^{-\nu },\mathrm{for}\nu =3\frac{{\gamma }_{\varphi }+r}{r+1},$$

(37)

here r is a coincidence parameter, which takes an analytic expression for r, becomes a constant, thereby alleviating the coincidences problem. The solution of the second Friedmann’s equation $3M_{\mathrm{pl}}{H}^2=8\pi \rho$, for the result, obtained in Equation (37), has a form $a\propto t^{2/\nu }$. Thus, the Hubble parameter is defined as

$$H=\frac{2}{\nu t}=\frac{2(r+1)}{3({\gamma }_{\varphi }+r)}\frac{1}{t}.$$

(38)

The energy density parameter is defined as ${\mathsf{\Omega }}_{\varphi }=\frac{8\pi M_{\mathrm{pl}}^2}{3H^2}{\rho }_{\varphi }$, as well as ${\mathsf{\Omega }}_{\varphi }=\frac{1}{r+1}$. Equating these equations and inserting Equation (38), we will have

$${\rho }_{\varphi }={\displaystyle \frac{M_{\mathrm{pl}}^2}{6\pi }}{\displaystyle \frac{1+r}{{({\gamma }_{\varphi }+r)}^2}}{\displaystyle \frac{1}{t^2}}.$$

(39)

The combination with Equation (36) gives

$$\dot{\varphi }=\sqrt{{\displaystyle \frac{M_{\mathrm{pl}}^2{\gamma }_{\varphi }(1+r)}{6\pi }}}{\displaystyle \frac{1}{{({\gamma }_{\varphi }+r)}^2}}{\displaystyle \frac{1}{t}},$$

(40)

thus, the consequence of the condition ${\rho }_{\varphi }\sim {\rho }_{\mathrm{m}}$ is the logarithmic evolution of the scalar field $\varphi$ with time.

Applying the equation for the energy density for the scalar field ${\rho }_{\varphi }=\frac{1}{2}{\dot{\varphi }}^2+V\left(\varphi \right)$ and Equation (36), it can be derived

$${\rho }_{\varphi }=\frac{2V\left(\varphi \right)}{2-{\gamma }_{\varphi }}=\frac{{\dot{\varphi }}^2}{{\gamma }_{\varphi }},$$

(41)

which together with Equations (39) and (40) leads to

$$V\left(\varphi \right)={\displaystyle \frac{M_{\mathrm{pl}}^2}{6\pi }}(1-{\displaystyle \frac{{\gamma }_{\varphi }}{2}}){\displaystyle \frac{1+r}{{({\gamma }_{\varphi }+r)}^2}}{\displaystyle \frac{1}{t^2}}\Rightarrow {\displaystyle \frac{\partial V\left(\varphi \right)}{\partial \varphi }}=-\lambda V\left(\varphi \right),$$

(42)

where $\lambda =\sqrt{\frac{24\pi }{M_{\mathrm{pl}}^2{\gamma }_{\varphi }(1+r)}}$. Equation (42) implies that the potential has the exponential form

$$V\left(\varphi \right)=V_0{e}^{-\lambda (\varphi -{\varphi }_0)}.$$

(43)

A significant drawback of this model is the absence of a convincing explanation for the onset of the interaction of dark energy and matter at the epoch of transition from the decelerated to the accelerated expansion of the universe. The thermal quantum-field theory treatment of the quintessence dark energy coupled to the matter field shows that one can consistently recover different expansion regimes of the universe, including the late-time acceleration, however more work is needed to relate the matter field to a viable dark matter candidate [191,192].

3. Constraints From Observational Data

3.1. Type Ia Supernovae

The observed magnitudes of type Ia supernovas are one of the best data for constraining the distance redshift relationship through the determination of the luminosity distance. In the $\varphi$CDM models, the distances tend to be smaller compared to the $\mathsf{\Lambda }$CDM predictions at the same redshift. This provides an opportunity for differentiating these models from each other.

One of the first studies in this direction was performed in Podariu and Ratra [193]. They used three datasets of SNe Ia apparent magnitude versus redshift: (i) R98 data [162], both including and excluding the unclassified SN Ia 1997ck at $z=0.97$ (with 50 and 49 SNe Ia apparent magnitude data, respectively), (ii) P99 data [2], and (iii) a third set with the corrected/effective stretch factor magnitudes for the 54 Fit C SNe Ia of P99 apparent magnitude data, and obtained constraints on the $\varphi$CDM model with RP potential ($\varphi$CDM-RP model) (see Figure 4).

Caresia et al. [194] obtained constraints on parameters of the $\varphi$CDM with the RP and Sugra potentials [177,195], and also the extended quintessence models with the inverse power-law RP potential [196,197], from datasets of apparent magnitude versus redshift measurements of 176 SNe Ia [2,162,198], and data of the SuperNovae Acceleration Probe (SNAP) satellite [199]1. Obtained constraints on model parameters are shown in Figure 5 and Figure 6. No useful constraints on the model parameters were found for the Sugra potential, while $1\sigma$ constraints of $\alpha <0.8$ and $\alpha <0.6$, for both the extended and ordinary quintessence models using the RP potential, were obtained using the SNe Ia apparent magnitude and SNAP satellite data respectively.

Doran et al. [200] considered a DE model parameterized as [200]

$${\mathsf{\Omega }}_{\varphi }\left(a\right)=\frac{e^{R\left(a\right)}}{1+e^{R\left(a\right)}},w\left(a\right)=w_{0}lna/{(1-blna)}^2,$$

(47)

where $R\left(a\right)=ln({\mathsf{\Omega }}_{\varphi }\left(a\right)/(1-{\mathsf{\Omega }}_{\varphi }\left(a\right))$ corresponds to

$$R\left(a\right)=R_0-\frac{2w_{0}lna}{1-blna},$$

(48)

the constant b is defined by the EoS parameter at present epoch $w_0$, the dark energy density parameter at present epoch ${\mathsf{\Omega }}_{\varphi 0}$, and the parameter ${\mathsf{\Omega }}_e$ characterizing the amount of dark energy at early times to which it asymptotes for very large redshifts, as

$$b=-3w_0\left(ln\frac{1-{\mathsf{\Omega }}_e}{{\mathsf{\Omega }}_e}+ln\frac{1-{\mathsf{\Omega }}_{\varphi 0}}{{\mathsf{\Omega }}_{\varphi 0}}\right).$$

(49)

Using a combination of datasets from SNe Ia [162], Wilkinson Microwave Anisotropy Probe (WMAP) [201], Cosmic Background Imager (CBI) [202], Very Small Array (VSA) [203], SDSS [204], and HST [205], the authors find $w_0<-0.8$ and ${\mathsf{\Omega }}_e<0.03$ at the $1\sigma$ confidence level; the contours are shown in Figure 7. It should be noted that the SNe Ia apparent magnitude data are most sensitive to $w_0$, while CMB temperature anisotropies and LSS growth rate are the best constraints of ${\mathsf{\Omega }}_e$ (see Figure 8).

Fuzfa & Alim [206] studied the $\varphi$CDM model with the RP and Sugra potentials in a spatially closed universe. The estimated values of ${\mathsf{\Omega }}_{\mathrm{m}0}$ and ${\mathsf{\Omega }}_{\varphi 0}$, using SNe Ia apparent magnitude data from the SNLS collaboration [207], are quite different than those for the standard spatially flat $\mathsf{\Lambda }$CDM model (Figure 9). Such a result is expected due to the different cosmic acceleration and dark matter clustering predicted between quintessence models and the standard $\mathsf{\Lambda }$CDM model, arising from differences in cosmological parameters, even at $z=0$. The quintessence scalar field creates more structures outside the filaments, lighter halos with higher internal velocity dispersion, as seen from N-body simulations performed by the authors to study the influence of quintessence on the distribution of matter on large scales.

Pavlov et al. [208] found that for the $\varphi$CDM-RP model in a spacetime with nonzero spatial curvature, the dynamical scalar field has an attractor solution in the curvature dominated epoch, while the energy density of the scalar field increases relative to that of the spatial curvature. In the left panel of Figure 10, we see that the values ${\mathsf{\Omega }}_{\mathrm{m}0}=0.27$ and $\alpha =3$ are consistent with these constraints for a range of values ${\mathsf{\Omega }}_{\mathrm{k}0}$, for a set of values of $H_0{t}_0$2. The right panel of Figure 10 shows a similar analysis for several values of the cosmological test parameter $▵({\mathsf{\Omega }}_{\mathrm{m}0},{\mathsf{\Omega }}_{\mathrm{k}0},\alpha )=\delta \left(t_0\right)/(1+z_i)\delta \left(t_i\right)$, where $\delta \left(t_0\right)$ and $\delta \left(t_i\right)$ are the values of the matter density contrast at respectively at the present time $t_0$, and an arbitrary time $t_i$ such that $a\left(t_i\right)\ll a\left(t_0\right)$, i.e., a time when the universe is well approximated by the Einstein-de Sitter model in the matter-dominated epoch.

Farooq et al. [209] constrained the $\varphi$CDM-RP model in a spacetime with non-zero spatial curvature, as well as the XCDM model, using the Union2.1 compilation of 580 SNe Ia apparent magnitude measurements of Suzuki et al. [210], Hubble parameter observations [28,30,211,212], and the $0.1\le z\le 0.75$ BAO peak length scale measurements [21,22,213] (see Figure 11). They constrain the spatial curvature density parameter today to be $|{\mathsf{\Omega }}_{\mathrm{k}0}|\le 0.15$ at $1\sigma$ confidence level, and more precise data are required to tighten the bounds on the parameters.

Assuming that the Hubble constant $H_0$ tension of the $\mathsf{\Lambda }$CDM model is actually a tension on the SNe Ia absolute magnitude $M_B$, Nunes & Di Valentino [139] assessed the $M_B$ tension by comparing of spatially flat $\mathsf{\Lambda }$CDM model, wCDM and IDE models using two datasets compilation SNe Ia Pantheon sample [163]+ BAO [22,24,25,215,216] + big bang nucleosynthesis (BBN) [217] and SNe Ia Pantheon sample + BAO [22,24,25,215,216] + BBN [217] + $M_B$ [218] (see Figure 12). They found that the IDE model can alleviate both the $M_B$ and $H_0$ tensions with a coupling different from zero at 2$\sigma$ confidence level with a preference for a compilation of Pantheon + BAO + BBN + $M_B$ datasets.

3.2. Cosmic Microwave Background Radiation Data

The CMB provides a very accurate determination of the angular diameter distance at a redshift of $z\sim 1000$. This measurement is sensitive to the entire expansion of the universe over this wide range of redshifts. As pointed out before, $\varphi$CDM models tend to predict smaller distances and can therefore be constrained with the CMB geometric measurements.

In one of the first such studies, Doran et al. [219] used CMB temperature anisotropy data from the BOOMERANG and MAXIMA experiments [220,221] to distinguish quintessential inflation models with different EoS parameters, described by a kinetic term $k\left(\varphi \right)$ of the cosmon field3: (i) the RP potential with $k\left(\varphi \right)=1$, (ii) the leaping kinetic term model which has $V\left(\varphi \right)=M_{\overline{\mathrm{pl}}}^{4}exp(-\varphi /M_{\overline{\mathrm{pl}}})$, $M_{\overline{\mathrm{pl}}}=\sqrt{8\pi }{M}_{\mathrm{pl}}$ is the reduced Plank mass, $k\left(\varphi \right)=k_{\min }+tanh[(\varphi -{\varphi }_1)/M_{\overline{\mathrm{pl}}}]+1$, ${\varphi }_1\approx 277$ eV and $k_{\min }=[0.05,0.1,0.2,0.26]$ [222], and (iii) the exponential potential with $V\left(\varphi \right)=M_{\overline{pl}}^{4}exp(-\sqrt{2}\alpha \varphi /M_{\overline{\mathrm{pl}}})$, $\alpha =\sqrt{3/2{\mathsf{\Omega }}_{\varphi 0}}$, and $k\left(\varphi \right)=1$ [134]. The dark energy density parameters today and at last scattering epoch, ${\mathsf{\Omega }}_{\varphi 0}$ and ${\mathsf{\Omega }}_{Œ\mathrm{ls}}$, and the averaged EoS parameter of the field $\varphi$ are used to parameterize the separation of peaks in CMB temperature anisotropies, which can be used to measure the value of ${\mathsf{\Omega }}_{\varphi }$ before the last scattering (see Figure 13).

Caldwell et al. [223] investigated how early quintessence dark energy, i.e., a non-negligible quintessence energy density during the recombination and structure formation epochs, affects the baryon-photon fluid and the clustering of dark matter, and thus the CMB temperature anisotropy and the matter power spectra. They showed that early quintessence is characterized by a suppressed ability to cluster at small length scales, as suggested by the compilation of data from WMAP [224,225], CBI [226,227], Arcminute Cosmology Bolometer Array Receiver (ACBAR) [228], the LSS growth rate dataset of Two degree Field (2dF) Galaxy Redshift Survey [229,230,231], and $L_{y-\alpha }$ forest [232,233]; these are shown in Figure 14. Furthermore, quintessential inflation models are compatible with these data for a constant spectral index of primordial density perturbations, as seen in the left panel of Figure 14.

Pettorino et al. [234] studied a class of extended $\varphi$CDM models, where the scalar field is exponentially coupled to the Ricci scalar and is described by the RP potential. The projection of the ISW effect on the CMB temperature anisotropy4 is found to be considerably larger in the exponential case with respect to a quadratic non-minimal coupling as seen in Figure 15. This reflects the fact that the effective gravitational constant depends exponentially on the dynamics of the scalar field.

Mukherjee et al. [235] conducted a likelihood analysis of the Cosmic Background Explorer - Differential Microwave Radiometers (COBE-DMR) sky maps to normalize the $\varphi$CDM-RP model in flat space5. As seen from Figure 16, this model remains an observationally viable alternative to the standard spatially flat $\mathsf{\Lambda }$CDM model.

Samushia and Ratra [238] constrainted model parameters of the $\mathsf{\Lambda }$CDM model, the XCDM model, and the $\varphi$CDM-RP model using galaxy cluster gas mass fraction data [239], for this, they introduced an auxiliary random variable as opposed to integrating over nuisance parameters of the Markov Chain Monte Carlo (MCMC) method. Two different sets of priors were chosen to study the influence of the type of priors on the obtained results – one set has [7] $h=0.73\pm 0.03$, ${\mathsf{\Omega }}_{\mathrm{b}}{h}^2=0.0223\pm 0.0008$ (1$\sigma$ errors), and the other set has $h=0.68\pm 0.04$ [240,241], and ${\mathsf{\Omega }}_{\mathrm{b}}{h}^2=0.0205\pm 0.0018$ [242]. The obtained constraints on the $\varphi$CDM model with the RP potential are shown in Figure 17. We see that ${\mathsf{\Omega }}_{\mathrm{m}}$ is better constrained than $\alpha$, whose best-fit value is $\alpha =0$, corresponding to the standard spatially flat $\mathsf{\Lambda }$CDM model, however, the scalar field $\varphi$CDM model is not excluded.

Chen et al. [243] constrained the scalar field $\varphi$CDM-RP model and the $\mathsf{\Lambda }$CDM model with massive neutrinos assuming two different neutrino mass hierarchies in both the spatially flat and non flat universes, using a joint dataset comprising of CMB temperature anisotropy data [12,244], BAO peak length scale data from 6dF Galaxy Survey (6dFGS), from SDSS - Main Galaxy Sample (MGS), Baryon Oscillation Spectroscopic Survey (BOSS)-LOWZ (galaxies within the redshift range $0.2<z<0.43$), BOSS CMASS-DR11 (galaxies within the redshift range $0.43<z<0.7$) [23], the joint light-curve analysis (JLA) compilation from SNe Ia apparent magnitude measurements [245], and the Hubble Space Telescope $H_0$ prior observations [29]. Assuming three species of degenerate massive neutrinos, they found the $2\sigma$ upper bounds of $\sum m_{\nu }<0.165\left(0.299\right)$ eV and $\sum m_{\nu }<0.164\left(0.301\right)$ eV respectively for the spatially flat (spatially non-flat) $\mathsf{\Lambda }$CDM model and the spatially flat (spatially non-flat) $\varphi$CDM model (see Figure 18). The inclusion of spatial curvature as a free parameter leads to a significant expansion of the confidence regions for $\sum m_{\nu }$ and other parameters in spatially flat $\varphi$CDM models, but the corresponding differences are larger for both the spatially non-flat $\mathsf{\Lambda }$CDM and spatially non-flat $\varphi$CDM models.

Park & Ratra [246] constrained the spatially flat tilted and spatially non-flat untilted $\varphi$CDM-RP inflation model by analyzing CMB temperature anisotropy angular power spectrum data from the Planck 2015 mission [247], BAO peak length scale measurements [26], a Pantheon collection of 1048 SNe Ia apparent magnitude measurements over the broader redshift range of $0.01<z<2.3$ [163], Hubble parameter observation [21,25,28,30,31,32,33,34,211,248], and LSS growth rate measurements [25] (see Figure 19 and Figure 20). Constraints on parameters of the spatially non-flat model was improved from $1.8\sigma$ to more than $3.1\sigma$ confidence level by combining CMB temperature anisotropy data with other datasets. Present observations favor a spatially closed universe with the spatial curvature contributing about two-thirds of a percent of the current total cosmological energy budget. The spatially flat tilted $\varphi$CDM model is a $0.4\sigma$ better fit to the observational data than is the standard spatially flat tilted $\mathsf{\Lambda }$CDM model, i.e., current observational data allow for the possibility of dynamical dark energy in the universe. The spatially non flat tilted $\varphi$CDM model better fits the DES bounds on the rms amplitude of mass fluctuations ${\sigma }_8$ as a function of the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}$ but it does not provide such a good agreement with the larger multipoles of Planck 2015 CMB temperature anisotropy data as the spatially flat tilted $\mathsf{\Lambda }$CDM model.

Constraints on model parameters in the XCDM and $\varphi$CDM-RP (spatially flat tilted) inflation models using the compilation of CMB [247] and BAO data [22,23,24,249,250,251] were derived by Ooba et al. [249]. The authors calculated the angular power spectra of the CMB temperature anisotropy using the CLASS code of Blas et al. (2011) [250], and executed the MCMC analysis with Monte Python (Audren et al. [251]). Results of this analysis are shown in Figure 21.

Having one additional parameter compared to the standard spatially-flat $\mathsf{\Lambda }$CDM model, both $\varphi$CDM and XCMB models better fit the TT + lowP + lensing + BAO peak length scale data than does the standard spatially-flat $\mathsf{\Lambda }$CDM model. For the $\varphi$CDM model, $▵{\chi }^2=-1.60$, and for the XCDM model, $▵{\chi }^2=-1.26$ relative to the $\mathsf{\Lambda }$CDM model. The improvement over the standard spatially-flat $\mathsf{\Lambda }$CDM model in $1.3\sigma$ and in $1.1\sigma$ for the XCDM model are not significant, but these dynamical dark energy models cannot be ruled out. Both the $\varphi$CDM and XCMB dynamical dark energy models reduce the tension between the Planck 2015 (Aghanim et al. [247]) CMB temperature anisotropy and the weak lensing constraints of the rms amplitude of mass fluctuations ${\sigma }_8$.

Park & Ratra [252] also constrained the Hubble constant $H_0$ value in the spatially flat and spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, $\varphi$CDM-RP models using various combinations of datasets: BAO peak length scale measurements [26], a Pantheon collection of 1048 SNe Ia apparent magnitude measurements over the broader redshift range of $0.01<z<2.3$ [163], and Hubble parameter observations [21,25,28,30,31,32,33,34,211,248]. The resulting constraints are shown in Figure 22. According to this analysis, the dataset slightly favors to the untilted spatially non-flat dynamical XCDM and $\varphi$CDM quintessential inflation models, as well as smaller Hubble constant $H_0$ values.

The compilation of the South Pole Telescope polarization (SPTpol) CMB temperature anisotropy data [253], alone and in combination with Planck 2015 CMB temperature anisotropy data [247] and non-CMB temperature anisotropy data, consisting of the Pantheon Type SNe Ia apparent magnitude measurements [163], BAO peak length scale measurements [22,24,25,26,248], Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211], and LSS growth rate data [25] was used by Park & Ratra [254] to obtain constraints on parameters of the spatially flat and untilted spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, scalar field $\varphi$CDM-RP quintessential quintessential inflation models The results obtained from constraints on parameters of the untilted spatially non-flat $\varphi$CDM model with the inverse power-law RP potential using only SPTpol CMB temperature anisotropy data and with combination of other datasets are presented in Figure 23. In each dark energy model, constraints on cosmological parameters from SPTpol measurements, Planck CMB temperature anisotropy and non-CMB temperature anisotropy measurements are largely consistent with one another. Smaller angular scale SPTpol measurements (used jointly with only Planck CMB temperature anisotropy data or with the combination of Planck CMB temperature anisotropy data and non-CMB temperature anisotropy data) favor the untilted spatially closed models.

Di Valentino et al. [88] explored the IDE models to find out if these models can resolve both the Hubble constant $H_0$ tension problem of the standard spatially flat $\mathsf{\Lambda }$CDM model and resolve the contradictions between observations of Hubble constant in high and low redshifts in the spatially non-flat $\mathsf{\Lambda }$CDM scenario.

The authors constrained on parameters of the spatially flat IDE and $\mathsf{\Lambda }$CDM models as well as the spatially non-flat IDE and $\mathsf{\Lambda }$CDM models applying CMB Planck 2018 data [13], BAO [22,24,25] measurements, 1048 data points in the redshift range $z\in (0.01,2.3)$ of the Pantheon SNe Ia luminosity distance data [163], a Gaussian prior of the Hubble constant ($H_0=74.03\pm 1.42\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$ at 1$\sigma$ CL), obtained from a reanalysis of HST data by the SH0ES collaboration [81].

Based on the results of this observational analysis, it was found that the Planck 2018 CMB data favor spatially closed hypersurfaces at more than 99% CL (with a significance of 5$\sigma$). While a larger value of the Hubble constant, i.e., alleviation of the Hubble constant tension (with a significance of 3.6$\sigma$) has been obtained for the spatially non-flat IDE models. The authors concluded that searches for other forms of the interaction function $\xi$ and the EoS for the dark energy component in IDE models are needed, which may further ease the tension of the Hubble constant. 1$\sigma$ and 2$\sigma$ confidence level contours on parameters of the spatially non-flat IDE model are shown in Figure 24.

3.3. Large Scale Structure Growth Rate Data

Another potentially powerful probe of $\varphi$CDM signatures is the growth rate in low redshift LSS. The growth rate is expected to be stronger in $\varphi$CDM models compared to their $\mathsf{\Lambda }$CDM counterparts.

Pavlov et al. [255] constrained the spatially flat $\varphi$CDM-RP, the XCDM, the wCDM, and the $\mathsf{\Lambda }$CDM models from future LSS growth rate data, by considering that the full sky space-based survey will observe $H_{\alpha }$-emitter galaxies over 15000 ${\mathrm{deg}}^2$ of the sky. For the bias and density of observed galaxies, they applied the predictions of Orsi et al. [256] and Geach et al. [257], respectively. They also assumed that half of the galaxies would be detected within the reliable redshift range, which roughly reflects the expected outcomes of proposed space missions, such as the ESA Euclidean Space Telescope (EUCLID) mission and the NASA Wide-Field Infrared Telescope (WFIRST) mission. The obtained results are shown in Figure 25, where we see that measurements of the LSS growth rate in the near future will be able to constrain scalar field $\varphi$CDM models with an accuracy of about 10%, considering the fiducial spatially flat $\mathsf{\Lambda }$CDM model, an improvement of almost an order of the magnitude compared to those from currently available datasets [213,258,259,260,261,262,263]. Constraints on the growth index parameter $\gamma$ are the most restrictive in the $\mathsf{\Lambda }$CDM model than in other models. In the $\varphi$CDM model, constraints on the growth index parameter $\gamma$ are about a third more tighter than in the wCDM and XCDM models.

Pavlov et al. [264] also obtained constraints on the above DE models from Hubble parameter $H\left(z\right)$ observations [28,30,211,212], from Union2.1 compilation of 580 SNe Ia apparent magnitude measurements [210], and a compilation of 14 independent LSS growth rate measurements within the redshift range $0.067\le z\le 0.8$ [21,22,213,265]. The authors performed two joint analyses, first for the combination of $H\left(z\right)$ and SNe Ia apparent magnitude data, and the other for measurements of LSS growth rate, Hubble parameter $H\left(z\right)$ and SNe Ia apparent magnitude; the results of these analyses are presented in Figure 26. Constraints on cosmological parameters of the spatially flat $\varphi$CDM model from LSS growth rate data are quite restrictive. In combination with SNe Ia apparent magnitude versus redshift data and Hubble parameter measurements, LSS growth rate data are consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model, as well as with the spatially flat $\varphi$CDM model.

Avsajanishvili et al. [266] constrained the parameters ${\mathsf{\Omega }}_{\mathrm{m}}$ and $\alpha$ in the spatially flat $\varphi$CDM-RP model. Applying only measurements of the LSS growth rate [267], the authors obtained a strong degeneracy between the model parameters ${\mathsf{\Omega }}_{\mathrm{m}}$ and $\alpha$, Figure 27 (Left panel). This was followed by obtaining constraints from a compilation of data from the LSS growth rate measurements [267], and the distance-redshift ratio of the BAO peak length scale observations and prior distance from CMB temperature anisotropy [268], which eliminated the degeneracy between ${\mathsf{\Omega }}_{\mathrm{m}}$ and $\alpha$, giving ${\mathsf{\Omega }}_{\mathrm{m}}=0.30\pm 0.04$ and $0\le \alpha \le 1.30$ at $1\sigma$ confidence level (the best-fit value for the model parameter $\alpha$ is $\alpha =0$). Constraints on ${\mathsf{\Omega }}_{\mathrm{m}}$ and $\alpha$ from data compilation of Gupta et al. (2012) and Giostri et al. (2012) are presented in Figure 27 (Right panel).

Avsajanishvili et al. [269] also constrained various quintessence and phantom scalar field $\varphi$CDM models presented in Table 1 and Table 2 using observational data predicted for the Dark Energy Spectroscopic Instrument (DESI) [248]. The parameters of these models were constrained using MCMC methods by comparing measurements of the expansion rate of the universe $H\left(z\right)$, the angular diameter distance, and the LSS growth rate predicted for the standard spatially flat $\mathsf{\Lambda }$CDM model with corresponding values calculated for the $\varphi$CDM models. Results of constraints for the Zlatev-Wang-Steinhardt potential, the phantom pNGb potential, and the inverse power-law RP potential are shown in Figure 28 and Figure 29. To compare quintessence and phantom models, Bayesian statistical tests were conducted, namely the Bayes factor, as well as the $AIC$ and $BIC$ information criteria, were calculated. The $\varphi$CDM scalar field models could not be unambiguously preferred, from the DESI predictive data, over the standard $\mathsf{\Lambda }$CDM spatially flat model, the latter still being the most preferred dark energy model. The authors also investigated how the $\varphi$CDM models can be approximated by the CPL parametrization, by plotting the CPL-$\mathsf{\Lambda }$CDM 3 sigma confidence level contours, using MCMC techniques, and displayed on them the largest ranges of the current EoS parameters for each $\varphi$CDM model. These ranges were obtained for different values of model parameters or initial conditions from the prior ranges. The authors classified the scalar field models based on whether they can or cannot be distinguished from the standard spatially flat $\mathsf{\Lambda }$CDM model at the present epoch, as seen in Figure 31. They found that all studied models can be divided into two classes: models that have attractor solutions and models whose evolution depends on initial conditions.

Figure 28. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters ($V_0$, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h, ${\varphi }_0$, $\dot{{\varphi }_0}$), for which the spatially flat $\varphi$CDM model with the Zlatev-Wang-Steinhardt potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 28. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters ($V_0$, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h, ${\varphi }_0$, $\dot{{\varphi }_0}$), for which the spatially flat $\varphi$CDM model with the Zlatev-Wang-Steinhardt potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 29. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters (k, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h, $V_0$, ${\varphi }_0$, $\dot{{\varphi }_0}$), for which the spatially flat $\varphi$CDM model with the phantom PNGB potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 29. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters (k, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h, $V_0$, ${\varphi }_0$, $\dot{{\varphi }_0}$), for which the spatially flat $\varphi$CDM model with the phantom PNGB potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 30. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters ($\alpha$, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h), for which the spatially flat $\varphi$CDM model with the RP potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 30. 1$\sigma$ and 2$\sigma$ confidence level contour plots for various pairs of free parameters ($\alpha$, ${\mathsf{\Omega }}_{\mathrm{m}0}$, h), for which the spatially flat $\varphi$CDM model with the RP potential is in the best-fit with the standard spatially flat $\mathsf{\Lambda }$CDM model. The figure is adapted from [269].

Figure 31. (Left panel) The comparison of the possible $w_0$ and $w_a$ values for quintessence dark energy potentials in the spatially flat scalar field $\varphi$CDM models with the CPL - $\mathsf{\Lambda }$CDM 1$\sigma$, 2$\sigma$, and 3$\sigma$ confidence level contours. (Right panel) The comparison of possible $w_0$ and $w_a$ values for phantom dark energy potentials in the spatially flat scalar field $\varphi$CDM models with the CPL - $\mathsf{\Lambda }$CDM 1$\sigma$, 2$\sigma$, and 3$\sigma$ confidence level contours. The figure is adapted from [269].

Figure 31. (Left panel) The comparison of the possible $w_0$ and $w_a$ values for quintessence dark energy potentials in the spatially flat scalar field $\varphi$CDM models with the CPL - $\mathsf{\Lambda }$CDM 1$\sigma$, 2$\sigma$, and 3$\sigma$ confidence level contours. (Right panel) The comparison of possible $w_0$ and $w_a$ values for phantom dark energy potentials in the spatially flat scalar field $\varphi$CDM models with the CPL - $\mathsf{\Lambda }$CDM 1$\sigma$, 2$\sigma$, and 3$\sigma$ confidence level contours. The figure is adapted from [269].

Peracaula et al. [270] constrained the spatially flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models by constructing three datasets: DS1/SP consisting of SNe Ia apparent magnitude+$H\left(z\right)$+BAO peak length scale+LSS growth rate+CMB temperature anisotropy data with matter power spectrum SP; DS1/BSP consisting of SNe Ia apparent magnitude+$H\left(z\right)$+BAO peak length scale+LSS growth rate+CMB temperature anisotropy data with both matter power spectrum and bispectrum; and DS2/BSP, which involves BAO peak length scale+LSS growth rate+CMB temperature anisotropy data with both matter power spectrum and bispectrum. These datasets include 1063 SNe Ia apparent magnitude data [79,163], 31 measurements of $H\left(z\right)$ from cosmic chronometers [35,211], 16 BAO peak length scale data [271,272], LSS growth rate data, specifically 18 points from data [21,272,273], one point from the weak lensing observable $S_8$ [274], full CMB likelihood from Planck 2015 TT+lowP+lensing [12]. The obtained constraints are shown in Figure 32 and Figure 33. The authors tested the effect of separating the expansion history data (SNe Ia apparent magnitude+$H\left(z\right)$) from CMB temperature anisotropy characteristics and LSS formation data (BAO peak length scale+LSS), where LSS includes redshift-space distortions (RSD) and weak lensing measurements, and found that the expansion history data are not particularly sensitive to the dynamic effects of dark energy, while compilation of data BAO peak length scale+LSS+CMB temperature anisotropy is more sensitive. Also the influence of the bispectral component of the matter correlation function on the dynamics of dark energy is studied. For this, BAO peak length scale+LSS data were considered, including both the conventional power spectrum and the bispectrum. As a result, when the bispectral component is excluded, the results obtained are consistent with previous studies by other authors, which means that no clear signs of dynamical dark energy have been found in this case. On the contrary, when the bispectrum component was included in the BAO peak length scale+LSS growth rate dataset for the $\varphi$CDM model, a significant dynamical dark energy signal was achieved at $2.5-3\sigma$ confidence level. The bispectrum can therefore be a very useful tool for tracking and examining the possible dynamical features of dark energy and their influence on the LSS formation in the linear regime.

Park & Ratra [275] constrained the tilted spatially flat and untilted spatially non-flat XCDM model by applying the Planck 2015 CMB temperature anisotropy data [247], BAO peak length scale measurements [26], a Pantheon collection of 1048 SNe Ia apparent magnitude measurements over the broader redshift range $0.01<z<2.3$ [163], Hubble parameter observations [21,25,28,30,31,32,33,34,211,248], and LSS growth rate measurements [25], and obtained results as shown in Figure 34 and Figure 35. These data slightly favor the spatially closed XCDM model over the spatially flat $\mathsf{\Lambda }$CDM model at $1.2\sigma$ confidence level, while also being in better agreement with the untilted spatially flat XCDM model than with the spatially flat $\mathsf{\Lambda }$CDM model at the $0.3\sigma$ confidence level. Current observational data is unable to rule out dynamical dark energy models. The dynamical untilted spatially nonflat XCDM model is compatible with the Dark Energy Survey (DES) limits on the current value of the rms mass fluctuations amplitude ${\sigma }_8$ as a function of the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}$, but it does not give such a good agreement with higher multipoles of CMB temperature anisotropy data, as the standard spatially flat $\mathsf{\Lambda }$CDM model.

3.4. Baryon Acoustic Oscillations Data

Samushia & Ratra [276] constrained the standard spatially flat $\mathsf{\Lambda }$CDM, the XCDM, and the$\varphi$ CDM-RP models from BAO peak length scale measurements [17,20], in conjunction with WMAP measurements of the apparent acoustic horizon angle, and galaxy cluster gas mass fraction measurements [239]. These constraints are presented in Figure 36. It is seen that the measurements of Percival et al. (2007) constrain the $\varphi$CDM model less effectively (left panel of Figure 36), while measurements of joint BAO peak length scale and galaxy cluster gas mass of the $\varphi$CDM model give consistent and more accurate constraints than those derived from other data, i.e., $\alpha <3.5$ (right panel of Figure 36).

The above models were also constrained by Samushia et al. [277] using lookback time versus redshift data [278], passively evolving galaxies data [211], current BAO peak length scale data, and SNe Ia apparent magnitude measurements. Applying a bayesian prior on the total age of the universe based on WMAP data, the authors obtained constraints on the $\varphi$CDM model as shown in Figure 37. Constraints on the $\varphi$CDM model by joint datasets consisting of measurements of the age of the universe, SNe Ia Union apparent magnitude and BAO peak length scale are more tighter than those obtained from datasets consisting of data of the lookback time and the age of the universe.

The quintessential inflation model with the generalized exponential potential $V\left(\varphi \right)\propto exp(-\lambda {\varphi }^n/M_{\mathrm{pl}}^n),n>1$ was studied by Geng et al. [131]. The authors extended this model including massive neutrinos that are non-minimally coupled with a scalar field, obtaining observational constraints on parameters using combinations of data: CMB temperature anisotropy [244,244], BAO peak length scale from BOSS [23,263], and 11 SNe Ia apparent magnitudes from Supernova Legacy Survey (SNLS) [207]. It was found that the upper bound on possible values of the sum of neutrino masses $\sum m_{\nu }<2.5$ eV is significantly larger than in the spatially flat $\mathsf{\Lambda }$CDM model (Figure 38). The authors concluded that the model under consideration is in good agreement with observations and represents a successful scheme for the unification of primordial inflaton field causing inflation in the very early universe and dark energy causing the accelerated expansion of the universe at the present epoch.

The compilation of CMB angular power spectrum data from the Planck 2015 mission [247], and BAO peak length scale measurements from the matter power spectra obtained by missions: 6dFGS [22], BOSS, LOWZ and CMASS [23], and SDSS-MGS [24] was applied by Ooba et al. [279] to obtain constraints on the spatially non-flat quintessential inflation $\varphi$CDM-RP model. The theoretical angular power spectra of the CMB temperature anisotropy were calculated using the Cosmic Linear Anisotropy Solving System (CLASS) code of Blas et al. [250], and the MCMC analysis was performed with Monte Python of Audren et al. [251]. The results of this analysis are presented in Figure 39. The authors also used a physically consistent power spectrum for energy density inhomogeneities in the spatially non-flat (spatially closed) quintessential inflation $\varphi$CDM model, and found that the spatially closed $\varphi$CDM model provides a better fit to the lower multipole region of CMB temperature anisotropy data compared to that provided by the tilted spatially flat $\mathsf{\Lambda }$CDM model. The former reduces the tension between the Planck and the weak lensing ${\sigma }_8$ constraints, while the higher multipole region of the CMB temperature anisotropy data is in better agreement with the tilted spatially flat $\mathsf{\Lambda }$CDM model than with the spatially closed $\varphi$CDM model (see Figure 40).

Ryan et al. [280] constrained the parameters of the $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models from BAO peak length scale measurements [22,24,25,26,248], and the Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211]. The results obtained for the $\varphi$CDM model are presented in Figure 41, which shows that this dataset is consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model. Depending on the value of the Hubble constant $H_0$ as a prior and the cosmological model under consideration, data provides evidence in favor of the spatially non-flat scalar field $\varphi$CDM model.

Chudaykin et al. [281] obtained constraints on the parameters of the oCDM, XCDM (here $w_0$CDM), and wCDM models by using the joint analysis from data of BAO peak length scale, BBN and SNe Ia apparent magnitude. The resulting constraints are completely independent of the CMB temperature anisotropy data but compete with the CMB temperature anisotropy constraints in terms of parameter error bars. The authors consequently obtained the value of the spatial curvature density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{k}0}=-0.{043}_{-0.036}^{+0.036}$ at 1$\sigma$ confidence level, which is consistent with the spatially flat universe; in the spatially flat XCDM model, the value of the dark energy EoS parameter at present epoch $w_0=-1.{031}_{-0.048}^{+0.052}$ at 1$\sigma$ confidence level, which approximately equals to the value of the EoS parameter for the $\mathsf{\Lambda }$CDM model; values of the $w_0$ and $w_a$ in the CPL parameterization of the EoS parameter of the wCDM model $w_0=-0.{98}_{-0.11}^{+0.099}$ and $w_a=-0.{33}_{-0.48}^{+0.63}$ at 1$\sigma$ confidence level. The authors also found that the exclusion of the SNe Ia apparent magnitude data from the joint data analysis does not significantly weaken the resulting constraints. It means that when using a single external BBN prior, full-shape and BAO peak length scale data can provide reliable constraints independent of CMB temperature anisotropy constraints. The resulting constraints on model parameters of the spatially flat XCDM and wCDM models are shown in Figure 42. The authors also tightened the observational constraints on cosmological parameters with the inclusion of the hexadecapole ($l=4$) moment of the redshift-space power spectrum (see Figure 43).

Bernui et al. [67] investigated the effect of BAO measurements on IDE models that have significantly different dynamic behavior compared to the prediction of the standard $\mathsf{\Lambda }$CDM model. The authors used the compilation of 15 transversal 2D BAO measurements [282,283] and CMB data [86] to constrain IDE models. It was found that transversal 2D BAO and traditional 3D BAO measurements can generate completely different observational constraints on the coupling parameter in IDE models. Moreover, in contrast to the joint Planck + BAO analysis, where it is not possible to solve the Hubble constant $H_0$ tension, the joint Planck + BAO (transversal) analysis agrees well with the measurements made by the SH0ES team and applied to the IDE models, solves the Hubble constant $H_0$ tension. 1$\sigma$ and 2$\sigma$ confidence level contours constraints on the coupling parameter $\xi$ in IDE model using the 2D transversal 2D BAO are shown in Figure 44.

3.5. Hubble Parameter Data

Samushia & Ratra [284] used the Simon, Verde & Jimenez (SVJ) [211] definition of the redshift dependence of the Hubble parameter $H\left(z\right)$ (so-called SVJ $H\left(z\right)$ data) to constrain cosmological parameters in the scalar field $\varphi$CDM-RP model. According to the results obtained (see Figure 45), using the $H\left(z\right)$ data, the constraints on the matter density parameter ${\mathsf{\Omega }}_{\mathrm{m}}$ are more stringent than those on the model parameter $\alpha$. Constraints on the matter density ${\mathsf{\Omega }}_{\mathrm{m}}$ are approximately as tight as the ones derived from the galaxy cluster gas mass fraction data [285] and from the SNe Ia apparent magnitude data [286].

Chen & Ratra [287] analyzed constrains on the model parameters of the $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models, using 13 Hubble parameter $H\left(z\right)$ data versus redshift [28,212]. The authors showed (see Figure 46) that the Hubble parameter $H\left(z\right)$ data yield quite strong constraints on the parameters of the $\varphi$CDM model. The constraints derived from the $H\left(z\right)$ measurements are almost as restrictive as those implied by the currently available lookback time observations, and the GRB luminosity data, but more stringent than those based on the currently available galaxy cluster angular size data. However, they are less restrictive than those following from the joint analysis of SNe Ia apparent magnitude and BAO peak length scale data. The joint analysis of the Hubble parameter $H\left(z\right)$ data with SNe Ia apparent magnitude and BAO peak length scale data favor the standard spatially flat $\mathsf{\Lambda }$CDM model but do not exclude the dynamical scalar field $\varphi$CDM model.

In [288], Farooq et al. obtained constrains on the parameters of the $\varphi$CDM-RP, the XCDM, the wCDM, and the $\mathsf{\Lambda }$CDM models from analysis of measurements of the BAO peak length scale, SNe Ia apparent magnitude [210], 21 Hubble parameter $H\left(z\right)$ [28,30,211,212]. The results of this analysis are shown in Figure 47. Constraints are more restrictive with the inclusion of 8 new $H\left(z\right)$ measurements [30] than those derived by Chen & Ratra [287]. This analysis favors the standard spatially flat $\mathsf{\Lambda }$CDM model but does not exclude the scalar field $\varphi$CDM model.

Farooq & Ratra [289] worked out constrains on the parameters of the $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models from measurements of the Hubble parameter $H\left(z\right)$ at redshift $z=2.3$ [290] and 21 lower redshift measurements [28,30,211,212]. Constraints with the inclusion of the new $H\left(z\right)$ measurement of Busca et al. are more restrictive than those derived by Farooq et al., Figure 48. As seen in this figure, the $H\left(z\right)$ constraints depend on the Hubble constant prior to $H_0$ used in the analysis. The resulting constraints are more stringent than those which follow from measurements of the SNe Ia apparent magnitude of Suzuki et al. (2012). This joint analysis consisting of measurements of $H\left(z\right)$, SNe Ia apparent magnitude, and BAO peak length scale favor the standard spatially flat $\mathsf{\Lambda }$CDM model, but the dynamical scalar field $\varphi$CDM model is not excluded as well.

Farooq & Ratra [291] found constraints on the parameters of the $\varphi$CDM-RP model from the compilation of 28 independent measurements of the Hubble parameter $H\left(z\right)$ within the range of redshift $0.07\le z\le 2.3$. Measurements of $H\left(z\right)$ require a currently accelerating cosmological expansion at $3\sigma$ confidence level. The authors determined the deceleration-acceleration transition redshift $z_{\mathrm{da}}=0.74\pm 0.05$. This result is in good agreement with the result obtained by Busca et al. [290], which is $z_{\mathrm{da}}=0.82\pm 0.08$ based on 11 measurements of $H\left(z\right)$ from BAO peak length scale data within the range of redshift $0.2\le z\le 2.3$. The resulting constraints with different priors of $H_0$ are demonstrated in Figure 49.

Farooq et al. [214] analyzed constraints on the parameters of the spatially flat $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models from a compilation of measurements of the Hubble parameter $H\left(z\right)$. To get this compilation, the authors used weighted mean and median statistics techniques to combine 23 independent lower redshifts $z<1.04$, Hubble parameter $H\left(z\right)$ measurements, and define binned forms of them. Then this compilation was combined with 5 $H\left(z\right)$ measurements at the higher redshifts $1.3\le z\le 2.3$. The resulting constraints are shown in Figure 50. As seen from the figure, the weighted mean binned data are almost identical to those derived from analysis using 28 independent measurements of $H\left(z\right)$. Binned weighted-mean values of $H\left(z\right)/(1+z)$ versus redshift data are presented in Figure 51. These results are consistent with a moment of the deceleration-acceleration transition at redshift $z_{da}=0.74\pm 0.05$ derived by Farooq & Ratra [291], which corresponds to the standard spatially flat $\mathsf{\Lambda }$CDM model.

Chen et al. [292] used 28 measurements of Hubble parameter $H\left(z\right)$ within the redshift range $0.07\le z\le 2.3$ [21,28,30,31,211,290,293] to define the value of the Hubble constant $H_0$ in the $\varphi$CDM-RP, the wCDM, and the spatially flat and spatially non-flat $\mathsf{\Lambda }$CDM models. The result obtained for the $\varphi$CDM-RP model is shown in Figure 52. The value of the Hubble constant $H_0$ is found as: for the spatially flat and spatially non-flat $\mathsf{\Lambda }$CDM model, $H_0=68.3_{-3.3}^{+2.7}\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$ and $H_0=68.4_{-3.3}^{+2.9}\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$; for the wCDM model, $H_0=65.0_{-6.6}^{+6.5}\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$; for the $\varphi$CDM model, $H_0=67.9_{-2.4}^{+2.4}\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$ (at 1$\sigma$ confidence level). The obtained $H_0$ values are more consistent with the smaller values determined from the recent CMB temperature anisotropy and BAO peak length scale data and with the values derived from the median statistics analysis of Huchra’s compilation of $H_0$ data.

Farooq et al. [142] determined constraints on the parameters of the $\varphi$CDM-RP, the XCDM, the wCDM, and the $\mathsf{\Lambda }$CDM models in the spatially flat and spatially non-flat universe. The authors used the updated compilation of 38 measurements of the Hubble parameter $H\left(z\right)$ within the redshift range $0.07\le z\le 2.36$ [21,25,28,30,31,32,33,34,211,248]. The result for these constraints is shown in Figure 53. The authors determined the redshift of the cosmological deceleration-acceleration transition, $z_{\mathrm{da}}$, and the value of the Hubble constant $H_0$ from the $H\left(z\right)$ measurements. The determined values of $z_{\mathrm{da}}$ are insensitive to the chosen model, and depend only on the assumed value of the Hubble constant $H_0$. The weighted mean of these measurements is $z_{\mathrm{da}}=0.72\pm 0.05(0.84\pm 0.03)$ for $H_0=68\pm 2.8(73.24\pm 1.74)\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$. The authors proposed a model-independent method to determine the value of the Hubble constant $H_0$. The $H\left(z\right)$ data are consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model while do not rule out the spatially non-flat XCDM and spatially non-flat $\varphi$CDM models.

3.6. Quasar Angular Size Data

Ryan et al. [143] determined constraints on the parameters of the spatially flat and spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, $\varphi$CDM-RP models using BAO peak length scale measurements [22,24,25,26,248], the Hubble parameter $H\left(z\right)$ data [21,30,31,32,33,34,211], and quasar (QSO) angular size data [294,295]. 1$\sigma$, 2$\sigma$ and 3$\sigma$ confidence level contours constraints on the parameters of the spatially non-flat $\varphi$CDM model with the RP potential from $H\left(z\right)$, QSO and BAO peak length scale datasets are presented in Figure 54. Depending on the chosen model and dataset, the observational data slightly favor both the spatially closed hypersurfaces with ${\mathsf{\Omega }}_{\mathrm{k}0}<0$ at $1.7\sigma$ confidence level, and the dynamical dark energy models over the standard spatially flat $\mathsf{\Lambda }$CDM model at a slightly higher than $2\sigma$ confidence level. Furthermore, depending on the dataset and the model, the observational data favor a lower Hubble constant value than the one measured by the local data at $1.8\sigma$ confidence level to $3.4\sigma$ confidence level.

Cao et al. [296] found constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models using $H_{II}$ starburst galaxy apparent magnitude measurements [297,298], the compilation of 1598 X-ray and UV flux measurements of QSO 2015 data within the redshift range $0.036\le z\le 5.1003$ and 2019 QSO data [299,300] only and in conjunction with BAO peak length scale measurements [22,24,25,26,248], Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211]. The constraints on the parameters of the spatially flat and spatially non-flat $\varphi$CDM model with the RP potential obtained from datasets mentioned above are shown in Figure 55. A combined analysis of all datasets leads to the relatively model-independent and restrictive estimates for the values of matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}$ and the Hubble constant $H_0$. Depending on the cosmological model, these estimates are consistent with a lower value of $H_0$ in the range of $2.0\sigma$ to $3.4\sigma$ confidence level. Combined datasets favor the spatially flat $\mathsf{\Lambda }$CDM, while at the same time do not rule out dynamical dark energy models.

The compilation of 1598 X-ray and UV flux measurements of QSO 2015 data within the redshift range $0.036\le z\le 5.1003$ and 2019 QSO data [299,300] only and in conjunction with BAO peak length scale measurements [22,24,25,26,248], Hubble parameter $H\left(z\right)$ data[21,28,30,31,32,33,34,211] was applied by Khadka & Ratra [145] to impose constraints on the parameters of the tilted spatially flat and untilted spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP quintessential inflation models. Obtained constraints for the untilted spatially non-flat $\varphi$CDM-RP model from the combination of various datasets and extended QSO data only are presented in Figure 56. In most of the models, the QSO data favor the values of the matter density parameter ${\mathsf{\Omega }}_{\mathrm{m}0}\sim 0.5-0.6$, while in a combined analysis of QSO data with $H\left(z\right)$ + BAO peak length scale dataset, the values of the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}$ are shifted slightly towards larger values. A combined set of data QSO + BAO peak length scale + $H\left(z\right)$ is consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model, but favors slightly both the spatially closed hypersurfaces and the dynamical dark energy models.

Khadka & Ratra [146] obtained constraints on the parameters of the tilted spatially flat and untilted spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, $\varphi$CDM-RP quintessential inflation models from a compilation of 808 X-ray and UV flux measurements of QSOs (quasi-stellar objects) within the redshift range $0.061\le z\le 6.28$ alone [299] and in conjunction with BAO peak length scale measurements [22,24,25,26,248], Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211]. 1$\sigma$, 2$\sigma$ and 3$\sigma$ confidence level contours constraints on the parameters of the untilted spatially non-flat $\varphi$CDM model with the RP potential from the combination of various datasets are presented in Figure 57. The constraints using only the QSO data are significantly weaker but consistent with those from the combination of the $H\left(z\right)$ + BAO peak length scale data. Combined analysis from QSO + $H\left(z\right)$ + BAO peak length scale data is consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model but slightly favors both closed spatial hypersurfaces and the untilted spatially non-flat $\varphi$CDM model.

Cao et al. [301] found constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models using the higher-redshift GRB data [302,303], starburst galaxy ($H_{II}$G) measurements [297,298,304], and QSO angular size (QSO-AS) data [294,295]. Constraints from the combined analysis of cosmological parameters of the spatially flat and non-flat $\varphi$CDM-RP model are presented in Figure 58. The constraints from the combined analysis of these datasets are consistent with the currently accelerating cosmological expansion, as well as with the constraints obtained from the analysis of the Hubble parameter $H\left(z\right)$ data and the measurements of the BAO peak length scale. From the analysis of the $H\left(z\right)$ + BAO peak length scale + QSO-AS + $H_{II}$G + GRB dataset, the model-independent values of the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}=0.313\pm 0.013$ and the Hubble constant $H_0=69.3\pm 1.2\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$ are obtained. This analysis favors the spatially flat $\mathsf{\Lambda }$CDM model but also does not rule out dynamical dark energy models.

Khadka & Ratra [147] determined constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from the compilation of X-ray and UV flux measurements of 2038 QSOs which span the redshift range $0.009\le z\le 7.5413$ [300,305]. The obtained results are shown in Figure 59. The authors found that for the full QSO dataset, parameters of the X-ray and UV luminosities $L_X-L_{UV}$ relation used to standardize these QSO data depends on the cosmological model, and therefore cannot be used to constrain the cosmological parameters in these models. Subsets of these QSOs, limited by redshift $z\le 1.5-1.7$, obey the $L_X-L_{UV}$ relation in a way that is independent of the cosmological model and can therefore be used to constrain the cosmological parameters. Constraints from these smaller subsets of lower redshift QSO data are generally consistent, but much weaker than those inferred from the Hubble parameter $H\left(z\right)$ and the BAO peak length scale measurements.

Cao et al. [151] determined constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models by analyzing total of 1383 measurements consisting of 1048 Pantheon SNe Ia apparent magnitude measurements of Scolnic et al. (2018) [163], and 20 binned SNe Ia apparent magnitude measurements of DES Collaboration [306,307], 120 QSO measurements [299,300,305], 153 $H_{II}$G data [297,298,304], 11 BAO peak length scale measurements [22,24,25,26,248], 31 Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211]. Constraints on the parameters of the spatially non-flat $\varphi$CDM model with the RP potential from that analysis of the data are shown in Figure 60. From the analysis of those datasets, the model-independent estimates of the Hubble constant, $H_0=68.8\pm 1.8\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, as well as the matter density parameter at the present epoch, ${\mathsf{\Omega }}_{\mathrm{m}0}=0.294\pm 0.020$ are obtained. While the constraints favor dynamical dark energy and slightly spatially closed hypersurfaces, they do not preclude dark energy from being a cosmological constant and spatially flat hypersurfaces.

Khadka & Ratra [148] found constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from 78 reverberation-measured $M{g}_{II}$ time-lag QSOs within the redshifs range $0.0033\le z\le 1.89$ [308,309]. The authors applied the radius-luminosity or $R-L$ relation to standardized 78 $M{g}_{II}$ QSOs data. In each model, the authors simultaneously determined the $R-L$ relation and parameters in these models, thus avoiding the problem of circularity. It was found that values of the $R-L$ relation parameter are independent of the model used in the analysis, which makes it possible to establish that current $M{g}_{II}$ QSOs data are standardizable candles. Constraints on parameters of the spatially flat and non-flat $\varphi$CDM-RP models, using $M{g}_{II}$ QSO-78 and BAO peak length scale + $H\left(z\right)$ data, are shown in Figure 61. Constraints derived from the QSO data only are significantly weaker than those derived from the combined set of the BAO peak length scale and the Hubble parameter $H\left(z\right)$ measurements but are consistent with both of them. The constraints obtained from the $M{g}_{II}$ QSOs data in conjunction with the BAO peak length scale + $H\left(z\right)$ measurements agree with the spatially flat $\mathsf{\Lambda }$CDM model as well as with spatially non-flat dynamical dark energy models.

Khadka & Ratra [149] found that the recent compilation of the QSO X-ray and UV flux measurements [305] includes the QSO data that appear to be not standardized via the X-ray luminosity and the UV luminosity $L_X-L_{UV}$ relation parameters that are dependent on both the cosmological model and the redshift, so it should not be used to constrain the model parameters. These data include a compilation of seven different subsamples. The authors analyzed these subgroups, and some combinations of subgroups to define which QSO subgroups are responsible for questions specified in the paper of Khadka & Ratra [147]. They considered that the largest of the seven sub-samples in this compilation, SDSS-4XMM QSOs, which contribute about $2/3$ of all QSOs have the $L_X-L_{UV}$ ratios that depend on both the accepted cosmological model and the redshift, and thus are the source of a similar problem found earlier when collecting the full QSO data.

The second and third largest subsamples, SDSS-Chandra and XXL QSOs, which together account for about $30\%$ of total QSO data, appear to be standardized. Constraints on the cosmological parameters from these subsamples are weak and consistent with the standard spatially flat $\mathsf{\Lambda }$CDM model or with the constraints from the better-established cosmological probes. Constraints on the cosmological parameters of the spatially flat and spatially non-flat $\varphi$CDM models with the RP potential, using SDSS-Chandra, XXL QSO data as well as $H\left(z\right)$ data, BAO peak length scale data are presented in Figure 62.

Khadka et al. [150] used 118 $H\beta$ QSO measurements [310] within the redshift range $0.0023\le z\le 0.89$ to simultaneously constrain cosmological model parameters and QSO 2-parameter radius-luminosity $R-L$ relation parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models. The authors found that the $R-L$ relation parameters for $H\beta$ QSOs data are independent in models under investigation, therefore QSO data seem to be standardizable through $R-L$ relation parameters. The constraints derived using $H\beta$ QSO data are weak, slightly favoring the currently accelerating cosmological expansion, and are generally in the $2\sigma$ tension with the constraints derived from analysis of the measurements of the BAO peak length scale and the Hubble parameter $H\left(z\right)$. Constraints on the cosmological parameters of the spatially flat and non-flat $\varphi$CDM-RP model, from the $H\beta$ QSO measurements, the $H\left(z\right)$ and BAO peak length scale data are presented in Figure 63.

Khadka et al. [311] determined constraints on the parameters of the spatially flat and spatially non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models using the observations of 66 reverberation-measured $M{g}_{II}$ QSOs within the redshift range $0.36\le z\le 1.686$. Constraints on the cosmological parameters of the spatially flat and spatially non-flat $\varphi$CDM models with the RP potential from various QSO datasets are shown in Figure 64. The authors also studied the two- and three-parameter radius-luminosity $R-L$ relations [312,313] for $M{g}_{II}$ QSO sources, and found that these relations do not depend on the assumed cosmological model, therefore they can be used to standardize QSO data. The authors found for the two-parameter $R-L$ relation that the data subsets with low-${\Re }_{FeII}$ and high-${\Re }_{FeII}$ obey the same $R-L$ relation within the error bars. Extending the two-parameter $R-L$ relation to three parameters does not lead to the expected decrease in the intrinsic variance of the $R-L$ relation. None of the three-parameter $R-L$ relations provides a significantly better measurement fit than the two-parameter $R-L$ relation. The results obtained differ significantly from those found by Khadka et al. [150] from analysis of reverberation-measured $H\beta$ QSOs.

Cao et al. [153] determined constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, $\varphi$CDM-RP models, as well as on the QSO radius-luminosity $R-L$ relation parameters from the 38 $C_{IV}$ QSO reverberation-measured data in the redshift range $0.001064\le z\le 3.368$. An improved method is used that takes into account more accurately the asymmetric error bars for the time-delay measurements. The authors found that the parameters of the $R-L$ relation do not depend on the cosmological models considered, and therefore, the $R-L$ relation can be used to standardize the $C_{IV}$ QSO data. Mutually consistent constraints on the cosmological parameters from $C_{IV}$, $M{g}_{II}$ and $H\left(z\right)$ + BAO peak length scale data allow conducting the analysis from $C_{IV}$ + $M{g}_{II}$ dataset as well as from the $H\left(z\right)$ + BAO peak length scale + $C_{IV}$ + $M{g}_{II}$ datasets. Although the $C_{IV}$ + $M{g}_{II}$ cosmological constraints are weak, they slightly (at $\sim 0.1\sigma$ confidence level) change the constraints from the $H\left(z\right)$ + BAO peak length scale + $C_{IV}$ + $M{g}_{II}$ datasets. The constraints on the cosmological parameters of the spatially flat and non-flat $\varphi$CDM-RP from various QSO datasets are shown in Figure 65.

3.7. Gamma Ray Burst Distances Data

Samushia & Ratra [314] derived constraints on the parameters of the spatially flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models using the observational datasets of SNe Ia Union apparent magnitude data [315], BAO peak length scale data [17], measurements of gamma-ray burst (GRB) distances [316,317]. The authors applied two methods for analyzing the GRB data fitting luminosity relation of GRB, Wang’s method [317] and Schaefer’s method [316]. The constraints on the cosmological parameters of the $\varphi$CDM model from analysis of the SNe Ia Union apparent magnitude data and the BAO peak length scale measurements, with and without the GRB measurements are presented in Figure 66. The constraints from the GRB data obtained by two different methods disagree with each other at more than 2$\sigma$ confidence level. The cosmological parameters of the $\varphi$CDM model could not be tightly constrained only by the current GRB data.

Khadka & Ratra [318] performed an analysis of constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from measurements of the peak photon energy and bolometric fluence of 119 GRBs extending over the redshift range of $0.34\le z\le 8.2$ [302,303], and Amati relation parameters [319], BAO peak length scale measurements [22,24,25,26,248], Hubble parameter $H\left(z\right)$ data [21,28,30,31,32,33,34,211]. Resulting constraints on the parameters of the spatially flat and spatially non-flat $\varphi$CDM model with the RP potential are presented in Figure 67.

The Amati relation between the peak photon energy of the GRB in the cosmological rest frame, $E_p$ and $E_{\mathrm{iso}}$ is given as

$$log\left(E_{\mathrm{iso}}\right)=a+blog\left(E_p\right),$$

(52)

where a and b are free parameters defined from data, representing points of intersection and slope in the Amati relation, respectively. $E_p$ and $E_{\mathrm{iso}}$ are specified as

$$E_{\mathrm{iso}}=\frac{4\pi D_{\mathrm{L}}^2(z,p)S_{\mathrm{bolo}}}{(1+z)},E_p=E_{p,\mathrm{obs}}(1+z),$$

(53)

where $D_{\mathrm{L}}(z,p)$ is the luminosity distance, p is a cosmological parameter, $S_{\mathrm{bolo}}$ is the measured bolometric fluence, $E_{p,\mathrm{obs}}$ is the measured peak energy of the GRB.

The resulting Amati relation parameters are almost identical in all considered cosmological models, which confirms the use of the Amati relation parameters to standardize these GRBs data. The constraints on the cosmological parameters of the models under consideration from the GRB data are consistent with the constraints obtained from the analysis of the BAO peak length scale and the measurements of the Hubble parameter $H\left(z\right)$ but are less restrictive.

Khadka et al. [320] analyzed constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from the GRB data. The authors considered eight different GRB datasets to test whether the current GRB measurements, which probe a largely unexplored range of cosmological redshifts, can be used to reliably constrain the parameters of these models. The authors applied the MCMC analysis implemented in Monte Python to find the most appropriate correlations and cosmological parameters for the eight GRB samples, with and without the BAO peak length scale and the $H\left(z\right)$ data.

They applied three Amati correlation samples [319] and five Combo correlation samples [321] to obtain correlations and constraints on the model parameters. Constraints on the parameters of the spatially non-flat $\varphi$CDM-RP model, using various datasets of GRB, as well as the BAO peak length scale + $H\left(z\right)$ data, are shown in Figure 68. The authors found that the cosmological constraints, determined from the A118 sample consisting of 118 bursts, agree but are much weaker than those following from the BAO peak length scale and the $H\left(z\right)$ data. These constraints are consistent with the spatially-flat $\mathsf{\Lambda }$CDM as well as with the spatially non-flat dynamical dark energy models.

Cao et al. [152] applied the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models in the analysis of the three (ML, MS, and GL) ($L_0-t_b$) Dianotti-correlated sets of GRB measurements collected by Wang et al. [322] and Hu et al. [323] that together explore the redshift range $0.35\le z\le 5.91$. The authors found that each dataset, as well as the combinations of MS + GL, ML + GL, and ML + MS, obey the cosmological model-independent Dainotti correlations [324,325,326]) and therefore are standardized. The luminosity of the plateau phase for GRBs that obey the Dainotti correlation is defined as

$$L_0={\frac{4\pi D_L^2{F}_0}{(1+z)}}^{1-{\beta }^{\prime }},$$

(54)

here $F_0$ is the GRB X-ray flux, ${\beta }^{\prime }$ is the spectral index in the plateau phase, and $D_L$ is the luminosity distance.

The authors applied these GRB data in combination with the best currently available Amati-correlated GRB data of Amati [319] that explore the redshift range $0.3399\le z\le 8.2$ to constrain the cosmological model parameters. As a result, constraints are weak, providing lower bounds on the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}$, moderately favoring the non-zero spatial curvature, and largely consistent with both the currently accelerated cosmological expansion and with constraints determined on the basis of more reliable data. Constraints of cosmological parameters of the spatially flat and non-flat $\varphi$CDM-RP model, using the Dianotti-correlated sets of the GRB measurements as well as the $H\left(z\right)$ and BAO peak length scale data are presented in Figure 69.

Cao et al. [154] used the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models to analyze compilation of data from 50 Platinum GRB within the redshift range $0.553\le z\le 5.0$. The authors found that these data obey the three-parameter fundamental plane or Dainotti correlation, independent of the cosmological model, and therefore they are amenable to standardization and can be used to constrain cosmological parameters. To improve the accuracy of the constraints for the GRBs data only, the authors excluded ordinary GRB data from the larger Amati-correlated A118 dataset of 118 GRBs and analyzed the remaining 101 Amati-correlated GRBs with 50 Platinum GRB datasets. This joint dataset of 151 GRBs is being investigated within the little-studied redshift range $z\in (2.3,8.2)$. Due to the consistency of cosmological constraints from the platinum GRB data with the $H\left(z\right)$ + BAO peak length scale dataset, the authors combined platinum GRB and the $H\left(z\right)$ + BAO peak length scale data to carry out the analysis and found small changes in the cosmological parameter constraints compared to the constraints from the $H\left(z\right)$ + BAO peak length scale data. The resulting constraints from the GRBs only are more stringent than those from the $H\left(z\right)$ + BAO peak length scale dataset but are less precise. The constraints on the cosmological parameters of the spatially flat and spatially non-flat $\varphi$CDM model with the RP potential, using platinum GRB measurements along with the $H\left(z\right)$ and BAO peak length scale data are presented in Figure 70.

Cao et al. [155] proposed the constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models, using the extended set of the GRB data including the 50 platinum GRBs within the redshift range $0.553\le z\le 5$ by Dainotti et al. [327], the LGRB95 data that contains 95 long GRBs measurements within the redshift range $0.297\le z\le 9.4$ by Dainotti et al. [327]. The compilation of the 145 GRB data sets was also used. The constraints on the cosmological parameters of the spatially flat and spatially non-flat $\varphi$CDM model with the RP potential, using various GRB datasets are shown in Figure 71. The authors also examined which of two correlations, the two-dimensional Dainotti correlation [328] or the three-dimensional Dainotti correlation [329,330], fits better the GRB datasets. Based on the results of $AIC$, $BIC$, and Deviation Information Criterion ($DIC$) analysis, the authors found that the three-dimensional Danotti correlation is much more preferable than the two-dimensional one for the GRB datasets.

3.8. Starburst Galaxy Data

Mania & Ratra [331] analyzed constraints on the parameters of the $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models from the $H_{II}$ starburst galaxy apparent magnitude versus redshift data of Siegel et al. [332]. The authors followed the Percival et al. [213] procedure to obtain these constraints. The results are demonstrated in Figure 72. These constraints are largely consistent but not as restrictive as those derived from the measurements of the BAO peak length scale, the SNe Ia apparent magnitude, and the CMB temperature anisotropy.

Cao et al. [333] derived constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from the compilation of the $H_{II}$ starburst galaxy ($H_{II}$G) data of Gonz$\acute{a}$lez-Mor$\acute{a}$n et al. [304] and the $H_{II}$G data of Gonz$\acute{a}$lez-Mor$\acute{a}$n et al. [334]. The authors tested the model independence of the QSO angular size measurements. They found that the new compilation of 2019 $H_{II}$G data provides tighter constraints and favors lower values of the cosmological parameters than those from the 2019 $H_{II}$G data. The use of QSO measurements gives model-independent constraints on the characteristic linear size $l_m$ of QSO within a sample. Analysis of the data of the $H\left(z\right)$, BAO peak length scale, the SNe Ia apparent magnitude-Pantheon, the SNe Ia apparent magnitude-DES, QSO, and the latest compilation of the $H_{II}$G data provides almost model-independent estimates of the Hubble constant, the matter density parameter at the present epoch, and the characteristic linear size, respectively, as $H_0=69.7\pm 1.2\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, ${\mathsf{\Omega }}_{\mathrm{m}0}=0.295\pm 0.021$, and $l_m=10.93\pm 0.25$ pc. Constraints on the parameters of the spatially non-flat $\varphi$CDM model with RP potential from various combinations of the $H_{II}$G, QSO, BAO peak length scale, and the $H\left(z\right)$ datasets, are shown in Figure 73.

Cao & Ratra [156] performed analysis of constraints on the parameters of the spatially flat and non-flat $\mathsf{\Lambda }$CDM, XCDM, and $\varphi$CDM-RP models from joint datasets consisting of data of the updated 32 $H\left(z\right)$ Hubble parameter, 12 BAO peak length scale, 1048 Pantheon SNe Ia apparent magnitudes, 20 binned DES-3yr SNe Ia apparent magnitudes, 120 QSO-AS and 78 $M{g}_{II}$ reverberation-measured QSO, 181 $H_{II}$ starburst galaxy, and 50 Platinum Amati-correlated GRB. As a result, the authors found that constraints from each dataset are mutually consistent. There is a slight difference between constraints determined from the set QSO-AS + $H_{II}$G + $M{g}_{II}$ QSO + A118 data and those from QSO-AS + $H_{II}$G + $M{g}_{II}$ QSO + Platinum + A101 data, so the authors considered only the cosmological constraints from the joint dataset $H\left(z\right)$ + BAO peak length scale + SNe Ia apparent magnitudes + QSO-AS + $H_{II}$G + $M{g}_{II}$ QSO + A118 (HzBSNQHMA). The model-independent value of the Hubble constant $H_0=69.7\pm 1.2\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, and the matter density parameter at present epoch, ${\mathsf{\Omega }}_{\mathrm{m}0}=0.295\pm 0.017$ obtained by using the HzBSNQHMA dataset. The obtained value of the constraint for $H_0$ lies in the middle of the spatially flat $\mathsf{\Lambda }$CDM model result of Planck Collaboration 2018 of Aghanim et al. [13] and the local expansion rate $H\left(z\right)$ result of Riess et al. [335], a bit closer to the former. Based on the $DIC$ analysis, the spatially flat $\mathsf{\Lambda }$CDM model is the most preferable, but both dynamic dark energy models and space curvature are not ruled out. Constraints on the cosmological parameters of the spatially flat and non-flat $\varphi$CDM-RP model, from various datasets, are shown in Figure 74.

3.9. X-Ray Gas Mass Fraction of Clusters Data

Using Chandra measurements of X-ray gas mass fraction of 26 rich clusters obtained by Allen et al. [336], Chen & Ratra [285] constrained the parameters of the $\varphi$CDM-RP, $\mathsf{\Lambda }$CDM, and the XCDM models. Resulting constraints are consistent with those derived from other cosmological tests but favor more the spatially flat $\mathsf{\Lambda }$CDM model, Figure 75. Constraints on the parameters of the $\varphi$CDM model are tighter than those derived from the SNe Ia apparent magnitude data of Podariu & Ratra [193], Waga & Frieman [337], redshift-angular size data of Chen & Ratra [338], Podariu et al. [339], gravitational lensing statistics of Chae et al. [340], Figure 75 (Left panel).

Wilson et al. [286] used the R04 gold SNe Ia apparent magnitude versus the redshift data of Riess et al. [162], and X-ray gas mass fraction of clusters data of Allen et al. [336] to constrain the $\varphi$CDM-RP model; the results are given in Figure 76. According to these results, the standard spatially flat $\mathsf{\Lambda }$CDM model is more preferable, but the $\varphi$CDM model is not ruled out either. The contours obtained from joint R04 gold SNe Ia apparent magnitude data and galaxy cluster gas mass fraction data are tighter constrained than those obtained by Podariu & Ratra [193] from earlier SNe Ia apparent magnitude versus redshift data.

Constraints on the model parameters $w_0$ and $w_a$ of the wCDM model using the X-ray temperature data of massive galaxy clusters within the redshift range $0.05\le z\le 0.83$ with massive galaxy clusters ($M_{\mathrm{cluster}}>8\times {10}^{14}{h}^{-1}{M}_{\odot }$ within a comoving radius of $R_{\mathrm{cluster}}=1.5h^{-1}\mathrm{Mpc}$), were determined by Campanelli et al. [341]. The results are presented in Figure 77. Current data on massive clusters weakly constrain $w_0$ and $w_a$ parameters around the $(w_0,w_a)=(-1,0)$ values corresponding to the $\mathsf{\Lambda }$CDM model. In the analysis including data from the galaxy cluster number count, Hubble parameter $H\left(z\right)$, CMB temperature anisotropy, BAO peak length scale, and the SNe Ia apparent magnitude, the values of $w_0=-1.{14}_{-0.16}^{+0.14}$ and $w_a=0.{85}_{0.60}^{+0.42}$ were obtained at $1\sigma$ confidence level.

Chen and Ratra [342] applied angular size versus redshift measurements for galaxy clusters from Bonamente et al. [343] to constraint parameters of the $\varphi$CDM-RP, the XCDM, and the $\mathsf{\Lambda }$CDM models. X-ray observations of the intracluster medium in combination with radio observations of the Sunyaev-Zel’dovich effect of galaxy clusters make it possible to estimate the distance from the angular diameter $d_A$ of galaxy clusters. The authors applied the 38 angular diameter distance measurements of Bonamente et al. (2006) to constrain cosmological parameters of the models presented above. The results are demonstrated in Figure 78. The analysis of the angular size measurements along with the more restrictive BAO peak length scale data and the SNe Ia apparent magnitude measurements favors the spatially flat $\mathsf{\Lambda }$CDM model but does not exclude the $\varphi$CDM model.

3.10. Reionization Data

Mitra et al. [144] studied the influence of dynamical dark energy and spatial curvature on cosmic reionization. For this aim, the authors examined reionization in the tilted spatially flat and untilted spatially non-flat XCDM and $\varphi$CDM-RP quintessential inflation models. Statistical analysis was performed based on a principal component analysis and the MCMC analysis using a compilation of the lower-redshift reionization data by Wyithe & Bolton [344], Becker & Bolton [345] to estimate uncertainties in the model reionization histories. The obtained constraints for the tilted spatially flat and untilted spatially non-flat dynamical inflation $\varphi$CDM model with the RP potential are shown in Figure 79. The authors found that regardless of the nature of dark energy, there are significant differences between the reionization histories of the spatially flat and spatially non-flat cosmological models. Although both the flat and non-flat models fit well the low-redshift $z\le 6$ reionization observations, there is a discrepancy between high-redshifts $z\ge 7$ Lyman-$\alpha$ emitter data by Songaila & Cowie [346], Prochaska et al. [347] and the predictions from spatially non-flat models.

3.11. Gravitational Lensing Data

Constraints on the parameters of two $\varphi$CDM models, with the RP and the pNGb potentials, were analyzed by Waga & Frieman [337]. These models predict radically different futures for our universe. In the model with the RP potential, the expansion of the universe will continue to accelerate. In the model with the pNGb potential, the present epoch of the expansion of the universe with acceleration will be followed by a return to the matter-dominated epoch. For these observational tests, the authors used the compilation of measurements: gravitational lensing statistics [348,349,350,351,352], and the high-z SNe Ia apparent magnitudes [162,353,354]. The results of these studies are presented in Figure 80, where it is shown that a large region of parameter space for the considered models is consistent with the SNe Ia apparent magnitude data if ${\mathsf{\Omega }}_{m0}>0.15$. The authors obtained the constraint on the model parameter $\alpha$ of the RP potential, $\alpha <5$. The $\varphi$CDM model with the pNGb potential is constrained by the SNe Ia apparent magnitude and lensing measurements at 2$\sigma$ confidence level.

Statistics of the strong gravitational lensing based on Cosmic Lens All-Sky Survey data of Myers et al. [355], Browne et al. [356] was applied by Chae et al. [340] to constrain parameters of the $\varphi$CDM-RP model. The results are presented in Figure 81. The maximum of the likelihood accords to the values of the matter density parameter at present epoch ${\mathsf{\Omega }}_{\mathrm{m}0}=0.34$ and the model parameter $\alpha =0$, i.e., to the standard spatially flat $\mathsf{\Lambda }$CDM model. For the $68\%$ confidence level, $0.18<{\mathsf{\Omega }}_{\mathrm{m}0}<0.62$ and $\alpha <2.7$, while for $95\%$ confidence level, ${\mathsf{\Omega }}_{\mathrm{m}0}=1$ and $\alpha =8$. Strong gravitational lensing constraints are favorable for the standard spatially flat $\mathsf{\Lambda }$CDM model, and consistent with Chen & Ratra [338] constraints from the SNe Ia apparent magnitude data, but are weaker.

3.12. Compact Radio Sources Data

The compact radio source angular size versus redshift data of Gurvits et al. [357] were used by Chen & Ratra [338] to derive constraints on the parameters of the $\varphi$CDM-RP model. These constraints are consistent with the results obtained from the SNe Ia apparent magnitude data of [2,162], but they are less restrictive, Figure 82.

Podariu et al. [339] used double radio galaxies called FRIIb sources, redshift-angular size data to constrain the parameters of the $\varphi$CDM-RP model in the spatially flat universe. These constraints are consistent both with the results obtained from the SNe Ia apparent magnitude data of [2,162] as well as with the results obtained from the compact radio source redshift-angular size data of Chen & Ratra in [338], but they are less restrictive, Figure 83.

4. Discussion and Conclusions

In this review, we presented papers devoted to observational constraints on cosmological parameters in dynamical dark energy models through cosmological observations. Our review does not claim to be a complete presentation of all research conducted by scientists in this area. We considered the most significant papers among numerous ones, where the authors applied different types of methods and observational constraints with various observational datasets to investigate dynamical dark energy models. Most of papers presented here are devoted to the study of the quintessence scalar field $\varphi$CDM model with the inverse power-law RP potential. This model is a simplest and a typical representative of a family of tracker quintessence scalar models, and in general, describes properties and features of tracker quintessence scalar field models. Due to the simplicity of the potential form, this model has attracted and will continue to attract many scientists to study it. This review is a kind of historical cross-section of the study of dynamical dark energy models, in which it is clearly seen that the complication, refinement, and increase in the diversity of cosmological data and methods for studying dynamical dark energy models lead to more precise constraints on values of cosmological parameters. At the same time, despite the refinement of observational data and complications of methods for studying dark energy in the universe, current observational data favor the standard spatially flat $\mathsf{\Lambda }$CDM model, while not excluding dynamical dark energy models and spatially closed hyperspaces.

We look forward to a larger and better compilation of various cosmological data, which should provide much tighter constraints on cosmological parameters in dynamical dark energy models than those obtained to date. To study GRB and X-ray for investigating the early universe, it is scheduled to launch: the Space-based multiband astronomical Variable Objects Monitor (SVOM) mission [358] (expected in 2023), the Transient High-Energy Sky and Early Universe Surveyor (THESEUS) mission [359] (expected in 2037), the Hydrogen Intensity and Real-time Analysis Experiment(HIRAX) (https://hirax.ukzn.ac.za) (planned). To investigate the weak lensing surveys BAOs peak length scale and RSD, it is planned to launch: the 4-metre Multi-Object Spectroscopic Telescope (4MOST) (https://www.eso.org/sci/facilities/develop/instruments/4MOST.html) (expected in 2023), and the BAO from Integrated Neutral Gas Observations (BINGO) project (https://bingotelescope.org) (planned). To investigate the acceleration expansion of the universe, the nature of the dark universe, the dynamics and evolution of the universe, and the growth of LSS in the universe, it is scheduled to launch: the Euclidean Space Telescope (EUCLID) (https://www.euclid-ec.org/) (expected in 2023), the Spectro-Photometer for the History of the universe (SPHEREx) (https://spherex) (expected in 2025), the Wide-Field Infrared Telescope (WFIRST) (https://web.archive.org/web/20150214063216/https://wfirst.gsfc.nasa.gov/observatory/) (expected in 2027), the ArmazoNes high Dispersion Echelle Spectrograph (ANDES) (https://elt.eso.org/instrument/ANDES/) (planned), the Extremely Large Telescope (ELT) (https://elt.eso.org) (expected in 2027), the Rubin Observatory Legacy Survey of Space and Time (Rubin/LSST) (https://lsst.org) (expected in 2024-2034), the Simons Observatory (SO) (https://simonsobservatory.org) (expected in 2024-2029). To explore the CMB radiation, it is planned to launch: the Cosmic Microwave Background-Stage IV (CMB-S4) experiment (https://cmb-s4.org) (expected in 2029-2036), and the Lite Satellite for the studies of B-mode polarization and Inflation from Cosmic Background Radiation Detection (LiteBIRD) (https://litebird.html) (planned), to study the fingerprint of primordial gravitational waves in CMB, it is also planned the SPIDER experiment (https://spider.princeton.edu).

After completing these missions, very precise measurements of GRB, X-ray temperature of massive galaxy clusters, the expansion rate of the universe $H\left(z\right)$, BAO peak length scale, CMB radiation, the angular diameter distance, and LSS growth rate of matter density fluctuations in the universe will be obtained. These precise measurements will constrain parameters in many dark energy models, and some of them may be precluded.