# The Peebles–Vilenkin quintessential inflation model revisited

## Abstract

We review the well-known Peebles–Vilenkin (PV) quintessential inflation model and discuss its possible improvements in agreement with the recent observations. The improved PV model depends only on two parameters: the inflaton mass *m*, and another smaller mass *M*; where the latter has to be chosen in order to undertake that, at present time, the dark energy density of the universe is approximately about 70% of the total energy budget of the universe. The value of the inflaton mass *m* is calculated using the observational value of the power spectrum of the scalar perturbations, and the value of mass *M*, which depends on the reheating temperature, is calculated by solving the corresponding dynamical system whose initial conditions are taken at the matter-radiation equality and are obtained from three observational data: the red shift at the matter-radiation equality, the ratio of the matter energy density to the critical one at the present time and the current value of the Hubble parameter.

## 1 Introduction

The understanding of physical cosmology at the fundamental level is quite cloudy, especially when a unified picture of the universe’s evolution is searched for. The inflation [1, 2, 3, 4, 5, 6, 7] − a rapid accelerating stage of the early universe − and quintessence [8, 9, 10, 11, 12, 13, 14, 15] − another accelerating stage of the late universe − are two significant phases of the universe’s evolution which are probably the main focus areas of the scientific community at present. Since inflation and quintessence present two different stages of the universe evolution, typically, they are considered as the effects of two different exotic sources. The scalar field theory has been found to be an excellent candidate for the inflationary scenario and for quintessence phase, another weakly interacting scalar field is usually considered. The common feature of these scenarios is that both of them should have an accelerating phase, but at the end are taking two different fields one for the inflation and the other for the quintessence. This disparity naturally raised a question to Peebles and Vilenkin (PV) and as a consequence they introduced, for the first time, a potential for the scalar field that allows inflation for early universe and quintessence for the current universe. This model by Peebles and Vilenkin is widely known as the “*quintessential inflation*” [16]. The introduction of the quintessential inflationary model also triggered other investigators [17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30].

Without any doubt, the “*quintessential inflation*” model by Peebles and Vilenkin is really elegant by its construction. The model is also very simple because it depends only on two parameters, one which characterizes the inflation and the other characterizes the quintessence phase. The potential has two pieces, one for early inflation and the other for quintessence. The inflationary piece is quartic in the PV model [16] and it is matched abruptly with a inverse power law potential (i.e., the quintessence potential) which is responsible to drive the current cosmic acceleration. Due to this abrupt matching, a phase transition from inflation to a kination regime occurs [31], where the adiabatic evolution of the universe is broken, and thus, the particles are produced following a reheating mechanism, such as, instant preheating or gravitational particle production of heavy massive or massless particles.

Due to simplicity and potentiality, the original PV model naturally gained a massive attention in the cosmological community. However, from the recent observational predictions, the model has been dignosed with some limitations. In particular, it was found that the quartic inflationary piece of this model leads to theoretical values of the spectral index (\(n_s\)) and the ratio of tensor to scalar perturbations (*r*) which do not enter into the corresponding two-dimensional marginalized joint contour at \(95\%\) confidence level [32]. While interestingly, if the quartic part of the inflationary potential is turned into quadratic one, then the aforementioned problem does not encounter. That means if the quartic potential is changed by a quadratic one, then for the typical number of *e*-folds in the quintessential inflation, i.e., between 60 and 75 (see for instance [25, 27]), the theoretical values provided by this potential enters in this contour [26]. Thus, the parameter characterizing this piece of the potential is the mass of the inflaton field, which is determined from the value of the power spectrum of scalar perturbations when the pivot scale leaves the Hubble radius. Moreover, the reheating mechanism in [16] is the gravitational particle production of massless particles which gives a reheating temperature of the order of 1 TeV, which according to the observational predictions seems to be not enough to solve the overproduction of Gravitational Waves (GW) and as a result this could affect the success of the Big Bang Nucleosynthesis process.

Thus, looking into the observational limitations of the PV model, in the present article we investigate the consequences of the replacement of the original quartic piece of the inflationary potential by the quadratic one and to study the evolution of the model up to the present epoch, which is related to the numerical value of the parameter *M* that characterizes the quintessence piece of the potential. In order to perform the calculations from both analytical and numerical grounds, we need three observational parameters, namely the redshift at the matter-radiation equality, the ratio of the matter energy density to the critical one at the present time and the current value of the Hubble parameter, which in the present work are chosen to be the central values of those parameters, obtained by the \(\Lambda \)CDM based Planck’s estimation [33].

The paper is organized as follows: In Sect. 2 we present our improved version of the original Peebles–Vilenkin quintessential inflation model, and its dynamics, i.e., the evolution of the universe, is studied from the beginning of inflation up to the end of the kination epoch. Section 3 is devoted to the study of the evolution of the universe from the end of kination to the matter-radiation equality for two different situations, namely, the massive particles produced at the end of inflation decay into lighter ones -in order to produce a relativistic plasma in thermal equilibrium- before or after the end of the kination phase. In Sect. 4 we study the evolution of the universe from the matter-radiation equality to the present where mostly we perform numerical calculations. The dynamics given by a quintessence exponential potential is studied in Sect. 5. Finally, we conclude the present work in Sect. 6 with all the findings in brief. The units used throughout the paper are, \(\hbar =c=1\), and we denote the reduced Planck’s mass by \(M_{pl}\equiv \frac{1}{\sqrt{8\pi G}}\cong 2.44\times 10^{18}\) GeV.

## 2 The original model

The first observational limitation of the model comes from the quartic inflationary potential as follows. For a number of *e*-folds in the range 60 and 75, which is usual in quintessential inflation, the spectral index, namely \(n_s\), and a ratio of tensor to scalar perturbations, namely *r*, do not enter in the marginalized joint confidence contour in the plane \((n_s, r)\) at \(2\sigma \) C.L. However, the values provided by a quadratic potential enter in this contour. Thus, it seems that the inflationary piece of the model might be changed, for example from quartic potential to quadratic potential, in order to match with the recent observational data [32, 33, 34, 35].

Another observational limitation of the model comes from the reheating mechanism. In the original PV model, the authors consider a reheating mechanism via gravitational particle production of massless particles that allows one to obtain a reheating temperature in the TeV regime. This reheating temperature is compatible with some of the usual Big Bang Nucleosynthesis (BBN) bounds, but it cannot prevent the overproduction of the gravitational waves (GWs). To overpass this problem one can consider other kind of reheating mechanisms such as the instant preheating [36, 37] or the gravitational production of heavy massive particles [38, 39]. Effectively, due to the phase transition from inflation to kination, there is an overproduction of GWs (see for instance Sect. 5 of [40]). Then, in order that this overproduction does not alter the BBN success, at the reheating time, the ratio of the energy density of GWs to the energy density of the produced particles has to be less than \(10^{-2}\) [16]. As was shown in [41], this bound is satisfied when the reheating occurs via instant preheating, and in the case that the reheating is via gravitational production of superheavy particles, the bound is only satisfied when its decay in lighter particles is after the end of the kination period (see for instance [38]).

To end this Section some remarks are in order:

### Remark 1

*e*-folds from the moment that the pivot scale crosses the Hubble radius to the end of inflation, is, for example, between 65 and 75, which usually happens in quintessential inflation due to the kination period after inflation [27], then the improved PV-model (2) enters in the \(2\sigma \) C.L. for the Planck likelihoods: Planck TT, TE, EE + low E, and Planck TT, TE, EE + low E + lensing. On the other hand, if one takes into account the “

*tensor sector*” and wants that a quintessential model matches with the Planck TT, TE, EE + low E+ lensing + BK14 + BAO likelihood, one has to consider other kind of potentials, such as plateau potentials [28] or \(\alpha \)-attractors [41, 45].

### Remark 2

Potentials with a sudden break have interesting properties. For example, in [46] a model with a local singularity of the potential in the slow-roll phase, was considered to study the deviation from a flat power spectrum. For our potential (2), the first derivative has a discontinuity at \(\varphi =-M_{pl}\) which enhances the gravitational production of superheavy particles as was shown in [47]. In fact, the greatest is the order of the first discontinuous derivative the lower is the energy density of the superheavy gravitationally produced particles, and thus the lower is the reheating temperature. This means that, in quintessential inflation, for smooth potentials such as plateau potentials or \(\alpha \)-attractors the particle creation has to be done via instant preheating [37]. On the other hand, as has been recently suggested, the abundance of dark matter could be explained via the production of only gravitationally interacting massive particles (GIMP) [48, 49, 50, 51], which could not be applied to smooth potentials, however, this mechanism of production of dark matter seems to work very well in PV models [52].

### Remark 3

which directs that for \(\alpha \) of the order of 1 and for a number of *e*-folds greater than 60, the ratio of tensor to scalar perturbations is less than 0.003. Thus, the spectral index and the tensor/scalar ratio enter perfectly in the two dimensional marginalized joint confidence contour at \(1\sigma \) CL for the Planck TT, TE, EE + low E+ lensing + BK14 + BAO likelihood.

## 3 Evolution from kination to matter-radiation equality

During the phase transition from inflation to kination the particles are produced. When the produced particles have very heavy masses, which occur in instant preheating or when one only considers heavy massive particles conformally coupled to gravity, these particles have to decay into light particles to form a relativistic plasma in thermal equilibrium whose energy density will eventually be dominant in order to match with the hot Friedmann universe. Two different cases may arise: when the decay of the heavy massive particles occurs before or after the end of the kination regime. Here, we will study both cases separately. It is also important to take into account that during this period the potential energy of the inflaton field, due its low value compared with the kinetic energy could be safely disregarded, which implies that the dynamical equations could be solved analytically.

### 3.1 Decay before the end of kination

We consider reheating via gravitational particle production of massive particles obtaining a reheating temperature is of the order \(T_{rh}=100\) TeV [38] and via instant preheating leading to a reheating temperature of the order \(T_{rh}=10^9\) GeV [36, 37].

To do it, we consider the central values obtained in [33] (see the second column in Table 4) of the red shift at the matter-radiation equality \(z_{eq}=3365\), the present value of the ratio of the matter energy density to the critical one \(\Omega _{m,0}=0.308\), and \(H_0=67.81\; \text{ Km/sec/Mpc }=5.94\times 10^{-61} M_{pl}\). Then, the present value of the matter energy density is \(\rho _{m,0}=3H_0^2M_{pl}^2\Omega _{m,0}=3.26\times 10^{-121} M_{pl}^4\), and at matter-radiation equality we will have \(\rho _{eq}=2\rho _{m,0}(1+z_{eq})^3=2.48\times 10^{-110} M_{pl}^4=8.8\times 10^{-1} \text{ eV }^4\). Now, using the relation at the matter-radiation equality \(\rho _{eq}=\frac{\pi ^2}{15}g_{eq}T_{eq}^4\) with \(g_{eq}=3.36\) (see [53]), we get \(T_{eq}=3.25\times 10^{-28} M_{pl}=7.81\times 10^{-10}\) GeV.

### Remark 3.1

*M*is completely degenerate as reported from the latest astronomical datasets [38], where the addition of baryon acoustic oscillations data into the cosmic microwave background radiation cannot break such a degeneracy. The low redshifts sample like Pantheon from the Supernovae Type Ia, and the Hubble parameter measurements from the cosmic chronometers also return similar conclusion. For \(V_4\) (that means, \(V_{\alpha }\) when \(\alpha =4\)) the central values of these parameters are (see the third column of the table 3 of [38]) \(\Omega _{m,0}=0.306\) and \(H_0=67.92 \frac{km/sec}{Mpc}\cong 5.95 \times 10^{-61} M_{pl}\). Then, taking into account that \(T_0\cong 2.7\) K \(\cong 2.33\times 10^{-13}\) GeV \(\cong 9.7\times 10^{-32} M_{pl}\) one gets, \(z_{eq}=3321\).

- 1.Reheating via production of heavy massive particles conformally coupled to gravity:$$\begin{aligned} \varphi _{eq} =\,&\varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl}\left( 1-\sqrt{\frac{2H_{eq}}{3H_{rh}}}\right) \nonumber \\ =\,&\varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl}\left( 1-\sqrt{\frac{2}{3}}\left( \frac{g_{eq}}{g_{rh}} \right) ^{1/4}\frac{T_{eq}}{T_{rh}}\right) \nonumber \\ \cong \,&\varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl} \cong 39.4 M_{pl}. \end{aligned}$$(14)$$\begin{aligned} {\dot{\varphi }}_{eq}=\,&{\dot{\varphi }}_{rh}\frac{t_{rh}}{t_{eq}} \sqrt{\frac{t_{rh}}{t_{eq}}}=\frac{4}{3}M_{pl}H_{eq}\sqrt{\frac{H_{eq}}{H_{rh}}}\nonumber \\ =&\,\frac{4\pi }{9}\sqrt{\frac{g_{eq}}{5}}\left( \frac{g_{eq}}{g_{rh}} \right) ^{1/4}\nonumber \\ \frac{T_{eq}^3}{T_{rh}}\cong \,&2.3\times 10^{-15} \text{ eV }^2, \end{aligned}$$(15)
- 2.Instant preheating:$$\begin{aligned} \varphi _{eq}= & {} \varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl} \left( 1-\sqrt{\frac{2H_{eq}}{3H_{rh}}}\right) \nonumber \\= & {} \varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl} \left( 1-\sqrt{\frac{2}{3}}\left( \frac{g_{eq}}{g_{rh}} \right) ^{1/4} \frac{T_{eq}}{T_{rh}}\right) \nonumber \\\cong & {} \varphi _{rh}+2\sqrt{\frac{2}{3}}M_{pl} \cong 24.4 M_{pl}. \end{aligned}$$(16)$$\begin{aligned} {\dot{\varphi }}_{eq}= & {} {\dot{\varphi }}_{rh}\frac{t_{rh}}{t_{eq}} \sqrt{\frac{t_{rh}}{t_{eq}}}=\frac{4}{3}M_{pl}H_{eq}\sqrt{\frac{H_{eq}}{H_{rh}}}\nonumber \\= & {} \frac{4\pi }{9}\sqrt{\frac{g_{eq}}{5}}\left( \frac{g_{eq}}{g_{rh}} \right) ^{1/4}\frac{T_{eq}^3}{T_{rh}}\nonumber \\\cong & {} 2.3\times 10^{-19} \text{ eV }^2. \end{aligned}$$(17)

### Remark 3.2

Since the Big Bang Nucleosynthesis occurs at temperatures about 1 MeV, for a reheating temperature, \(T_{rh}=100\) TeV, we have \(\Omega _{\varphi }(t_{BBN})\sim 10^{-16}\). However, if one wants a greater value of this parameter one has to consider lower reheating temperatures satisfying \(T_{rh}\gtrsim 1\) MeV.

### 3.2 Decay after the end of kination

In this case, which is only possible when reheating is due to the production of heavy massive particles, (in the case of instant preheating this will could produce an undesired new inflationary era [37, 43]), it is possible to obtain reheating temperature very close to 1 MeV [38]. So, here we consider \(T_{rh}=1\) MeV, which means that at the BBN epoch, \(\Omega _{\varphi }(t_{BBN})=\frac{{2}}{3}\cong 0.66\), and at the matter-radiation equality, \(\Omega _{\varphi , eq}\sim 10^{-13}\).

*heat efficiency*defined by \(\Theta =\frac{\rho _{\chi , kin}}{\rho _{\varphi , kin}}\) [54], and taking into account that

Summary of the initial conditions at the matter-radiation equality at different reheating temperatures is shown

Serial no. | Reheating temperature (\(T_{rh}\)) | \((x_{eq}, y_{eq})\) |
---|---|---|

1 | 100 TeV | \((39.4, 2.3\times 10^{-11})\) |

2 | \(10^9\) GeV | \((24.4, 2.3\times 10^{-15})\) |

3 | 1 MeV | (39.81, 0) |

*Calculation of the heat efficiency*\(\Theta \): The energy density of the produced massive particles with mass \(m_{\chi }=5\times 10^{-4}M_{pl}\) is given by \(\rho _{\chi ,kin}\cong 10^{-5}\left( \frac{m}{m_{\chi }} \right) ^2m^4= 6.25\times 10^{-31} M_{pl}^4\) [38] and the one of the inflaton field is \(\rho _{\varphi , kin}=3H_{kin}^2M_{pl}^2= \frac{1+\sqrt{3}}{2}m^2M_{pl}^2\cong 3.41\times 10^{-11} M_{pl}^4\), thus \(\Theta =1.83\times 10^{-20}\), which means that

## 4 Evolution from the matter-radiation equality

*e*-folds up to the present epoch, namely, \(N\equiv -\ln (1+z)=\ln \left( \frac{a}{a_0}\right) \). Now, using the variable

*N*, one can recast the energy density of radiation and matter respectively as,

*N*at the matter-radiation equality.

*K*is a parameter (with some dimension) that we will determine right now. Now, using the variable, \(N = - \ln (1+z)\), defined above and also using the conservation equation \(\ddot{\varphi }+3H{\dot{\varphi }}+V_{\varphi }=0\), one can construct the following non-autonomous dynamical system:

*N*, \({\bar{H}}=\frac{H}{K}\) and \({\bar{V}}=\frac{V}{K^2M_{pl}^2}\). Moreover, the Hubble equation now looks as

- 1.
For the reheating temperature \(T_{rh}=100\) TeV (the heavy massive particles decay before the end of kination): \(x_{eq}=39.4\) and \(y_{eq}=2.3\times 10^{-11}\).

- 2.
For the reheating temperature \(T_{rh}=10^9\) GeV (instant preheating): \(x_{eq}=24.4\) and \(y_{eq}=2.3\times 10^{-15}\).

- 3.
For the reheating temperature \(T_{rh}=1\) MeV (the heavy massive particles decay after the end of kination): \(x_{eq}=39.81\) and \(y_{eq}=0\).

*M*, which depends on the reheating temperature, we have solved numerically the dynamical system (29) with initial conditions \(x_{eq}\) and \(y_{eq}\) at \(N_{eq}=-8.121\), for different values of \({\bar{M}}\), which leads to the value \({\bar{H}}_0=3.53\times 10^{-2}\). Numerically, we have obtained that,

- 1.
\(T_{rh}=100\) TeV, \({\bar{M}}=7.43 \Longrightarrow M=18.1\) GeV.

- 2.
\(T_{rh}=10^9\) GeV, \({\bar{M}}=5.46 \Longrightarrow M=13.3\) GeV.

- 3.
\(T_{rh}=1\) MeV, \({\bar{M}}=7.48\Longrightarrow M=18.3\) GeV.

- 1.
For the potential \(V_2\) taking \(M={\bar{M}}\) eV, one gets \( {\bar{V}}_2(x)\cong 1.2\times 10^{-3} \frac{{\bar{M}}^4}{(1+x)^2}\). Numerically, we have obtained that, \({\bar{M}}=7.70,\; 6.11,\; 7.74\), for \(T_{rh} = 100\) TeV, \(T_{rh} = 10^9\) GeV, and \(T_{rh } = 1\) MeV respectively.

- 2.
In the same way, taking \(M=10^{2} {\bar{M}}\) TeV, one has \( {\bar{V}}_6(x)\cong 3.7\times 10^{-1} \frac{{\bar{M}}^8}{(1+x)^6}\). And by numerical calculations, we obtained that, \({\bar{M}}=8.62,\; 6.09,\; 8.69\), for \(T_{rh} = 100\) TeV, \(T_{rh} = 10^9\) GeV, and \(T_{rh } = 1\) MeV respectively.

*t*and the time

*N*as follows

From the numerical simulations, for the fixed values of \(\alpha \) (\(= 4\)) and reheating temperature \(T_{rh}=100\) TeV, we find that the epoch describing the phase \(\rho _m=\rho _{\varphi }\) happened at \(N= -0.28\) which in terms of the cosmic time gives, \( t-t_0= -1.77\times 10^{32} \text{ eV }^{-1}\cong 3.6\) billion years. That means, the equality of the matter and the scalar field happended at 3.6 billion years ago. And for \(w_{eff}\cong -1\Longleftrightarrow \frac{{\dot{H}}}{H^2}\cong 0\), i.e., the universe enters in a de Sitter phase at late times happens at \(N=1.40 \), that means, in terms of the cosmic time, this will happen within \( t-t_0=\) \(1.11\times 10^{33} \text{ eV }^{-1}\cong 22\) billion years.

*C*and \(\beta \) are parameters. Inserting \(\varphi _{tra}=-M_{pl}+Ct^{\beta }\) into (35) one obtains

We now close this section with the graphical variations of the cosmological parameters for the quintessence potential. Let us note that in all plots, we have considered the time period from \(N_{eq}\) to \(N=4\). In Fig. 2 we describe the evolution of the energy densities of different fluid components in the logarithmic units from which one can see that at present time the scalar field dominates over matter and radiation. The dimensionless density parameters for matter, radiation and the scalar field are shown in the left panel of Fig. 3 in the right panel of Fig. 3) we show the evolution of the effective EoS, \(w_{eff}\) from which one can clearly visualize a smooth transiton from \(w_{eff} = 0\) to the region with \(w_{eff} < -1/3\) and moreover we also find that \(w_{eff}\) approaches toward \(-1\) in an asymptotic manner. Finally, we compare the evolution of the tracker solution and our solution in Fig. 4 from which we may conclude that similar situation has been depicted in Fig. 2a of Ref. [18] showing that the tracker solution, which is defined during the matter domination era, does not catch the physical solution \(\varphi \) at the present time, and the universe is never driven by the tracker solution.

## 5 Exponential quintessence potential

*K*as in the previous section and writing \(M= {\bar{M}}\times 10^{-44} M_{pl}\) one can calculate that, for \(x\ge -1\) one has, \({\bar{V}}_{\gamma }(x)=4.14 \times 10^{18}{\bar{M}}^2 e^{-\gamma (x+1)}\).

## 6 Concluding remarks

The quintessential inflation model by Peebles and Vilenkin (PV) is an elegant unified description for the early- and late- evolutions of the universe [16] and this is the first attempt to unify these distant phases using a single scalar field potential. For extreme simplicity of the model and its potentiality as well, the PV model certainly gained a massive attention to the cosmological community since the end of nineties. Subsequently, with the rapid developments in the observational science, the theory of quintessential inflation has become a major area of cosmology for further examinations with a hope to offer a observationally viable single theoretical description for the universe’s evolution starting from its early phase to current stage.

Although the PV model is quite classic connecting inflation to quintessence, but according to the observational data, the model needs some simple improvements for the following reasons. For the inflationary piece of the model described by the quartic potential, the theoretical values of the spectral index (\(n_s\)) and the ratio of tensor to scalar perturbations (*r*) do not enter into the corresponding two-dimensional marginalized joint contour at \(95\%\) CL as reported by [32]. However, on the contrary, if the quartic part of the inflationary model is replaced by the quadratic function of the potential, then this problem does not appear. Additionally, for the reheating mechanism adopted in [16], the gravitational particle production of massless particles gives a reheating temperature of the order of 1 TeV, which according to the observational predictions is not so able to solve the overproduction of Gravitational Waves (GW). As a consequence, this might affect the success of the Big Bang Nucleosynthesis process.

Thus, keeping the above limitations, we have taken an attempt to perform some simple modifications of the PV model in agreement with the observational bounds. We have replaced the quartic piece of the inflationary potential by the quadratic one and consider the gravitational production of heavy massive particles for the reheating of our universe [38]. We find that the newly constructed quintessential inflation model, whose parameter *M* depends on the reheating temperature, can well behave with the observational data. In fact, we have studied the evolution of the universe starting from the matter-radiation equality up to present time by presenting the graphical variations of various cosmological parameters. In terms of the effective equation of state, \(w_{eff}\), we find that after the matter-radiation equality, the universe enters into the matter dominated era (\(\equiv w_{eff} = 0\)) and then to the present accelerating epxansion (\(w_{eff} < -1/3\)) and consequently, \(w_{eff} \rightarrow -1\), in an asymptotic manner. Finally, in Sect. 5, we have made a comparison of the quintessence potential of the improved PV model to that of an exponential potential.

Last but not least, we anticipate that the proposed improved version of the quintessential inflationary model will offer a new range of possibilities, both from theoretical and observational grounds because the improvements that we propose should subsequently improve other cosmological parameters in a similar fashion and this will enable one to understand the real improvement of this model. From the observational direction, in particular, there are several interesting investigations can be performed. The constraints using likelihood from Planck 2018 is a necessary work. Moreover, the inclusion of next generation of cosmological data sets will be surely interesting in order to quantify the free parameters of this model for a better conclusion. These all are kept for future works.

## Notes

### Acknowledgements

This investigation has been supported by MINECO (Spain) Grants MTM2014-52402-C3-1-P and MTM2017-84214-C2-1-P, and in part by the Catalan Government 2017-SGR-247. SP acknowledges the research grant through the Faculty Research and Professional Development Fund (FRPDF) Scheme of Presidency University, Kolkata, India.

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