Strong Gravitational Lensing by a Charged Kiselev Black Hole

We study the gravitational lensing scenario where the lens is a spherically symmetric charged black hole (BH) surrounded by quintessence matter. The null geodesic equations in the curved background of the black hole are derived. The resulting trajectory equation is solved analytically via perturbation and series methods for special choice of parameters and the distance of the closest approach to black hole is calculated. We also derive the lens equation giving the bending angle of light in the curved background. In the strong field approximation, the solution of the lens equation is also obtained for all values of the quintessence parameter $w_q$. For all $w_q$, we show that there are no stable closed null orbits and that corrections to the deflection angle for the Reissner-Nordstr\"om black hole when the observer and the source are at large, but finite, distances from the lens do not depend on the charge up to the inverse of the distances squared. A part of the present work, analyzed however with a different approach, is the extension of {\it Phys. Rev. D \textbf{92}, 084042 (2015)} where the uncharged case has been treated


I. INTRODUCTION
It is predicted by General Relativity (GR) that in the presence of a mass distribution, the light is deflected. However, it was not entirely a new prediction by Einstein, in fact, Newton had obtained a similar result by a different set of assumptions. In 1936, Einstein [1] noted that if a star (lens), the background star (source) and the observer are highly aligned then the image obtained by the deflection of light of a background star due to another star can be highly magnified. He also noted that optical telescopes at that time were not enough capable to resolve the angular separation between images.
In 1963, the discovery of quasars at high redshift gave the actual observation to the gravitational lensing effects. Quasars are central compact light emitting regions which are extremely luminous. When a galaxy appears between the quasar and the observer, the resulting magnification of images would be large and hence well separated images are obtained. This effect was named macro-lensing. The first example of gravitational lensing was discovered (the quasar QSO 0957+561) in 1979 [2].
The weak field theory of gravitational lensing is based on the first order expansion of the smallest deflection angle. It has been developed by several authors such as Klimov [3], Liebes [4], Refsdal [5], Bourassa [6][7][8], and Kantowski [9]. They were succeeded in explaining astronomical observations up to now (for more detailed see [10]).
Due to a highly curved spacetime by a black hole (BH), the weak field approximation is no longer valid. Ellis and Virbhadra obtained the lens equation by studying the strong gravitational fields [11]. They analyzed the lensing of the Schwarzchild BH with an asymptotically flat metric. They found two infinite sets of faint relativistic images with the primary and secondary images. Fritelli et al. [12] obtained exact lens equation and they compared them with the results of Virbhadra and Ellis. By using the strong field approximation, Bozza et al. [13] gave an analytical expressions for the magnification and positions of the relativistic images. From recent observational measurements, we can see that our Universe is dominated by a mysterious form of energy called "Dark Energy". This kind of energy is responsible for the accelerated expansion of our Universe [14,15]. Dark energy acts as a repulsive gravitational force so that usually it is modeled as an exotic fluid. One can consider a fluid with an equation of state in which the state parameter w(t) depends on the ratio of the pressure p(t) and its energy density ρ(t) such as: w(t) = p(t) ρ(t) . So far, wide variety of dark energy models with dynamical scalar fields have been proposed as alternative models to the cosmological constant. Such scalar field models include: quintessence [16][17][18][19], k-essence [20], quintom [21,22], phantom dark energy [23] and others.
Quintessence is a candidate of dark energy which is represented by an exotic kind of scalar field that is varying with respect to the cosmic time. The solution for a spherically symmetric spacetime geometry surrounded by a quintessence matter was derived by Kiselev [16]. There are few works focused on studying the Kiselev black hole (KBH). Thermodynamics and phase transition of the Reissner-Nordström BH surrounded by quintessence are given in [17,18,25]. The thermodynamics of the ReissnerNordstrmde Sitter black hole sur-rounded by quintessence has been investigated by one of us [18] and has led to the notion of two thermodynamic volumes. The properties of charged BH surrounded by the quintessence were studied in [18,26]. New solutions that generalize the Nariai horizon to asymptotically de Sitter-like solutions surrounded by quintessence have been determined in [18]. The detailed study of the photon trajectories around the charged BH surrounded by the quintessence is given in [27]. Recently, A. Younas and collaborators worked on the strong gravitational lensing by Schwarzschild-like BH surrounded by quintessence [24].
In the following paper, we will extend that work by adding a charge Q (charged KBH). We will consider the lensing phenomenon only for the case of nondegenerate horizons. By computing the null geodesics, we examine the behavior of light around a charged KBH. We analyze the circular orbits (photon region) for photons. Furthermore, we observe how both the quintessence and the charge parameters affects the light trajectories of massless particles (photons), when they are strongly deflected due to the charged KBH. We will not restrict the investigation to the analytically trackable cases w q = −1/3 and w q = −2/3, as some works did [26][27][28]; rather, we will consider the full range of the quintessence parameter w q and we will rely partly on the work done by one of us [18].
The paper is structured as follows: In Sec. II, we study the charged KBH geometry and we derive the basic equations for null geodesics. Additionally, in that section we write down the basic equations for null geodesics in charged Kiselev spacetime along with the effective potential and the horizons. In Sec. III, the analytical solution of the trajectory equation is obtained via perturbation technique. Sec. IV is devoted to the study of the lens equation to derive the bending angle. The strong field approximation of the lens equation is discussed as well. Finally, we provide a conclusion in Sec. VI. Throughout this paper, we adopt the natural system of units where c = G = 1 and the metric convention (+, −, −, −).

II. BASIC EQUATIONS FOR NULL GEODESICS IN CHARGED KISELEV SPACETIME
The geometry of a charged KBH surrounded by quintessence is given by [16] Here, M is the mass of the BH, w q is the quintessence state parameter (having range between −1 ≤ w q < −1/3), σ is a positive normalization factor and Q is the charge of the BH. The equation of state for the quintessence matter with isotropic negative pressure p q is linear of the form where ρ q is the energy density given by (taking G =h = 1) For a detailed metric derivation and a discussion of its properties, we refer the reader to the original paper by Kiselev [16]. For a further discussion see [17,18]. Note that not all the values of w q are manageable to find analytically solutions to the trajectory equation (See Sec. II). However, the cosmological constant case, corresponding to w q = −1, and the case w q = −2/3 are relatively simple.

A. Horizons in charged Kiselev black hole
In order to study the trajectories of photons near the space-time (1), one has to understand where the horizons are located for the charged KBH. In order to find the horizons, we require f (r) = 0, which depends on four parameters M, Q 2 , w q and σ. It has become custom to fix M, Q 2 and w q [17,18] and investigate the properties of these BHs upon constraining the values of σ in terms of M, Q 2 and w q . We proceed the same way in this work.
We are only interested in the case where the BH has three distinct horizons: a cosmological horizon r ch , an event horizon r eh , and an inner horizon r ah with r ch > r eh > r ah and f < 0 for 0 < r < r ah , f > 0 for r eh < r < r ch , (5) f < 0 for r > r ch .
The photon paths are all confined in the region where f ≥ 0. For M, Q 2 and w q fixed, the constraints for having three positive distinct roots of f (r) = 0 depend on the ratio Q 2 /M 2 . There will be three distinct horizons if [18] where Here u ch = 1/r ch , u eh = 1/r eh , u ah = 1/r ah . The points of intersection of the dashed parabola and the continuous line provide the locations of the three horizons (11): (u ch , u eh , u ah ). The point of intersection of the dotted parabola and the continuous line provides the only local maximum value (18) of the potential V eff (16) for u ch < u < u eh , which is the location of the photon sphere: u ps .
or if [18] where In Ref. [18] it was shown that under the above constraints (7) and (8) we have Introducing the variable u = 1/r, the horizon equation becomes f (r) = f (u) = 0, yielding the values of the three horizons. This equation takes the following form (−2 ≤ 3w q + 1 < 0) Figure 1, which is a plot of the parabola y = 1 − 2Mu + Q 2 u 2 and the curve y = σu 3w q +1 , shows the existence of three distinct horizons for Q 2 /M 2 ≤ 1 and Q 2 /M 2 > 1.
In the remaining part of this work we assume that the constraints (7) and (8) are satisfied.

B. Equations of motion for a photon
In the presence of a spherically symmetric gravitational field, we can confine the photon orbits in the equatorial plane by taking θ = π/2. Therefore, the Lagrangian for a photon travelling in a charged KBH spacetime will be given by where the dot represents the derivative with respect to the affine parameter λ for null geodesics. The Euler-Lagrange equations for null geodesics yielḋ In the above equations, E and L are constants known as the energy and angular momentum per unit mass. Using the condition for null geodesics g µν u µ u ν = 0, we obtain the equation of motion for photonṡ Here, b is the impact parameter which is a perpendicular line to the ray of light converging at the observer from the center of the charged KBH. Further, photons experience a gravitational force in the presence of the gravitational field. This force can be expressed via the effective energy potential which is given by ( In the left hand side of the above equation, the first term corresponds to a centrifugal potential, the second term represents the relativistic correction, the third term is due to the presence of the quintessence field while the fourth term appears due to the presence of electric charge. The terms appearing with positive (negative) signs correspond to repulsive (attractive) force fields.
In terms of u, V eff reads Since f (u eh ) = f (u ch ) = 0 and, by (5), f > 0 for u ch < u < u eh (u ch = 1/r ch , u eh = 1/r eh ), using (16) we see that V eff (u eh ) = V eff (u ch ) = 0 and V eff > 0 for u ch < u < u eh too. In the non-extremal case, in which we are interested, this implies that the potential V eff may have only an odd number of extreme values between the two horizons u ch and u eh ; that is, n + 1 local maxima and n local minima with n ∈ N. These extreme values are determined by the constraint dV eff /du = 0 which reads In absolute value, the slope of the parabola on the lhs of (18) is larger than that of the parabola on the lhs of (11) [recall −1 ≤ w q < −1/3]. Thus, referring to Fig. 1, the parabola on the lhs of (18) intersects the curve y = σu 3w q +1 at one and only one point between the two horizons u ch and u eh which provides the point at which the potential V eff has a local maximum and is, by this fact, the location of the photon sphere u ps . Therefore there is no stable closed orbit for the photons. If E 2 = V eff max , the photons describe unstable circular orbits. If E 2 < V eff max , the motion will be confined between the event horizon and the smaller root of V eff = E 2 or between the cosmological horizon and the larger root of V eff = E 2 . If E 2 > V eff max , the motion will be confined between the event and cosmological horizons.
In (16), if we take Q = 0, the effective potential reduces to the KBH effective potential, When we take σ = 0, (16) reduces to the Reissner-Nordström BH effective potential for photons, Further, when σ = Q = 0, the effective potential for the Schwarzschild BH is given by In Figs. 2 and 3, the effective potential V eff , i.e. Eq. (16), is plotted to study the behaviour of photons near a charged KBH for the non-extreme case where 0 < σ < 0.17 and 0 < Q < 1. We observe that in each curve, there are no minima. In these graphs each curve corresponds to the maximum value V max which means that for photons, only an unstable circular orbit exists. In these two figures, the effective potentials of Kiselev (19), Reissner-Nordström (20) and Schwartzschild (21) black holes are displayed as references. In Fig. 2 (Fig. 3), the quintessence parameter σ is varying (fixed) and the charge Q is fixed (varying). Both graphs are reciprocal to each other. We observe that by increasing the value of σ (Q), the photon has more (less) possibility to fell into the black hole.  In terms of u = 1/r, we rewrite (15) aṡ Combining this with (14) we obtain the following equations:

III. SOLUTION TO THE TRAJECTORY EQUATION
The presence of a cosmological horizon does not make sense to investigate the photon paths beyond it as is the case beyond the event horizon. The usual bending formula [30], developed for asymptotically flat solutions, no longer applies. The bending angle may be derived upon integrating either (23) or (24). The usually used approach is that of Ishak and Rindler [31]. In the so-far treated problems, σ is zero, so the approach consists in integrating which yields u 0 = sin φ/R, then construct by a perturbation approach a solution to of the form u = u 0 + u 1 , where in (25) the terms in u n with n > 1 are seen as perturbations in the limit u → 0. The approach described above does not hold if σ = 0 and −1 ≤ w q < −1/3; since −1 ≤ 3w q + 2 < 1, the term proportional to σ in (24) is rather a leading term in the limit u → 0. In the presence of quintessence, one should first solve or (with −1 ≤ w q < −1/3) as if M = 0 and Q = 0, then by a perturbation approach one solves (24). Unfortunately, Eqs. (26) and (27) are not tractable analytically except in the cases w q = −1 and w q = −2/3. In the tractable case w q = −2/3, Eq. (26) reduces to and it possesses the particular solution Since (24) is not equivalent to (23), from which it has been derived, one determines c from the reduced expression of (23) upon taking M = 0 and Q = 0: Substituting (29) into (30), we obtain and Figure 4 shows the real path that the light follows and the path that the light would follow in empty space (σ = 0, M = 0, Q = 0) for the same value of the physical ratio b = L/E of the angular momentum and energy. From that figure, it is obvious that in empty space c = 1/b, which is the same expression Eq. (31) reduces to on setting σ = 0. Here φ + ϕ = π/2 and tan ψ = r f |dφ/dr| = u f |dφ/du| (40).
If quintessence is the unique acting force (M = 0 and Q = 0), the minimum distance of approach r n , as shown in Fig. 4, corresponds to φ = π/2 and is derived from (32) by This can be derived directly from the definition of r n , which is the nearest distance from the light path to the lens. This is such that the r.h.s of (23) is 0, yielding the same expression as in (33).
In bending-angle problems the parameter b is assumed to be large to allow for series expansions in powers of 1/b. Since quintessence is not supported observationally, we make the statement that σ ≪ 1, which we will make clearer in the next section [Eq. (47)].
All authors who worked on the bending angle in a de Sitter-like geometry draw similar figure as Fig. 4 , but they make no distinction between b and r n ; rather, they use loosely a common notation R for b and r n . This remains more or less justified as far as quintessence is not taken into consideration where one may write b > ∼ r n . As we mentioned earlier, in bending-angle problems the parameter b is assumed large to allow for series expansions in powers of 1/b, so in presence of quintessence, one has to further assume bσ = Lσ E ≪ 1 [Eq. (47)] in order to have b > ∼ r n . In presence of quintessence, corrections in the expression of r n are needed: If σ ≪ 1 and bσ ≪ 1 we obtain to the first order in 1/b [see Eq. (39) for further orders of approximation] Now, substituting u = u 0 + u 1 into (24) reduces to (w q = −2/3) where u 0 is given by (32). A particular exact solution is where c is given by (31) and the coefficients (C 1 , C 2 , C 3 ) are related to the coefficients (B 1 , B 2 , B 3 ), which were first evaluated in Ref. [27], by C 1 = B 1 − sin φ, C 2 = B 2 , and C 3 = B 3 . 16 sin φ − 1 16 sin 3φ . Under the constraints σ ≪ 1 and bσ ≪ 1, expansions of the r.h.s of (36) and of u 0 (32) yield For (37) to hold it is sufficient that the products Mσ bσ and Q 2 σ 2 bσ remain much smaller than unity. This conclusion is easily derived from the requirement that u 1 /u 0 ≪ 1. As to the minimum distance r n = 1/u n , this is given by [setting φ = π/2 in (37)] We see that the mass M contributes to the second order while Q 2 contributes to the third order of the series expansion in powers of 1/b.

IV. LENS EQUATION -BENDING ANGLE
The expression of the angle ψ defined as the angle the direction φ makes with the light path at r, as depicted in Fig. 4, is given by [35] tan ψ = r f dφ dr = u f dφ du , or, preferably, by [36] sin ψ = bu f (u).
Series expansion of φ may be determined upon reversing the expansion (37). This is a cumbersome work which we will avoid in this section. Rather, we will rely on (40) and on the integral form of φ (23), to determine the deflection angle α. Figure 5 depicts a light path along with the locations of the lens (L: black hole), observer (O), source (S), and image (I). The observer sees the image along the direction OI, which is tangent to the light path at O. The angles β and θ are the angular positions of the source and image. The image location θ is the angle ∠ IOL, which is by definition ψ o = θ. The distances from the lens to the observer and to the source are denoted by r o = 1/u o and r s = 1/u s , respectively. The nearest distance from the light path to the lens, denoted by r n = 1/u n , is such that the r.h.s of (23) is 0, yielding In the special case w q = −2/3, we obtain 1/b 2 = u n (u n − 2Mu 2 n + Q 2 u 3 n − σ) a series solution of which is given by (39). In this section, instead of b, we will employ u n as an independent parameter around which we expand the deflection angle α. Let F(u) denote the function on the r.h.s of (23) where we have used (42). From Fig. 5, we see that the deflection angle α is given by where the sum of the first two terms is, according to  and ψ s = π − arcsin(bu s f (u s )). Using (42) in these expressions we arrive at The first line in (46) is the expression of the deflection angle we would have obtained had we assumed the observer and the source to be at spatial infinity (u o ≡ 0 and u s ≡ 0). The four last terms in (46) are corrections added to the asymptotically-flat expression of the deflection angle. From now on, we assume that the independent parameters (u o ≪ 1, u s ≪ 1, u n ≪ 1) are small compared to unity but are not 0. Another important parameter is σ. Since quintessence has not been observed in the cosmos, it is legitimate to assume σ ≪ 1; rather, we assume considering thus quintessence as a perturbation to the Reissner-Nordström black hole (the constarint max(u o , u s ) ≪ u n is satisfied by definition of u n ). The evaluation of (46) consists in determining the series expansion of its r.h.s in powers of the independent parameters (σ ≪ 1, u o ≪ 1, u s ≪ 1, u n ≪ 1). We will not assume the location of the observer to correspond to φ o = π/2, as some authors did [27,38], for this introduces a wrong term [39] in the series expansion 1 of α.

A. Case w q = −2/3
Conditions (47) being observed, we find in the case w q = −2/3: In the first line we recognize the expression of the deflection angle for the Reissner-Nordström black hole as determined in Ref. [37] (in Eq. (2.8) of Ref. [37], γ = 1 corresponds to Reissner-Nordström black hole and to obtain the first line in (48) from Eq. (2.8) of Ref. [37] insert r + + r − = 2M, r + r − = Q 2 , and r 2 + + r 2 − = 4M 2 − 2Q 2 , where r − < r + are the two horizons). The second line in (48) is a correction to the deflection angle for the Reissner-Nordström black hole when the observer and the source are at large, but finite, distances from the lens. Notice that this correction up to the power 2 in u o and u s does not depend on the charge of the black hole. The remaining terms, proportional to σ, are corrections due to quintessence.
The power series in the r.h.s of (48) has been determined as follows. The series expansions of the arcsin terms in (46) in powers of (σ, u o , u s , u n ) is straightforward; the series expansion of the first line in (46) has been done in Appendix A of Ref. [37]. In this work we show how to derive the series expansion of the first term in the second line of (46); the series expansion of the second term is obtained by mere substitution u o ↔ u s . In all calculations the series expansions are obtained in the order given in (47); that is, we first expand with respect to σ to order 1, then expand with respect to (u o , u s ) to order 2, and finally we expand with respect to u n to order 2 too. In the final expansion (48) we have kept all the terms with order not exceeding 2.
Set u = u o x and 0 ≤ x ≤ 1. The first term in the second line of (46) becomes yielding in the case w q = −2/3 where the integration over x is straightforward.
B. Case for all −1 ≤ w q < −1/3 In this section, we will obtain the general expression for the deflection angle for any value of w q . For simplicity, let us introduce a new constant which makes Eq. (23) easier to handle. Now, all the exponents in u in (23) are positive or zero. Since −1 ≤ w q < −1/3, the new constant lies between 0 ≤ γ < 2. Now, let us compute each term of Eq. (46) separately.
For sake of simplicity we will name each term of (46) as follows, so that Eq. (46) can be expressed as The final expression for α needs to be separated in three ranges of γ: i) γ = 0 , ii) 0 < γ ≤ 1 and iii) 1 < γ < 2.
In the following sections, we will follow the same idea as in Sec. V A to compute all these terms for any γ.

Computing I 1
Let u = u n x with 0 ≤ x ≤ 1. First, we expand the integrand of I 1 up to first order in σ and then up to second order in u n . By doing that, for 0 ≤ γ ≤ 1 the expansion of the integrand of (52) takes the form and for 1 < γ < 2, Integration over x will depend on γ so that it is not possible to write down an explicit result for I 1 for a general γ. Therefore, for 0 ≤ γ ≤ 1, we can write I 1 as follows Note that lim γ→0 Γ((γ + 1)/2)/Γ(γ/2) = 0 and lim γ→0 Γ((γ + 1)/2)/(γΓ(γ/2)) = √ π/2 are finite, so that the above expression is well defined for γ = 0. Now, for the range 1 < γ < 2, the integral becomes (59)

Computing I 2
First, we will compute the first term of I 2 and then we can directly use that result to compute the second term of I 2 by changing u o for u s . As we did before, we set u = u o x and expand up to first order in σ and then up to second order in u 0 . Finally, we need to take expansions up to second order in u n . The integrand of the first term of I 2 is then expanded as follows, Therefore, by integrating over x and then compute the second integral by changing u o by u s we arrive at

Computing I 3
By expanding the term I 3 as we did before, i.e., first up to first order in σ, then up to second order in u o and finally up to second order in u n we find

Computing α
Now, we have all the ingredients to find the final expression for α for a general γ. If we replace all the terms computed before in (55), for γ = 0 we find for 0 < γ < 1 we get Finally, for 1 < γ < 2 we find that the deflection angle becomes We see from (63)-(65), as was the case with (48) corresponding to γ = 1, that the corrections to the deflection angle for the Reissner-Nordström black hole (in the absence of quintessence) when the observer and the source are at large, but finite, distances (r o = 1/u o , r s = 1/u s ) from the lens do not depend on the charge up to u 2 o and u 2 s . All these corrections do not depend on σ and are symmetric functions of (u o , u s ), so they are easily recognized in Eqs. (63) to (65) and (48). Corrections due to quintessence are all functions of σ. Setting σ = 0 in any one of the equations (63) to (65) and (48) yields the deflection angle for the Reissner-Nordström black hole.
All integrals over x in Eqs. (63) to (65) do converge and could be given in closed forms, however, for some values of γ only. For instance, for γ = 3/2 the integral in (65) is given in terms of the complete elliptic integral E(m) and the complete elliptic integral of the first kind How quintessence affects the deflection angle can be seen from the coefficient C σ of σ in Eqs. (63)-(65), and (48). For instance, in (65) we have For fixed (u 0 , u s , u n ) satisfying (47), the coefficient C σ has a smooth variation for 1 ≤ γ < 2. This follows from the series expansions of C σ in the vicinity of γ = 2 and γ = 1, respectively: By (47), the second term in (67) is neglected with respect to the first term, so the coefficient C σ varies roughly between 0 (68) and some factor of π for 1 ≤ γ < 2. Thus, for γ larger than unity, the effect of quintessence almost drops and the values of the deflection angle are not very sensitive to variations in the values of γ.

VI. CONCLUSION
The motion of photons around black holes is one of the most studied problems in black hole physics. The behavior of light near black holes is important to study the structure of spacetime near black holes. In particular, if the light returns after circling around the black hole to the observer, it cause a gravitational lens phenomenon. Light passing by the black hole will be deflected by angle which can be large or small depending on its distance from the black hole.
In present paper, we have extended our previous work for the Kiselev black hole by including the effects of the electric charge. This extra parameter enriches the structure of spacetime with an additional horizon. By solving the geodesic equations, we have obtained the null geodesic structure for this black hole. Moreover the lens equation provides the information about the bending angle. For a general w q , we managed to find an analytical expression for the bending angle in the strong deflection limit considering quintessence as a perturbation to the Reissner-Nordström. Since this geometry is non asymptotically flat, one needs to be very careful to compute the bending angle since the standard approach, i.e. using the bending formula (See [30]), cannot be applied any more.
Instead of this approach, by using perturbation techniques and series expansions (assuming some physical conditions on the parameters), we directly integrate Eq. (23) for all w q to find the bending angle. The final expression of the bending angle in the strong limit Eqs. (63) to (65) and (48) contain some corrections to the deflection angle obtained by a Reissner-Nordström black hole, which are proportional to the normalization parameter σ, as well as corrections due to the finiteness of the distances of the source and observer to the lens.
It is instructive to compare the results of deflection in the presence of quintessence with those in the presence of phantom fields. In Ref. [37] light paths of normal and phantom Einstein-Maxwell-dilaton black holes have been investigated. It was emphasized that, in the presence of phantom fields, light rays are more deflected than in the normal case. Adopting the Bozza's formalism [40], the authors of Ref. [41] have shown that the lensing properties of the phantom field black hole are quite similar to that of the electrically charged Reissner-Norström black hole, i.e., the deflection angle and angular separation increase with the phantom constant. A similar approach was adopted in [42] to study lensing by a regular phantom black hole. These authors have demonstrated that the deflection angle does not depend on the phantom field parameter in the weak field limit, whereas the strong deflection limit coefficients are slightly different form that of Schwarzschild black hole (see also [43]). In our case, C σ (66) is positive for 1 < γ < 2. This means that the deflection angle is a bit larger if quintessence is present.
As a future work, one can also study the lensing for other interesting configurations such as "Nariai BHs", "ultra cold BHs" and also for rotating black holes surrounded by quintessence matter. This type of work might be important to study the highly redshifted galaxies, quasars, supermassive black holes, exoplanets and dark matter candidates, etc.