Fermionic spectral functions in backreacting p-wave superconductors at finite temperature

We investigate the spectral function of fermions in a p-wave superconducting state, at finite both temperature and gravitational coupling, using the AdS/CF T correspondence and extending previous research. We found that, for any coupling below a critical value, the system behaves as its zero temperature limit. By increasing the coupling, the “peak-dip-hump” structure that characterizes the spectral function at fixed momenta disappears. In the region where the normal/superconductor phase transition is first order, the presence of a non-zero order parameter is reflected in the absence of rotational symmetry in the fermionic spectral function at the critical temperature.


Introduction
One of the most relevant open problems in condensed matter theory is the understanding of high temperature superconductors. It is known that the standard BCS theory of low temperature superconductivity does not fit with the observed phenomenology, and that the correct description must take into account the high correlation of electrons in the fundamental state, that result in a strongly interacting Hamiltonian for the excitations. In such strongly interacting system, the usual perturbative treatment of quantum field theory does not apply, and the research has diversified into a bunch of alternative approaches [1].
In this context, an interesting issue is the description of the fermionic degrees of freedom, both in the normal and superconducting phases. These materials generically present a "strange-metal" phase which is not described by the standard Landau theory of the Fermi JHEP04(2017)087 liquid (for example, the resistivity scales linearly with temperature, while Landau theory predicts a quadratic behavior). Because of that, they are some times called "non-Fermi liquids". The fermionic spectral function is studied by making use of ARPES spectroscopy [2], uncovering a rich structure with the Fermi surface evolving into Fermi arcs as temperature and/or doping are varied and a gap opens in some directions of momentum space.
Superconductors are classified according to the symmetry of their gap function [3]. From this point of view, conventional BCS superconductors correspond to s-wave symmetry. Regarding unconventional high temperature superconductors, cuprates are believed to have d-wave symmetry, while some rutenates like Sr 2 RuO 4 are supposed to have a p-wave gap.
Holographic superconductors [4][5][6][7] are a class of theoretical models that share many defining features with high temperature superconductors. In particular, they are strongly coupled systems in which a superconducting phase arises at low temperatures. Moreover, the normal and superconducting states can propagate fermions that do not fit in the standard Landau description. The main difference with the laboratory systems is that, since holographic superconductors are described by means of the AdS/CFT correspondence, they require a large number of degrees of freedom at any spatial point, a condition referred as the "large N limit".
The AdS/CFT correspondence [8][9][10] is a powerful tool to study strongly interacting systems. Roughly, it describes a d-dimensional quantum field theory in the strong coupling regime (or "boundary theory") in terms of a weakly coupled gravity theory in at least one dimension higher (or "bulk theory"). The background of the bulk theory asymptotes Antide Sitter (AdS) space-time, while the boundary theory lives in the Minkowskian conformal boundary of AdS. Finite temperature states of the boundary theory are described by black hole backgrounds on the bulk side. On the other hand, finite chemical potential for a conserved particle number of the field theory is included by adding charge to the bulk solution.
In this setup, to model superconductors at finite temperature and chemical potential, a dynamical charged field describing the condensate needs to be added to the bulk theory. With this, we expect that for high temperatures the bulk background would be the AdS-Reissner-Nördstrom charged black hole dual to the normal phase, while for low temperatures the black hole would acquire a "hair" of the condensate field, that extends non-trivially up to the boundary. This is indeed what happens in the known holographic superconductor models.
For example, the s-wave holographic superconductor is modeled by adding a charged scalar field to the bulk, that is the dual to the scalar condensate. Below a critical temperature a solution with non trivial scalar hair appears, which have less free energy than the AdS Reissner-Nördstrom solution that describes the normal state. This hairy black hole breaks the U(1) gauge symmetry and, according to the AdS/CFT correspondence, this is interpreted in the field theory as the spontaneous symmetry breaking of a U(1) global symmetry due to the scalar condensate [4,5,[11][12][13].
In this paper we are interested in p-wave holographic superconductors, where the condensate is some component of a vector field. In order for it to be charged, a non-Abelian gauge field is required. In this system the normal phase is a solution with non JHEP04(2017)087 trivial electric component in some direction of the gauge algebra, representing the charge of the AdS Reissner-Nördstrom black hole. We assume that this choice breaks the gauge group to a residual U(1) gauge symmetry. Similarly to the s-wave case, the normal solution is energetically favored until a critical temperature is reached; below which a solution with a magnetic component in other gauge direction becomes non trivial, breaking spontaneously both the residual gauge U(1) and the spatial rotational symmetries. 1 This is interpreted according to AdS/CFT as giving rise to a new phase in the boundary system, with a non trivial vector condensate that spontaneously breaks a global U(1) symmetry [6]. The inclusion of the back-reaction of the gauge fields produces a change in the order of the phase transition at a critical gravity coupling, passing from second order to first order [14][15][16][17].
Holographic fermions in the normal phase were studied in references [18][19][20][21][22] among others, the conductivities for these systems were computed in [23,24]. The emerging picture is that of a Fermi liquid with a well defined Fermi surface, with or without longlived quasi-particles depending on the value of the parameters. Useful lectures on these subjects are [25,26]. Regarding the superconducting phase, fermionic degrees of freedom on the s-wave superconductor were studied in [27][28][29][30]. On the p-wave superconductor on the other hand, they were first analyzed in [15], for the case of vanishing temperature at finite gravitational coupling. The case of finite temperature was studied in the probe limit in [31]. It is the aim of this work to extend the computation to include both the effect of non-zero gravitational coupling and finite temperature [7].
The paper is divided as follows. In section 2 we review the solutions that describe a p-wave superconductor, for vanishing and non-vanishing temperature. Section 3 is devoted to the study of the equations of motion of fermions in the fundamental representation of SU(2), the analysis of the boundary conditions, and the computation of the correlation functions following [15,32]. In section 4 we present the numerical results, while that section 5 is left to discussion and conclusions. Two appendices with some relevant results regarding the spectral function are added at the end.
2 Bosonic sector: the holographic p-wave superconductor In this section we establish our conventions and revisit the construction of solutions dual to holographic p-wave superconductors [6], to be extensively used in rest of the paper. We first concentrate in the bulk solution, and then give the boundary interpretation.

The bulk gravitational solution
Our starting point is a gravitational theory whose bosonic sector is a gravity-Yang-Mills system in a 3 + 1 dimensional space-time, with Minkowskian metric G M N with M, N = 0, 1, 2, 3 and signature (− + ++), and gauge group SU(2) with Hermitean generators τ a 1 Higgs fields can be added but we will not do so here. Also isotropic solutions with A 1 x 1 = A 2 x 2 = 0 that preserve the diagonal subgroup of U(1)gauge × SO(2)rotation can be obtained. However they always have free energy higher than the anisotropic solutions to be considered here, as showed explicitly in reference [34].

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with a = 0, 1, 2. The action reads Here κ 2 ≡ 8 π G N with G N the Newton constant, L is the AdS scale related to the negative cosmological constant through Λ ≡ −3/L 2 , e is the gauge coupling and the gauge field The equations of motion derived from this action read where "∇" stands for the usual geometric covariant derivative. We are interested in solutions of the form [6,14,17,34] To understand this ansatz, we first observe that a non-vanishing φ(z) breaks the SU(2) gauge symmetry down to U(1) τ 0 , and selects a preferred time direction t. Then, a nonvanishing "magnetic" component W (z) breaks the residual U(1) τ 0 completely, and establishes a spatial anisotropy between x and y. Then if we take into account back-reaction effects the system cannot support a rotationally invariant metric, and that is why we need to include not only f (z) and s(z) but also an eventually non-trivial g(z). Replacing into the equations (2.2) we get JHEP04(2017)087 These symmetries will be useful in what follows in order to fix the asymptotic values of some of the fields. The expressions (2.4) represent a system of second order ordinary differential equations on the independent variable z, which moves in a certain interval z ∈ [z UV , z IR ]. It must be solved with boundary conditions at the frontiers z UV and z IR reflecting the desired physical situation. In what follows, we define z UV = 0 as the boundary of AdS. Close to z UV , the above equations can be expanded in powers of z and solved, to get the asymptotic behaviors where we used the first two symmetries in (2.5) to fix the normalization conditions s(0) = g(0) = 1, in such a way to identify the x µ 's as Minkowskian coordinates at infinity. The third symmetry will be used differently according to whether we are studying the zero or finite Beckenstein-Hawking entropy cases in the forthcoming sections. Now, by taking µ = 0 the boundary condition breaks explicitly the SU(2) gauge symmetry to a U(1) τ 0 subgroup. Next, putting W UV = 0, implies that there is no explicit breaking of the residual U(1) τ 0 gauge symmetry. Then, a non-vanishing value of the quantity W UV signals a spontaneous breaking of the remaining gauge U(1) τ 0 and rotational symmetries.
On the opposite extreme of the geometry, the value of z IR and the details of the asymptotic expansions depend on whether we want to study a solution with zero or finite entropy. In any case the Hawking temperature of the solution is determined by

Vanishing Beckenstein-Hawking entropy
In this case, we extend the geometry to the z IR → ∞ region to set our boundary conditions there. In such region, the equations of motion dictate the following behaviors

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In the above expressions we imposed smoothness conditions by putting to zero the coefficient of the divergent part of the solution to the linearised system. Generically, solutions with boundary conditions (2.6) and (2.8) are domain walls that interpolate between two AdS spaces with equal scales and different light velocities, and describe the true vacuum of the theory. According to (2.7), other than zero entropy they also have zero temperature. Such solutions were first studied in [15,33] and revisited more recently in [34]. We fix µ = 1 by using the last scaling symmetry in (2.5).
In figure 1 the functions f (z), g(z), W (z), φ(z) and s(z) corresponding to different values of the coupling λ are displayed. We see that rotational and gauge symmetries are broken by the functions g(z) and W (z). The linear behavior of W (z) at the boundary signals the breaking of the U(1) τ 0 remaining gauge symmetry. When λ → λ * ≈ 0.995 (corresponding to g YM * ≈ 0.71) a horizon at z h ≈ 2.462 forms and the solution tends to the extremal AdS-Reissner-Nördstrom black hole 3 (2.9) For couplings above this quantum critical value λ * only the AdS-Reissner-Nördstrom solution is present.

Non-vanishing Beckenstein-Hawking entropy
Now we consider solutions with a horizon at z IR = z h < ∞ such that f (z h ) ≡ 0. The asymptotic expansion of the well-behaved solution near the horizon reads The boundary conditions (2.6) and (2.10) are compatible with the AdS-Reissner-Nördstrom black hole solution where Q 2 ≡ λ 2 µ 2 z h 2 /2. The Hawking temperature of this black-hole solution is given by The zero temperature limit corresponds to the extremal (finite entropy) AdS-Reissner-Nördstrom black hole with Q 2 = 3 considered above in equation (2.9). In fact, the extremal condition implies that the relation λ * z h = √ 6 should hold, consistent with the values numerically found, λ * ≈ 0.995 and z h ≈ 2.462.
Conditions (2.6) and (2.10) are also compatible with a hairy "magnetic" W (z) = 0 solution, that breaks the residual U(1) τ 0 gauge symmetry. To obtain it, we carry out JHEP04(2017)087 numerical computations where, by using the last scaling symmetry in (2.5), we fix the position of the horizon at the value, z h = 1 [6,14].
In terms of the scaling invariant temperature T /µ, one gets that the AdS-Reissner-Nördstrom black hole solution is energetically favored for temperatures above a critical temperature T c . For lower temperatures, the non symmetric hairy solution is selected. As discussed for different models [12,35,36] one can interpret this result by stating that a condensate is formed above a black hole horizon because of a balance of gravitational and electrostatic forces.

The boundary QFT interpretation
The SU(2) gauge invariance of action (2.1) is realized in the boundary dual as a global SU(2) internal symmetry. The presence of a non-vanishing value of φ(z) at the boundary is interpreted as a finite chemical potential µ for the particles charged under such symmetry, and breaks the SU(2) global symmetry to a residual global U(1) τ 0 . The choice of the boundary condition W UV = 0 corresponds to turning off the source of the dual operator J 1 x in the QFT side, whose expectation value is given by W UV . In consequence the quantity W UV = J 1 x can be considered as the order parameter of the QFT, a non-vanishing value of which W UV = 0 signals the spontaneous breaking of the residual global U(1) τ 0 and rotational symmetries. A solution with non-vanishing W UV is thus interpreted as the dual of a p-wave superconducting phase [6]. On the other hand, the normal state of the system is described by the AdS-Reissner-Nördstrom solution (2.11) with W UV = 0.
The Hawking temperature of the bulk solution is interpreted as the temperature of the thermal bath in contact with the boundary theory. Since the AdS-Reissner-Nördstrom solution is energetically favoured for temperatures above T c , we can say the dual theory is in its normal phase for T > T c , while it goes into a superconducting anisotropic phase for T < T c . The value of T c and the order of the phase transition depend on the coupling λ. In figure 2(a) we display the phase diagram of the p-wave superconductor. We can distinguish three regions of the gravitational coupling, namely • When 0 ≤ λ ≤ λ c ≈ 0.62 the system has a second order phase transitions from the low temperature, hairy phase to the high temperature, normal phase at some T c (blue critical line).
• When λ c < λ ≤ λ * ≈ 0.995 the phase transitions become first order (red critical line). We note the presence of two spinodal curves above and below the critical line that signal the emergence of the two-branched hairy solution (T 1 ) and the disappearance of the unstable branch (T 2 ) respectively.
• For λ > λ * the symmetry broken phase ceases to exist.
The order parameter W UV and the free energies are shown in figures 2(b) and 2(1)(2)(3) respectively, for three different typical couplings In what follows, after introducing fermions in the bulk, we analyze how their spectral function changes over the whole phase diagram. 3 Fermionic sector: adding fermions to the holographic p-wave superconductor Now let us move on the fermionic sector, introducing fermionic degrees of freedom in the above defined setup. We do so in the gravitational side, and we interpret the numerical results from the QFT point of view.

Dirac spinors in the gravitational background
We consider Dirac spinors in the fundamental representation of SU (2), defined by the JHEP04(2017)087 Local gamma-matrices obey {Γ A , Γ B } = 2 η AB , and allow us to define a covariant derivative as usual and to introduce the projectors on eigenstates of Γ 3 given by P ± ≡ 1 2 (1∓Γ 3 ) with eigenvalues ∓1. It is well-known that a boundary term is needed to have a well-defined variational principle [37,38]. If we fix the boundary value of the Dirac fields to be the left (right)handed part Ψ + ≡ P + Ψ (Ψ − ≡ P − Ψ), the action to be considered is To solve these equations, we find convenient to work in momentum space and re-scale the spinors as Ψ( . By using the following representation of the Dirac Γ matrices where the 2+1 dimensional γ µ -matrices are: The equations of motion (3.4) then reads The generators of the Lorentz subgroup in 2 + 1 dimensions are, which displays the reducibility of the spinorial representation with respect to spin(1, 2), being i σ3/2 and −i σ1/2 the boosts generators and σ2/2 the generator of rotations in the (x − y)-plane. The left/right colored spinors ψ ± k (z) are thus Dirac spinors of the boundary theory.

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Now we can make explicit the color indices by writing ψ ± k = (ψ ± k αi ) where α = 1, 2 and i = 1, 2 are boundary spinor and color indices respectively. It will be convenient in what follows to introduce the four-tuples u k (z) and v k (z) as and the 4 × 4 real matrix In terms of this notation, equations (3.7) are compactly written as where we put m = 0 as we concentrate in such particular case in the rest of the paper. These equations need to be solved for the eight functions u k (z), v k (z). Since they are first order equations, the solutions are written in terms of eight undetermined constants. These constants are fixed by choosing boundary conditions at the frontiers z UV = 0 and z IR of the domain of the variable z. We make the choice of fixing the left-handed part Ψ + at the boundaries, that is u k (z), the action being as in (3.3) with the upper sign. Then, when we impose our boundary conditions at z IR , four of those constants are determined.
Equations (3.10) can be solved iteratively in the vicinity of any point z 0 by writing Here P entails for path ordering. The evolution operators C(z; z 0 ) and S(z; z 0 ) map the values u

Ingoing boundary conditions for vanishing Beckenstein-Hawking entropy
When the Beckenstein-Hawking entropy vanish, the boundary conditions must be imposed at z IR → ∞. The matrix U(z) is constant there where (w IR , s IR , g IR ) were introduced in (2.8). The eigenvalues of U IR are given by (3.14) The matrix U IR 2 is symmetric (although U IR it is not) and then it is diagonalizable by an Let us take z 0 = z ir 1, and let us consider the region z > z ir 1. There the evolution operators read where D = Diag(1/κ + , 1/κ + , 1/κ − , 1/κ − ). Now equations (3.11) implies that in the large z limit we have Let us first consider κ ± 2 > 0, and then κ ± ≡ + κ ± 2 . The condition that the solution to be well-behaved implies that the coefficients of the positive exponentials must vanish,

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yielding the solution where the initial values of the fields satisfy the linear relation Similar result is obtained when κ + 2 < 0 and/or κ − 2 < 0 under the imposition of ingoing boundary conditions, with the replacement κ ± → −i sign(ω) −κ ± 2 in (3.18). Regarding the case κ ± 2 = 0, that will be of particular importance later, we get implying the behaviors Notice that these are regular at the horizon witout imposing any additional relation between u (ir) k and u (ir) k .

Ingoing boundary conditions for non-vanishing Beckenstein-Hawking entropy
When the Beckenstein-Hawking entropy does not vanish, the horizon sits at z h = 1, and the matrix U(z) is not a constant matrix there but presents a simple pole where T is the Hawking temperature introduced in (2.12). Notice that C is pure imaginary, hermitian and satisfies C 2 = 1. Let us take now |1 − z ir | 1, and let us look at the near horizon region z ir < z ≤ 1. The evolution operators (3.12) at leading order then read From (3.11) they yield the solution

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Ingoing boundary conditions at the horizon fix again a linear relation between u After imposing this condition the near horizon solution reads, (3.26)

The ultraviolet behavior
Let us take now z 0 = z UV = 0 in equations (3.11), and consider the region close to the AdS boundary z → 0. There the matrix U(z) goes to a constant 27) and the evolution operators (3.12) at leading order are Plugging back into (3.11), the leading behavior results (3.29)

Normal modes and the Dirac cones
Normal modes can be defined generically as the "most normalizable" regular solutions with real energy. In the fermionic massless case we are considering, the behavior close to the AdS boundary is given by (3.29). The natural way to define normal modes should be to search for solutions where the leading terms at the boundary vanish. However, according to the boundary terms included in our action (3.3), the best thing we can do is to define fermionic normal modes as regular solutions with u (UV) k ≡ u k (z UV ) = 0. Due to the smoothness/ingoing boundary conditions on the horizon, the remaining components v (UV) k ≡ v k (z UV ) are then completely determined, and no condition can be imposed on them. In fact, let us take z 0 = z ir and z = z UV = 0 in (3.11) (3.30) But as we saw in subsections 3.1.1 and 3.1.2 a linear relation v k holds where, according to (3.19) or (3.25), the unimodular matrix L is given by L = U IR PD P t or L = C respectively. 5 Therefore (3.30) can be written as (3.31) 5 The normal modes are strictly defined at T = 0, so we will restrict to this case.

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which shows that for general momenta v (UV) k is determined once u (UV) k is given. However, for normal modes we fix the particular boundary condition u (UV) k = 0, and so there can exist a non trivial solution iff This equation defines a constraint in momentum space for any value of the frequency, where the normal modes live. Now, let us give some heuristic arguments to analyze some limits of this equation: • In first term let us consider highly energetic particles. Since they probe the near boundary region being essentially blind to the IR region, we can use (3.28) as an approximation for their evolution operators, i.e. C(0; z ir ) C(z ir ; 0) 1 , S(0; z ir ) −S(z ir ; 0) −U UV z ir . In such case, equation (3.32) reads Therefore in this limit the normal modes have their momentum and frequency such that the eigenvalues of U UV , given by (λ vanish. The equations λ ± 2 = 0 can then be taken as an approximation of the constraint C(ω, k x , k y ) = 0 for large |ω|. They define the two UV Dirac cones C U V ± [15], whose apexes are located at (ω, k x , k y ) = (∓µ/2, 0, 0), and that satisfy x +k 2 y = µ 2 /4}. Notice that they present rotational symmetry in the momentum plane, indicating that such symmetry is preserved in the UV.
• On the other hand, if we consider low energy modes, they probe the large z region being essentially blind to the UV part of the geometry. Then for κ 2 ± = 0 we can use (3.16) as an approximation for their evolution operators. The constraint (3.32) this time becomes C(ω, k x , k y ) e (κ + +κ − ) z ir = 0 (3.35) which cannot be satisfied for any choice of momentum and frequency. Then we are left with the case κ 2 ± = 0, where (3.36) So the constraint C(ω, k x , k y ) = 0 can be approximated as κ ± 2 = 0. This defines the two IR Dirac cones C IR ± [15]. Their apexes are located at (ω, k x , k y ) = (0, ∓w IR /2, 0), and they satisfy C IR Notice that rotational symmetry in the momentum plane is broken in the IR.

Fermionic operators in the QFT
From the AdS/CFT point of view, the above defined spinor field in the bulk has a spinorial fermionic dual operator O(x) in the boundary QFT, which transforms in the doublet representation of SU (2). The two point correlation functions of such operator can be computed by deriving the on-shell action with respect to a source identified roughly with the boundary value of the spinor field. In this subsection we present the computation of the retarded fermionic correlator closely following references [15].
When we evaluate the action (3.3) on a solution of the equations of motion only the boundary term contributes. In terms of the vector notation (3.8) it takes the form However, as noted before, a relation exist for general momenta between the boundary value of the fields; from (3.31) we get Then the on-shell action is In our four-tuple notation, the sources u From here, using equation (3.39), we can read the correlation function From the point of view of the fermionic theory, the relevant observable to analyze the fermionic dynamics is the spectral function ρ(k), defined as It is a non-negative quantity, a fact that from the holographic point of view was shown in [15] in the T = 0 case; we review and extend the analysis for finite T in the appendix A. For translational invariant weakly coupled theories, a Kähllen-Lehmann representation for G R (k) implies that ρ(k) generically presents delta-like singularities (peaks) as a function of the frequency, on the quasiparticle states of definite dispersion relation, see for example [39]. Of particular relevance is the spectral function valued at zero frequency ρ(0, k x , k y ), whose peaks will be labeled (k * x , k * y ). At vanishing temperature, these peaks correspond to the Fermi momenta (k F x , k F y ), and their locus in momentum space determines the Fermi surface. Notice that the normal modes at ω = 0 sit on such surface, since the matrix M k is singular for them.

Numerical results
We perform an extensive numerical study of parameter space, to analyze how the gravitational coupling affects the spectral function as the temperature is varied. The results are contained in the figures displayed in this section. We plotted the spectral function as a function of (k x , k y ) for different values of T at fixed ω and λ, and as a function of ω for fixed values of (k x , k y ), for different values of λ and T .
In figure 3 we present the plots of the spectral function as a function of ω for fixed (k x , k y ) and low λ < λ c , and a low temperature T < T c . It is seen that the intersections with the IR light-cones are smoothed at non-zero temperature with respect to the T = 0 case, as it can be seen by comparing with figure 8 of reference [15]. In the small ω region, the spectral function oscillates giving rise to a single peak and then it goes to a constant non-vanishing value for ω = 0.
In figure 4 we give the spectral function in the normal and superconducting phase at T < T c for different momenta. Is is observed the absence of parity symmetry in ω in the normal phase in agreement with [19], and the presence of such symmetry in the superconducting phase, result observed for the T = 0 case in [15]. Figures 5 to 13 show the evolution of the spectral function as a function of the temperature. Each figure corresponds to a fixed λ and ω. In all cases, as the temperature decreases starting from the critical temperature, the spherical symmetry is rapidly lost, the local maxima become sharper and approach the locus of the normal modes. Notice that, although for illustrative reasons we have included the locus of the normal modes in all plots, as mentioned in the footnote 5 at section 3.1.4, these modes are strictly defined only at T = 0. By comparing the location of the maxima in, for example, figure 6 subfigure (b) with figure 5 subfigure (f), or figure 7 subfigure (b) with figure 6 subfigure (f), we see that for higher temperatures they approach the locus of the normal modes corresponding to a higher frequency. This is due to the fact that the temperature and frequency are measured in units of the chemical potential µ, so rising T /µ can be interpreted as lowering the scale µ , which in turn corresponds to rising ω/µ.

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The sets formed for figures 5 to 7, figures 8 to 10, and figures 11 to 13 respectively correspond to three fixed values of λ, smaller, equal and bigger than λ c . Each figure in the set shows plots of the spectral function for different temperatures at a fixed value of ω. The value of ω decreases from figure to figure inside each set. It is evident by comparing figures corresponding to the same temperature inside a single set, that region in which the spectral function is appreciable in momentum space gets smaller as ω decreases for fixed λ. By comparing different sets we see that the dependence on temperature and frequency of the spectral function is milder for λ > λ c than in the cases λ ≤ λ c . Notice also that even if spherical symmetry is absent, it seems to be recovered as the frequency is increased. For λ > λ c and high frequencies, figure 11, normal modes does not exist. This is in agreement with the absence of a region between the IR and the UV Dirac cones. Instead, in figure 13, two small, open and disconnected regions are present, where normal modes show up. Figures 14 to 16 correspond to three different values of λ, smaller, equal and bigger than λ c . On the left, the spectral surface ω = 0 is shown for different temperatures. On the right, the spectral function as a function of the frequency is plotted for several temperatures, for three different momenta. Of these, subfigures (1) are plotted at the momentum (k x , k y ) * = (k * , 0) that corresponds to one of the two maxima of the spectral surface at each temperature, and runs to the Fermi momentum as the temperature goes to zero. Defining the Fermi momentum k F as the location of one of the maxima when the temperature vanishes T = 0, the Fermi surface consists of the two points ±(k F x , k F y ) = (±k F , 0). It is observed that the peaks in the spectral function as a function of ω in subfigures (2) (3) move to the left and get sharper as the temperature decreases. A similar sharpening appears in subfigure (1), even if it is more difficult to appreciate with our numerical methods. This corresponds to the appearance of the normal modes at T = 0. Interestingly, in subfigure (1) the peaks also sharpen as the temperature approaches T c .
As the temperature goes to zero, the spectral density in 14 to 16 subfigure (1) approach a continuum background with a delta-like peak at ω = 0. This allows us to interpret the inverse height of the peak at ω = 0 as a rough estimator of its width, i.e. of the quasiparticle lifetime. In figure 17 we plotted the value of the spectral density at ω = 0 as a function of temperature. For small enough temperature, such value increases as the temperature decreases, indicating the expected sharpening of the quasiparticle peak. Interestingly, the peak sharpen not only as the temperature goes to zero, but also as it approaches T c , where it matches with the value of the normal phase.

Discussion
In this paper we have studied the spectral function of the fermionic degrees of freedom on a back-reacted holographic p-wave superconductor at finite temperature and entropy, extending previous work in the literature.
At zero temperature, the normal modes exist inside the UV Dirac cones and outside the IR ones. This behavior is consistent with the appearance of Fermi arcs whenever the intersection of UV and IR Dirac cones does not allow for a closed Fermi surface. The normal modes can be interpreted as setting a relation between frequency and momenta JHEP04(2017)087  that can be understood as a quasiparticle dispersion relation. The support of the spectral density is completely contained inside the IR Dirac cones and at the sharp divergences at the normal modes.
At finite temperature, the region where the spectral function is numerically appreciable gets reduced as the temperature is decreased, the peaks at the normal modes becoming sharper. There is a breaking of rotational invariance that gets stronger as the temperature is decreased. However, our results show that such temperature dependence is milder as the gravitational coupling is increased.
The spectral density evaluated at the Fermi momentum presents a quasiparticle peak at vanishing frequency, the width of which can be interpreted as the quasiparticle lifetime. In our plots, we see that the quasiparticle stabilizes as the temperature is decreased, what is expected due to the presence of the normal modes, and also as the temperature appoaches the critical temperature of the superconducting transition.           The starting point is the (on-shell) conserved current where on the right we used our ansatz introduced after (3.4). The conservation equation reads, Here the matrix S(z) ≡ −i U(z) C is hermitian, S(z) † = S(z), and in the second equality we have introduced the notation (3.8) with the matrix C giving in (3.3), while that in the last equality we used the equations of motion (3.10). From (A.2) we conclude that, when evaluated on-shell, Q(z; k) = Q(k) is a conserved quantity, and even if we do not know the explicit solution to the equations of motion we can evaluate it in known limits.
In first term we consider the UV limit; with the help of the asymptotic behavior (3.29), the relation (3.38) and the definition (3.41) we obtain If we assume that Q UV (k) ≥ 0, and being the vector u (UV) k arbitrary, we must conclude that the hermitian matrix i G R (k) − G R (k) † is non-negative. From the definition (3.42) we conclude that, In second term we consider the IR limit; in this case we have to distinguish two cases. When the entropy vanishes the asymptotic behavior for z → ∞ is of the form where the vector b t = (b 1 , b 2 , b 3 , b 4 ) is read from (3.18) in terms of u (ir) k but such relation is not relevant here. From (A.2) we get

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Working in momentum-space, Ψ(x, z) = z 3/2 e i kµ x µ ψ + k (z) ψ − k (z) and after introducing the notation (3.8), the equations of motion result as in (3.10) with the constant matrix U defined by The general solution of (3.10) is Let us define, and take as b.c. a ± = 0; it is clear that in the first case it is just a smoothness condition when z → ∞. With this b.c. the solution can be written From the definition (3.38) and the AdS/CFT recipe equation (3.41) we read the retarded Green function The spectral function is then obtained from (3.42), We see that the b.c. adopted for z → ∞ together with the introduction in equation (B.5) of the right signs in the definition of the roots of λ ± 2 in the region where they are negative, i.e. inside the Dirac cones (and where the spectral function is non-zero) is what assure the positivity of the spectral function. And when φ = 0, the relevant case in the IR limit at null entropy considered in the paper, they coincide with the ingoing b.c. in the region κ ± 2 < 0 considered in subsection 3.1.1.

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As a last remark, it is easy to see that these b.c. effectively follow from the prescription of smoothness after shifting ω → ω + i with → 0 + ; in fact if we assume that λ ± 2 < 0 we have, and then the exponential will be well-behaved at z → ∞ if (B.5) holds [15].
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