Issue 
A&A
Volume 589, May 2016



Article Number  A96  
Number of page(s)  20  
Section  Extragalactic astronomy  
DOI  https://doi.org/10.1051/00046361/201424738  
Published online  20 April 2016 
Shaping the GeVspectra of bright blazars
^{1}
Institut für Astro und Teilchenphysik, LeopoldFranzensUniversität
Innsbruck, 6020
Innsbruck, Austria
email: lars.hunger@brainlinksbraintools.unifreiburg.de
^{2}
Institut für Theoretische Physik, LeopoldFranzensUniversität
Innsbruck, 6020
Innsbruck,
Austria
^{3}
BrainlinksBraintools, University of Freiburg,
79104
Freiburg im Breißgau,
Germany
Received: 3 August 2014
Accepted: 15 February 2016
Aims. The nonthermal spectra of jetted active galactic nuclei (AGN) show a variety of shapes and degrees of curvature in their low and high energy components. From some of the brightest FermiLAT blazars, prominent spectral breaks at a few GeV have been regularly detected, which is inconsistent with conventional cooling effects. We study the effects of continuous timedependent injection of electrons into the jet with differing rates, durations, locations, and powerlaw spectral indices, and evaluate its impact on the ambient emitting particle spectrum that is observed at a given snapshot time in the framework of a leptonic blazar emission model. With this study, we provide a basis for analyzing ambient electron spectra in terms of injection requirements, with implications for particle acceleration modes.
Methods. The emitting electron spectrum is calculated by Compton cooling the continuously injected electrons, where target photons are assumed to be provided by the accretion disk and broad line region (BLR). From this setup, we calculate the nonthermal photon spectra produced by inverse Compton scattering of these external target radiation fields using the full Compton crosssection in the headon approximation.
Results. By means of a comprehensive parameter study we present the resulting ambient electron and photon spectra, and discuss the influence of each injection parameter individually. We found that varying the injection parameters has a notable influence on the spectral shapes, which in turn can be used to set interesting constraints on the particle injection scenarios. By applying our model to the flare state spectral energy distribution (SED) of 3C 454.3, we confirm a previous suggestion that explained the observed spectral changes at a few GeV by a combination of the Comptonscattered disk and BLR radiation. We determine the required injection parameters for this scenario. We also show that this spectral turnover can also be understood as Comptonscattered BLR radiation only, and provide the corresponding injection parameters. Here the spectral turnover is explained by a corresponding break in the ambient electron spectrum. In a similar way, we also applied our model to the FSRQ PKS 1510089, and present two possible model fits. Here, the GeVspectrum is either dominated by Comptonscattered accretion disk radiation or is a combination of Comptonscattered disk and BLR radiation. We provide the required injection parameters for these fits. In all four scenarios, we found that impulsive particle injection is disfavored.
Conclusions. The presented injection model that is embedded in a leptonic blazar emission model for external Comptonloss dominated jets of AGN aims towards bridging jet emission with acceleration models using a phenomenological approach. Blazar spectral data can be analyzed with this model to constrain injection parameters, in addition to the conventional parameter values of steadystate emission models, if sufficient broad multifrequency coverage is provided.
Key words: galaxies: jets / galaxies: active / gamma rays: galaxies / radiation mechanisms: nonthermal
© ESO, 2016
1. Introduction
Jetted active galactic nuclei (AGN) comprise the most numerous variable source population in the γray sky (e.g., Ackermann et al. 2013). Their jets are considered as the site of intense broadband emission, with apparently random flaring events, shich cover the electromagnetic band from the radio up to GeV, or TeV energies. Variability timescales for this continuum emission range from months (radio) down to few minutes (TeV). Their broadband spectral energy distribution (SED) can be described as having two broad components, with the lower energy component usually attributed to synchrotron radiation from a population of relativistic electrons in the magnetized emission region. The origin of the photons of the higher energy component is still under debate, and strongly depends on the relativistic particle content of the jet (e.g., Reimer & Böttcher 2013). In many cases, it is only by considering leptonic processes together with external target photon fields that can lead to snapshot or timeaveraged SEDs that are in agreement with the corresponding multifrequency observations (e.g., Böttcher et al. 2013). An often used approach for calculating these SEDs is based on an ad hoc assumption of the emitting electron spectrum as having logparabolic shapes, (broken) power laws with possible exponential cutoffs, and with the minimum and maximum electron energies, energy of possible breaks and power law indices or curvature of this spectrum as free parameters (e.g., Dermer et al. 2009; Finke & Dermer 2010; Dermer et al. 2014).
The observation of spectral breaks in the high energy photon spectra of bright flat spectrum radio quasars (FSRQ) was among the first findings of the FermiLAT in the extragalactic γray sky (Abdo et al. 2009, 2010d, and confirmed subsequently in Ackermann et al. 2011). Typically, bright FSRQs (and also some low frequency peakedBL Lacs (LBLs) and intermediate frequency peakedBL Lacs (IBLs)) show γray spectra that can be described phenomenologically either by broken power laws or logparabolas with strong concave curvature (Harris et al. 2014) between 1 and 10 GeV, which is too low to be caused by absorption in the extragalactic background light (e.g., Abdo et al. 2010c), and with a powerlaw index change much larger than expected from cooling (ΔΓ = 0.5). For example, the turnover in the GeV spectra of FSRQ 3C 454.3 is located at ~2.5 GeV with a power law index change of about ΔΓ = 1.1 ± 0.1. The break energy does not seem to be correlated with the γray luminosity. Several scenarios have been proposed to explain these breaks. These range from photon pair production in the broadline region of the source (BLR; Poutanen & Stern 2010), to a twocomponent γray spectrum (Finke & Dermer 2010), or GeV breaks in the photon spectra owing to corresponding breaks in the electron spectra (Abdo et al. 2010d).
Some recent studies, however, have cast doubt on the internal absorption scenario, which would predict welldefined break energies in the AGN’s source frame. Harris et al. (2012) did not find such universal values of the break energies. Kohler & Nalewajko (2015) described the occurence of spectral breaks, which were investigated from a set of 40 bright LATblazars as “random”. In fact they report a tendency for short duration flares to possess stronger curvature than those hat are integrated over a longer timescale. The other two nonabsorption scenarios mentioned above invoke ad hoc broken powerlaw particle spectra. Ghisellini & Tavecchio (2009) show that KleinNishina or simple cooling effects cannot explain the strength and shape of the observed peaks (see however, Cerruti et al. 2013 who propose a highenergy cutoff at GeV energies from KleinNishina effects in scattering Ly_{α} photons).
Using the ambient particle spectrum as an input parameter, however, broadly ignores the buildup of this emitting particle spectrum that is impacted by the various particle energy losses, and gains through particle energization mechanisms which, in general, requires a timedependent treatment of the problem. As a consequence one can not gain much information on the particle acceleration mechanisms at work in these environments from modeling broadband SEDs this way.
In the present work we attempt to improve on this situation by studying the impact of various injection scenarios of relativistic particles on the resulting emitting particle and photon spectrum. Specifically, we calculate the ambient particle spectrum that results from injection during a finite time range in the past, and viewed at a given (snapshot) time. Comparing to the broken powerlaw, emittingparticle spectra, which are required in broadband modeling of blazar snapshot SEDs, will then help us draw inferences on the required particle acceleration mechanisms.
In this sense, our approach differs from works which directly implement a specific acceleration mechanism into an emission code (e.g., Diltz & Böttcher 2014).
We restrict ourselves to leptonic emission processes in blazar jets here where external photon fields, such as accretion disk radiation and radiation partly rescattered at the BLR, present the dominant target for particlephoton interactions. This setup is expected to be suitable for application to those radioloud jetted AGN, which show a strong accretion disk radiation field, such as FSRQs and LBLs. The analog procedure, including hadronic interactions as well, is more complex and will be postponed to a subsequent paper.
We aim to explain the observed breaking spectra at GeVenergies, and hence focus here on steep spectrum LATAGN. This is unlike Pacciani et al. (2014), whose study on spectral shapes is based on a data set in which those periods are exclusively considered where the sources emitted significant >10 GeV photons and are therefore associated with hard γray spectrumflaring events. Diltz & Böttcher (2014) complemented their timedependent leptonic blazar emission code with an implementation of a FermiII acceleration scenario, in addition to timedependent particle “pickup”, with the goal of identifying observational signatures for the origin of flares. Hence they studied the effect of a perturbation of various input parameters that could potentially be associated with causing outbursts on top of a steadystate situation. They explored observational signatures such as correlations between lightcurves at different frequencies, possible time lags, etc. Our present work attempts to explore the impact of a specific injection history on the resulting highenergy spectrum thereby offering an alternative explanation for the often observed strong breaks in bright FSRQ spectra at GeVenergies.
Section 2 of this paper describes the emission model used here (an external inverse Compton emission model that broadly follows Dermer & Schlickeiser 1993; Dermer et al. 2009), and the calculation of the emitting electron spectrum, which is the result of radiative losses that impact upon an electron population that has been continuously injected while propagating along the jet. Such continuously injected electron spectra, like the one we use in this work, were first proposed by Mücke & Pohl (2000). We present a detailed parameter study in Sect. 3, and summarize and discuss the results of our work in Sect. 4.
2. Model
2.1. Basic model
Fig. 1
Geometry of the blazar jet model considered in this work (figure adapted from Dermer & Schlickeiser 1993). 
We consider the AGN to be powered by accretion onto a supermassive Schwarzschild black hole of mass M_{BH}. The central black hole is surrounded by a ShakuraSunyaev accretion disk (Shakura & Sunyaev 1973). Accretion disk photons, with energy ε^{∗}, enter the jet under the angle . These photons are scattered into the angle with scattered photon energy , by the jet electrons. The plasma outflow of the jet starts at a distance z_{0} from the central black hole and flows along the symmetry axis of the system with bulk Lorentz factor Γ and the velocity β_{Γ}c, where . Figure 1 illustrates the basic model used in this work. Other than in the model of Dermer & Schlickeiser (1993), electrons are injected continuously along the jet axis between heights z_{a} and z_{b} with a timedependent injection rate ∝z(t)^{− α}, with α being a free parameter. We consider cooling of the injected electrons as being dominantly the result of inverse Compton losses on external target radiation fields. Two target photon fields are considered here: the aforementioned accretion disk radiation, which generally enters the jet under small angles , and the accretion disk radiation that has been backscattered by the BLR. Most of this backscattered radiation enters the jet under angles θ^{∗}> 90°, which leads to a different scattering behavior. Because the two target photon fields have different angular distributions in the jet frame, the inverse Compton scattered photon distributions that are produced by each of the target photon fields shows correspondingly different spectral shapes. The BLR model used here largely follows Dermer et al. (2009) and is described in Sect. 2.2.1.
In the following, quantities with asterisks are in the rest frame of the accretion disk. All energies are in units of the electron rest mass m_{e}c^{2}.
2.2. Compton cooling rates
We consider Compton cooling of electrons in the comoving frame of the jet. This radiative cooling rate is dependent on the differential Compton photon production rate, (1)which is dependent on

n_{ph}(ε,Ω,z), the photon density of the target photon field at solid angle (Ω), energy (ε) and position (z) along the jet axis;

n_{e}(γ,Ω_{e}), the electron density at electron Lorentz factor γ and the solid angle (Ω_{e});

the differential Compton scattering cross section
Here, describes the threedimensional collision angle.
We assume that the electron density is isotropic in the comoving frame of the jet, . To calculate the energy loss rate, we set , where δ() denotes the Delta distribution. By only considering relativistic electrons, the assumption γ ≫ 1 is justified. Furthermore, we use the Thomson approximation for the differential crosssection with the δapproximation in the headon case: (2)where σ_{T} denotes the Thomson crosssection. This is valid as long as ε′ ≡ γε(1−cos(ψ)) ≤ 1. For ε′> 1 (KleinNishina regime) we assume that the crosssection is zero when calculating the cooling rates, since the KleinNishina crosssection declines rapidly at high energies.
With these approximations, the integrations over Ω_{e} and ε are trivial. To achieve further simplification, we average the azimuthally symmetric problem over φ implying ⟨ cos(ψ) ⟩ = μμ_{s}.
The integrations then lead to (3)To make progress in calculating the scattered differential photon production rate the two differential target photon densities n_{ph} (in the comoving frame) are required. Their calculations are shown in the following two sections.
2.2.1. BLR target photon density
Fig. 2
Our BLR model, which consists of a spherically symmetric shell of gas between R_{i} and R_{o} and a density gradient ζ with n_{e}(R) ∝ R^{ζ} (figure adapted from Dermer et al. 2009). 
Figure 2 sketches the BLR model used here, mainly following Dermer et al. (2009), where the BLR target photon field is the result of reprocessing the accretion disk radiation and with any direct BLR line emissivity being neglected. For the purpose of calculating the target photon field rescattered at the BLR (BLR target photon field), we consider the central source as an isotropically emitting point source.
An anisotropic central source would slightly increase the energy density caused by the BLR in the jetframe with distance from the illuminating disk (Ghisellini & Madau 1996).
The central source radiation is isotropically Thomsonscattered by material of the BLR, back to a distance z (above the black hole) on the jet axis. We consider a spherically symmetric shell of thin gas for the scattering BLR material with a density gradient inside this shell (see Fig. 2). Taking into account a clumpy BLR, instead, would require the introduction of further free parameters (cloud radius distribution) while the expected impact on the distribution of the reprocessed radiation likely stays small for not too large cloud sizes: one would expect additional inhomogenities to some extent on top of an Rdependence from the BLR density gradient.
The calculations here are all carried out in the rest frame of the BLR.
The Thomsonscattered photon density is obtained by (4)Here x^{2} = R^{2} + z^{2}−2zRcos(θ), and ṅ(ε_{∗};R), the differential BLRscattered photon density rate, is given by (5)where

Ṅ_{ph}(ε_{∗}) is the central source photon production rate;

gives the fraction of the incoming flux that is scattered;

is the geometric dilution from an isotropic source.
With spherical coordinates and Eq. (5), Eq. (4) we find: (6)Since inverse Compton scattering is angle dependent, we need the angledependent target photon spectrum. With , μ_{∗} = cos θ_{∗} and by changing the variables to g = R/z we get (7)We use the law of sines to calculate the angle μ_{∗} under which the scattered photons reach the point z: (8) defines a line. If the scattering process takes place on that line, a photon emitted into the angle μ arrives with angle μ_{∗} at point z. Formally, there are two solutions with the positive one being the physically relevant one for the already φintegrated quantity .
Carrying out the integration we find: (9)where and Here describes the radius R at which the photons, emitted into the angle μ, have to be scattered to end up in μ_{∗}. is the electron density at the scattering point. This means Π(μ_{∗},z) gives a measure for the total number of photons that end up in the angle element μ_{∗} at point z along the jet axis.
Π cannot be solved analytically, but numerically. The results of these calculations, which we find in agreement with Dermer et al. (2009), are shown in Fig. 3. The figure shows the angular distribution of the BLR photons for different positions z. For z ≥ R_{o} there are no incoming photons from the front (μ_{∗}< 0) since there is no scattering BLR material in front of z.
Fig. 3
Angle dependence of for a BLR extending from 10^{2} to 10^{5}R_{g} for different values of z (in R_{g}) and ζ, in agreement with Dermer et al. (2009). 
The central source photonproduction rate Ṅ_{ph}(ε_{∗}) is calculated by assuming that this photon source emits a monochromatic spectrum with luminosity L_{0}: (10)Here L_{0} = L_{edd}l_{edd}, with L_{edd} the Eddington luminosity of the black hole. Tavecchio & Ghisellini (2008) have shown that the BLR radiation, simulated with the photoionization code CLOUDY, as the target field for inverse Compton scattering can be adequately approximated by a blackbody with a peak at 1.5 times the Ly_{α}frequency, when considering the IC spectrum above a few keV. Afterwards, we approximate this blackbody with a monochromatic spectrum.
Fig. 4
Comparison of radiative electron energyloss rates. Here we choose BLR1 at z = 100 as an example, while noting that the qualitative picture, with the negligible BLR losses, is the same in all the cases we considered in our study. We compare with synchrotron loss rates for a B = 4.5 G magnetic field. a) Radiative electron energy loss rates for varying z for electron energy γ = 500 and BLR1 with τ_{BLR} = 0.01. b) Radiative electron energy loss rates for varying γ at z = 100 and BLR1 with τ_{BLR} = 0.01. BLR shows the BLR energy loss used in our calculations, here we set the energy loss in the KleinNishina regime to 0. 
The resulting BLR target photon density is (11)To transform this into the comoving frame we use ε_{∗} = Γε(1 + β_{Γ}μ) and , to get (12)
2.2.2. Accretion disk target photon density
To calculate the accretion disk photon density in the comoving jetframe, we follow the procedure outlined in Dermer & Schlickeiser (1993). The accretion disk target photon density at the point z is given by (13)with (14)and the surface energy flux for a ShakuraSunyaev disk is (15)Here , Ṁ is the mass accretion rate and R_{i} = 6R_{g} for a Schwarzschild black hole with R_{g} = GM/c^{2} the gravitational radius. In gravitational units, , Eq. (15) becomes (16)with Φ_{F} = 8.43 × 10^{24}Ψ cm^{2} s^{1} and Ψ = l_{edd}/ϵ_{f}M_{8} where M_{8} is the black hole mass in 10^{8} solar masses.
We use a monochromatic approximation for the blackbody radiation that is emitted locally at a specific radius of the accretion disk. The mean photon energy emitted at a radius is then given by (17)By combining Eqs. (14), (16) and, (17) we get (18)After substituting Ṅ_{ph} in Eq. (13) with Eq. (18) and transforming the result into the comoving frame we find (19)
2.3. Energy loss and equation of motion
2.3.1. Energy loss in the BLR radiation field
With the differential target photon density, we now calculate the scattered photon density. We use Eq. (12) together with Eq. (3) to calculate ṅ^{BLR}(ε_{s},μ_{s},z). By integrating over all scattering angles μ_{s}, and all scattering energies ε_{s}, we get the energyloss rate of a single electron of given γ: (20)After integrating over ε_{s} we get: (21)Because the electron energy loss rate depends on (1 − μμ_{s})^{2}/ (1 + β_{Γ}μ)^{2} photons with incident angles μ< 0 contribute more strongly to the electron energy loss rate than photons with incident angles μ> 0. The small number of reprocessed BLR photons causes the energy loss due to the BLR to be negligible for the cases that we considered here (see Fig. 4).
2.3.2. Energy loss in the accretion disk photon field
The procedure is analogous to the BLR case: we use Eq. (3) to calculate the differential photon production rate for one electron: (22)This leads to the energyloss rate induced by the accretion disk target photons of (23)The very good approximation for the solution of Eq. (23) in the nearfield regime (z< 0.1Γ^{4}(1 + β_{Γ})^{4}) is given by Dermer & Schlickeiser (1993), which we use in the following.
2.3.3. Thomson scattering criterion
The energy loss rates are calculated in the Thomson regime, and are therefore only valid for ε′ ≡ γε(1−cos(ψ)) ≤ 1 while, in the KleinNishina regime, the cross section is set to zero. After transforming the target photon energy ε into the rest frame of the BLR, we obtain the Thomson limit criterion: (24)Again, we use the monochromatic approximation for both external target photon fields to confine the range of γ, where both energy loss rates are in the Thomson regime. Since 1 − βcos(ψ) can never be larger than 2, the scattering will always be in the Thomson regime if the following relation is fulfilled: (25)The accretion disk photons will mainly enter the jet from behind, i.e. μ_{∗} ≈ 1. In this case, the Thomson criterion for scattering the accretion disk target photons is: (26)The BLR photons that are most important for the problem will enter the jet from the front, μ_{∗} ≈ −1. In this case the Thomson criterion changes to: (27)For larger γ, the rate of inverse Compton scattering in the BLR reduces to the KleinNishina regime, which we neglect in the following. We can neglect the energy loss in the KleinNishina regime for the BLR target photons. This neglect is justified since the energy loss owing to the BLR is negligible with respect to the energy loss caused by the accretion disk target photons in the cases that are considered in this work (see Fig. 4). In the cases we studied, the accretion disk photons are usually scattered in the Thomson regime.
2.3.4. Omission criterium for synchrotron energy losses
In particular, this work targets accretion radiationstrong blazars such as FSRQs. Here synchrotron energy losses of the charged particles are typically weak when compared to Compton losses (see also Fig. 4). In the Thomson limit, synchrotron losses can therefore be neglected when, in the jetframe, the magnetic field energy density is much lower than the sum of all target photon fields, i.e.: (28)The jetframe accretion disk energy density in the near field regime for a Schwarzschild black hole reads (see Dermer & Menon 2009), while the jetframe BLR radiation field is given by where the galaxyframe BLR energy density u_{BLR} can be evaluated following Finke & Dermer (2010). In the case of negligible BLR Compton energy losses, Eq. (28) reduces to: where l_{edd}L_{edd} = ϵ_{f}Ṁc^{2} (see Dermer & Schlickeiser 1993).
2.4. The emitting electron spectrum
The equation of motion of the relativistically outflowing jet with constant velocity β_{Γ}c is (29)The time interval in the rest frame of the disk is related to the comoving frame by δt^{∗} = Γδt. By combining Eq. (29) with Eq. (21) and using the solution of Eq. (23) in the nearfield regime we get (30)which describes the change of electron energy over a distance dz. We note that, while in the model of Dermer & Schlickeiser (1993) only Compton energy losses in the disk radiation field are discussed, here we also take energy losses from Compton scattering in the BLR radiation field into account. The initial value problem for calculating the electron spectrum consists of Eq. (30), the point z, the injection point z_{i}, and the Lorentz factor γ that the electrons possess, after having propagated from z_{i} to z. This can only be solved numerically. For all , the BLR component does not play a role. In this case Eq. (30) simplifies to (31)which has an analytic solution: (32)We consider the continuous injection of an electron powerlaw spectrum, with spectral index s, into a moving plasma blob along the jet at an injection rate that depends on the height above the disk and with an injection index α. The electron spectrum injected at height z_{i} can be described by , with Q_{0} the normalization parameter. Using Eq. 32, the cooled injected electron spectrum then has the form (33)(see also Dermer & Schlickeiser 1993).
When continuously injecting powerlaw electron spectra into the moving plasma blob with a given injection rate ∝, the resulting emitting electron spectrum N_{e}(γ,z) is a superposition of the cooling electron spectra that have been injected and weighted by the corresponding injection rate. This is described by (34)where (35)describe the limits of the cooling electron spectrum (see also Mücke & Pohl 2000).
An electron that was injected with an initial energy γ_{i} cooled down to after having propagated a distance z_{travel} = z − z_{i}. Accordingly, corresponds to the energy that an electron injected at point z_{i} with the energy γ_{1} possesses after having propagated from z_{i} to z. The two Heaviside functions and prevent all electrons that are injected outside of the contributing energy range from adding to N_{e}(γ,z).
2.5. Calculating the photon spectrum
Having determined the emitting electron spectrum, we now proceed to calculate the scattered photon spectrum of both the accretion disk target photon field and the BLR target photon field. For this purpose, we follow Dermer et al. (2009). The νF_{ν} spectrum is given by where d_{L} is the distance to the source.
Here with z_{r} the redshift of the photons that are emitted by the source. The νL_{ν} spectrum is related to the photon production rate via (36)where is the (observer frame) volume of the emitting plasma blob with a radius R_{b}. We now calculate the photon scattering in the rest frame of the accretion disk. Equation (1) in the rest frame of the accretion disk reads (37)where, again, the headon approximation has been used, which implies Ω_{e} = Ω_{s}.
To calculate the scattered photon spectrum, we use the full Compton crosssection with the scattering treated in the headon approximation: (38) is the invariant collision energy after having averaged over φ and (39)with The Heaviside function gives the integration limits: (40)is the lowest γ value at which an electron can still transfer enough energy to a photon so that it reaches the energy after the scattering. (41)is the highest photon energy, so that the smallest energy transfer still yields a scattered photon with .
After transforming the emitting electron spectrum (calculated in the comoving frame) into the rest frame of the accretion disk by (42)we combine Eq. (36) with Eqs. (37)–(39) and (42) to arrive at (43)for the νL_{ν} spectrum.
The final photon spectrum that is due to the BLR target photons is calculated by using Eq. (11) in conjunction with Eq. (43).
To calculate the target photon density n_{ph}(ε^{∗},μ^{∗}) that is produced by the accretion disk photons, we integrate over the whole disk first. We substitute Ṅ_{ph} in Eq. (13) with Eq. (18) and get (44)From we introduce with andScaling the length scales and in terms of the gravitational radius R_{g} we obtain (45)This can be used in conjunction with Eq. (43) to find the scattered photon spectrum that is produced by the accretion disk target photon field. The total photon spectrum produced is the sum of the photon spectra from both target photon fields.
We note that a further leptonic highenergy radiation process which contributes to the broadband blazar SED is synchrotronself Compton (SSC) scattering. In the case of quasars with strong accretion disks, as considered in this work, the radiative output from this process has been found to typically dominate in a rather small energy range at Xrays (see e.g., Böttcher 2000; Dermer et al. 2009). Hence its contribution to the overall shape of the SED is markedly limited. We therefore do not include this process in our model, noting that our studies and the predictions given in the following should be considered with care at Xray energies.
3. Results
We present the electron and photon spectra following the calculations outlined in Sects. 2.2 and 2.5. For our calculations we set the black hole mass to 10^{8}M_{⊙} (noting that the spectral shape only depends weakly on the black hole mass), the bulk Lorentz factor to Γ = 25, a fraction of l_{edd} = 0.1 of the Eddington luminosity for the central source and use a value of ϵ_{∗ 0} = 25(m_{e}c^{2})^{1} eV as the characteristic photon energy of the BLR (monochromatic) spectrum. Here, synchrotron energy losses can be neglected for field values smaller than ~ G.
In the following, we focus on photon spectra up to ~10 GeV. Hence, γray absorption during propagation through the diffuse extragalactic background light can be neglected here (e.g., Abdo et al. 2010c). We also neglect internal γray absorption in the external radiation fields, which could potentially affect the spectral shape beyond ~50 GeV for typical bright FermiLAT FSRQs (see Sect. 4), and focus our spectral considerations below this energy. We also note that most FermiLAT FSRQs were not detected beyond such energies owing to their typically strong spectral decline at a few GeV (e.g., Ackermann et al. 2011), although few notable exceptions (e.g., 3C 279 (MAGIC Collaboration 2008), 4C +21.35 (Aleksić et al. 2011), PKS 1510089 H.E.S.S. Collaboration et al. 2013) exist.
Below, the photon spectra are shown in the observer frame using a source redshift of z_{r} = 1. All distances are given in terms of the gravitational radius R_{g}.
In our parameter study, we discuss the impact of varying selected parameters, with respect to a reference model, on the resulting particle and photon spectra. The varied parameters are:

the height z above the disk where the emission region is located at observing time t_{obs};

the injectionrate index α at the position z;

the starting and end points z_{a}<z and z_{b}>z_{a} of the particle injection; we set z = z_{b} unless specified otherwise;

the spectral index s and the high (low) energy cutoff, γ_{2} (γ_{1}), of the injected powerlaw electron spectrum ;

the geometry of the BLR:

R_{i}, R_{o}, inner and outer border of the BLR;

ζ describes the density decline inside the BLR, ;

the BLR optical depth ;

The free parameters of the BLR are combined to result in four different BLR configurations BLR1BLR4 (see Table 1) that are used to explore their effect on the emitting electron and photon spectrum. For the reference model, we use the following parameters: s = 3,α = 2,z_{a} = 200,z = z_{b} = 2000,γ_{1} = 1000,γ_{2} = 5 × 10^{5},τ_{BLR} = 0.01, and BLR1 as the BLR geometry. We use a dimensionless injection energy parameter to provide the total injected particle energy E_{inj} in each model in terms of the total injected particle energy of the reference model, .
3.1. The BLR geometry
Fig. 5
IC photon spectra (and ambient electron spectrum as an inlay in panel b for the reference model) for different BLR geometries used. a) Composite IC photon spectrum for the case of BLR1. b) Resulting IC photon spectra when varying the BLR geometries. The inlay shows the underlying ambient electron spectrum. 
List of BLR geometries used.
We first study the influence of different BLR geometries (as listed in Table 1) upon the inverse Compton (IC) photon spectrum. Geometries BLR1 and BLR2 follow a ζ = −2 density distribution of the BLR gas. Here most of its density is located close to the inner BLR boundary. BLR3 and BLR4 follow a constant density distribution between the inner and the outer radius of the BLR. The BLR geometry has no significant influence on the shape of the electron spectrum, a consequence of the electron energyloss rates in the BLR being rather low in general (see Sect. 2.2.1).
Figure 5a shows the total IC photon spectrum being composed of two components: the lower energy one is produced by IC scattering the accretion disk target photons, the second component, with a peak at around 3 GeVs, is produced by scattering the BLR target photons. Using different BLR configurations with respect to the emission region leads to quite different IC spectra, as we present in Fig. 5b.
The BLR3 gas is distributed in a rather thin shell. With the emitting region located at z = 2000 at the time of observation, i.e., beyond the outer boundary of the BLR3, the BLR photons enter the blob from behind with a collision angle similar to the accretion disk photons. The BLR3 contribution is drowned out by the much more numerous accretion disk photons. Hence, Fig. 5b shows that the total IC spectrum for the BLR3 case is nearly indistinguishable from the dominating accretion disk IC component (Fig. 5a).
In the BLR1 configuration the emission region is located within the BLR with parts of the BLR1 gas being in front of this region. Target photons from this front part experience a higher energy transfer than the photons from the accretion disk, therefore they are scattered to higher energies. Hence at high energies, the BLR IC component starts to poke through the accretion disk IC component (Fig. 5b). This behaviour becomes most prominent in the BLR2 configuration, where an even larger fraction of the BLR gas lies in front of the blob. Here again, the high energy BLR peak is produced by target photons that are backscattered by the BLR gas in front of the emission region.
The resulting IC spectrum from the BLR4 configuration, also shown in Fig. 5b, displays a shifted BLR peak position with respect to BLR1 and BLR2. In the BLR4 configuration, the emission region is located on the outer edge of the BLR. No target photons enter the blob from the front, but a large number of target photons enter from the sides. The maximum energy transfer for these photons is smaller than for photons that enter the blob from the front, thereby shifting the peak position of the IC component to smaller energies.
In summary, if the ambient electron spectrum is unambiguously determined, the relative position of the emission region with respect to the BLR geometry influences the relative strength of BLR and accretion disk component, and may shift the peak energy of the BLR IC component.
3.2. The luminosity of the accretion disk
The accretion disk luminosity, here measured in terms of a fraction l_{edd} of the Eddington luminosity, directly influences the density of the target radiation field along the jet. Higher accretion disk luminosities lead to increased particle cooling; the ambient electron spectrum reaches to lower minimum electron energies (see Fig. 6a). Consequently, the corresponding IC scattered photon spectra also reach lower energies as shown in Fig. 6b, as do the corresponding synchrotron radiation spectra.
3.3. The injected particle spectrum
The injected electron spectrum, a simple power law with spectral index s, is bracketed by the lowenergy and highenergy cutoff particle Lorentz factors γ_{1} and γ_{2}. The effects of varying γ_{1}, γ_{2} and s with respect to the reference model are explored below.
Fig. 6
Emitting electron (left) and resulting photon spectra (right) for various l_{edd}. Where l_{edd} = 0.01 we also show the photon components produced by both target photon fields separately. 
Fig. 7
Emitting electron (left) spectra and corresponding photon spectra (right) for γ_{1} that varies with respect to the reference model. The total injected particle energies are strongly determined by γ_{1}. For γ_{1} = (100,500,1000,1500), we find Υ_{inj} = (10.1,2.0,1,0.7). 
Fig. 8
Emitting electron (left) and corresponding photon spectra (right) for spectral injection indices s, varying with respect to the reference model. The total injected electron energies for s = (2,3,4) are Υ_{inj} = (4.7 × 10^{3},1,5.1 × 10^{4}). In the case of s = 4, the photon components produced by both target photon fields are shown separately as well. 
In Fig. 7a we show the resulting electron spectra when γ_{1} is varied, while leaving all the other parameters unchanged. Clearly, at γ = γ_{1} a break in the emitting electron spectrum generally occurs unless the injection rate is very steep (see Sect. 3.4). The amount of the spectral index change at the break energy can be understood as follows: For energies larger than γ_{1}, electrons are continuously injected and cooled at the same time. Hence, the produced powerlaw spectrum in this regime depends on the injected electron spectral index s. At electron energies smaller than γ_{1}, only cooled particles accumulate. Thus the spectral shape depends on the injection rate index α (see Sect. 3.4). The combination of s and α thus influences the broadness of the break in the emitting particle spectrum. In particular, breaks that are larger than typical cooling breaks, as implied, e.g., from observed GeV spectra of bright LAT FSRQs, become possible here.
The corresponding photon spectra are shown in Fig. 7b. The peak of the emitting electron spectrum translates into peaks in the corresponding components of the photon spectra. The different incident angles of the BLR target photon component, as compared to the accretion disk component, lead to a larger range of electron energies that can scatter photons up to the same energy. The geometric area from which the target photons can contribute to a certain scattered photon energy slowly decreases, leading to a more gradual decrease, rather than a sharp cutoff towards high energies. The BLR peak is shifted to higher energies with respect to the accretion disk peak, again the reason is the different incident angle distribution of the BLR target photons. In the BLR component, headon scattering with a higher energy transfer to the photon is common. Thus electrons with the same energy lead to higher energetic scattered photons for the BLR target photons than for the accretion disk photons. In Fig. 7b, we also note the decreasing contribution of the Compton scattered BLR radiation to the total photon spectrum with increasing γ_{1}, a consequence of scattering in the KleinNishina regime of the crosssection with increasing energy.
As mentioned above, a change of the spectral injection index s impacts the energy range above γ_{1} in the emitting particle spectrum, becoming softer for softer injection spectra, and behaving as n_{e}(γ) ∝ γ^{− s−1}. Hence for a given injection rate index α, the spectral break in the emitting particle spectrum becomes broader for harder injection spectra (see Fig. 8a). For sufficient broad ambient electron spectra, the corresponding photon spectra from IC scattering the accretion disk and BLR radiation tend to merge into one component as is shown in Fig. 8b. Again, we also note the impact of the IC scattering in the KleinNishina regime, which leads, for the same ambient electron spectrum, to softer photon spectra of the BLRscattered component, as compared to the accretion disk scattered IC component beyond the respective peak energy.
Fig. 9
Emitting electron spectra (left) and corresponding photon spectra (right) for γ_{2} that vary with respect to the reference model. The total injected electron energy is rather insensitive to γ_{2}. For γ_{2} = (3000,5000,8000,10 000) we find Υ_{inj} = (0.7,0.8,0.9,0.9). In the case of γ_{2} = 3000, we show the photon components produced by both target photon fields. 
Very high energy electrons cool efficiently in the dense target radiation fields. Hence the particle spectrum above γ_{1} quickly rearranges to a state where injection rates balance the loss rates. For a sufficiently large highenergy cutoff of the injected electron spectrum, γ_{2}, where the radiative loss timescales at γ_{2} are much smaller than the injection timescale, any variation of this parameter therefore only marginally impacts on the resulting emitting electron and photon spectrum: the ambient particle spectra become very similar after only a short time owing to severe Compton losses.
For cases where the injected electron spectrum is bounded to an energy range where injection rates reach at least the radiative loss rates, a variation of γ_{2} results in a corresponding cutoff of the ambient particle and photon spectra, as shown in Fig. 9. The values used in Fig. 9 for γ_{2} within the reference model lead to a turnover of the photon spectrum in the tens of MeV energy range when accretion disk photons are scattered, and in the GeV energy range when BLR target photons are scattered. The two photon components are visibly seperated only for sufficiently low γ_{2}.
3.4. The particle injection mode
The effects of different particle injection scenarios on the resulting emitting electron and photon spectra are explored in this section. Particle injection starts within the jet at height z_{a} above the accretion disk and continues with a rate ∝ (where α is the injection rate index) up to a height z_{b}.
Fig. 10
Ambient electron (left) and photon spectra (right) with different injection rate parameters α, with respect to the reference model. The total injected electron energies for α = (0,1,2,3,4) are calculated to Υ_{inj} = (4 × 10^{5},512,1,0.3,9 × 10^{6}). In the case of α = 4, we also show the IC components produced by both target photon fields separately. 
The injection rate index α controls the spectral shape of the ambient particle spectrum below γ_{1} and (together with s) the spectral index change of the break. Figure 10 shows that harder prebreak spectral shapes develop for steeper injection rate distributions (large α). This can be understood as follows: particles in the prebreak regime γ<γ_{1} are cooled electrons, which have suffered energy losses while propagating at least a distance that corresponds to , where z_{i} was the injection point. This implies a direct relation between γ and z_{i}. Hence those particles injected at point z_{i} contribute to the ambient spectrum at γ<γ_{1}. Since cooling rates are highest where the injection starts (at z_{a}), the number of particles injected there contribute to the lowest energies γ ≪ γ_{1} in the ambient spectrum. As a consequence, for very steep injection rate distributions, rather soft ambient spectra develop while, for shallow injection distributions, hard emitting particle spectra build up at γ<γ_{1} (see Fig. 10). Specifically, for constant injection rates (α = 0), we find an approximately ∝γ^{− 1/2} behaviour at γ<γ_{1}. For α = 3, injection rates decrease with distance z at the same rate as the cooling decreases. The ambient electron spectrum becomes independent of the blob location, and the wellknown n_{e} ∝ γ^{2} emitting electron spectrum develops for γ<γ_{1}. For welldeveloped electron distributions, α does not impact the spectral shape at γ>γ_{1}.
Particle injection starts within the jet at height z_{a} above the accretion disk. Figure 11 shows the resulting electron and photon spectra for different values of z_{a}, all other injection parameters are kept constant.
Fig. 11
Ambient electron (left) and photon spectra (right) when varying z_{a} (in R_{g}) with respect to the reference model. The injected total electron energies for z_{a} = (100,200,500,1000) are Υ_{inj} = (2.1,1,0.33,0.1). The total injected energy decreases with rising z_{a}. 
A higher cooling rate in the accretion disk radiation field, as well as a longer total cooling time (due to larger z − z_{a} distance), leads to lower electron energies with decreasing z_{a} (see Fig. 11a). Hence, the corresponding photon spectrum below γ_{1} (Fig. 11b) softens and extends to very low energies depending on z_{a}.
Fig. 12
Ambient electron (left) and photon spectra (right) when varying the distances between the points z and z_{b} (in R_{g}), with respect to the reference model. The total injected electron energy is Υ_{inj} = 1 in all cases. For z = 2100, we also show the IC photon components produced by the two target photon fields considered separately. 
Next, we explore the situation of a finite particle injection duration (corresponding to a distance z_{b} − z_{a} in the jet) where the resulting spectra are observed at a given time after the last particle injection has occured. This time corresponds to a distance z − z_{b} in the jet. Figure 12 shows the resulting electron and photon spectrum for various z with fixed points z_{a} and z_{b}. Because of the strong energy dependence of the electron cooling (with higher energy electrons cooling faster than lower energy electrons; see Sect. 3.3) we observe the exponential high energy cutoff in the electron spectrum moving to lower energies while, below γ_{1}, the electron spectrum does not change significantly.
The influence of the electron cutoff is reflected in the corresponding photon spectrum. Although the electron injection spectral index s is constant, the postbreak photon spectrum becomes softer, owing to the lower energies of the electron energy cutoff. In Fig. 12b, we also show the total photon spectrum decomposed into the ICscattered accretion disk and BLR photon spectrum. We note that the turnover in the photon spectrum at a few GeV has its origin in the break of the underlying electron spectrum.
Fig. 13
ambient electron (left) and photon spectra (right) for various z_{b} (in R_{g}) with respect to the reference model. The total injected electron energies for z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (0.9,1,1.04,1.06). For z_{b} = 1000, the IC photon components produced by the two target photon fields are also shown separately. 
We now explore the impact of a changing injection duration upon the resulting spectra. For this purpose, we vary z_{b} while keeping z_{a} fixed, and analyse the resulting particle and photon spectra at z = z_{b}. The longer the injection at a given rate, the higher the total injected particle energy. At the same time, the particles cool, at a, generally, decreasing rate with increasing distance from the black hole. Hence, we find a strong dependence of the resulting spectral shapes upon the interplay between the injection and energyloss rates. Therefore, we also present our results for various injection rate indices α.
For a sufficiently shallow decrease of the injection rate, a pileup forms in the emitting particle spectrum at γ = γ_{1}, with the spectral index below γ_{1} becoming harder. This is a result of the cooling rate of particles at low energies not being sufficiently large to be able to fully balance the injection rate at these energies. Long injection times at sufficiently large z ensure an accumulation of particles at low energies, with reduced cooling rates leading to the pileups becoming more prominent with increasing z_{b}. This is demonstrated in Figs. 13a and b, where the spectra are shown for α = 2 and various z_{b}.
Electrons pile up at a given particle energy γ in a spectrum when, in momentum space, the net change of the number of electrons entering this γbin (either from injection or from cooling down from a higher energy bin γ + dγ) and leaving this bin to γ − dγ, due to cooling, is positive. For an increasing cooling rate with energy, this occurs at the lowenergy end of the injected spectrum, i.e., at γ = γ_{1}. For broad injection distributions α< 3 particle injection at large z, where cooling rates are diminished, is still significant. This facilitates accumulating particles within an energy bin. A pileup forms. As noted above, for α = 3, the emitting electron spectrum becomes independent of the blob location, and hence also of z_{b}. Thus, in this case, a pileup does not form (see Fig. 14a). For α> 3, the effects discussed above reverse and the spectral index becomes softer after the break γ = γ_{1}. In Fig. 14c we present the case of α = 7. Here the injection scenario becomes more “instantaneouslike”, and we follow the evolution of the injected spectrum for a time that corresponds to (z_{b} − z_{a}) /β_{Γ}c. For increasing z_{b}, the emitting electron spectrum steepens while extending to low energies γ<γ_{1} owing to cooling. In the limit of large z_{b}, all electrons have cooled and the injected power law is mapped into the γ<γ_{1} energy regime. The overall peak of the emitting electron spectrum for an instantaneouslike injection is therefore found at the lowenergy end. Here, the emitting electrons correspond to the cooled particles that were injected at γ_{1}. Their energy depends on the cooling rate, which is highest at the injection point z_{a}.
The corresponding photon spectra (see Figs. 13b, 14b and d) reflect the shapes of the respective ambient electron spectra, with some impact of the relative position of the emitting region with respect to the BLR (the latter has been discussed in more detail in Sect. 3.1). We note the shift of the IC peaks in Fig. 14d to lower energies which is due to the corresponding emitting electron spectra peaking in these cases at the very lowenergy end.
Fig. 14
Photon and ambient electron spectra for z_{b} (in R_{g}) and α with respect to the reference model. The total injected electron energies for α = 3 and z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (2.7,2.75,2.8,2.8) × 10^{3} while, for α = 7, the total injected electron energies for z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (5.8,5.8,5.8,5.8) × 10^{13}. For α = 3 and α = 7 with z_{b} = 1000, we also show the IC photon components produced by the two target photon fields separately. a) Normalized electron spectra for various z_{b} (in R_{g}) and α = 3. b) Corresponding photon spectra for various z_{b} (in R_{g}) and α = 3. c) Normalized electron spectra for various z_{b} (in R_{g}) and α = 7. d) Corresponding photon spectra for various z_{b} (in R_{g}) and α = 7. 
4. Modeling the 3C 454.3 and PKS 1510089 multifrequency SEDs
To show the viability of our model, we apply it to quasisimultaneous broadband data that was collected during the November 2010 outburst of 3C 454.3 (Abdo et al. 2011; Wehrle et al. 2012), with a particular focus on the FermiLAT spectrum that shows a distinct spectral decline at a few GeV. Additionally, we use our model to also fit the quasisimultaneous broadband SED of PKS 1510089, as reported in Abdo et al. 2010b. The lowenergy photon data provides additional valuable constraints on the emitting electron distributions. Within our model, we calculate the synchrotron radiation from the ambient electron distribution following Dermer et al. (2009), assuming a tangled magnetic field of strength B, and including synchrotronself absorption.
4.1. Modeling the 3C 454.3 multifrequency SED
Fig. 15
Twocomponent IC model fit to multifrequency data of 3C 454.3. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 2. a) Emitting electronspectrum. b) Synchroton spectrum with Swift, Herschel and Submillimeter Array data taken during the November 2010 flare (Wehrle et al. 2012). c) Gammaray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). d) Zooming into the γray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). 
Fig. 16
DominantBLR IC model fit with multifrequency data of 3C 454.3. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 2. a) Emitting electron spectrum. b) Synchroton spectrum with Swift, Herschel and Submillimeter Array data taken during the November 2010 flare (Wehrle et al. 2012). c) Gammaray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). d) Zooming into the γray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). 
In the following, we discuss two possible model fits to the data. The parameter values used for these fits are listed in Table 2, including the required particle power P_{par} of the complete injection event, which was calculated by assuming that the total power in particles (electrons and cold protons) is tenfold the power in nonthermal electrons, the magnetic field power P_{B}, and the equipartition field B_{eq}.
In Fig. 15 we present a model representation of the broadband data with parameter values similar to those used in Finke & Dermer (2010). The size of the BLR used in our model agrees well with Bonnoli et al. 2011, but is different from the one used in Finke & Dermer (2010). Other slight differences in the fit parameter values are due to the different data set we used. We note that the (observer frame) sizes of the emitting region, which are used in the model fits we present, are roughly around the size limits inferred by Sbarrato et al. (2011). Here, we searched for particle injection parameter values that lead, in the framework of our model, to an ambient snapshot electron spectrum similar to the ad hoc ambient electron spectrum used in the aforementioned paper. We find that continuous electron injection is indeed able to generate a broken powerlaw emitting electron spectrum that is similar to the one assumed in Finke & Dermer (2010). For this model fit, the γray photon spectrum is explained by the combination of a BLR and an accretion disk target photon component in the same way as in Finke & Dermer (2010). We found reasonable fits for a range of particle injection parameter values. The injection spectral index s of the electron spectrum is required to lie within the range of 2 and 3. The model fit is somewhat insensitive to changes in α, the injection rate index, providing α ≤ 4. For α> 4, the ambient electron spectrum would become too soft to be able to fit the low energy part (<1 eV) of the optically thin synchrotron radiation component. The parameter γ_{1} controls the position of the break in the emitting electron spectrum. Hence the model fit is quite sensitive to changes in this parameter. We found reasonable fits with γ_{1} between 800 and 1300. Furthermore, sensible fits were found when z = z_{b} was between 1500 and 3000. For γ_{2}> 20 000 the postbreak (>3 GeV) spectral index does not adequately represent the data. For γ_{2}< 10 000 the GeVspectrum becomes twopeak shaped, which does not fit the data well. The first injection point z_{a} is not well constrained here by the data since it merely influences the prebreak photon spectrum. Reasonable fits can be achieved for values between z_{a} = 100 and 800.
In the previous section, we demonstrated that broken powerlaw ambient electron spectra with changes in the spectral index, which are greater than the cooling break, can develop as a result of the continuously varying injection of nonthermal particles along the jet. We apply this property to the broadband data of 3C 454.3 to demonstrate that the observed decline of the GeVspectrum in bright FSRQs can be consistently modeled by this kind of scenario. Unlike in the previous fit, where two IC components are required, this scenario requires only one, but dominating IC component. In Fig. 16, we show a model fit to the data with a higher optical thickness (τ_{BLR} = 0.05) of the BLR. As a consequence, the BLR IC component dominates at γray energies >10 MeV. The GeV spectral turnover here is due to a corresponding break in the emitting electron spectrum, i.e., not the result of a combination of the accretion disk and BLR IC component. This different behavior also leads to differences with respect to the sensitivity of the model parameter values. The parameter value of z_{a} here is more constrained, since the prebreak emission of the BLR IC component dominates in the subGeV energy range (around 100 MeV). We require z_{a}< 200 to adequately fit the data. Similarly, changes in the last injection point z_{b} also impact the shape of the resulting ambient spectrum in the pre as well as postbreak regime. Choosing z_{b} between 2000 and 3000 leads to reasonable model fits. The injection rate index α influences the prebreak spectrum, and is therefore rather tightly constrained, as well, to values between α = 4 and 4.5, with electron injection spectral indices lying in the range s = 1.5–2.5. This choice also leads to a satisfying model representation of the observed synchrotron spectrum. The parameter values for γ_{1} and γ_{2} are similarly constrained, as in the previous model fit.
In summary, both model fits to the flare 3C 454.3 data set point towards gradually decreasing injection rates that start close to the inner boundary of the BLR but do not extend beyond the outer boundary of the BLR at the time of observations. Nalewajko et al. (2014) explored the efficiency of several constraints for the location of the blazar zone, such as the collimation, SSC, cooling and internal γray opacity constraints. Although, in our modeling, we adopted a somewhat weaker accretion disk and BLR luminosity than Nalewajko et al. (2014) for the November 2010 flare of 3C 454.3, we find that the blazar zone location in our model fits is in agreement with Nalewajko et al. (2014).
The injection spectrum is found to be surprisingly narrow, between γ ~ 10^{3}−10^{4}. The Thomson optical thickness τ_{BLR} of the diffuse BLR gas influences the relative importance of the BLR and accretion disk IC components. Accordingly, for a very low τ_{BLR}, the spectral decline observed at a few GeV from 3C 454.3 can be explained by the combination of both IC components while, for sufficiently larger τ_{BLR}, the GeVbreak in the photon spectrum is due to an intrinsic break in the emitting electron spectrum where the injection properties play a decisive role. The break energy is determined by the lowenergy cutoff γ_{1} of the injected electron spectrum. The observed, approximately constant, break energies that are independent of flux state (e.g., Abdo et al. 2011) imply a correspondingly constant γ_{1} for a constant Doppler factor, if there is no rapid change from a continuous to impulsivelike injection mode (or vice versa). The energy density of the magnetic field for these model fits is found below the jetframe disk energy density up to distances ~2000–3000 R_{g} above the black hole, and therefore justifies the neglect of synchrotron losses up to these distances.
Potentially, γray absorption, followed by pair production in the BLR radiation field, may impact the emerging photon spectrum (e.g., Donea & Protheroe 2003). Here, not only absolute luminosities of the BLR are important, but also its geometrical structure. For example, for a flat BLR geometry in blazars with typical BLR parameters, Lei & Wang (2014) demonstrate that high energy photons up to tens of GeV can escape this region.
We therefore investigate the importance of this process for the above parameter values. For a smooth broadband target spectrum, most of the photonphoton interactions take place in a small energy interval that is centered on (e.g., Reimer 2007) in the galaxy frame owing to the strongly peaked crosssection near the threshold. Gammagamma absorption in the BLR radiation field therefore modifies the observed γray spectrum beyond ϵ ≈ 3.1(ϵ_{0 ∗}(1 + z_{r}))^{1}, which is above the highest photon energy detected from this source for our parameter choice of ϵ_{0 ∗} = 10(m_{e}c^{2})^{1} eV.
During the April and September 2013 outbursts of this source, Pacciani et al. (2014) noted a very different flaring behavior: hard LATflares with exceptional hard powerlaw spectra, as opposed to the soft flaring events from 3C 454.3 that are considered in this work, which typically show strong declines or even cutoffs in the GeV range. From γγpair production arguments and the nondetection of any KNcurvature during these hard flare events, Pacciani et al. (2014) argue that the emission region must be beyond or at the outer rim of the BLR, where the bulk of the gammarays are produced by Comptonization of photons from the IR torus.
Model parameters fitting the November 2010 flare state SED of 3C 454.3.
4.2. Modeling the PKS 1510089 multifrequency SED
The FSRQ PKS 1510089 at redshift ~0.361 is among the best observed γray blazars with a wellconstrained SED from radio to γ rays. We apply our model to the quasisimultanuous broadband data from the January 2009 flare, as published in Abdo et al. (2010b), the first flare in a series of outbursts from this source in early 2009. These observations indicate variability on timescales of a day down to a few hours (e.g., Abdo et al. 2010a). Though PKS 1510089 is a known VHE FSRQ (Wagner et al. 2010), it has not been detected at VHEs during the considered outburst. Apart from γray observations, this source has also been monitored during the 2009 activity at radio, optical (including polarization measurements) and Xrays (Marscher et al. 2010). The appearance of two new knots on VLBA 43 GHz radio maps around August 2008 and April 2009, which move with superluminal speeds of ~24c and ~22c along the jet, seem to indicate a relation between these flaring events and their appearance (Marscher et al. 2010). The optical polarization vector started rotating by ~720° just after the flare that we consider here. The FermiLAT spectrum, during the January 2009 flare, indicates a pronounced steep decline at a few GeV, which has been observationally described by a logparabolic shaped spectrum (Abdo et al. 2010a).
Model parameters fitting the SED of PKS 1510089.
We present two sets of parameter values (see Table 3) that have been found to represent the data from the January 2009 flare well. Here again, the listed particle power P_{par} (including electrons and cold protons) is given as tenfold the total injected power of the nonthermal electrons. To quantify the black hole mass and accretion disk luminosity, we use M_{8} = 5 and l_{edd} = 0.16, which agrees well with data presented in Pucella et al. (2008).
In Fig. 17, we show a model fit where the joint Comptonscattered disk and BLR radiation explains the observed LATspectrum. In this fit, we keep the BLR geometry unchanged with respect to the 3C 454.3 fits, and use a (observerframe) size of the emitting region of R_{b} = 1 × 10^{15} cm, in agreement with Abdo et al. (2010a) and the inferred limits of Sbarrato et al. (2011). We now discuss the robustness of the parameter values used for our model fit. As in the fit to 3C 454.3, the model is quite sensitive to changes in γ_{1} since it controls the position of the breaks in the electron spectrum and, in turn, also controls the position of the respective breaks in the photon spectra. The injection spectral index s for this fit is required to lie between 1.5 and 2.5 for a reasonable fit. The model fit is again rather insensitive to changes in the injection parameter α since changes in this parameter mostly influence the spectral index before the break in the respective photon spectra. We get the best fit for z = z_{b} = 3000R_{g}, but values from 2000R_{g} to 4000R_{g} also lead to reasonable fits. For γ_{2}, we can achieve reasonable fits up to a value of 2 × 10^{4}, otherwise the model does not describe the high energy part (>1 GeV) of the data adequately. As in the 3C 454.3 case, the first injection point z_{a} is not well constrained. Values between z_{a} = 200R_{g} and z_{a} = 800R_{g} lead to reasonable fits. We note that the parameter values for this fit are quite similar to the ones used for the 3C 454.3 data set.
In Fig. 18 we present a model that is able to explain the γray data with Comptonscattered accretion disk radiation only. Here, the break in the GeVspectrum is generated by the break in the corresponding emitting electron spectrum. By reducing the geometric thickness of the BLR and keeping a realistic BLR optical depth, the importance of the BLR as a target photon field is diminished for the emitting region, since it is located at snapshot time just beyond the BLR border. Particle injection started when the emission region was inside the BLR and stopped just beyond the border of the BLR. We found that the accretion disk radiation dominated the target photon field energy density in this case. Other than the change of the BLR geometry, the fit parameter values are similar to the ones fitting the twocomponent model with only slight changes in γ_{1} and the bulk Doppler factor. Our fit is found to be sensitive again to changes in γ_{1} since it controls the position of the break. The injected electron spectrum is as narrow as in the 3C 454.3 fit, extending from γ ~ 10^{3}−10^{4}. For the other parameters, we reached reasonable fits at roughly the same parameter ranges that we used for the twocomponent fit.
Fig. 17
Twocomponent IC model fit to multifrequency data of PKS 1510089. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 3. a) Emitting electron spectrum. b) Synchroton spectrum fit to data from Abdo et al. (2010b). c) Gammaray spectrum with FermiLAT data Abdo et al. (2010b). d) Zooming into the γray spectrum with FermiLAT data (Abdo et al. 2010b). 
Fig. 18
Dominant accretiondisk IC model fit with multifrequency data of PKS 1510089. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 3. a) Emitting electron spectrum. b) Synchroton spectrum fit to data from Abdo et al. (2010b). c) Gammaray spectrum with FermiLAT data (Abdo et al. 2010b)). d) Zooming into the γray spectrum with FermiLAT data (Abdo et al. 2010b). 
Both model fits to the PKS 1510089 data require a continuous injection scenario with gradually decreasing injection rates. Thus, impulsive injection scenarios (i.e., α> 5) are again disfavored. In both of our model representations of the PKS 1510089 data set, the accretion disk IC component is more prominent than in the 3C 454.3 fits. The energy density of the magnetic field for these model fits is found below the jetframe disk energy density up to distances ~2000–3000R_{g} above the black hole, and therefore justifies the neglect of synchrotron losses up to these distances.
Abdo et al. (2010a) modelled this flare by also using a stationary leptonic blazar model, however, they were using parameter values that put more emphasis on the (assumed nonstratified) BLR and less on the accretion disk radiation field than our model parameter set values (and also the modeling of Böttcher et al. (2013) of this source). As a consequence the LATdata are explained rather by dominantly Comptonscattered BLRphotons from lower energetic electrons than our model envisions. The corresponding SSC component is found to be negligible.
Interestingly, our spectral modeling of this flaring event being due to the Compton scattered accretion disk and BLR photons from a ~1 G magnetized jet emission region, is in qualitative agreement with the scenario Marscher et al. (2010) proposed for this activity period.
Nalewajko et al. (2014) place the emission region of the April 2009 flare of this source outside the BLR, while no constraints were put on the January 2009 outburst. Our model fit parameters for this January 2009 flare point towards an emission region that is located inside the BLR at the time of this flare. If the series of flares in 2009 of PKS 1510089 were causally connected, possibly originating from the same socalled blob that was moving along the jet, then the location of this blob that caused the January 2009 flare would be well outside the BLR at the time of the April 2009 flare, assuming no strong blobbraking. This would be compatible with the results of Nalewajko et al. (2014).
We note that the Herschel PACS & SPIRE data from observations of this source in late 2011 (Nalewajko et al. 2012) lie above our model curves. Hence, if this IR flux were comparable during the here considered 2009 event, these IR photons would have to be produced by a further region within the jet with possibly some notable contribution from the dusty torus.
Similar to 3C 454.3 (see Sect. 4.1), we find γγpair production being negligible for the parameter set used for the above model fits and below the last LAT data point (Barnacka 2013).
Chen et al. (2012) modelled the last flare in the extended early 2009 flaring episode of this source by using a timedependent Monte Carlo FokkerPlanck code, where the emission region is treated as an extended cylindrical volume within the jet. In addition to a particle “pickup” term in the FokkerPlanck equation, they also included a stochastic acceleration term and took into account all external and internal target photon fields. Although, in their modeling, they did not discuss pronounced GeV spectral turnover, but rather focused on spectral variability, they note the impact of not only internal but also external lighttravel time effects causing complex spectral shapes and variations in this March 2009 flaring event. In our approach to explain complex highenergy spectral shapes, we found that the injection history already has a strong impact, and is able to reproduce the typically observed pronounced turnovers at GeV energies.
5. Summary and conclusion
Within the framework of a leptonic emission model for blazars, where inverse Compton scattering on external radiation fields dominates, we considered the case of continuous particle injection of a given simple power law along the jet with various injection rates, durations, and locations of the emission region within the jet. We calculated the emitting particle spectrum that results from this kind of setup at a snapshot time t_{obs}, taking into account radiative cooling (in the Thomson regime) in the accretion disk and BLR radiation field during injection selfconsistently. This prescription offers the possibility to explain a broad range of ambient electron spectral shapes, including spectral breaks that are significantly larger than simple cooling breaks. The injection properties may provide valuable information on the acceleration mode at work. Hence, our simple phenomenological prescription has the potential to find interesting clues in this aspect by rigorously analyzing the ambient electron spectrum that is required for the broadband fit of a given quasisimultaneous multifrequency data set, in conjunction with constraints that are inferred from correlated variability studies and γray opacity arguments.
For example, the peak of the emitting electron spectrum can, in general, be linked to the minimum injection energy γ_{1}m_{e}c^{2} if the injection rate distribution is not too steep. For impulsivelike injections (i.e., large α within our model) the peak in the ambient particle spectrum is, instead, associated with the smallest cooled electron energy. The peak in the electron spectrum results in corresponding spectral turnovers in the Comptonscattered photon components. Thus γ_{1} is a parameter that may influence the γray break energy.
Our model has the potential to describe broad highenergy components, as well as doublepeaked ones (with one peak corresponding to Comptonscattered accretion disk photons, and the second one from ICscattered BLR radiation field). The former case arises for not too steep injection spectra, while very steep ones, or injections where γ_{2} is suitably small, can give SEDs with doublepeaked γray spectra. In general the injection spectral index s, together with γ_{2} and the time since last injection (given the accretion disk luminosity), mostly determine the postbreak shape of the spectrum. For example, fitting the flare state SEDs of 3C 454.3 and PKS 1510089 required rather conservative injection indices (s = 2–3), as expected from, for example, Fermi acceleration.
The injection rate index α strongly influences the ambient electron spectrum ahead of the peak. Observationally, this may be visible below the photon turnover frequency in case of one Comptonscattered component that dominates the highenergy regime, or in the synchrotron component in the optically thin prebreak energy range. The accretion disk IC component would mask the lowenergy part of the BLR IC component in a twocomponent IC scenario. Accordingly, the rate of injection might be directly reflected in the prebreak shape of the GeVspectrum in the former case.
Limits in the initial injection point z_{a} of the flare can be derived if the smallest particle energy in the cooled electron spectrum can be estimated, given the accretion disk luminosity.
In summary, if the ambient electron spectrum is unambiguously determined (e.g., from the optically thin synchrotron spectrum), it is possible to set limits on the injection rate index α. Together with analyzing the high energy component with sufficient broadband coverage and a fair knowledge of the accretion disk radiation, the remaining particle injection properties can be constrained.
We have demonstrated this for the SEDs of two FSRQs, 3C 454.3 and PKS 1510089 where the flare state broadband SEDs have been analyzed to derive information on the required injection scenario. Two principally different scenarios per source were found to be viable: a onecomponent IC model, where either the Comptonscattered BLR or accretion disk radiation field dominates, and a twocomponent model as proposed in Finke & Dermer (2010) for 3C 454.3. Accordingly, the origin of the observed spectral turnover at a few GeV is either found in the corresponding break in the ambient electron spectrum, or is due to the combination of Comptonscattered accretion disk and BLR radiation field.
The observed turnover energy in the GeV range is, in both scenarios, approximately determined by ∝.
A constant GeV break energy that is independent of flux state has been reported for 3C 454.3 (Abdo et al. 2011), which implies that γ_{1} is broadly independent of the flux level for not significantly changing beaming parameters during flux variations. The required injection parameters for both cases of the two sources studied disfavor impulsivelike/instantaneous electron injection, but point towards rather narrow particle spectra injected continuously with a gradually decreasing rate into the moving plasma blob. For all of our model fits, the emitting region is either inside or just beyond the BLR, which is compatible with the results of Nalewajko et al. (2014), thus making the BLR an integral part of the model. In this context, we also note that the BLR geometry impacts the resulting γray spectra. A good knowledge of the BLR structure therefore improves accurate and unambiguous modeling of the γray spectrum. In all scenarios, a further spectral break would be expected at a few tens of MeV. In the onecomponent IC scenario for 3C 454.3, this break arises from the combination of ICscattered accretion disk and BLR photons. The break energy is determined by the smallest energy in the ambient electron spectrum, which in turn is influenced by the initial injection point z_{a}. In the twocomponent IC scenario, this energy corresponds to the IC scattered (in the accretion disk) ambient particle break energy or the smallest energy of this spectrum. Potentially, these scenarios could, observationally, be distinguished by an improved coverage of the 0.1–1 eV (12.4–1.3 μm) energy range of the optically thin jet emission quasisimultaneously to the γray observations, and/or precision measurements at MeV energies, in conjunction with GeV observations, which might become possible with future projects like AstroMeV^{1} or the proposed GAMMALIGHT (Morselli et al. 2013) instrument. Extending the GeV energy range of the FermiLAT instrument down to few tens of MeV and using the LAT Pass 8 eventlevel analysis (Atwood et al. 2013) may already provide a possibility of distinguishing between models that show notably different spectral signatures in that energy range, as is the case, of the presented 3C 454.3 models.
Acknowledgments
We thank Benoît Lott for valuable discussions and providing tables of the 3C 454.3 data. We also acknowledge particularly valuable discussions with Chuck Dermer and Ann Wehrle on this work. This project was funded by the FWF Doctoral School CIM Computational Interdisciplinary Modelling under contract W 1227N16 (DKplus CIM), and by a Marie Curie International Reintegration Grant (grant 24803) within the 7th European Community Framework Programme. The publication is supported by the Austrian Science Fund (FWF). This work was performed on the computational resource bwUniCluster funded by the Ministry of Science, Research and the Arts BadenWürttemberg and the Universities of the State of BadenWürttemberg, Germany, within the framework program bwHPC.
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All Tables
All Figures
Fig. 1
Geometry of the blazar jet model considered in this work (figure adapted from Dermer & Schlickeiser 1993). 

In the text 
Fig. 2
Our BLR model, which consists of a spherically symmetric shell of gas between R_{i} and R_{o} and a density gradient ζ with n_{e}(R) ∝ R^{ζ} (figure adapted from Dermer et al. 2009). 

In the text 
Fig. 3
Angle dependence of for a BLR extending from 10^{2} to 10^{5}R_{g} for different values of z (in R_{g}) and ζ, in agreement with Dermer et al. (2009). 

In the text 
Fig. 4
Comparison of radiative electron energyloss rates. Here we choose BLR1 at z = 100 as an example, while noting that the qualitative picture, with the negligible BLR losses, is the same in all the cases we considered in our study. We compare with synchrotron loss rates for a B = 4.5 G magnetic field. a) Radiative electron energy loss rates for varying z for electron energy γ = 500 and BLR1 with τ_{BLR} = 0.01. b) Radiative electron energy loss rates for varying γ at z = 100 and BLR1 with τ_{BLR} = 0.01. BLR shows the BLR energy loss used in our calculations, here we set the energy loss in the KleinNishina regime to 0. 

In the text 
Fig. 5
IC photon spectra (and ambient electron spectrum as an inlay in panel b for the reference model) for different BLR geometries used. a) Composite IC photon spectrum for the case of BLR1. b) Resulting IC photon spectra when varying the BLR geometries. The inlay shows the underlying ambient electron spectrum. 

In the text 
Fig. 6
Emitting electron (left) and resulting photon spectra (right) for various l_{edd}. Where l_{edd} = 0.01 we also show the photon components produced by both target photon fields separately. 

In the text 
Fig. 7
Emitting electron (left) spectra and corresponding photon spectra (right) for γ_{1} that varies with respect to the reference model. The total injected particle energies are strongly determined by γ_{1}. For γ_{1} = (100,500,1000,1500), we find Υ_{inj} = (10.1,2.0,1,0.7). 

In the text 
Fig. 8
Emitting electron (left) and corresponding photon spectra (right) for spectral injection indices s, varying with respect to the reference model. The total injected electron energies for s = (2,3,4) are Υ_{inj} = (4.7 × 10^{3},1,5.1 × 10^{4}). In the case of s = 4, the photon components produced by both target photon fields are shown separately as well. 

In the text 
Fig. 9
Emitting electron spectra (left) and corresponding photon spectra (right) for γ_{2} that vary with respect to the reference model. The total injected electron energy is rather insensitive to γ_{2}. For γ_{2} = (3000,5000,8000,10 000) we find Υ_{inj} = (0.7,0.8,0.9,0.9). In the case of γ_{2} = 3000, we show the photon components produced by both target photon fields. 

In the text 
Fig. 10
Ambient electron (left) and photon spectra (right) with different injection rate parameters α, with respect to the reference model. The total injected electron energies for α = (0,1,2,3,4) are calculated to Υ_{inj} = (4 × 10^{5},512,1,0.3,9 × 10^{6}). In the case of α = 4, we also show the IC components produced by both target photon fields separately. 

In the text 
Fig. 11
Ambient electron (left) and photon spectra (right) when varying z_{a} (in R_{g}) with respect to the reference model. The injected total electron energies for z_{a} = (100,200,500,1000) are Υ_{inj} = (2.1,1,0.33,0.1). The total injected energy decreases with rising z_{a}. 

In the text 
Fig. 12
Ambient electron (left) and photon spectra (right) when varying the distances between the points z and z_{b} (in R_{g}), with respect to the reference model. The total injected electron energy is Υ_{inj} = 1 in all cases. For z = 2100, we also show the IC photon components produced by the two target photon fields considered separately. 

In the text 
Fig. 13
ambient electron (left) and photon spectra (right) for various z_{b} (in R_{g}) with respect to the reference model. The total injected electron energies for z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (0.9,1,1.04,1.06). For z_{b} = 1000, the IC photon components produced by the two target photon fields are also shown separately. 

In the text 
Fig. 14
Photon and ambient electron spectra for z_{b} (in R_{g}) and α with respect to the reference model. The total injected electron energies for α = 3 and z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (2.7,2.75,2.8,2.8) × 10^{3} while, for α = 7, the total injected electron energies for z_{b} = (1000,2000,3000,4000) are Υ_{inj} = (5.8,5.8,5.8,5.8) × 10^{13}. For α = 3 and α = 7 with z_{b} = 1000, we also show the IC photon components produced by the two target photon fields separately. a) Normalized electron spectra for various z_{b} (in R_{g}) and α = 3. b) Corresponding photon spectra for various z_{b} (in R_{g}) and α = 3. c) Normalized electron spectra for various z_{b} (in R_{g}) and α = 7. d) Corresponding photon spectra for various z_{b} (in R_{g}) and α = 7. 

In the text 
Fig. 15
Twocomponent IC model fit to multifrequency data of 3C 454.3. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 2. a) Emitting electronspectrum. b) Synchroton spectrum with Swift, Herschel and Submillimeter Array data taken during the November 2010 flare (Wehrle et al. 2012). c) Gammaray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). d) Zooming into the γray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). 

In the text 
Fig. 16
DominantBLR IC model fit with multifrequency data of 3C 454.3. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 2. a) Emitting electron spectrum. b) Synchroton spectrum with Swift, Herschel and Submillimeter Array data taken during the November 2010 flare (Wehrle et al. 2012). c) Gammaray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). d) Zooming into the γray spectrum with FermiLAT data taken during the November 2010 flare (Abdo et al. 2011). 

In the text 
Fig. 17
Twocomponent IC model fit to multifrequency data of PKS 1510089. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 3. a) Emitting electron spectrum. b) Synchroton spectrum fit to data from Abdo et al. (2010b). c) Gammaray spectrum with FermiLAT data Abdo et al. (2010b). d) Zooming into the γray spectrum with FermiLAT data (Abdo et al. 2010b). 

In the text 
Fig. 18
Dominant accretiondisk IC model fit with multifrequency data of PKS 1510089. The model is shown in red with the data points shown in blue. The model parameter values are listed in Table 3. a) Emitting electron spectrum. b) Synchroton spectrum fit to data from Abdo et al. (2010b). c) Gammaray spectrum with FermiLAT data (Abdo et al. 2010b)). d) Zooming into the γray spectrum with FermiLAT data (Abdo et al. 2010b). 

In the text 
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