The power of blazar jets

The power of blazar jets

Annalisa Celotti and Gabriele Ghisellini
S.I.S.S.A., V. Beirut 2–4, I-34014 Trieste, Italy
INAF – Osservatorio Astronomico di Brera, V. Bianchi 46, I–23807 Merate, Italy

We estimate the power of relativistic, extragalactic jets by modelling the spectral energy distribution of a large number of blazars. We adopt a simple one–zone, homogeneous, leptonic synchrotron and inverse Compton model, taking into account seed photons originating both locally in the jet and externally. The blazars under study have an often dominant high energy component, which, if interpreted as due to inverse Compton radiation, limits the value of the magnetic field within the emission region. As a consequence, the corresponding Poynting flux cannot be energetically dominant. Also the bulk kinetic power in relativistic leptons is often smaller than the dissipated luminosity. This suggests that the typical jet should comprise an energetically dominant proton component. If there is one proton per relativistic electrons, jets radiate around 2–10 per cent of their power in high power blazars and 3–30 per cent in less powerful BL Lacs.

galaxies: active - galaxies:jets - radiative processes: non–thermal
pagerange: LABEL:firstpageLABEL:lastpagepubyear: 2002

1 Introduction

The radiation observed from blazars is dominated by the emission from relativistic jets (Blandford & Rees 1978) which transport energy and momentum to large scales. As the energy content on such scales already implies in some sources jet powers comparable with that which can be produced by the central engine (e.g. Rawlings & Saunders 1991), only a relatively small fraction of it can be radiatively dissipated on the ‘blazar’ (inner) scales.

However we still do not know the actual power budget in jets and in which form such energy is transported, namely whether it is mostly ordered kinetic energy of the plasma and/or Poynting flux. In addition, the predominance of one or the other form can change during their propagation. These of course are crucial pieces of information for the understanding on how jets are formed and for quantifying the energy deposition on large scales.

In principle the observed radiation can – via the modelling of the radiative dissipation mechanism – set constraints on the minimum jet power and can even lead to estimates of the relative contribution of particles (and the corresponding bulk kinetic power), radiation and magnetic fields. The modelling depends of course on the available spectral information and conditions on the various jet scales (i.e. distances from the central power–house). Attempts in this direction include the work by Rawlings & Saunders (1991), who considered the energy contained in the extended radio lobes of radio–galaxies and radio–loud quasars. By estimating their life–times they could calculate the average power needed to sustain the emission from the lobe themselves (Burbidge 1959).

At the scale of hundreds of kpc the Chandra satellite observations, if interpreted as inverse Compton scattering on the Cosmic Microwave Background (Tavecchio et al. 2000; Celotti, Ghisellini & Chiaberge 2001), indicate that jets of powerful blazars are still relativistic. This allowed Ghisellini & Celotti (2001) to estimate a minimum power at these distances for PKS 0637–752, the first source whose large scale X–ray jet was detected by Chandra. Several other blazars were studied by Tavecchio et al. (2004), Sambruna et al. (2006) and Tavecchio et al. (2007) who found that the estimated powers at large scales were comparable (within factors of order unity) with those inferred at much smaller blazar scales.

Celotti & Fabian (1993) considered the core of jets, as observed by VLBI techniques, to derive a size of the emitting volume and the number of emitting electrons needed to account for the observed radio luminosity. The bulk Lorentz factor, which affects the quantitative modelling, was estimated from the relativistic beaming factor required not to overproduce, by synchrotron self–Compton emission, the observed X–ray flux (e.g. Celotti 1997).

A great advance in our understanding of blazars came however with the discovery that they are powerful –ray emitters (Hartman et al. 1999). Their –ray luminosity often dominates (in the powerful flat spectrum radio–loud quasars, FSRQs) the radiative power, and its variability implies a compact emitting region. The better determined overall spectral energy distribution (SED) and total observed luminosity of blazars constrain – via pair opacity arguments (Ghisellini & Madau 1996) – the location in the jet where most of the dissipation occurs. For a given radiation mechanism the modelling of the SED also allows to estimate the power requirements and the physical conditions of this emitting region. Currently the models proposed to interpret the emission in blazars fall into two broad classes. The so-called ‘hadronic’ models invoke the presence of highly relativistic protons, directly emitting via synchrotron or inducing electron–positron (e) pair cascades following proton-proton or proton–photon interactions (e.g., Mannheim 1993, Aharonian 2000, Mücke et al. 2003, Atoyan & Dermer 2003). The alternative class of models assumes the direct emission from relativistic electrons or e pairs, radiating via the synchrotron and inverse Compton mechanism. Different scenarios are mainly characterised by the different nature of the bulk of the seed photons which are Compton scattered. These photons can be produced both locally via the synchrotron process (SSC models, Maraschi, Ghisellini & Celotti 2002), and outside the jet (External Compton models, EC) by e.g. the gas clouds within the Broad Line Region (BLR; Sikora, Begelman & Rees 1994, Sikora et al. 1997) reprocessing 10 per cent of the disk luminosity. Other contributions may comprise synchrotron radiation scattered back by free electrons in the BLR and/or around the walls of the jet (mirror models, Ghisellini & Madau 1996), and radiation directly from the accretion disk (Dermer & Schlickeiser 1993; Celotti, Ghisellini & Fabian, 2007).

Some problems suffered by hadronic scenarios (such as pair reprocessing, Ghisellini 2004) make us favour the latter class of models. By reproducing the broad band properties of a sample of –ray emitting blazars via the SSC and EC mechanisms, Fossati et al. (1998) and Ghisellini et al. (1998; hereafter G98) constrained the physical parameters of a (homogeneous) emitting source. A few interesting clues emerged. The luminosity and SED of the sources appear to be connected, and a spectral sequence in which the energy of the two spectral components and the relative intensity decrease with source power seems to characterise blazars, from low power BL Lacs to powerful FSRQs (opposite claims have been put forward by Giommi et al. 2007; see also Padovani 2006). This SED sequence translates into an (inverse) correlation between the energy of particles emitting at the spectral peaks and the energy density in magnetic and radiation fields (Ghisellini, Celotti & Costamante 2002; hereafter G02). An interpretation of such findings is possible within the internal shock scenario (Ghisellini 1999; Spada et al. 2001; Guetta et al 2004), which could account for the radiative efficiency, location of the dissipative region and spectral trend if the particle acceleration process is balanced by the radiative cooling. In such a scenario the energetics on scales of 10 Schwarzschild radii is dominated by the power associated to the bulk motion of plasma. This is in contrast with an electromagnetically dominated flow (Blandford 2002; Lyutikov & Blandford 2003).

Within the frame of the same SSC and EC emission model, in this work we consider the implications on the jet energetics, the form in which the energy is transported and possibly the plasma composition. In particular we estimate the (minimum) power which is carried by the emitting plasma in electromagnetic and kinetic form in a significant sample of blazars at the scale where the –ray emission – and hence most of the luminosity – is produced. Such scale corresponds to a distance from the black hole of the order of cm (Ghisellini & Madau 1996), a factor 10–100 smaller than the VLBI one. The found energetics are lower limits as they only consider the particles required to produce the observed radiation, and neglect (cold) electrons not contributing to the emission.

In Section 2 the sample of sources is presented. In Section 3 we describe how the power in particles and field have been estimated, and the main assumptions of the radiative model adopted. The results are reported in Section 4 and discussed in Section 5. Preliminary and partial results concerning the power of blazar jets were presented in conference proceedings (see e.g. Ghisellini 1999, Celotti 2001, Ghisellini 2004).

We adopt a concordance cosmology with km s Mpc, and .

2 The sample

The sample comprises the blazars studied by G98, namely all blazars detected by EGRET or in the TeV band (at that time) for which there is information on the redshift and on the spectral slope in the –ray band.

To those, FSRQs identified as EGRET sources since 1998 or not present in G98 have been added, namely: PKS 0336–019 (Mattox et al. 2001); Q0906+6930 (the most distant blazar known, at , Romani et al. 2004; Romani 2006); PKS 1334–127 (Hartman et al. 1999; modelled by Foschini et al. 2006); PKS 1830–211 (Mattox et al. 1997; studied and modelled by Foschini et al. 2006); PKS 2255–282 (Bertsch 1998; Macomb, Gehrels & Shrader 1999). and the three high redshift () blazars 0525–3343; 1428+4217 and 1508+5714, discussed and modelled in G02.

As for BL Lacs, we have included 0851+202 (identified as an EGRET source, Hartman et al. 1999; modelled by Costamante & Ghisellini 2002; hereafter C02) and those detected in the TeV band besides Mkn 421, Mkn 501, and 2344+512, which were already present in G98. These additional TeV BL Lacs are: 1011+496 (Albert et al. 2007c; see C02); 1101–232 (Aharonian et al. 2006a; see C02 and G02); 1133+704 (Albert et al. 2006a; see C02); 1218+304 (Albert et al. 2006b; see C02 and G02); 1426+428 (Aharonian et al. 2002; Aharonian et al. 2003; see G02); 1553+113 (Aharonian et al. 2006b; Albert et al. 2007a; see C02); 1959+650 (Albert et al. 2006c; see C02); 2005–489 (Aharonian et al. 2005a; see C02 and G02); 2155–304 (Aharonian et al. 2005b; Aharonian et al. 2007b; already present in G98 as an EGRET source); 2200+420 (Albert et al. 2007b; already present in G98 as an EGRET source); 2356–309 (Aharonian et al. 2006a; Aharonian et al. 2006c; see C02 and G02). Finally, we have considered the BL Lacs modelled in G02, namely 0033+505, 0120+340, 0548–322 and 1114+203.

In all cases the observational data were good enough to determine the location of the high energy peak, a crucial information to constrain the model input parameters. The total number of sources is 74: 46 FSRQs and 28 BL Lac objects, 14 of which are TeV detected sources. The objects are listed in Table 1 together with the input parameters of the model fit.

3 Jet powers: assumptions and method

As already mentioned and widely assumed, the infrared to –ray SED of these sources was interpreted in terms of a one–zone homogeneous model in which a single relativistic lepton population produces the low energy spectral component via the synchrotron process and the high energy one via the inverse Compton mechanism. Target photons for the inverse Compton scattering comprise both synchrotron photons produced internally to the emitting region itself and photons produced by an external source, whose spectrum is represented by a diluted blackbody peaking at a (comoving) frequency Hz. We refer to G02 for further details about the model.

The emitting plasma is moving with velocity and bulk Lorentz factor , at an angle with respect to the line of sight. The observed radiation is postulated to originate in a zone of the jet, described as a cylinder, with thickness as seen in the comoving frame, and volume . is the cross section radius of the jet.

The emitting region contains the relativistic emitting leptons and (possibly) protons of comoving density and , respectively, embedded in a magnetic field of component perpendicular to the direction of motion, homogeneous and tangled throughout the region. The model fitting allows to infer the physical parameters of the emitting region, namely its size and beaming factor, and of the emitting plasma, i.e. and . These quantities translate into jet kinetic powers and Poynting flux.

Assuming one proton per relativistic emitting electron and protons ‘cold’ in the comoving frame, the proton kinetic power corresponds to


while relativistic leptons contribute to the kinetic power as:


where is the average random Lorentz factor of the leptons, measured in the comoving frame, and , are the proton and electron rest masses, respectively.

The power carried as Poynting flux is given by


The observed synchrotron and self–Compton luminosities are related to the comoving luminosities (assumed to be isotropic in this frame) by , where the relativistic Doppler factor . The EC luminosity, instead, has a different dependence on , being anisotropic in the comoving frame, with a boosting factor (Dermer 1995). The latter coincides to that of the synchrotron and self–Compton radiation for i.e. when the viewing angle is . For simplicity, we adopt a boosting for all emission components.

Besides the jet powers corresponding to protons, leptons and magnetic field flowing in the jet, there is also an analogous component associated to radiation, corresponding to:


where is the radiation energy density measured in the comoving frame.

We refer to G02 for a detailed discussion on the general robustness and uniqueness of the values which are inferred from the modelling. Here we only briefly recall the main assumptions of this approach.

The relativistic particles are assumed to be injected throughout the emitting volume for a finite time . Since blazars are variable (flaring) sources, a reasonably good representation of the observed spectrum can be obtained by considering the particle distribution at the end of the injection, at , when the emitted luminosity is maximised. In this respect therefore the powers estimated refer to flaring states of the considered blazars and do not necessarily represent average values.

As the injection lasts for a finite timescale, only the higher energy particles have time to cool (i.e. ). The particle distribution can be described as a broken power–law with the injection slope below and steeper above it. We adopt a particle distribution that corresponds to injecting a broken power–law with slopes and below and above the break at . Thus the resulting shape of depends on 1) the injected distribution and 2) the cooling time with respect to .

The limiting cases in relation to 2) can be identified with powerful FSRQs and low power BL Lacs. For FSRQs the cooling time is shorter than for all particle energies (fast cooling regime) and therefore the resulting is a broken power–law with a break at , the energy of the leptons emitting most of the observed radiation, i.e.


For low power BL Lacs only the highest energy leptons can cool in (slow cooling regime), and if the cooling energy (in ) is ( is the highest energy of the injected leptons), we have:


For intermediate cases the detailed is fully described in G02.

3.1 Dependence of the jet power on the assumptions

We examine here the influence of the most crucial assumptions on the estimated powers.

  • Low energy cutoff — A well known crucial parameter for the estimates of powers in particles, which is poorly fixed by the modelling, is the low energy distribution of the emitting leptons, parametrised via a minimum (i.e. for say ). Indeed particles of such low energies (if present) would not contribute to the observed synchrotron spectrum, since they emit self–absorbed radiation. They would instead contribute to the low energy part of the inverse Compton spectrum, but: i) in the case of SSC emission, their contribution is dominated by the synchrotron luminosity of higher energy leptons; ii) in the case of EC emission their radiation could be masked by the SSC (again produced by higher energy leptons) or by contributions from other parts of the jet.

    However in very powerful sources there are indications that the EC emission dominates in the X–ray range and thus the observations provide an upper limit to . In such sources there is direct spectral evidence that is close to unity. Fig. 1 illustrates this point. It can be seen how the model changes by assuming different : only when 1 a good fit of the soft X–ray spectrum can be obtained. For such powerful blazars, the cooling time is short for leptons of all energies, ensuring that extends down at least to a few. The extrapolation of the distribution down to with a slope therefore implies that the possible associated error in calculating the number of leptons is .

    For low power BL Lacs the value of is much more uncertain. In the majority of cases , and our extrapolation assuming again a slope translates in an uncertainty in the lepton number . Thus and could be smaller up to this factor.

    Figure 1: Top panel: SED of 1127–145 ‘fitted’ by our model, assuming . Dashed line: the contribution of the accretion disk luminosity, assumed to a be represented by a black–body. Bottom panel: zoom in the X–ray band. The solid lines corresponds to the modelling with different values of (as labelled), illustrating that in this source the low energy cut–off cannot be significantly larger than unity.
  • Shell width — Another key parameter for the estimate of the kinetic powers is . We set . controls and therefore in the slow cooling regime. Variability timescales imply that . Although there is no obvious lower limit to which can be inferred from observational constraints, the choice of a smaller can lead to an incorrect estimate of the observed flux, unless the different travel paths of photons originating in different parts of the source are properly taken into account. As illustrative case consider a source with : the photons reaching the observer are those leaving the source at 90 from the jet axis (in the comoving frame). Assume also that the source emits in this frame for a time interval . If , then a (comoving) observer at 90 can detect photons only from a ‘slice’ of the source at any given time. Only when the entire source can be seen (Chiaberge & Ghisellini 1999). This is the reason to assume .

  • Filling factor — Our derivations are based on the assumption of a single homogeneous emitting region. However it is not implausible to imagine that the emitting volume is inhomogeneous, with filaments and/or smaller clumps occupying only a fraction of the volume. How would this alter our estimates? As illustrative case let us compare the parameters inferred from the SED modelling from a region of size with one filled by emitting clouds of typical dimension and density . As the synchrotron and Compton peak frequencies determine univocally the value of the magnetic field, in order to model the SED the same field have to permeate the clumps. This in turn fixes the same total number of synchrotron emitting leptons. If the high energy component is due to EC the same spectrum is then produced, independently of the filling factor. In the case of a dominant SSC emission, instead, it is necessary to also require that the ensemble of clouds radiate the same total SSC spectrum, i.e. that each cloud has the same scattering optical depth of the whole homogeneous region (i.e. ).

    In both cases (SSC and EC) the kinetic power derived by fitting the SED is the same, but in the clumped scenario the required Poynting flux can be less (since in this case the same magnetic field permeates only the emitting clouds). This thus strengthens our conclusions on the relative importance of and at least in the case of BL Lacs.

4 Results

The model fitting allowed us to derive the intrinsic physical parameters of the sources as described in Section 3. The interesting quantities thus inferred are reported in Table 1 in the Appendix. In the Appendix we also report the SEDs of all the blazars in our sample and the corresponding spectral models. Histograms reproducing the distributions of powers for the populations of FSRQs, BL Lacs and TeV sources are shown in Fig. 2. As said these estimates refer to a minimum random Lorentz factor (see below) and assumes the presence of one proton per emitting lepton.

Different classes of sources (FSRQs, BL Lacs and TeV detected BL Lacs) form a sequence with respect to their kinetic powers and Poynting flux distributions. Within each class, the spread of the distributions is similar.

The robust quantity here is , directly inferred from observations and rather model independent as it relies only on , providing a lower limit to the total flow power. ranges between erg s. and reach powers of erg s, while if a proton component is present erg s. Fig. 2 also shows the distribution of , which corresponds to the rest mass of the emitting leptons, neglecting their random energy, i.e. .

In Fig. 3 the distributions of the energetics corresponding to the powers shown in Fig. 2 are reported. These have been simply computed by considering a power ‘integrated’ over the time duration of the flare, as measured in the observer frame, . The energy distributions follow the same trends as the powers.

In order to directly compare the different forms of power with respect to the radiated one, in Fig. 4 , and are shown as functions of .

Finally, Fig. 5 shows the ratios , and as functions of . In general all three ratios tend to be smaller for increasing , the (anti) correlation being most clear for (mid panel). This is the direct consequence of interpreting the trend observed in blazar SEDs in terms of cooling efficiency: in the fast cooling regime (powerful sources) low energy leptons (and thus small ) are required at any given time. Vice–versa, in the less powerful (TeV) BL Lacs is close to unity: indeed in the slow cooling regime the mean random Lorentz factor of the emitting leptons approaches (and slightly exceeds in several cases) . In the latter sources assuming one proton per emitting lepton results in which is also comparable to , namely approaches unity at low .

In the following we discuss more specifically the results for high (FSRQs) and low power (BL Lacs) blazars.

Figure 2: Power associated to protons, relativistic electrons (or e), Poynting flux, radiatively emitted and bulk energy of cold leptons. Hatched areas correspond to BL Lacs and TeV detected sources. As detailed in the text these values assume that all leptons are relativistic, , and that there is one proton per lepton.
Figure 3: Energy in protons, relativistic leptons, Poynting flux and emitted radiatively. Hatched areas correspond to BL Lacs. The energetics have been calculated multiplying the powers by .

4.1 Flat Spectrum Radio Quasars

Powerful blazars include FSRQs and some BL Lac objects whose classification is uncertain, due to the presence of broad (albeit with small equivalent width) emission lines (e.g. PKS 0537–441).

Fig. 4 shows that the kinetic power associated to a plasma dominated (in terms of inertia) by relativistic leptons (electrons and/or e) would be typically insufficient to account for the observed radiation.

As exceeds and for leptons of all energies is shorter then the dynamical time, the radiating particles must be continuously injected/re–accelerated. Thus there should be another source of power other than that associated to leptons (see the bottom panel of Fig. 2) able to provide energy to the emitting particles.

The power in Poynting flux, , has values comparable to (Fig. 4). This component is never dominating, as expected from the fact that the luminosity of all FSRQs is predominantly in the high energy component, interpreted as EC emission, which implies that , controlling the synchrotron output, is limited. In principle, there exists a degree of freedom for the estimate of the magnetic field resulting from the uncertainty on the external radiation energy density. The more intense the external radiation density, the larger the magnetic field, to produce the same Compton to synchrotron luminosity ratio. Nevertheless can vary only in a relatively narrow range, being constrained both by the peak frequency of the synchrotron component and by the observational limits on the external photon field if this is due – as the model postulates – to broad line and/or disc photons.

Figure 4: Powers associated to the bulk motion of cold protons, emitting leptons and Poynting flux as functions of the radiative output . Triangles: FSRQs, circles: BL Lac objects, filled circles: TeV detected BL Lacs. The dashed lines correspond to equal powers.
Figure 5: The fraction of radiated (, top panel), in relativistic leptons (, mid panel) and in magnetic fields (, bottom panel) as functions of . The TeV BL Lac with efficiency exceeding unity is Mkn 501. Symbols as in Fig. 4.

As neither the Poynting flux nor the kinetic power in emitting leptons are sufficient to account for the radiated luminosity let us then consider the possible sources of power.

The simplest hypothesis is that jets are loaded with hadrons. If there were a proton for each emitting electron, the corresponding would be dominant, a factor 10–50 larger than (see Fig. 2 and Fig. 4). This would imply an efficiency () of order 2–10 per cent.

These efficiencies are what expected if jets supply the radio lobes. There are two important consequences. Firstly, a limit on the amount of electron–positron pairs that can be present. Since they would lower the estimated , only a few (2–3) e per proton are allowed (see also Sikora & Madejski 2000). Secondly, and for the same reason, the lower energy cut–off of cannot exceed a few.

The inferred values of appear to be large if compared to the average power required to energise radio lobes (Rawlings & Saunders 1991). However our estimates refer to flaring states. To infer average values information on the flare duty cycle would be needed. While in general this is not well known, the brightest and best observed –ray EGRET sources (3C 279, Hartman et al. 2001, and PKS 0528+134, Ghisellini et al. 1999) indicate values around 10 per cent (GLAST will provide a excellent estimate on this). If a duty cycle of 10 per cent is typical of all FSRQs, the average kinetic powers becomes 10 times smaller than our estimates, and comparable with the Eddington luminosity from systems harbouring a few M black hole.

The power reservoir could be in principle provided also by the inertia of a population of ‘cold’ (i.e. non emitting) e pairs. In order to account for – say to provide erg s – they should amount to a factor larger than the number of the radiating particles, corresponding to a scattering optical depth , where is the Thomson cross section and the value of refers to the radiating zone111Throughout this work the notation and cgs units are adopted.. Conservation of pairs demands at cm, i.e. the base of the jet (assuming that there ). Such high values of however would imply both rapid pair annihilation (Ghisellini et al. 1992) and efficient interaction with external photons, leading to Compton drag on the jet and to a visible spectral component in the X–ray band (Sikora, Begelman & Rees 1994; Celotti, Ghisellini & Fabian 2007).

Within the framework of the assumed model, jets of high power blazars have then to be heavy, namely dynamically dominated by the bulk motion of protons, as both leptons and Poynting flux do not provide sufficient power to account for the observed emission and supply energy to the radio lobes. A caveat however is in order, as the inferred quantities – in particular the magnetic field intensity – refer to the emitting region. It is thus not possible to exclude the presence of a stronger field component whose associated Poynting flux is energetically dominant.

4.2 BL Lac objects

Typically for BL Lacs. This follows the fact that the –ray luminosity in the latter objects is of the same order (or even larger222Examples are 1426+428 (Aharonian et al. 2002; Aharonian et al. 2003) and 1101–232 (Aharonian et al. 2006a) once the absorption of TeV photons by the IR cosmic background is accounted for.) than the synchrotron one and for almost all sources the relevant radiation mechanism is SSC, without a significant contribution from external radiation. If the self–Compton process occurred in the Thomson regime then , but often the synchrotron seed photons for the SSC process have high enough energies (UV/X–rays) that the scattering process is in the Klein–Nishina regime: this implies even for comparable Compton and synchrotron luminosities. This result is rather robust indicating that also in BL Lacs the inferred Poynting luminosity cannot account for the radiated power on the scales where most of it is produced.

Since , relativistic leptons cannot be the primary energy carriers as they have to be accelerated in the radiating zone – since they would otherwise efficiently cool in the more compact inner jet region – at the expenses of another form of energy.

As before, two the possibilities for the energy reservoir: a cold leptonic component or hadrons.

The required cold e density is again 10 times that in the relativistic population. Compared to FSRQs, BL Lacs have smaller jet powers and external photon densities. Cold e could actually survive annihilation and not suffer significantly of Compton drag, if the accretion disk is radiatively inefficient. For the same reason, these cold pairs would not produce much bulk Compton radiation (expected in the X–ray band or even at higher energies if the accretion disk luminosity peaks in the X–rays).

Still the issue of producing these cold pairs in the first place constitutes a problem. Electron–photon processes are not efficient in rarefied plasmas, while photon–photon interactions require a large compactness at MeV energies, where the SED of BL Lacs appears to have a minimum (although observations in this band do not have high sensitivity).

Alternatively, also in BL Lacs the bulk energy of hadrons might constitute the energy reservoir. Even so, one proton per relativistic lepton provides sometimes barely enough power, since the average random Lorentz factor of emitting leptons in TeV sources is close to (see Fig. 4).

This implies either that only a fraction of leptons are accelerated to relativistic energies (corresponding to larger than what estimated above), or that TeV sources radiatively dissipate most of the jet power. If so, their jets have to decelerate. Such option receives support from VLBI observations showing, in TeV BL Lacs, sub–luminal proper motion (e.g. Edwards & Piner 2002; Piner & Edwards 2004). And indeed models accounting for the deceleration via radiative dissipation have been proposed, by e.g. Georganopoulos & Kazanas (2003) and Ghisellini, Tavecchio & Chiaberge (2005). The latter authors postulate a spine/layer jet structure that can lead, by the Compton rocket effect, to effective deceleration even assuming the presence of a proton per relativistic lepton. While these models are more complex than what assumed here it should be stressed that the physical parameters inferred in their frameworks do not alter the scenario illustrated here (in these models the derived magnetic field can be larger, but the corresponding Poynting flux does not dominate the energetics).

The simplest option is thus that also for low luminosity blazars the jet power is dominated by the contribution due to the bulk motion of protons, with the possibility that in these sources a significant fraction of it is efficiently transferred to leptons and radiated away.

Figure 6: Top panel: The blazar sequence in the plane (). The dashed lines corresponding to and are not formal fits, but guides to the eye. Bottom panel: The blazar sequence in the plane , where is the sum of the proton, lepton and magnetic field powers. Again, the dashed line is not a formal fit. Symbols as in Fig. 4.

4.3 The blazar sequence

The dependence of the radiative regime on the source power can be highlighted by directly considering the random Lorentz factor of leptons responsible for both peaks of the emission (synchrotron and inverse Compton components) as a function of the comoving energy density (top panel of Fig. 6). corresponds to the fraction of the total radiation energy density available for Compton scattering in the Thomson regime. In powerful blazars this coincides with the energy density of synchrotron and broad line photons, while in TeV BL Lacs it is a fraction of the synchrotron radiation.

The figure illustrates one of the key features of the blazar sequence, offering an explanation of the phenomenological trend between the observed bolometric luminosity and the SED of blazars, as presented in Fossati et al. (1998) and discussed in G98 and G02. The inclusion here of TeV BL Lacs confirms and extends the relation towards high (low ). The sequence appears to comprise two branches: the high branch can be described as , while below the relation seems more scattered, with objects still following the above trend and others following a flatter one, .

The steep branch can be interpreted in terms of radiative cooling: when , the particle distribution presents two breaks: below , between and (which is the slope of the injected distribution ), and above . Consequently, for , the resulting synchrotron and inverse Compton spectral peaks are radiated by leptons with given by:


thus accounting for the steeper correlation. The scatter around the correlation is due to different values of and to sources requiring , for which (see Table 1).

When , instead, all of the injected leptons cool in the time . If , coincides with , while it is still equal to when . This explains why part of the sources still follow the relation also for small values of .

The physical interpretation of the branch is instead more complex, since in this case , which is a free parameter of the model. As discussed in G02, one possibility is that corresponds to a pre–injection phase (as envisaged for internal shocks in Gamma–Ray Bursts). During such phase leptons would be heated up to energies at which heating and radiative cooling balance. If the acceleration mechanism is independent of and , the equilibrium is reached at Lorentz factors , giving raise to the flatter branch.

The trend of a stronger radiative cooling reducing the value of in more powerful jets is confirmed by considering the direct dependence of on the total jet power . This is reported in the bottom panel of Fig. 6. The correlation approximately follows the trend and has a scatter comparable to that of the relation.

4.4 The outflowing mass rate

The inferred jet powers and the above considerations supporting the dominant role of allow to estimate a mass outflow rate, , corresponding to flaring states of the sources, from


A key physical parameter is given by the ratio between and the mass accretion rate, , that can be derived by the accretion disk luminosity: , where is the radiative efficiency:


Rawlings & Saunders (1991) argued that the average jet power required to energise radio lobes is of the same order of the accretion disk luminosity as estimated from the narrow lines emitted following photoionization (see also Celotti, Padovani, & Ghisellini 1997 who considered broad lines to infer the disc emission). Here jet powers in general larger than the accretion disk luminosity have been instead inferred: for powerful blazars with broad emission lines the estimated ratio is of order 10–100 (see Table 2). As in these systems typically and for accretion efficiencies , inflow and outflow mass rates appear to be comparable during flares.

A challenge for the –ray satellite GLAST will be to reveal whether low–quiescent states of activity correspond to episodes of lower radiative efficiency or reduced and in the latter case to distinguish if a lower is predominantly determined by a lower or .

4.5 Summary of results

  • The estimated jet powers often exceed the power radiated by accretion, which can be derived directly for the most powerful sources, whose synchrotron spectrum peaks in the far IR, and via the luminosity of the broad emission lines in less powerful FSRQs (see e.g. Celotti, Padovani & Ghisellini 1997; Maraschi & Tavecchio 2003).

  • For powerful blazars (i.e. FSRQs) the radiated luminosity is in some cases larger than the power carried in the relativistic leptons responsible for the emission.

  • Also the values of the Poynting flux are statistically lower than the radiated power. This directly follows from the dominance of the Compton over the synchrotron emission.

  • If there is a proton for each emitting electron, the kinetic power associated to the bulk motion in FSRQs is a factor 10–50 larger than the radiated one, i.e. corresponding to efficiencies of 2–10 per cent. This is consistent with a significant fraction being able to energise radio lobes. The proton component has to be energetically dominant (only a few electron–positron pairs per proton are allowed) unless the magnetic field present in the emitting region is only a fraction of the Poynting flux associated to jets.

  • For low power BL Lacs the power in relativistic leptons is comparable to the emitted one. Nevertheless, an additional reservoir of energy is needed to accelerate them to high energies. This cannot be the Poynting flux, that again appears to be insufficient.

  • The contribution from kinetic energy of protons is an obvious candidate, but since the average random Lorentz factors of leptons can be as high as in TeV sources, one proton per emitting electrons yields .

  • This suggests that either only a fraction of leptons are accelerated to relativistic energies or that jets dissipate most of their bulk power into radiation. In the latter case they should decelerate.

  • The jet power (inversely) correlates with the energy of the leptons emitting at the peak frequencies of the blazar SEDs. This indicates that radiative cooling is most effective in more powerful jets.

  • The need for a dynamically dominant proton component in blazars allows to estimate the mass outflow rate . This reaches, during flares, values comparable to the mass accretion rate.

5 Discussion

The first important result emerging from this work is that the power of extragalactic jets is large in comparison to that emitted via accretion. This result is rather robust, since the uncertainties related to the particular model adopted are not crucial: the finding follows from a comparison with the emitted luminosity, which is a rather model–independent quantity, relying only on the estimate of the bulk Lorentz factor. The findings about the kinetic and Poynting powers instead depend on the specific modelling of the blazar SEDs as synchrotron and Inverse Compton emission from a one–zone homogeneous region. Hadronic models may yield different results. Furthermore, the estimated power associated to the proton bulk motion relies also on the amount of ‘cold’ (non emitting) electron–positron pairs in the jet. We have argued that if pairs had to be dynamically relevant their density at the jet base would make annihilation unavoidable. However the presence of a few pairs per proton cannot be excluded. If there were no electron–positron pairs, the inferred jet powers are 10–100 times larger than the disk accretion luminosity, in agreement with earlier claims based on individual sources or smaller blazar samples (Ghisellini 1999; Celotti 2001; Maraschi & Tavecchio 2003; Sambruna et al. 2006). Such large powers are needed in order to energise the emitting leptons at the (–ray) jet scale and the radio–lobes hundreds of kpc away.

The finding that blazar jets are not magnetically dominated is also quite robust, but only in the context of the (widely accepted) framework of the synchrotron–inverse Compton emission model. In this scenario the dominance of the high energy (inverse Compton) component with respect to the synchrotron one limits the magnetic field. This is at odd with magnetically driven jet acceleration, though this appears to be the most viable possibility. In blazars thermally driven acceleration, as invoked in Gamma–Ray Bursts, does not appear to be possible. In Gamma-Ray Bursts the initial fireball is highly opaque to electron scattering and this allows the conversion of the trapped radiation energy into bulk motion (see e.g. Meszaros 2006 for a recent review). In blazars the scattering optical depths at the base of the jet are around unity at most, and even invoking the presence of electron–positron pairs to increase the opacity is limited by the fact that they quickly annihilate. Thus, if magnetic fields play a crucial role our results would require that magnetic acceleration must be rapid, since at the scale of a few hundreds Schwarzschild radii, where most of radiation is produced, the Poynting flux is no longer energetically dominant (confirming the results by Sikora et al. 2005). However models of magnetically accelerated flows indicate that the process is actually relatively slow (e.g. Li, Chiueh & Begelman 1992, Begelman & Li 1994). Apparently the only possibility is that the jet structure is more complex than what assumed and a possibly large scale, stronger field does not pervade the dissipation region, as also postulated in pure electromagnetic scenarios (see e.g. Blandford 2002, Lyutikov & Blandford 2003).

The third relevant results refers the difference between FSRQs and BL Lacs. This concerns not only their jet powers but also the relative role of protons in their jets. BL Lacs would be more dissipative and therefore their jets should decelerate. This inference depends on assuming one proton per emitting lepton also in these sources, and this is rather uncertain (i.e. there could be more than one proton per relativistic, emitting electron). If true, it can provide an explanation to why VLBI knots of low power BL Lacs are moving sub-luminally and in turn account for the different radio morphology of FR I and FR II radio–galaxies, since low power BL Lacs are associated to FR I sources.


We thank the referee, Marek Sikora, for his very constructive comments and Fabrizio Tavecchio for discussions. The Italian MIUR is acknowledged for financial support (AC).


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(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14)
0202149 0.405 5 5.0e-2 17 5.0 0.8 100 1.8e3 210 3.2 4.e-2 250 210
0208512 1.003 8 3.0e-2 15 2.6 2.5 900 4.0e4 900 4.0 2 240 32
0234285 1.213 20 2.5e-2 16 3.0 4.0 100 3.0e3 100 3.78 5 220 4.3
0336019 0.852 20 1.0e-1 16 3.0 1.0 200 4.0e3 200 3.7 7 400 10.7
0420014 0.915 20 3.0e-2 16 3.0 2.8 500 6.0e3 500 3.5 1.5 240 15.8
0440003 0.844 20 1.8e-2 16 3.3 2.8 800 1.0e4 800 3.5 1 280 28.1
0446112 1.207 15 8.0e-2 16 3.0 0.45 800 1.0e4 800 3.7 1.5 250 26.2
0454463 0.858 15 1.5e-2 16 3.5 1.6 800 1.0e4 800 3.7 1 270 41.5
0521365 0.055 8 1.0e-2 15 9.0 2.2 1.2e3 1.5e4 1.2e3 3.2 2.e-2 200 161
0528134 2.07 30 7.5e-1 16 3.5 9.0 200 1.0e4 200 3.5 40 370 1
0804499 1.433 20 7.0e-2 16 3.5 5.0 270 3.0e3 270 4.1 20 340 2.6
0805077 1.837 15 8.0e-2 15 3.0 3.2 300 3.0e3 300 3.4 27 400 4.1
0827234 2.05 15 6.0e-2 15 3.0 7.0 300 3.0e3 300 3.4 16 400 5.6
0836710 2.172 18 0.4 14 2.6 3.4 35 6.0e3 35 3.7 20 500 6.6
0906693 5.47 15 0.4 18 2.5 0.7 800 6.0e3 800 3.7 50 700 4.9
0917449 2.18 10 5.0e-2 15 3.0 6.0 350 3.0e3 350 3.1 9 400 12.6
0954556 0.901 20 5.0e-3 15 3.0 1.1 2.0e3 8.0e5 2.0e3 3.7 0.5 300 90.8
1127145 1.187 25 6.0e-2 18 2.5 3.3 70 2.0e3 70 3.4 12 420 4.2
1156295 0.729 24 3.0e-2 15 2.7 5.0 400 6.0e3 400 3.4 10 400 6.0
1222216 0.435 20 6.0e-3 15 4.0 2.2 200 6.0e3 200 3.9 1 300 39.7
1226023 0.158 6 6.0e-2 12 5.0 7.5 50 6.0e3 50 4.2 25 600 20.4
1229021 1.045 10 4.0e-2 15 4.0 4.5 200 6.0e3 200 4.4 8 500 21.3
1253055 0.538 22 5.0e-2 15 3.5 2.2 250 2.0e3 250 3.2 3.5 400 19.4
1313333 1.210 20 2.5e-2 15 3.5 1.3 200 3.0e3 775 3.0 1 300 43.5
1334127 0.539 15 5.5e-3 12 4.0 3.0 300 4.0e3 300 3.9 2 350 46.4
1406076 1.494 17 8.0e-2 15 3.3 0.54 700 6.0e3 2.5e3 3.0 0.7 300 73.4
1424418 1.522 18 8.0e-2 16 3.3 2.8 400 4.0e3 400 3.8 20 500 6.3
1510089 0.361 8 2.0e-3 16 2.7 3.5 10 2.0e3 62.4 3.7 1.3 310 62.4
1606106 1.226 15 3.0e-2 16 2.7 1.0 200 2.0e3 200 3.7 10 500 15.7
1611343 1.404 15 2.8e-2 16 2.7 2.2 200 2.0e3 200 3.3 10 500 14.9
1622253 0.786 15 1.9e-2 16 4.0 1.0 250 3.0e3 250 3.4 0.7 300 72.8
1622297 0.815 13 7.0e-1 16 4.0 1.1 350 2.5e3 350 3.1 0.7 300 37.2
1633382 1.814 20 1.5e-1 17 2.6 1.2 200 7.0e3 200 3.2 12 500 8.6
1730130 0.902 20 1.6e-2 16 3.0 2.0 200 4.0e3 200 3.4 4 600 35.5
1739522 1.375 15 4.0e-2 16 3.0 1.4 200 5.0e3 200 3.1 6 400 16.4
1741038 1.054 15 3.5e-2 16 3.0 2.2 200 5.0e3 200 4.6 8 450 15.0
1830211 2.507 20 6.5e-2 15 3.0 1.3 140 4.0e3 140 4.1 7 320 7.7
1933400 0.965 15 1.4e-2 16 3.7 3.5 300 3.0e3 300 3.6 3 400 25.2
2052474 1.489 20 8.0e-2 16 3.7 2.0 300 3.0e3 300 3.6 6 400 11.9
2230114 1.037 20 5.0e-2 17 3.0 5.5 80 1.0e4 80 4.0 10 400 5.6
2251158 0.859 30 7.0e-2 16 3.5 6.5 60 4.0e4 60 3.4 30 340 1.1
2255282 0.926 10 2.0e-2 16 2.8 1.6 1000 2.5e3 1000 3.7 2 400 62.5
05253343 4.41 26 8.0e-2 17 2.8 1.5 80 2.0e3 80 3.7 130 1100 2.9
14284217 4.72 20 1.5e-1 16 3.2 4.0 23 2.0e3 23 3.5 70 700 2.9
15085714 4.3 20 1.3e-1 14 3.5 5.0 80 4.0e3 80 3.7 150 1100 4.4
Table 1: The input parameters of the model for FSRQs. (1) Source name; (2) redshift; (3) radius of emitting region in units of cm; (4) intrinsic injected power in units of erg s; (5) bulk Lorentz factor; (6) viewing angle; (7) magnetic field intensity (in Gauss); (8) minimum random Lorentz factor of the injected particles; (9) maximum random Lorentz factor of the injected particles; (10) ; (11) spectral slope of particles above the cooling break; (12) disk luminosity in units of erg s; (13) radius of the BLR in units of cm. (14) random Lorentz factor of the electrons cooling in .
Source Class
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15)
0033595 0.086 5 1.5e-5 20 1.8 0.2 7.0e4 1.0e6 1.0e5 3.1 1.0e5 HBL
0120340 0.272 4 3.6e-5 24 1.5 0.35 1.0e4 2.8e5 1.1e5 3.0 4.4e5 HBL
0219428 0.444 6 3.0e-3 16 3.0 3.8 4.0e3 6.0e4 4.0e3 3.6 147 LBL
0235164 0.940 25 5.0e-2 15 3.0 3.0 600 2.5e4 600 3.2 3 400 17.6 LBL
0537441 0.896 20 1.7e-2 15 3.0 5.0 300 5.0e3 300 3.4 5 400 12.3 LBL
0548322 0.069 10 1.0e-5 17 2.4 0.1 2.0e3 1.0e6 1.9e5 3.3 1.9e5 HBL
0716714 0.3 8 1.3e-3 17 2.6 2.7 1.5e3 2.5e4 1.5e3 3.4 264 LBL
0735178 0.424 8 2.0e-3 15 2.6 1.6 1.0e3 9.0e3 1.0e3 3.2 468 LBL
0851202 0.306 8 1.5e-3 15 2.6 1.6 1.0e3 9.0e3 1.0e3 3.2 521 LBL
0954658 0.368 15 2.0e-3 13 3.5 1.0 1.2e3 5.0e3 1.2e3 3.5 0.08 300 484 LBL
1114203 0.139 10 1.5e-4 17 2.5 0.5 1.5e4 3.0e5 1.5e4 4.5 5.0e3 HBL
1219285 0.102 6 4.0e-4 15 3.3 0.9 1.5e3 6.0e4 1.9e3 3.8 1.9e3 LBL
1604159 0.357 15 3.7e-3 15 3.8 0.7 800 5.0e4 800 3.6 0.2 200 134 LBL
2032107 0.601 10 1.0e-2 16 3.6 0.7 3.0e3 1.0e5 3.0e3 4.3 576 LBL
1011496 0.212 6 1.2e-3 20 1.7 0.3 1.0e4 4.0e5 1.2e4 4.2 1.2e4 TeV
1101232 0.186 6 2.0e-4 20 1.7 0.15 4.0e4 1.5e6 4.7e5 3.0 1.4e5 TeV
1101384 0.031 6 4.0e-5 18 2.0 0.09 1.0e3 4.0e5 2.2e5 3.2 2.2e5 TeV
1133704 0.046 6 3.5e-5 17 3.5 0.23 4.0e3 8.0e5 2.9e4 3.9 2.9e4 TeV
1218304 0.182 6 2.0e-4 20 2.7 0.6 4.0e4 7.0e5 4.0e4 4.0 6.3e3 TeV
1426428 0.129 5 2.0e-4 20 2.2 0.13 1.0e4 5.0e6 4.8e4 3.3 4.8e4 TeV
1553113 0.36 4 1.6e-3 20 1.8 1.1 6.0e3 4.0e5 6.0e3 4.0 920 TeV
1652398 0.0336 7 1.2e-3 14 3.0 0.2 9.0e5 4.0e6 9.0e5 3.2 6.2e4 TeV
1959650 0.048 6 2.9e-5 18 2.5 0.75 3.0e4 3.0e5 3.0e4 3.1 6.1e3 TeV
2005489 0.071 9 1.1e-4 18 2.6 2.4 3.0e3 8.0e5 3.0e3 3.3 427 TeV
2155304 0.116 5 9.0e-4 20 1.7 0.27 1.5e4 2.0e5 1.5e4 3.5 5.9e3 TeV
2200420 0.069 5 8.0e-4 14 3.3 0.7 1.8e3 1.0e6 1.8e3 3.9 2.5e-2 200 1.5e3 TeV
2344512 0.044 5 4.0e-5 16 4.0 0.4 3.0e3 9.0e5 1.7e4 3.1 1.7e4 TeV
2356309 0.165 8 2.5e-4 18 2.6 0.17 9.0e4 3.0e6 9.0e4 3.1 7.4e4 TeV
Table 1: (continue) – The input parameters of our model for BL Lac objects. Columns 1–14 as in the first part of the Table. Column (15): LBL=Low energy peak BL Lacs, HBL=High energy peak BL Lac, TeV=BL Lacs detected in the TeV band (all are also HBLs).
(1) (2) (3) (4) (5) (6) (7)
0202149 3.96 8.5e-2 1.7e-2 4.66 191.5 44.6
0208512 6.63 0.45 0.337 0.61 31.92 34.9
0234285 6.49 0.23 6.132 0.58 133.4 8.0
0336019 26.2 0.16 0.383 2.76 355.2 14.3
0420014 7.71 0.78 3.00 0.52 44.5 21.4
0440003 4.29 0.87 3.00 0.34 19.2 32.5
0446112 19.6 6.5e-2 4.4e-2 1.56 92.9 30.8
0454463 3.69 0.26 0.55 0.42 19.4 40.2
0521365 3.32 0.63 0.26 0.41 7.32 102
0528134 188.3 16.1 69.8 2.04 612 6.1
0804499 18.6 0.83 9.58 0.55 130.6 7.7
0805077 18.5 0.44 1.94 0.58 108.5 9.9
0827243 13.9 2.22 9.28 0.58 93.3 11.4
0836710 61.3 0.96 2.75 16.0 3940 7.5
0906693 129.1 0.19 0.13 2.50 373 12.3
0917449 11.3 2.03 3.03 0.72 72.1 18.3
0954556 0.85 0.10 0.41 9.64e-2 2.27 77.9
1127145 19.7 0.55 8.26 1.81 440.5 7.5
1156295 6.70 1.00 12.12 0.22 32.7 12.4
1222216 1.38 0.18 1.63 0.44 29.7 27.3
1226023 3.39 0.28 1.09 2.43 353.0 12.6
1229021 7.84 0.94 1.70 1.90 179.0 19.4
1253055 11.25 0.84 1.97 1.43 123.8 21.2
1313333 5.63 0.30 0.57 1.19 67.6 32.2
1334127 0.81 0.19 1.09 0.21 6.18 62.6
1406076 17.4 0.27 7.1e-2 2.60 82.5 58.0
1424418 20.7 0.68 2.43 0.88 130.2 12.4
1510089 0.45 4.6e-2 0.75 1.34 335.1 7.3
1606106 7.84 5.3e-2 0.22 1.17 124.9 17.3
1611343 7.19 0.26 1.04 0.88 92.4 17.4
1622253 4.74 0.18 0.21 1.66 73.1 41.6
1622297 53.9 1.16 0.20 9.02 502.4 33.0
1633382 42.2 0.38 0.62 2.60 355.5 13.4
1730130 4.18 0.42 1.53 0.97 65.5 27.2
1739522 10.1 0.18 0.42 1.00 96.0 19.0
1741038 9.17 0.26 1.04 169 191.8 16.2
1830211 15.4 8.8e-2 0.57 1.90 317.8 11.0
1933400 3.68 0.64 2.64 0.58 43.2 24.6
2052474 21.0 0.69 1.53 1.76 196.1 16.5
2230114 13.7 0.98 13.1 2.11 459.5 8.4
2251158 17.1 0.76 36.43 0.50 186.2 5.0
2255282 5.15 0.40 0.25 0.84 29.7 52.0
05253343 25.2 8.5e-2 1.65 1.79 504.4 6.5
14284217 41.9 0.50 6.13 6.71 2464 5.0
15085714 25.5 1.22 7.33 2.64 627.6 7.7
Table 2: Kinetic powers and Poynting fluxes (all in units of erg s) — (1) Source name; (2) Total (synchrotron + IC) radiative power ; (3) Synchrotron radiative power ; (4) Poynting flux ; (5) Kinetic power in emitting electrons ; (6) Kinetic power in protons , assuming one proton per electron; (7) Average random electron Lorentz factor
(1) (2) (3) (4) (5) (6) (7)
0033595 2.67e-3 2.45e-3 1.50e-3 2.22e-3 3.11e-4 1.3e4
0120340 1.15e-2 5.94e-3 2.16e-3 1.48e-2 8.22e-3 3299
0219428 0.78 0.42 0.50 5.99e-2 0.90 122
0235164 9.70 1.89 4.73 0.49 37.0 24.3
0537441 3.84 0.95 8.41 0.29 21.5 17.0
0548322 1.72e-3 1.36e-3 1.08e-3 8.64e-3 1.81e-2 877.3
0716714 0.38 0.26 0.50 8.87e-2 1.16 140
0735178 0.46 0.19 0.14 0.21 2.29 172
0851202 0.35 0.16 0.14 0.17 1.74 182
0954658 0.34 0.11 0.14 0.19 1.99 175
1114203 4.4e-2 2.42e-2 2.70e-2 2.45e-2 3.32e-2 1355
1219285 9.5e-2 3.76e-2 2.45e-2 0.10 0.56 325
1604159 0.75 3.59e-2 9.28e-2 0.20 4.62 79
2032107 2.74 0.33 4.69e-2 0.95 7.07 247
1011496 4.86e-2 1.34e-2 4.85e-3 5.90e-2 6.80e-2 1595
1101232 1.04e-2 9.13e-3 1.21e-3 7.58e-3 1.37e-4 1.0e5
1101384 5.51e-3 2.05e-3 3.54e-4 3.17e-2 0.10 576
1133704 9.55e-3 3.75e-3 2.06e-3 3.39e-2 6.80e-2 917
1218304 5.64e-2 3.19e-2 1.94e-2 1.50e-2 1.26e-2 2189
1426428 3.13e-2 7.10e-3 6.33e-4 4.77e-2 3.17e-2 2760
1553113 0.662 0.13 2.90e-2 0.175 0.793 404
1652398 2.50e-2 1.84e-2 1.43e-3 3.21e-3 2.61e-4 2.2e4
1959650 8.31e-3 7.58e-3 2.46e-2 1.95e-3 1.63e-3 2190
2005489 3.70e-2 3.54e-2 0.57 5.20e-3 4.17e-2 229
2155304 0.313 3.10e-2 2.73e-3 0.147 0.166 1627
2200420 0.153 2.64e-2 8.90e-3 0.136 0.752 332
2344514 7.33e-3 4.87e-3 3.83e-3 7.47e-3 1.20e-2 1141
2356309 1.61e-2 1.30e-2 2.24e-3 8.22e-3 1.15e-3 1.3e4
Table 2: (continue) — (1) Source name; (2) Total (synchrotron + IC) radiative power ; (3) Synchrotron radiative power ; (4) Poynting flux ; (5) Kinetic power in emitting electrons ; (6) Kinetic power in protons , assuming one proton per electron; (7) Average random electron Lorentz factor

Appendix A Appendix

We report here (figures and tables) the SEDs of all blazars in the sample (Figures 7–13), together with the results of the modelling (Tables 1 and 2).

Figure 7: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 8: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 9: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 10: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 11: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 12: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
Figure 13: SEDs of the blazars in our sample. The lines are the result of our modelling, with the parameters listed in Tab. 1.
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