Radio galaxies - the TeV challenge

Over the past decade, our knowledge of the \gamma-ray sky has been revolutionized by ground- and space-based observatories by detecting photons up to several hundreds of tera-electron volt (TeV) energies. A major population of the $\gamma$-ray bright objects are active galactic nuclei (AGN) with their relativistic jets pointed along our line-of-sight. Gamma-ray emission is also detected from nearby mis-aligned AGN such as radio galaxies. While the TeV-detected radio galaxies (TeVRad) only form a small fraction of the \gamma-ray detected AGN, their multi-wavelength study offers a unique opportunity to probe and pinpoint the high-energy emission processes and sites. Even in the absence of substantial Doppler beaming TeVRad are extremely bright objects in the TeV sky (luminosities detected up to 10^{45} erg/s), and exhibit flux variations on timescales shorter than the event-horizon scales (flux doubling timescale less than 5 minutes). Thanks to the recent advancement in the imaging capabilities of high-resolution radio interferometry (millimeter very long baseline interferometry, mm-VLBI), one can probe the scales down to less than 10 gravitational radii in TeVRad, making it possible not only to test jet launching models but also to pinpoint the high-energy emission sites and to unravel the emission mechanisms. This review provides an overview of the high-energy observations of TeVRad with a focus on the emitting sites and radiation processes. Some recent approaches in simulations are also sketched. Observations by the near-future facilities like Cherenkov Telescope Array, short millimeter-VLBI, and high-energy polarimetry instruments will be crucial for discriminating the competing high-energy emission models.


Introduction
An exciting discovery enabled by space-and ground-based high-energy observations is the detection of γ-rays from over 3,000 extragalactic sources. Active galactic nuclei (AGN, powered by accretion onto a few million to several billion solar mass black holes) form a major population of the γ-ray sky. AGN often produce collimated outflows, called relativistic jets (see Fig. 1), whose beams of radiation pierce through the Universe and reach us from the past, offering a unique opportunity to study the Universe when it was an order of magnitude younger than today. Despite the intensive study of AGN, the location and origin of their γ-rays remains a mystery. Some studies imply the emission region is located close to the central black hole [1][2][3][4][5]; while there are counterexamples which argue for γ-rays coming from farther out in the jet [6][7][8]. Extremely bright γ-ray flashes in AGN on time scales of minutes to hours have attracted the attention of the entire astronomical community, as this suggests that the particles that produce γ-rays can be accelerated with enormous efficiency in tiny regions within more extended sources. The question of what powers γ-ray AGN flares is ultimately related to the energy dissipation mechanism at work in their relativistic jets.
AGN jets are among the largest and most efficient particle accelerators in the Universe. However, where and how these particles produce high-energy radiation is still an open question. What are the particle acceleration processes, which type of particles are the primary energy drivers, and what are the high-energy interaction processes are key puzzles in high-energy astrophysics.
AGN having their jets pointed along our line-of-sight, called blazars, are the majority of the sources detected by the high-energy ground-and space-based telescopes. This goes along with the substantial Doppler boosting of their intrinsic emission. The radiation is beamed in our direction making these sources appear to be extremely bright and detectable even at larger redshifts. Blazars come in two flavors: BL Lacertae objects (BL Lacs) and flat spectrum radio quasars (FSRQs). In spite of the dissimilarity of their optical spectra -FSRQs show strong broad emission lines, while BL Lacs have only weak or no emission lines in their optical spectra -they share the same peculiar continuum properties (strong variability and high polarization). Most of the radiation we observe from these blazars is dominated by emission from the jet; however characteristic signatures of emission from the immediate vicinity of the central black hole (accretion disk or corona) have been also observed especially in FSRQs. The radio to optical emission (and X-rays in some cases) from blazars is mostly synchrotron radiation from the jet, produced by relativistic electrons interacting with the jet's magnetic field. High-energy emission, which often dominates the spectral energy distribution (SED), is from inverse-Compton scattering of thermal photons (from the accretion disk, the broad-line region, or the molecular torus) and/or non-thermal photons (synchrotron emission from the jet) by the jet's relativistic electrons in case of leptonic models [1, [9][10][11][12]. Gamma-ray emission could also be produced via photo-hadron interactions or by proton or charged µ/π synchrotron emission and subsequent cascades in the framework of hadronic models [9,12,13]. Detailed investigations of multi-wavelength flux and spectral variability of individual sources including cross-band (radio, optical, X-ray, γ-ray, and polarization), relative timing analysis of outbursts, and/or very long baseline interferometry (VLBI) component ejection/kinematics suggest that high-energy emission especially γ rays are associated with the compact regions of relativistic jets energized by the central SMBHs [e.g., 1,2,6,14-21]. However, many critical details of particle acceleration mechanisms and radiation processes are still unknown.
Mis-aligned or non-blazar AGN such as radio galaxies or Narrow line Seyfert 1 galaxies, although representing a small fraction (<2%) of the γ-ray detected sources, have emerged as an interesting class of γ-ray emitting AGN. Radio galaxies are a particularly interesting class of objects to understand several aspects of AGN physics and high-energy emission, i.e. how the relativistic outflows are launched and driven, what drives the particle acceleration, how and where high-energy emission is produced in jets. Several of these key questions can be addressed via studying the TeV-emitting radio galaxies (T eV Rad hereafter). This review paper summarizes the key observations of T eV Rad, with an overview about the possible particle acceleration processes and emission mechanisms, and concentrates on the jet structure and multi-wavelength variability rather than spectral modeling, which is a separate topic. The interested reader is referred to the review article by Rieger and Levinson [22].

Observations of the TeV emitting radio galaxies
Among the more than 30 radio galaxies observed by the Fermi/Large Area Telescope (LAT) reported in the LAT 8-year Point Source List (FL8Y : https://fermi.gsfc.nasa.gov/ssc/data/access/lat/fl8y/), six have also been detected at TeV energies (see Table 1). Most of these sources are relatively nearby; the closest is Centaurus A at a distance of 3.7 mega-parsec, while PKS 0625-35 1 at 220 mega-parsec distance is the farthest TeV-detected radio galaxy. Except from M87 and PKS 0625-35, with a black hole mass of a few 10 9 M ⊙ , the T eV Rad have black hole masses of the order of a few 10 8 M ⊙ , which is smaller than the average black hole mass of beamed radio galaxies a.k.a. blazars [36]. In fact, the closet T eV Rad, Centaurus A, hosts an even smaller black hole, (M BH ∼5×10 7 M ⊙ ). The radio morphology of these sources resemble blazars when viewed at larger angles. The beaming effects are fairly moderate in T eV Rad [apparent speed less than a few times the speed of light [37][38][39].
The detection of the nearest T eV Rad, Centaurus A core, at TeV energies was first reported by H.E.S.S. using more than 100 hours of observations taken during 2004-2006 [40]. The source has been later detected also at GeV energies by the Fermi/LAT [41]. Fermi/LAT also discovered the spatial extension in the source, detecting γ-rays from both the core and from the extended giant lobes [41]. The combined GeV-TeV spectrum of the source shows a clear excess at TeV energies and cannot be fitted via a single zone emission model [42]. Moreover, the origin of the extended γ-ray emission still remains an open question, although several models were proposed, i.e. inverse-Compton scattering of relic radiation from the cosmic microwave background and the infrared-to-optical extragalactic background light [41].
At a distance of ∼16 Mpc, M87 was the first TeV detected radio galaxy [43]. M87 is the brightest galaxy in the Virgo cluster. The source has been detected on several occasions both in flaring and quiescent states [44][45][46]. The fastest variability timescale observed in the source is ∼1 day [46]. Long-term variability on a few week timescales has also been reported for the source especially during quiescent states [45,47].
The Fermi telescope has detected 3C 84 since the beginning of its operation [48]. Fermi observations suggest that the GeV photon flux of the source has been continuously rising since then (see Section 4 for details). In 2009, the source was also detected at TeV energies [49,50]. In the end of 2016 and early 2017, the source has been through a dramatic flaring activity. During this epoch, the MAGIC telescopes detected the brightest flare ever observed in the source [L γ−ray ∼ 10 45 erg s −1 , 51] with a flux doubling timescale of ∼10 hours.
The radio galaxy IC 310 was first detected at TeV energies in 2009-2010 by the MAGIC telescope [52]. Variations on days to months timescales were observed in the source during this period. In November 12-13, 2012, a dramatic flare was observed in the source. During this exceptional variability phase, the observed flux doubling timescale of the observed TeV flares was as short as 5 minutes. This is the fastest variability timescale observed in a radio galaxy up to now [31]. This extreme flare is quite challenging to be explained within the framework of any existing theoretical mechanism (see Section 6 for details).
At a distance of 95 Mpc, 3C 264 is rather a new member in the family. Nearly 12 hours of VERITAS observations of the source between February 09, 2018 and March 16, 2018 confirms its detection at ∼5σ level [53]. TeV emission above 250 GeV from PKS 0625-35 was first reported in 2012 by H.E.S.S. [54]. Fermi observations of the source report variations on monthly timescales [55]. However, no variation has been seen seen at TeV energies. The source belongs to the category of low excitation line radio-loud AGN [56]. Radio observations find superluminal motion in the jet with apparent speeds up to ∼3 c [57]. The evidence of a one-sided jet and superluminal motion suggests the source to be more like a blazar.

Parent population
All T eV Rad are Fanaroff and Riley type I (FR1) sources. Moreover, most of the TeV-detected blazars (high-frequency peaked BL Lacs, HBL, in TeVcat: http://tevcat.uchicago.edu/) belong to the parent population of FR1 sources. The jetted AGN (also known as radio-loud AGN) are classified as FR1 and FR2 [59] sources on the basis of their jet luminosity at 178 MHz radio frequency. It was found that the sources with luminosity ≥5×10 24 W Hz −1 Sr −1 belong to the FR2 class, while the rest were classified as FR1 type [59]. The key difference between the two populations is their radio morphology. FR2s are more powerful radio galaxies, and their radio morphology is characterized by powerful edge-brightened double lobes with prominent hot spots, while the FR1s are lower-power sources, which exhibit rather diffuse edge-darkened lobes. Moreover, FR2s tend to be found in less dense environments compared to FR1s. When seen at small inclinations, FR1 sources are BL Lacs while FR2s are radio-loud quasars (an excellent discussion about AGN unification can be found in Urry and Padovani [60]).
It was found that at a given radio power, FR1s have fainter nuclear X-ray and ultra-violet (UV) emission [61,62] compared to FR2s, which indicates that FR1s might have fainter accretion disks. For instance, the accretion rate for the brightest T eV Rad 3C 84 (L V HE = 10 45 ergs −1 ) is well below 10% [Eddington ratio ∼3×10 −4 , 63]. The key question to answer is if this corresponds to different accretion modes in the two classes of sources [64]. If yes, it would be interesting to assess how it correlates to their observed TeV luminosity. Moreover FR1s may occupy less dense environments, enabling lower γγ-pair production opacity for the TeV photons. In dense environments, high-energy photons might get absorbed via a process called pair production when they interact with lower-energy (optical/UV) photons by producing electron-positron pairs.

Jet kinematics -speeds on parsec to kilo-parsec scales
The T eV Rad M87 is the best studied radio galaxy because of its extremely bright and spectacular jet extending up to several hundreds of kilo-parsecs. Figure 2 depicts the kilo-parsec scale radio, optical, and X-ray images (from top to bottom) of the M87 jet. The high-resolution VLBI observations show very sub-luminal speeds (∼0.01 c) on tens of parsec scales [38,65,66]. Later there is a sudden increase in the apparent speeds at a distance of ∼100 parsecs just prior to the stationary feature HST-1. Superluminal components with speeds up to 6c are detected after HST-1 (see Fig. 2), which is followed by a smooth deceleration [38,67]. A similar velocity pattern has observed in 3C 264. The sub-luminal apparent speeds (≤ 0.5 c) seemingly receive a kick at a distance of ∼100 parsec where the jet has a stationary knot/feature. On kilo-parsec scales apparent speeds up to 7 c have been observed in the source [39]. How exactly these velocity fields develop and evolve along the jet is still an open issue. The stationary features are Kovalev et al. 2007  thought to be the sites of recollimation shocks, which might have an interesting role in accelerating the sub-luminal motion to super-luminal speeds. There has been no dramatic change noticed in the apparent speed of the moving features in the other T eV Rad as a function of distance from the central engine. For instance, radio VLBI and X-ray observations suggest sub-luminal motion (speeds up to 0.5 c) both in the parsec and kilo-parsec scale jet of Centaurus A [68][69][70]. Similarly the observed speeds on parsec and kilo-parsec scales are sub-luminal (∼0.2 -0.9 c) in 3C 84 [8, [71][72][73], suggesting a viewing angle ≥45 • . The one-sided blazar like jet of IC 310 constrains the a viewing angle to be ≤38 • implying a moderate beaming [74]. VLBI observations measure an apparent speed of ∼0.9-3 c in the PKS 0625-35 jet, which constrains the viewing angle in the source to be ≤13 • (Angioni et al. 2018, submitted).
Structured and stratified velocity patterns have also been observed in the parsec-scale jets of some of the T eV Rad. For instance, a study by Mertens et al. [38] report a stratification in the M87 jet with a bright transverse velocity component. The jet flow in the source has a slow, mildly relativistic layer, sheath, (apparent velocity ∼0.5c) and a fast spine (apparent velocity ∼0.9c). The study also discovered a significant difference in the apparent speeds observed in the northern (0.5 c) and southern (0.2 c) limbs of the jet (the bright limbs in the source can be seen in Fig.  4). Likewise, limb brightening was discovered in the 3C 84 jet using the space-VLBI observations [76]. Hints of differential motion were also observed in Centaurus A [68].

Zooming into the event horizon scales
AGN jets are the most spectacular structures in the Universe and represent the "extreme" and "largest" members of a wide family of jet-powered phenomena, including γ-ray bursts (GRBs), X-ray binaries (XRBs), and young stellar objects (YSOs). Over the past few decades, there has been remarkable progress in our understanding of AGN jet physics especially because of the development of high-resolution VLBI (for more details refer to the recent review on millimeter-VLBI by Boccardi et al. [77]. Millimeter-VLBI observations offer an angular resolution of a few tens of micro-arcseconds, which allows a probe of the inner jet region on scales ≤50 gravitational radii (R g ).
Given its proximity and fairly bright jet at millimeter radio frequencies, M87 is the best studied source using high-resolution VLBI [38,65,75,78,79]. Global millimeter VLBI observations at 86 GHz radio frequency resolve a limb-brightened outflow down to ∼15 R g [75]. A high-resolution image of M87 taken at 86 GHz radio frequency is illustrated in Fig. 4. The Event Horizon Telescope (EHT) observations at 230 GHz and 345 GHz frequencies constrain the size of the event horizon of the central black hole to be less than 10 R g [79,80]. These high-resolution images provided a unique tool to test the different jet-launching models [78,79] Another interesting study is made using the space-VLBI observations. The space-VLBI observations of 3C 84 at 22 GHz radio frequency using the RadioAstron mission probed the inner jet profile up to 100 R g [76]. The study discovered a very broad jet base with a transverse radius larger than about 250 R g implying the jet to be more likely launched from the accretion disk. More interestingly, GMVA observations at 86 GHz radio frequency discovered a double-nuclear structure at the jet base (Oh et al. 2018, in preparation).
High-resolution VLBI observations therefore offer an unparalleled opportunity to probe and pinpoint the high-energy emitting sites in the immediate vicinity of the central black hole. Moreover, high-resolution polarization imaging is a unique technique to unravel the magnetic field topology on scales less than a few hundreds of gravitational radii. The tiny magnetized regions in the extended jets are the potential sites of high-energy emission [19, 81,82].

TeV variability
Like blazars, T eV Rad exhibit variability on multiple timescales i.e. sub-hour to days timescale flares are accompanied by long-term outbursts. For instance, multiple modes of flaring activity can be seen in the photon flux light of 3C 84 observed by the Fermi/LAT. Figure 6 presents the rapid flares superimposed on top of the long-term rising trend in the Fermi photon flux light curve (in blue). In the end of 2016, several extremely bright and rapid flares were observed by Fermi/LAT. The fastest flares seen by Fermi/LAT have flux doubling timescale of 9-12 hrs. In 2016-2017, the source was also detected multiple times at TeV energies by the MAGIC telescope [51]. During the course of this period, MAGIC detected the fastest and most luminous flare from 3C 84. An extremely bright (L γ ≃ 10 45 erg s −1 ) flare with a flux doubling timescale of ∼10 hours was observed on January 01, 2017 [51]. Flux variations on multiple timescales were also observed in IC 310 and M87.
Extremely short variability timescales in T eV Rad have attracted the attention of astrophysicists, as the observed timescales can reach down to the light crossing time of the black hole event horizon, t BH = r g /c, where r g is the gravitational radius of the black hole and c is the speed of light. For instance, the observed variability timescale (t var = 5 min) in IC 310 is much smaller than the event horizon light crossing Variations on sub-horizon scales have also been observed in blazars [84]. However in case of blazars, one can always argue that beaming effects make the observed timescale appear shorter. This requires the Doppler factor to be greater than 50, which has rarely been observed [37,73]. It is also important to note that the timescale of the flux variations in blazars is also affected by time-dilation in the frame co-moving with the jet. Since the Doppler factor, δ ≃ Γ jet (Lorentz factor in the jet), the projection effects (used to explain the ultra-fast variability in blazars) cancel out.
Understanding the physical processes responsible for the origin of the ultra-fast TeV flares is a key challenge in high-energy astrophysics. Sub-horizon scale variations and extremely luminous flares, especially in the absence of strong beaming effects, require (i) emission regions of extremely high electromagnetic energy, (ii) efficient particle acceleration mechanisms which could channel the electromagnetic energy to particle energy, and (iii) less-dense photon environments so that the emitted TeV photons do not get self-absorbed by γγ-pair production.

High-energy emitting sites
Locating the γ-ray emitting sites is a key challenge not only in case of radio galaxies but also for blazars. When the emission region is closer to the central black hole, there is higher proportion of electromagnetic energy available in the jet, making it easy to account for the observed extremely bright γ-ray flashes. However if the high-energy photons are produced too close to the black hole, the chances for them to escape through the rich photon environments are low. Nevertheless, at least some of these high-energy photons seem to survive even through dense environments. Photons produced further down in the jet have higher chances of not being absorbed; however accelerating particles to extreme high-energy is a quite challenge there (see Section 6 for more details).
The sub-horizon scale emitting regions, detected in IC 310, 3C 84, and M87, could either be very close to the black hole or further down in the jet. The TeV flare in IC 310 was interpreted as originating from the magnetospheric gap of the black hole (see Section 6) as it is hard to achieve the high luminosity and rapid variability further down in the jet. The rapid TeV flare in 3C 84 was also proposed to be produced in the magnetospheric gap; however achieving the extremely high luminosity requires an extremely fast rotating black hole and magnetic field higher than its equipartition value [4]. However these studies lack a conclusive observational evidence for the emission to be produced close to the black hole. Multi-frequency observations of M87 during an episode of extremely rapid flares provided an opportunity to study the TeV emitting regions in great detail. Strong TeV flares in the source were accompanied by an increase of the flux from the nucleus observed at 43 GHz radio frequency [5], suggesting the emission region to be located within the radio core (≤50 gravitational radii). The extreme compactness of the TeV emission region and the observed TeV-radio connection in M87 conclusively infer that the VHE emission is indeed produced very close to the black hole [5].
Hints of multiple γ-ray emitting regions have also been observed in T eV Rad. For instance, a study performed using the KVN (Korean VLBI Network) and γ-ray observations indicate the presence of multiple γ-ray emitting regions in 3C 84 [8]. Figure 6 presents a comparison of the flux variations observed at γ-ray and 230 GHz radio frequencies. The long-term rising trend is present in the flux variations seen both at radio and γ-ray frequencies. However the rapid flares do not have a one-to-one correspondence at the two frequencies. A formal cross-correlation analysis indicates two prominent peaks at around −500 and +400 days, which implies that γ-rays variations lead those at radio by −500 days and also lag behind by +400 days (see Fig. 7). A detailed investigation of the flux density variations in the spatially separated emission regions of the jet indicates the presence of multiple γ-ray emitting sites in the source. The study reported that there are two active regions producing γ-rays in the source, one very close to the black hole and another at a distance of ∼4 parsec in the source frame.
Fermi has detected γ-rays both from the core and the extended lobes of the nearest T eV Rad Centaurus A [41]. The source has a spatial extension of About 9 degrees across the sky, which corresponds to ∼600 kilo-parsec, and the γ-ray morphology is quite similar to its radio jet morphology, which implies γ-rays coming from both the central AGN core and extended kilo-parsec scale lobes. Given the detection of extended γ-ray emission at GeV energies and the absence of TeV variability, the extension of TeV emission cannot be discarded. It is important to note that Fermi/LAT has detected extended GeV emission also from Fornax A. It might be interesting to see for how many of these sources spatial extension can detected by using the future Cherenkov Telescope Array.

Particle acceleration mechanisms
The observed extremely rapid variability and enormously high γ-ray luminosity are clearly challenging to achieve in astrophysical jets as they require (i) particle acceleration to extreme high energies in presence of strong radiative loss (ii) variation on sub-horizon timescales, and (iii) conversion of large volumes of electromagnetic energy with enormous efficiency. Several mechanisms have been proposed to address the TeV challenge in astrophysical sources. Some recent ideas are summarized below.
The most common mechanism is relativistic shock i.e. the flow is accelerated to supersonic speeds and strong shocks are formed in the relativistic outflow because of (i) faster moving outflow runs into slower flow resulting in the formation of internal shock, (ii) the outflow encounters an obstacle (perhaps a molecular cloud) on its way, (iii) any other perturbation happening at the base of the jet could also form a shock wave to form and propagate down the jet. Relativistic shocks [85] seem to be effective in low-magnetization regimes and could explain the observed long-term variability from AGN fairly well [1,19,81,82, [86][87][88]. However, the luminous ultra-fast TeV flares observed from a number of AGN [4,31,84,89] are difficult be explained via the relativistic shock model especially in the absence of substantial Doppler beaming, and therefore challenge our understanding of particle acceleration processes.
Magnetic reconnection, a process by which magnetic energy is transferred to particle heat, bulk energy and non-thermal energy, is proposed to be an effective mechanism for energy dissipation [90][91][92][93][94] in magnetically dominated relativistic outflows. During magnetic reconnection, opposite polarity magnetic field lines exchange partners at "X-points" leading to breaking of flux freezing and change in magnetic field topology, which results in an explosive release of energy. For instance, solar flares seem to be powered by magnetic reconnection. However this picture is far too complex in case of relativistic outflows. Nevertheless, there has been great advancement in simulations to understand the relativistic magnetic reconnection. The particle-in-cell (PIC) magnetic reconnection simulations suggest that ultra-relativistic plasmoids generated by magnetic reconnection [91,92] can power the ultra-fast flares observed from TeV AGN. An example γ-ray light curve (top) and snapshot of relativistic magnetic reconnection (bottom) by an integrated modeling relying on first-principle PIC kinetic simulation and an advanced polarized radiation transfer simulation from Zhang et al. [90] are illustrated in Fig. 8. The study reports that plasmoid coalescences in the magnetic reconnection layer can produce highly variable multi-wavelength light curves, and also can explain polarization degree and polarization angle variations. A magnetospheric gap model was invoked to explain the sub-horizon scale flux variations in T eV Rad [4,31,95,96]. It has been proposed that a rotating black hole embedded in a strong magnetic filed (of the order of 10 4 -10 5 G) will induce an electric field, E, corresponding to a voltage drop across its event horizon, which facilitates an efficient electromagnetic extraction of the rotational energy of the black hole (for more details, see the review by Rieger [96]), and could be an efficient mechanism to power the TeV flares in AGN. The maximum extractable energy (L magnetosphere ) from the black hole however depends on the details of the gap configuration. For instance, L magnetosphere scales as the height of the magnetospheric gap (h) i.e. i.e. L magnetosphere ∼ L BZ (h/r g ) β , where L BZ is the maximum power from a fast rotating black hole [97] and β depends on the gap setup. The size of the gap can be constrained by the observed TeV variations (c.δt ≤ r g ), which further reduces the maximum L magnetosphere [details are refereed to 96,98]. Another important aspect of this model is the absorption of the emitted TeV photons by the thermal photon environment of the black hole. In order for the TeV photons to survive through the accretion disk environment, the magnetospheric gap model requires an under-luminous or radiatively inefficient accretion flow to avoid γγ-pair production. This enforces accretion rates to be below 1% of the Eddington scale. Putting this in the context of current observations, the model could explain the observed TeV flares in M87 fairly well; however the minute-scale TeV flare in IC 310 seems less likely to have a magnetospheric gap origin. The observed TeV luminosity in 3C 84 is also hard to match in the framework of the magnetospheric gap model unless the magnetic field threading the accretion disk is a factor of 1000 greater than its equipartition value.
Magnetoluminescence [99,100] has been recently proposed to explain the observed TeV flares from astrophysical sources. The basic idea is that rotating at the center of an AGN leads to writhing of magnetic flux ropes resulting in tangled and knotted magnetic field lines. The tightly wound magnetic flux ropes especially in the inner jet are highly dynamically unstable. The tangled/knotted flux lines when opened up or untangled could produce rapid γ-ray flares. It has been suggested that this phenomenon includes an implosion rather than explosion [100]. As a consequence, particles could be accelerated to significantly higher energies as the dissipating and cooling volume could be re-energized by the medium external to it. Electromagnetic detonation [100] is proposed as an alternative possibility, which might accelerate particles at the transition of high-magnetized outflow into low-magnetized outflow and energy-flux. Particles are subjected to unbalanced electric field at the transition and get accelerated (positive and negative charged particles are accelerated in opposite direction) to produced γ-rays. In comparison to magnetic reconnection which require the magnetic flux to channel into a small volume, electromagnetic detonation will have a larger volume for the conversion of electromagnetic energy into particle energy.

Future directions
Pinpointing the sub-horizon scale γ-ray emitting sites in kilo-parsec to mega-parsec scales AGN jets is a key challenge in high-energy astrophysics. A coordinated multi-wavelength and multi-messenger effort is needed to better understand it. The TeV emitting radio galaxies (T eV Rad) are a particularly interesting class of AGN to unravel the mystery of the origin of γ-ray emission. Some important considerations are: • T eV Rad are nearby AGN. The farthest detected T eV Rad is at a distance of 220 Mpc. Using the millimeter-VLBI observations, one can probe regions in the immediate vicinity of the central black hole i.e. down to a scale of less than 50 gravitational radii in the source frame (for more details about the imaging capabilities of the current and near-future high-resolution VLBI observations, check Boccardi et al. [77]). The mm-VLBI observations will provide an ultimate opportunity to probe the compact regions closer to the black hole, which are the potential sites of high-energy emission. High-resolution polarization imaging will probe the magnetic field strength and configuration of these compact emission regions, which is an essential piece of information in order to understand the high-energy acceleration processes. • Being seen off-axis, T eV Rad offer a unique opportunity to transversely resolve the jet. Using high-resolution VLBI one can transversely resolve the fine scale jet structure and can probe their flux intensity and polarization variations. VLBI astrometry observations could provide the exact location of the core. Having that, one could combine the high-resolution VLBI imaging and multi-wavelength observations to exactly pinpoint the location of γ-ray emitting sites. • There have been great advances in the theory and simulation front. Several details about plasma physics under extreme conditions can be better understood via simulations i.e. radiative signatures of relativistic magnetic reconnection [90][91][92][93][94], formation of jets and expulsion of magnetic flux from the central black hole [101][102][103], high-energy polarization signatures of shocks and reconnection [90,104,105]. A comparison of predictions from simulations with measurements will be crucial to understand the physical processes happening around black holes. • Cherenkov Telescope Array [106] with its sensitivity better than the existing GeV/TeV instruments and spatial resolution of the order of a couple of arc-minutes at TeV energies will provide observations up to 300 TeV. CTA will detect many more misaligned AGN and will also help us in separating nuclear and off-nuclear components especially for nearby sources. Having the potential to probe deeper into the spectral and variability characteristics of AGN, CTA will eventually revolutionize our understanding of the TeV sky. • The question of what powers γ-ray AGN flares is ultimately related to the energy dissipation mechanism at work. High-energy polarization observations will deliver an ultimate test for probing the energetic particle-acceleration processes and emission mechanisms: (i) leptonic versus hadronic models and (ii) shocks versus magnetic reconnection. High-energy polarimetry missions are on their way to unravel how the most efficient particle accelerators in the Universe work. For instance, the All-sky Medium Energy Gamma-ray Observatory (AMEGO: https://asd.gsfc.nasa.gov/amego/) will offer MeV polarization observations of the γ-ray bright AGN. The Imaging X-ray Polarimetry Explorer (IXPE: https://wwwastro.msfc.nasa.gov/ixpe/index.html) will observe polarization signatures from X-ray bright AGN.
• The recent observations of coincidence of a high-energy neutrino event with a flaring AGN, TXS 0506+056, indicates AGN as potential sources of high-energy neutrinos [107]. Multi-wavelength and multi-messenger observations of similar events will test if AGN jets are powerful sources of extra-galactic neutrinos and put constraints on lepto-hadronic models.
Given the flood of high quality data from the current and upcoming missions and great advances in theory/simulation, it is an exciting time for astronomers. There are several major discoveries to be made.