(Adafs/Riafs) in Llagns

Probing the Central Engine of Low-luminosity AGNs

with T. Storchi-Bergmann, M. Eracleous, F. Yuan, R. Mason, C. Ramos- Almeida, A. Alonso- Herrero, Fermi LAT Collaboration

Rodrigo Nemmen NASA Goddard Space Flight Center NASA Postdoctoral Fellow

Dec. 6th 2012 Torus Workshop, San Antonio Most AGNs today have low-luminosities (LLAGNs), very sub-Eddington, majority “LINERs”

Palomar spectroscopic survey ~500 nearby galaxies (Ho+ 97, Nagar+ 05, Ho 08, 09)

40 41 1 L 10 10 erg s h boli⇠ >1000x less luminous than quasars

(Ho 09)

Very sub-Eddington LLAGNs have peculiar SEDs: lack of quasar UV excess (“big blue bump”)

〈LLAGN SED〉based on Ho 99; Eracleous+ 10

Ho 99; Eracleous+10; Nemmen+ 12; Mason+ 12 LLAGNs have peculiar SEDs: lack of quasar UV excess (“big blue bump”)

Ho 99; Eracleous+10; Nemmen+ 12; Mason+ 12 Estimating the radiative efﬁciency of accretion in LLAGNs

= +

Mass-loss Black hole Diffuse gas from evolved gas supply (Bondi accretion) stars 4 1 M˙ 10 0.01 M yr ⇠ L 42 1 Assuming : rad 10% → Lbol & 10 erg s ⌘ Mc˙ 2 ⇠

Implication: ⌘rad 10% ⌧ Ho 08, 09 Low accretion rates: advection-dominated/radiatively inefﬁcient accretion (ADAFs/RIAFs) in LLAGNs

Low accretion Very hot 12 rates Ti ~ 10 (RS/R) K 9 11 Te ~ 10 - 10 K

Low radiative Optically thin efficiency (low densities) Video available at http://youtu.be/ nRGCNaWST5Q

Tchekhovskhoy+ 11

Narayan+98; Yuan 07; Narayan & McClintock 08 Physical scenario for LLAGN central engines

Narayan+ 08; Yuan+ Synchrotron + bremsstrahlung Blackbody

Inverse Compton scattering Internal shock Synchrotron

Synchrotron Putting “ADAF + truncated thin disks” to the test: 21 broadband SEDs of LLAGNs (LINERs) Eracleous+ 10

High spatial resolution: radio (VLA, VLBA), near IR, optical, UV (HST) and X-rays (Chandra)

Criteria for selection of SEDs to be modeled: Black hole mass (M-σ) Good X-ray spectrum

The “best” SEDs NGC 1097, M81, NGC 3998, NGC 266, NGC 1553, NGC 2681, NGC 4143, NGC 4278, M84, NGC 3169, NGC 3226, NGC 3379, M87, NGC 4579, NGC 4594, NGC 4261, NGC 4457, NGC 4494, NGC 4736 NGC 4548, NGC 4552 NGC 1097 12 Nemmen et al.

12 Nemmen et al.

Results NGC 1097

ADAF-dominated ﬁt

Nemmen+ 06

Figure 7. SEDs and coupled accretion-jet models for NGC 0266, NGC 1097 and NGC 1553. The left panel shows the AD models for each object while the right panel displays the JD models. The dashed, dotted and dot-dashed lines correspond to the emission from the ADAF, truncated thin disk and jet, respectively. The solid line when present represents the sum of the emission from all components.

12 Nemmen et al.

Results NGC 1097

Jet-dominated ﬁt

Nemmen+ 12

Chandra Chandra + Spitzer + HST SED of NGC 4594

log(luminosity) log(frequency)

Eracleous+ 10 NGC 4594: ADAF-dominated model

Accretion:

Jet:

Nemmen+ 12 NGC 4594: jet-dominated model

Jet:

Nemmen+ 12 LLAGNs: Some unresolved issues

Is there a truncated thin disk there? (IR)

ADAF or jet responsible for X-rays?

Smoking gun for ADAF? SEDs 22are poorly constrained for most Nemmen et al. LLAGNs

Median LINER SEDs

Data points from Eracleous+ 10 Models from Nemmen+ 12

Figure 20. a, left: The average SEDs (geometric mean) computed separately for the AD and JD models (dashed and dotted lines respectively). The data points correspond to the geometric mean computed by EHF10. b, right: 1 scatter around the average (model and observed) SEDs illustrating the diversity of individual SEDs. The solid line shows the average AD SED and the shaded region corresponds to the standard deviation from the AD models. The points correspond to the mean computed by EHF10 and the error bars show the scatter in the measurements. In the OUV, the ﬁlled circles correspond to measurements without any reddening correction whereas the open circles correspond to the maximal extinction correction.

nomenological one: we have more freedom in the jet ﬁtting compared to the ADAF model. We decided – keeping in mind the caveats men- tioned above – to quantify the deviation of the SED models and data using a simple statistic: the residual sum of squares statistic RSS, deﬁned as

RSS (y y )2 (2) ⌘ obs model i X where y = log ⌫L⌫ and the sum is carried over the observed data points. We sample the X-ray continuum using 3 data points from 0.5 keV to 10 keV and we do not take into account the upper limit data points. Given that in many sources the number of data points is smaller than the number of free parameters in the models, we computed the values of RSS only for the objects in the group A(see 2 of sources which we show in Table 4. Inspecting§ Table 4 we see that for most sources the RSS values of the AD and JD models are Figure 21. The average JD and AD model SEDs compared to quite similar. Based therefore purely on the RSS the average radio-loud and radio-quiet quasar SEDs computed by values, we can conclude that the evidence based Shang et al. (2011). on the broadband SED by itself is not strong enough to systematically favor one model over the from radio to X-rays, in particular the X-ray portion. other for the group of best-sampled LLAGNs. It is be desirable to quantify how well the AD The nature of the X-ray emission in LLAGNs has been and JD models ﬁt the data compared to each debated in the last few years by several authors favoring other in order to assess which one is favored by in some cases the AD or JD models based on the analysis the observations. A rigorous comparison of these of individual sources (e.g., Falcke & Marko↵ 2000; Yuan, scenarios would require estimates of the uncer- Marko↵ & Falcke 2002; Yuan et al. 2002; Yuan, Quataert tainty in the observed SEDs as well as the theo- & Narayan 2003; Wu, Yuan & Cao 2007; Marko↵ et al. retical uncertainties and degeneracies underlying 2008; Miller et al. 2010) or in a statistical sense based the models. Unfortunately, we do not have avail- on the fundamental plane of black hole activity (Mer- able the errors in the SEDs and estimating the loni, Heinz & Di Matteo 2003; Falcke, K¨ording & Marko↵ uncertainty in the models is not straightforward. 2004; Yuan & Cui 2005; Yuan, Yu & Ho 2009; Plotkin For instance, our jet model is basically a phe- et al. 2011). We suggest di↵erent routes to clarify this The Astronomical Journal,144:11(27pp),2012July Mason et al.

The Astronomical Journal,144:11(27pp),2012July New mid IR data:The Mason, Astronomical Journal Asmus,Mason,144:11(27pp),2012July et al. Perlman, + Mason et al.

Mason+12

The Astronomical Journal,144:11(27pp),2012July Mason et al.

Figure 14. SEDs of high-Eddington-ratio LLAGNs (log Lbol/LEdd > 4.6, category III). Symbols and lines as in Figure 13. −

Figure 14. SEDs of high-Eddington-ratio LLAGNs (log Lbol/LEdd > 4.6, category III). Symbols and lines as in Figure 13. Figure 14. SEDs of high-Eddington-ratio LLAGNs (log Lbol/LEdd > 4.6, category III). Symbols and lines as in Figure 13. − galaxies, and their MIIR–NIR/optical spectral slopes are flatter PAH− and [Ne ii]emissioninNGC4278meanthatthepresence than that of the average type 1 Seyfert. We find that the nuclear of the silicate features in this object is ambiguous, and the IR emission is dominated by synchrotron radiation from the 11.3 µmPAHbandinNGC4374couldcontributesignificantly galaxies, and their MIIR–NIR/optical spectral slopes are flatter PAH and [Ne ii]emissioninNGC4278meanthatthepresencegalaxies, and their MIIR–NIR/optical spectral slopes are flatter PAH and [Ne ii]emissioninNGC4278meanthatthepresence jet, consistent with the results for various radio galaxy samples to the measured value of S10 in that nucleus. However, the PAH than that of the average type 1 Seyfert. We find that the nuclear of the silicate features in thisthan(Leipski object that is et of ambiguous, al. the2009 average;vanderWolketal. and type the 1 Seyfert. We2010 find). that the nuclear offeatures the silicate in NGC features 4486 and in NGC this object 4594 are is weak ambiguous, and the and silicate the IR emission is dominated by synchrotron radiation from the 11.3 µmPAHbandinNGC4374couldcontributesignificantlyIRHigh-resolution emission is dominated SEDs can by show synchrotron whether radiation the IR from emission the 11.3emissionµmPAHbandinNGC4374couldcontributesignificantly in NGC 4486 is well known (Perlman et al. 2007; jet, consistent with the results for various radio galaxy samples to the measured value of S10 in thatjet,is energetically nucleus. consistent However, with dominated the the results PAH by for nonthermal various radio processes. galaxy However, samples toBuson the measured et al. 2009 value). Silicate of S10 in dust that features nucleus. are However, an unambiguous the PAH (Leipski et al. 2009;vanderWolketal.2010). features in NGC 4486 and NGC(Leipskiadditional 4594 are et weak information al. 2009 and;vanderWolketal. the issilicate needed to conclusively2010). rule out the featuressign that in dust NGC is 4486 present. and In NGC higher-luminosity 4594 are weak and AGNs, the silicate High-resolution SEDs can show whether the IR emission emission in NGC 4486 is wellpresence knownHigh-resolution (Perlman of a Seyfert-like et SEDs al. 2007 can torus.; show The whether well-known the IR MIR emission/X-ray emission infeatures NGC are 4486 characteristic is well known of type (Perlman 1 objects et al. and2007 are; is energetically dominated by nonthermal processes. However, Buson et al. 2009). Silicate dustisrelation features energetically can are be an used dominated unambiguous to estimate by nonthermal the MIR emission processes. that However, would be Busonan expected et al. 2009 result). of Silicate a direct dust view features of hot are dust an unambiguous in a roughly additional information is needed to conclusively rule out the sign that dust is present. In higher-luminosityadditionalexpected from information the AGNs, torus, is silicate and needed in at least to conclusively one galaxy (NGC rule out 4594) the signface-on that torus dust (Nenkova is present. et In al. higher-luminosity2008). Silicate emission AGNs, silicate is also presence of a Seyfert-like torus. The well-known MIR/X-ray emission features are characteristicpresencethe observed of type of a 1 MIR Seyfert-like objects luminosity and torus. are is The already well-known no more MIR than/ wouldX-ray emissionknown in features a few type are 2 AGNscharacteristic and can of be type reproduced 1 objects by and clumpy are relation can be used to estimate the MIR emission that would be an expected result of a direct viewrelationbe expected of can hot be dust from used in a to a torus, estimate roughly before the MIR accounting emission for that the would likely be antorus expected models result (Mason of et a al. direct2009 view; Nikutta of hot et dust al. 2009 in a; Alonso- roughly expectedFigure 13. fromSEDs the of radio-loud torus, and LLAGNs in at least with one log L galaxybol/LEdd (NGC< 4. 4594)6 (category II).face-on Dot-dashed torus lines (Nenkova show parabolic et al. fits2008 to the). nuclear Silicate radio emission/optical/UV is also data (Section 4.3.2). Other lines and symbols as in Figure 12. − expecteddominant from MIR the synchrotron torus, and component. in at least one This galaxy galaxy (NGC is therefore 4594) face-onHerrero torus et al. (Nenkova2011). This et al.explanation2008). Silicate seems emission unlikely for is also the the observed MIR luminosity is already no more than would known in a few type 2 AGNs andtheprobably can observed be reproduced an example MIR luminosity by of clumpy a genuine, is already “bare” no type more 2 than AGN would with knownradio-loud, in a few low-Eddington-ratio type 2 AGNs and nuclei can be for reproduced two reasons. by clumpy First, be expected from a torus, before accounting for the likely torus models (Mason et al. 2009beno; Nikutta obscuring expected et al. from torus2009 a (also; torus, Alonso- suggested before by accounting the low X-ray for the column, likely torussilicate models emission (Mason is rare et in al. type2009 2; Seyferts Nikutta (e.g., et al. Shi2009 et; al. Alonso-2006), dominant MIR synchrotron component. This galaxy is therefore Herrero et al. 2011). This explanationdominant21 seems MIR2 unlikelysynchrotron for component. the This galaxy is therefore Herrero et al. 2011). This explanation seems unlikely for the Section 5.3 we suggest a scenario that is consistent with the All of the host-dominated, low-Eddington-ratio2 10 cm− ;Gonz galaxiesalez-Mart´ ex-´ın et al. 2009b). The same may be so it would be surprising to encounter it in all three type 2 objects probablymorphological, an example spectral, of and a genuine, broadband “bare” SED type characteristics 2 AGN with of radio-loud,hibit strong low-Eddington-ratio PAH emission in theirprobablytrue nuclei× for central NGC for an two regions. example 4486. reasons. However, Although of a First, genuine, the emission “bare” from type a 2 torus AGN heated with radio-loud,in this sample. low-Eddington-ratio Second, as noted above,nuclei forsome two of reasons. these galaxies First, nothese obscuring LLAGNs. torus (also suggested by the low X-ray column, silicatecommonly emission used to is rare identify in type starburst 2no Seyferts obscuring galaxies, (e.g., torus Shi PAH et (also bands al. 2006 suggested are), by the low X-ray column, silicate emission is rare in type 2 Seyferts (e.g., Shi et al. 2006), 21 2 by the21 weak AGN2 in NGC 4486 would account for only 10% probably do not host a torus. 2 10 cm− ;Gonzalez-Mart´ ´ın et al. 2009b). The same may be so it would be surprising to encounter2 10 it incm all three;Gonz typealez-Mart´ 2 objects´ın et al. 2009b). The same may∼ be so it would be surprising to encounter it in all three type 2 objects × also observed in many other environmentsof× the observed− such luminosity, as the diffuse well within the error of the SED If not arising in a standard, Seyfert-like torus, the silicate true for NGC 4486. However, the emission from a torus heated ininterstellar this sample. medium Second, (ISM) as noted of dustytrue above, elliptical for NGC some galaxies 4486. of these However, (Kaneda galaxies the emission from a torus heated in this sample. Second, as noted above, some of these galaxies 5. DISCUSSION fitting used to investigate the synchrotron component. In terms emission bands could arise in diffuse, optically thin dust by the weak AGN in NGC 4486 would account for only 10% probablyet al. 2008 do). not Three host of a the torus. five LLAGNsbyof the weak IR in emission the AGN host-dominated, in there NGC is 4486 therefore would room account to for “hide” only a torus10% probablyperhaps associated do not host with a torus. the remains of a dissipating torus. We of the observed luminosity, well within the error of the∼ SED If not arising in a standard, Seyfert-like torus, the silicate ∼ We have compiled subarcsecond-resolution, 1–20 µmimag- low-Eddington-ratio category (NGCofin NGC the 4438, observed 4486. NGC Additional luminosity, 4457, evidence, and well within such the as the error minimal of the X-ray SED developIf not this arising line in of reasoninga standard, in Seyfert-like Section 5.3.Alternatively,the torus, the silicate fitting used to investigate the synchrotron component. In terms emission bands could arise in diffuse, optically thin dust ing of 22 LLAGNs, including new IR observations of 20 objects. NGC 5005) are included in thefittingabsorption stellar used population toward to investigate this analysis type the of2 synchrotron nucleus (Di component. Matteo et al. In2003 terms; emissionfeatures may bands be produced could arise in circumstellar in diffuse, dust optically shells. The thin weak, dust of the IR emission there is therefore room to “hide” a torus perhaps associated with the remains of a dissipating torus. We The data have been used to investigate the morphology of the Cid Fernandes et al. (2004)andGonzofPerlman thealez´ IR & Delgado emission Wilson et2005 thereal. (),2004 is is needed therefore). to support room to any “hide” assertion a torus that perhapsextended associated silicate emission with the in remains several of early-type a dissipating galaxies torus. Wehas in NGC 4486. Additional evidence, such as the minimal X-ray develop this line of reasoning8 in9 Section 5.3.Alternatively,the objects and their place on the standard MIR/X-ray plot and to Intermediate-age stars (10 –10 inNGCyr) NGC contribute 4486 4486. is an Additional unobscured30%–60% evidence, of type 2 AGN. such as the minimal X-ray developbeen shown this line to originate of reasoning in mass-losing in Section 5.3 stars.Alternatively,the (Bressan et al. absorption toward this type 2 nucleus (Di Matteo et al. 2003; features may be produced in circumstellar dust shells.∼ The weak, fill in a region of the SED hitherto lacking high-resolution infor- the optical light in these and manyabsorptionThe of IR the spectra toward other of LLAGNs this the type galaxies 2 in nucleus in this (Di category, Matteo 3/ et4ofwhich al. 2003; features2006), and may this be produced process in is circumstellar also likely to dust explain shells. the The silicate weak, Perlman & Wilson 2005), is needed to support any assertion that extended silicate emission in several early-type galaxies7 has mation. In addition, we have presented Spitzer IR spectroscopy those studies, but the contributionPerlmanare of type stars & 2aged Wilson objects,<102005 allyr is), appear is5% needed to show to support silicate any emission. assertion Thethat extendedfeatures in silicate NGC 4486 emission (Buson in et several al. 2009 early-type). galaxies has NGC 4486 is an unobscured type 2 AGN. been shown to originate in mass-losing stars (Bressan∼ et al. of 18/22 objects. or less. The PAH emission in theseNGC objects 4486 is may an unobscured be related to type 2 AGN. been shown to originate in mass-losing stars (Bressan et al. The IR spectra of the galaxies in this category, 3/4ofwhich 2006), and this process is also likely to explain the silicate As a pilot study intending to provide an overview of the IR the intermediate-age stellar population;The IR based spectra on the of analysis the galaxies of in this category, 3/4ofwhich 2006), and this process is also likely to explain the silicate are type 2 objects, all appear to show silicate emission. The features in NGC 4486 (Buson et al. 2009). properties of LLAGNs, the sample is somewhat heterogeneous the band ratios in a small sampleare of type early-type 2 objects, galaxies, all appear Vega to show silicate emission. The 20 features in NGC 4486 (Buson et al. 2009). and may be biased toward objects bright in the MIR. Rather than et al. (2010)concludethatthePAHmoleculesaresuppliedby mass-losing carbon stars formed within the last few Gyr. Further discuss statistical trends within the sample, then, in this section 20 20 we highlight some interesting properties of the galaxies, loosely detailed and quantitative studies of the PAH bands in LLAGNs divided into three groups with certain common elements. wouldbeofvalueindeterminingwhetherthefeaturesarerelated to the known intermediate-age population or whether they reveal active star formation that is difficult to detect in conventional 5.1. I. The Host-dominated, Low-Eddington-ratio Nuclei optical studies. At the low-luminosity end of the sample are nuclei with very 5.2. II. The Radio-loud, Low-Eddington-ratio Nuclei low Eddington ratios (log Lbol/LEdd < 4.6) that are faint compared to the surrounding host galaxy− emission. If a dusty Also at the low-Eddington-ratio, low-luminosity end of the torus is present in these objects, it is very likely too faint to sample, we highlight a set of galaxies with very strong radio contribute significantly to even the high-resolution, PSF-scaling emission. The nuclear SEDs of these objects do not show photometric measurements (Figure 6). the prominent mid-IR peak observed in “conventional” Seyfert

19 New mid IR data: we can begin to test accretion disk vs torus predictions

Plot from work in progress Not for online distribution

with Mason, Ramos-Almeida, Alonso-Herrero, Asensio-Ramos Jets from magnetically arrested BH accretion L81

In any case, we track the amount of mass and internal energy added (plasma β pgas/pmag 100). This configuration is unstable to the in each cell during the course of the simulation and we eliminate magnetorotational≡ instability≥ (MRI, Balbus & Hawley 1991) which this contribution when calculating mass and energy fluxes. drives MHD turbulence and causes gas to accrete. The torus serves Model A0.99f (Table 1) uses a resolution of 288 128 64 as a reservoir of mass and magnetic field for the accretion flow. × × along r-, θ-, and ϕ-, respectively, and a full azimuthal wedge, #ϕ Equation (1) shows that the BZ power is directly proportional to 2π.Thisset-upresultsinacellaspectratiointheequatorialregion,= the square of the magnetic flux at the BH horizon, which is deter- δr : rδθ : rδϕ 2:1:7.Tocheckconvergencewithnumerical mined by the large-scale poloidal magnetic flux supplied to the BH ≈ resolution, at t 14 674rg/c, well after the model reached steady by the accretion flow. The latter depends on the initial field con- state, we dynamically= increased the number of cells in the azimuthal figuration in the torus. Usually, the initial field is chosen to follow direction by a factor of 2. We refer to this higher resolution simu- isodensity contours of the torus, e.g. the magnetic flux function is 2 lation as model A0.99fh and to A0.99f and A0.99fh combined as taken as (1(r, θ) C1ρ (r, θ), where the constant factor C1 is model A0.99fc. We also ran model A0.99 with a smaller azimuthal tuned to achieve the= desired minimum value of β in the torus, e.g. wedge, #ϕ π. We find that the time-averaged jet efficiencies of min β 100. The resulting poloidal magnetic field loop is centred at = = the four A0.99xx models agree to within statistical measurement r rmax and contains a relatively small amount of magnetic flux. If uncertainty (Table 1), indicating that our results are converged with we= wish to have an efficient jet, we need a torus with more magnetic respect to azimuthal resolution and wedge size. flux, so that some of the flux remains outside the BH and leads to a Our fiducial model A0.99fc starts with a rapidly spinning BH MAD state of accretion (Igumenshchev et al. 2003; Narayan et al. (a 0.99) at the centre of an equilibrium hydrodynamic torus 2003). We achieve this in several steps. We consider a magnetic flux = (Chakrabarti 1985; De Villiers & Hawley 2003). The inner edge function, ((r, θ) r5ρ2(r, θ), and normalize the magnitude of the = of the torus is at r 15r and the pressure maximum is at magnetic field at each point independently such that we have β in = g = rmax 34rg (see Fig. 1a). At r rmax the initial torus has an aspect constant everywhere in the torus. Using this field, we take the initial = = θ% θ ϕ% 2π r ratio h/r 0.2 and fluid frame density ρ 1 (in arbitrary units). magnetic flux function as (2(r,θ) C2 = = B dAθ ϕ and ≈ = = θ% 0 ϕ% 0 % % The torus is seeded with a weak large-scale poloidal magnetic field tune C such that min β 100. This gives= a poloidal= field loop 2 = ! !

Where is the high-energy emission coming from?

ADAF

Falcke & Markoff 00, Merloni+ 03, Yuan+ 03, base Falcke+ 04, Wu+ 07, Markoff+ 08, Yuan+ 09, ... of jet

Fermi gamma-ray observations Progress: Radio – X-rays variability e.g., J. Miller+ 10

Figure 1. Shows results from the fiducial GRMHD simulation A0.99fc for a BH with spin parameter a 0.99; see Supporting Information for the movie. The = accreting gas in this simulation settles down to a magnetically arrested state of accretion. (Panels a–d): the top and bottom rows show, respectively, equatorial 2 (z 0) and meridional (y 0) snapshots of the flow, at the indicated times. Colour represents the logarithm of the fluid-frame rest-mass density, log10ρc = = (red shows high and blue low values; see colour bar), filled black circle shows BH horizon, and black lines show field lines in the image plane. (Panel e): time evolution of the rest-mass accretion rate, Mc˙ 2. The fluctuations are due to turbulent accretion and are normal. The long-term trends, which we show with a 2 Gaussian smoothed (with width τ 1500r /c)accretionrate, M˙ τ c ,aresmall(blackdashedline).(Panelf):timeevolutionofthelarge-scalemagneticflux, = g & ' φBH, threading the BH horizon, normalized by M˙ τ . The magnetic flux continues to grow until t 6000r /c. Beyond this time, the flux saturates and the & ' ≈ g accretion is magnetically arrested. (Panels (c) and (d) are during this period). The large amplitude fluctuations are caused by quasi-periodic accumulation and escape of field line bundles in the vicinity of the BH. (Panel g): time evolution of the energy outflow efficiency η (defined in equation (5) and here normalized 2 to M˙ τ c ). Note the large fluctuations in η,whicharewellcorrelatedwithcorrespondingfluctuationsinφBH.Dashedlinesinpanels(f)and(g)indicatetime & ' averaged values, φ2 1/2 and η ,respectively.Theaverageη is clearly greater than 100 per cent, indicating that there is a net energy flow out of the BH. & BH' & '

C ( 2011 The Authors, MNRAS 418, L79–L83 C Monthly Notices of the Royal Astronomical Society ( 2011 RAS Radio/ϒ-rays predicted for LLAGNs: diagnostic for jet/ADAF ϒ-ray dominance

Plot from work in progress Not for online distribution LLAGNs and Fermi LAT

Plot from work in progress Not for online distribution Conclusions

Radio to Υ-ray SEDs

Multiwavelength door is opening to: accretion state and jet physics of LLAGNs tool to constrain feeding/feedback parameters

LLAGNs The road ahead Observations: IR: with Mason, Ramos-Almeida, Alonso-Herrero, Asenso-Ramos

ϒ-rays (Fermi):

with Fermi LAT Collaboration

ALMA:

Theory: Accretion Electron heating in low-density plasmas? Transition between thin disk and ADAF? Outﬂows Efﬁciency of jet/winds production from ADAFs? Signature of winds from LLAGNs? Unifying black hole activity across the mass scale

Radio-loud Gamma-ray AGNs bursts

Nemmen et al. , Dec. 14th issue