Abstract
Active galactic nuclei (AGN) are energetic astrophysical sources powered by accretion onto supermassive black holes in galaxies, and present unique observational signatures that cover the full electromagnetic spectrum over more than twenty orders of magnitude in frequency. The rich phenomenology of AGN has resulted in a large number of different “flavours” in the literature that now comprise a complex and confusing AGN “zoo”. It is increasingly clear that these classifications are only partially related to intrinsic differences between AGN and primarily reflect variations in a relatively small number of astrophysical parameters as well the method by which each class of AGN is selected. Taken together, observations in different electromagnetic bands as well as variations over time provide complementary windows on the physics of different sub-structures in the AGN. In this review, we present an overview of AGN multi-wavelength properties with the aim of painting their “big picture” through observations in each electromagnetic band from radio to \(\gamma \)-rays as well as AGN variability. We address what we can learn from each observational method, the impact of selection effects, the physics behind the emission at each wavelength, and the potential for future studies. To conclude, we use these observations to piece together the basic architecture of AGN, discuss our current understanding of unification models, and highlight some open questions that present opportunities for future observational and theoretical progress.
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Notes
The mm/sub-mm band is missing from this paper because it mostly probes molecular gas that resides in the AGN host galaxy. However, with the high-resolution capabilities of the Atacama Large Millimeter/submillimeter Array (ALMA) we are starting to resolve the innermost parts of AGN down to parsec scales (Sect. 8.4).
The ratio between the observed luminosity and the Eddington luminosity, \(L_{\mathrm{Edd}} = 1.3 \times 10^{46}~(M/10^8~{\mathrm{M}}_{\odot })~\hbox {erg}~\hbox {s}^{-1},\) where \({\mathrm{M}}_{\odot }\) is one solar mass. This is the maximum isotropic luminosity a body can achieve when there is balance between radiation pressure (on the electrons) and gravitational force (on the protons).
Most presentations and posters can be found at http://www.eso.org/sci/meetings/2016/AGN2016.html.
Free-free emission originating in H II regions may substantially contribute to the overall radio spectrum of SFGs. This, however, is expected to occur at rest-frame frequencies higher than \({\sim }20\) GHz (e.g. Fig. 1 in Condon 1992). The contribution of this emission process to the overall radio spectrum is taken to be negligible for galaxies dominated in the radio regime by an AGN.
Any compact component coincident with the central galaxy was not taken into account.
The switch in \(L/L_\mathrm{Edd}\) is not to be taken as sharp but as a transition in a statistical sense. The fundamental physical separation of the various AGN types may be a function of more parameters (such as spin and BH mass) and one should keep in mind that the observational data used to constrain this separation are subject to measurement and computational uncertainties and biases (e.g. the role of environment in kinetic luminosity determinations, contamination of selection proxies by stellar, rather than AGN related processes, etc.; see, e.g. Mingo et al. 2014).
Note that, while it might be safe to assume that anything above \(P_{1.4~\mathrm{{GHz}}} \approx 10^{24}\) W Hz\(^{-1}\) has nothing to do with SF, this is only valid at low redshifts given the strong evolution of SFGs (e.g. Padovani 2016).
Derived for FIRST-SDSS AGN at \(z<0.3\) from the \({\sim }900\) deg\(^2\) LARGESS survey and spectroscopically classified.
Derived for Seyfert galaxies using \(1^{\prime \prime }\) angular resolution radio continuum data; see also Padovani et al. (2015).
The former class has been selected through X-ray, IR, and SED-criteria, while the latter has been identified via \({>}3\sigma \) radio-excess relative to the host galaxies’ IR-based SFRs, and red rest-frame optical colours, and lacking X-ray, IR, and SED-based signatures of AGN activity (Smolčić et al. 2017a; Delvecchio et al. 2017). In this study the SF related contribution to the total radio luminosity was statistically subtracted.
For Spitzer we refer specifically to the four broad bands of the IRAC instrument (Fazio et al. 2004) centred at 3.6, 4.5, 5.8 and 8 \(\upmu \)m (and referred to as [3.6], [4.5], [5.8] and [8.0] respectively), and to the 24 \(\upmu \)m band of the MIPS instrument (Rieke et al. 2004). For WISE we refer to all its four bands, centred at 3.4, 4.6, 12 and 22 \(\upmu \)m, usually referred to as W1–W4.
This is a set of correlations between properties observed in quasar spectra, which comes out of principal component analysis.
NIR spectroscopy can be used as well, but the sample size of objects with appropriate data is relatively small by comparison (but see, Ricci et al. 2017).
In this section we focus on high accretion-rate AGN (with an optically thick and geometrically thin accretion disk; i.e. \(L/L_{\mathrm{Edd}} > 0.01\)), which account for the majority of the BH growth in the Universe (e.g. Ueda et al. 2014; Aird et al. 2015). Low accretion-rate AGN (with an optically thin, geometrically thick, hot accretion flow; i.e. \(L/L_{{\mathrm{Edd}}} < 0.01\)) can also be selected at X-ray energies, although the accretion process is driven by advection of a hot plasma; see Sect. 2.1.4, Done et al. (2007), and Yuan and Narayan (2014) for more details.
With the exception of NGC 1068 and NGC 4945, two Seyfert 2 galaxies in which the \(\gamma \)-ray emission is thought to be related to their starburst component (Ackermann et al. 2012b).
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Acknowledgements
We thank the participants of the AGN Workshop “Active Galactic Nuclei: what’s in a name?” (see full list at http://www.eso.org/sci/meetings/2016/AGN2016/participants.html) for their presentations, Lisa Kewley, John Silverman, and Sylvain Veilleux for their role in the SOC, Phil Hopkins for his summary talk, Chris Harrison for producing Fig. 1, and Sarah Gallagher, Darshan Kakkad, Andrea Merloni, Kevin Schawinski, and an anonymous referee for reading the paper and providing helpful comments. DMA thanks the Science and Technology Facilities Council (STFC) for support through Grant ST/L00075X/1, and James Aird and Bret Lehmer for useful critical feedback. RJA was supported by FONDECYT Grant number 1151408. BDM thanks D. De Cicco for helpful discussions and acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 665778 via the Polish National Science Center Grant Polonez UMO-2016/21/P/ST9/04025. RCH acknowledges support from the National Science Foundation through grants 1515364 and 1554584, and from NASA through Grants NNX16AN48G, NNX15AP24G, and NNX15AU32H. GTR is grateful for the support of NASA-ADAP Grant NNX12AI49G, NSF Grant 1411773, and the Alexander von Humboldt Foundation. VS acknowledges support from the European Union’s Seventh Framework Programme under Grant agreement 337595 (ERC Starting Grant, ’CoSMass’).
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Padovani, P., Alexander, D.M., Assef, R.J. et al. Active galactic nuclei: what’s in a name?. Astron Astrophys Rev 25, 2 (2017). https://doi.org/10.1007/s00159-017-0102-9
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DOI: https://doi.org/10.1007/s00159-017-0102-9