Abstract
In this chapter we aim to address the question: can high-redshift AGN drive galaxy-wide outflows of ionised gas in the absence of extremely powerful radio jets? Most theoretical models of galaxy evolution predict that this must be the case. We investigate eight \(z=1.4\)–3.4 ultra-luminous infrared galaxies (ULIRGs) that host active galactic nuclei (AGN) activity, including known sub-millimetre luminous galaxies (SMGs). The targets have radio luminosities that are typical of high-redshift ULIRGs (\(L_{1.4~\mathrm {GHz}}=10^{24}\)–10\(^{25}\) W Hz\(^{-1}\)) and therefore are not radio-loud AGN and do not host extremely powerful radio jets. We present integral-field spectroscopy observations, covering the [O iii]\(\lambda \lambda 4959{,}5007\) emission-line doublet. We de-couple kinematic components due to the galaxy dynamics and mergers from those due to outflows. The four systems with the most powerful AGN host the signatures of large-scale energetic outflows, that is, extremely broad [O iii] emission-line profiles (FWHM \({\approx }\) 700–1400 km s\(^{-1}\)) across \(\approx \) 4–15 kpc (i.e., across the extent of the host galaxies). The four less powerful AGN display weaker evidence for spatially extended outflows; however, this may be due, in-part, to the lower quality data for these objects. We estimate that the outflows are depositing energy into the gas in their host galaxies at considerable rates (i.e., \(\dot{E}{\approx } 10^{43}\)–10\(^{45}\) erg s\(^{-1}\)). Based on the measured maximum velocities (\(v_\mathrm{{max}}{\approx }\) 400–1400 km s\(^{-1}\)) we find that a large fraction of the gas is likely to become unbound from their host galaxies, but it is unlikely to be completely removed from the galaxy haloes. We show that the power of the growing black holes in these objects (i.e., the AGN activity) is likely to be the dominant power source for driving the outflows; however, star formation may also play a role in some of the sources.
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Notes
- 1.
This value is approximately the mean value for radio-identified SMGs with an observed range of roughly \(\alpha =\) 0.2–1.5, which includes AGN (Ibar et al. 2010). Here we define a spectral index \(\alpha \) such that flux density, \(S_{\nu }\), and frequency, \(\nu \), are related by \(S_{\nu } \propto \nu ^{-\alpha }\).
- 2.
The one source from Swinbank et al. (2004) with FWHM \(>\) 700\(\,\hbox {km}\,\hbox {s}^{-1}\) that is not identified as an AGN (Fig. 3.7) has a complex spectrum and has not been covered by multi-wavelength observations in the literature. It is therefore not possible to rule out the presence of a significant AGN in this galaxy.
- 3.
- 4.
If we were to follow instead Dalla Vecchia and Schaye (2008) to estimate this energy input, the values would be a factor of \(\approx \)2 lower. Conversely, radiation pressure from star-formation could potentially contribute a comparable amount of pressure to stellar and supernovae winds in ULIRGs (Veilleux et al. 2005). As we are considering order of magnitude estimates only, these uncertainties do not affect our conclusions.
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Harrison, C.M. (2016). Energetic Galaxy-Wide Outflows in High-z ULIRGs Hosting AGN Activity. In: Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-28454-5_3
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