The Quasar Outflow Contribution to Agn Feedback: VLT Measurements of SDSS J0318-0600

Abstract

We present high spectral resolution VLT observations of the BAL quasar SDSS J0318-0600. This high quality data set allows us to extract accurate ionic column densities and determine an electron number density of n e =10 3.3±0.2 cm −3 for the main outflow absorption component. The heavily reddened spectrum of SDSS J0318-0600 requires purely silicate dust with a reddening curve characteristic of predominately large grains, from which we estimate the bolometric luminosity. We carry out photoionization modeling to determine the total column density, ionization parameter and distance of the gas and find that the photionization models suggest abundances greater than solar. Due to the uncertainty in the location of the dust extinction, we arrive at two viable distances for the main ouflow component from the central source, 6 and 18 kpc, where we consider the 6 kpc location as somewhat more physically plausable. Assuming the canonical global covering of 20% for the outflow and a distance of 6 kpc, our analysis yields a mass flux of 120 M ⊙ yr −1 and a kinetic luminosity that is ∼0.1% of the bolometric luminosity of the object. Should the dust be part of the outflow, then these values are ∼4× larger. The large mass flux and kinetic luminosity make this outflow a significant contributor to AGN feedback processes.

The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies

“…In fact, substantial feedback from accretion around supermassive black holes is required in cosmological semi-analytic models, semi-empirical models, and hydrodynamical simulations to achieve the steep slope of the high-mass end of the galaxy stellar mass function (e.g., Vogelsberger et al 2014a,b;Henriques et al 2015;Schaye et al 2015). Observationally, direct measurements of AGN driven winds in galaxies and radio jet induced bubbles in galaxy haloes have provided evidence for the mechanisms by which AGN feedback can affect galaxies, but typically only for a very small number of galaxies (e.g., McNamara et al 2000;Nulsen et al 2005;McNamara et al 2007;Dunn et al 2010;Fabian 2012;Cicone et al 2013;Liu et al 2013;Harrison et al 2014Harrison et al , 2016. Hence, whether or not AGN feedback actually quenches galaxies in statistically significant numbers remains an open question.…”

SimultaneousXMM-Newtonand HST-COS observation of 1H0419-577

“…Fe ii, Si ii, and C ii have been detected in a handful of cases (e.g. Moe et al 2009;Dunn et al 2010;Borguet et al 2012). In the X-rays the identification of metastable lines from O v is hampered by uncertainties in the predicted line wavelength (Kaastra et al 2004).…”

“…Only the fastest AGN wind (e.g. Moe et al 2009;Dunn et al 2010;Tombesi et al 2013) may be dynamically important in the evolution of the interstellar medium (Faucher-Giguère & Quataert 2012).…”

Massive quiescent galaxies at z > 3 in the Millennium simulation populated by a semi-analytic galaxy formation model

“…In addition, the AGN feedback model implemented in Guo11 mainly refers to the 'radio mode' feedback, which only operates on the cooling gas, yet does not affect the residual cold gas. However, when the AGN accretion rate is close to the Eddington limit, the 'quasar mode' AGN feedback (Croton et al 2006) could eject the residual cold gas from a galaxy in the form of a wind, with power at 5-10 per cent of the accretion power (Saez, Chartas & Brandt 2009;Dunn et al 2010). This 'quasar mode' AGN feedback is only partially represented by an enhanced feedback efficiency associated with starbursts (Croton et al 2006) but is not fully incorporated into the current model.…”