A RELATIONSHIP BETWEEN AGN JET POWER AND RADIO POWER

By K. Cavagnolo, B. McNamara, P. Nulsen, C. Carilli, C. Jones, L. Bîrzan. 2010

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Using Chandra X-ray and Very Large Array radio data, we investigate the scaling relationship between jet power, Pjet, and synchrotron luminosity, Pradio. We expand the sample presented in Bîrzan et al. to lower radio power by incorporating measurements for 21 giant elliptical galaxies (gEs) to determine if the Bîrzan et al. Pjet–Pradio scaling relations are continuous in form and scatter from gEs up to brightest cluster galaxies. We find a mean scaling relation of Pjet ≈ 5.8 × 1043(Pradio/1040)0.70 erg s−1 which is continuous over ∼6–8 decades in Pjet and Pradio with a scatter of ≈ 0.7 dex. Our mean scaling relationship is consistent with the model presented in Willott et al. if the typical fraction of lobe energy in non-radiating particles to that in relativistic electrons is ≳100. We identify several gEs whose radio luminosities are unusually large for their jet powers and have radio sources which extend well beyond the densest parts of their X-ray halos. We suggest that these radio sources are unusually luminous because they were unable to entrain appreciable amounts of gas.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8ab797be459f7d64542723c04e14fbf4059dccd5

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Citations in the corpus

DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, methodology): “When jet powers were not given in the references above, they were either found in the table of properties (Table 1) of the sample compiled by Wu (2009) or calculated from the 1.4 GHz flux available from the NASA Extragalactic Database using the scaling relation by Cavagnolo et al. (2010).”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, methodology): “For example, applying equations of Cavagnolo et al. (2010) we find that an Lmech = 5 × 10 44 erg s−1 jet could be hiding behind this rather small radio luminosity.”
Mechanical feedback from active galactic nuclei in galaxies, groups and clusters (2012, background): “…in abundance in the hot atmospheres of groups (Sun et al 2009, Dong et al 2010, Gitti et al 2010, Giacintucci et al 2011, O’Sullivan et al 2011a) and ellipticals (Nulsen New Journal of Physics 14 (2012) 055023 (http://www.njp.org/) 8 et al 2009, Cavagnolo et al 2010, Mulchaey and Jeltema 2010).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “Further cavity power measurements in systems ranging from giant elliptical galaxies to the most massive clusters have refined this correlation (e.g. Dunn et al. 2005, Rafferty et al. 2006, Bı̂rzan et al. 2008, Cavagnolo et al. 2010; see Fig.8).”
FROM THE BLAZAR SEQUENCE TO THE BLAZAR ENVELOPE: REVISITING THE RELATIVISTIC JET DICHOTOMY IN RADIO-LOUD ACTIVE GALACTIC NUCLEI (2011, methodology): “This value is then converted to Lkin from the linear fit (with 1-σ error), log Lkin = 0.64(±0.09) (log L300 − 40) + 43.54(±0.12) [ergs s −1 ] (1) taken from Cavagnolo et al. (2010).”
What drives the growth of black holes (2011, methodology): “…timescale for the lifetime of the radio source (for example from the buoyant rise time of the inflated bubble), we can then estimate the total mechanical power Pmech output by the AGN (e.g., Bı̂rzan et al., 2004; Dunn et al., 2005; Dunn & Fabian, 2008; Bı̂rzan et al., 2008; Cavagnolo et al., 2010).”
Kiloparsec-scale outflows are prevalent among luminous AGN: outflows and feedback in the context of the overall AGN population (2014, background): “1.4 GHz luminosity and the relationship in Cavagnolo et al. 2010).”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “…Capetti & Grandi (2006), [11] Di Matteo et al. (2003), [12] Machacek et al. (2006), [13] Allen et al. (2006), [14] McNamara et al. in prep, [15] Cavagnolo et al. (2010), [16] Chiaberge et al. (2003b), [17] O’Sullivan et al. (2011b),[18] Machacek et al. (2007), [19] David et al. (2009), [20]…”
Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, result): “The fraction of energy in non-radiating particles to that in relativistic electrons in a system such as NGC 7793 S26 is similar to the values found by (Cavagnolo et al. 2010) for a sample of AGN, Seyfert and giant elliptical galaxies.”
A hadronic origin for ultra-high-frequency-peaked BL Lac objects (2014, background): “Nevertheless, for radioloud AGN hosted by SMBHs with masses in the range 108−9 M , observational estimates of jet powers generally do not show any evidence for highly super-Eddington values (e.g. Cavagnolo et al. 2010).”
Blazar Flares as an Origin of High-energy Cosmic Neutrinos? (2018, background): “…(based on larger-scale jets than the blazar zone) have shown that the absolute jet power averaged over the lifetime of the AGN jet is Pj ∼< 10 45 − 1046 erg s−1 for Fanaroff-Riley I galaxies (Cavagnolo et al. 2010; Godfrey & Shabala 2013) that are believed to be off-axis counterparts of BL Lacs.”
The fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA (2015, methodology): “A number of studies (Birzan et al. 2008; Cavagnolo et al. 2010; McNamara & Nulsen 2012) have shown a high efficiency of the coupling between radio plasma and the surrounding ISM and inter-galactic medium (IGM) and mechanical power of the radio jets exceeding the synchrotron power.”
On the fundamental dichotomy in the local radio-AGN population (2012, methodology): “The jet mechanical luminosity was estimated from the 1.4GHz radio luminosity, using the relation of Cavagnolo et al. (2010), Lmech = 7.3 × 1036 ( L1.”
Cosmological simulations of black hole growth: AGN luminosities and downsizing (2013, background): “Using the relation of Cavagnolo et al. (2010) between the 1.4 GHz radio luminosity L1.”