The 1.4-GHz radio properties of hard X-ray-selected AGN

Panessa, F.; Tarchi, A.; Castangia, P.; Maiorano, E.; Bassani, L.; Bicknell, G. V.; Bazzano, A.; Bird, A. J.; Malizia, A.; Ubertini, P.

doi:10.1093/mnras/stu2455

Cited by 58 publications

(75 citation statements)

References 61 publications

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“…2). It is remarkable that our predictions for RQ AGNs are in agreement with the observational determinations, though within large uncertainties, by Panessa et al (2015) and Padovani et al (2015). This adds further validation to our overall picture for the radio emission from SFGs and RQ AGNs.…”

Section: Further Observational Constraintssupporting

confidence: 83%

“…(3), convert the bolometric power in X-rays via the Hopkins et al (2007) correction, and then derive the AGN radio power by using the relation between restframe X-ray and 1.4 GHz radio luminosity observed for a sample of (mainly) RQ AGNs by Panessa et al (2015; where α AGN ≈ 0.7 is the spectral index for an optically thin synchrotron emission. Consistently with observations (e.g., Brinkmann et al 2000;Panessa et al 2015), we consider a scatter σ log L X ≈ 0.4 around the resulting average relationshipL ν,AGN (L AGN ). The related statistics is given by…”

Section: Radio-quiet Agnsmentioning

confidence: 99%

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Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

Mancuso

Lapi

Prandoni

et al. 2017

ApJ

103

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We investigate the astrophysics of radio-emitting star-forming galaxies and active galactic nuclei (AGNs), and elucidate their statistical properties in the radio band including luminosity functions, redshift distributions, and number counts at sub-mJy flux levels, that will be crucially probed by next-generation radio continuum surveys. Specifically, we exploit the model-independent approach by Mancuso et al. (2016a,b) to compute the star formation rate functions, the AGN duty cycles and the conditional probability of a star-forming galaxy to host an AGN with given bolometric luminosity. Coupling these ingredients with the radio emission properties associated to star formation and nuclear activity, we compute relevant statistics at different radio frequencies, and disentangle the relative contribution of star-forming galaxies and AGNs in different radio luminosity, radio flux, and redshift ranges. Finally, we highlight that radio-emitting star-forming galaxies and AGNs are expected to host supermassive black holes accreting with different Eddington ratio distributions, and to occupy different loci in the galaxy main sequence diagrams. These specific predictions are consistent with current datasets, but need to be tested with larger statistics via future radio data with multi-band coverage on wide areas, as it will become routinely achievable with the advent of the SKA and its precursors.

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Section: Further Observational Constraintssupporting

confidence: 83%

Section: Radio-quiet Agnsmentioning

confidence: 99%

Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

Mancuso

Lapi

Prandoni

et al. 2017

ApJ

103

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“…In order to see if a combination of mechanisms could explain our result, we apply a simple test. From the AGN side, following a radio luminosity and X-ray luminosity correlation with a slope of 1.2 ± 0.15 (Panessa et al 2015) calibrated for AGN at high Eddington ratios (i.e., (L AGN /L Edd ) > 10 −3 ), we obtain ∆logL 1.4GHz = 1.2∆logL X−r ay . We then assume that AGN bolometric luminosity L AGN ∝ L X-ray with a constant correction factor (Brightman et al 2017); thus, ∆logL 1.4GHz = 1.2∆logL AGN .…”

Section: Agn Powermentioning

confidence: 85%

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

Shen

Lemaux

Lubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In this study we investigate 179 radio-IR galaxies drawn from a sample of spectroscopically-confirmed galaxies that are detected in radio and mid-infrared (MIR) in the redshift range of 0.55 ≤ z ≤ 1.30 in the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey. We constrain the Active Galactic Nuclei (AGN) contribution in the total IR luminosity (f AGN ), and estimate the AGN luminosity (L AGN ) and the star formation rate (SFR) using the CIGALE Spectral Energy Distribution (SED) fitting routine. Based on the f AGN and radio luminosity, radio-IR galaxies are split into: galaxies that host either high or low f AGN AGN (high-/lowf AGN ), and star forming galaxies with little to no AGN activity (SFGs). We study the colour, stellar mass, radio luminosity, L AGN and SFR properties of the three radio-IR sub-samples, comparing to a spec-IR sample drawn from spectroscopically-confirmed galaxies that are also detected in MIR. No significant difference between radio luminosity of these sub-samples was found, which could be due to the combined contribution of radio emission from AGN and star formation. We find a positive relationship between L AGN and specific SFR (sSFR) for both AGN sub-samples, strongly suggesting a co-evolution scenario of AGN and SF in these galaxies. A toy model is designed to demonstrate this co-evolution scenario, where we find that, in almost all cases, a rapid quenching timescale is required, which we argue is a signature of AGN quenching. The environmental preference for intermediate/infall regions of clusters/groups remains across the co-evolution scenario, which suggests that galaxies might be in an orbital motion around the cluster/group during the scenario.

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“…Here (and throughout this paper) the luminosities and BH mass are, respectively, in units of erg s −1 and M ⊙ . We refer this relationship as the original/standard M03 "Fundamental Plane" (hereafter FP) of back hole activity (for later work, see e.g., Falcke et al 2004;Körding et al 2006;Merloni et al 2006;Wang et al 2006;Panessa et al 2007;Li et al 2008;Gültekin et al 2009, hereafter G09;Plotkin et al 2012;Younes et al 2012;Dong & Wu 2015;Panessa et al 2015;Fan & Bai 2016;Liu, Han & Zhang 2016;Nisbet & Best 2016). Yuan, Cui & Narayan (2005) have proposed a coupled accretion-jet model for LLAGNs and BHBs (see Yuan & Narayan 2014 for a review).…”

Section: Introductionmentioning

confidence: 99%

Fundamental Plane of Black Hole Activity in the Quiescent Regime

Xie

Yuan

2017

ApJ

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A correlation among the radio luminosity (L R ), X-ray luminosity (L X ), and black hole mass (M BH ) in active galactic nuclei (AGNs) and black hole binaries is known to exist and is called the "Fundamental Plane" of black hole activity. predicts that the radio/X-ray correlation index, ξ X , changes from ξ X ≈ 0.6 to ξ X ≈ 1.2 − 1.3 when L X /L Edd decreases below a critical value ∼ 10 −6 . While many works favor such a change, there are also several works claiming the opposite. In this paper, we gather from literature a largest quiescent AGN (defined as L X /L Edd 10 −6 ) sample to date, consisting of 75 sources. We find that these quiescent AGNs follow a ξ X ≈ 1.23 radio/X-ray relationship, in excellent agreement with the Yuan & Cui prediction. The reason for the discrepancy between the present result and some previous works is that their samples contain not only quiescent sources but also "normal" ones (i.e., L X /L Edd 10 −6 ). In this case, the quiescent sources will mix up with those normal ones in L R and L X . The value of ξ X will then be between 0.6 and ∼ 1.3, with the exact value being determined by the sample composition, i.e., the fraction of the quiescent and normal sources. Based on this result, we propose that a more physical way to study the Fundamental Plane is to replace L R and L X with L R /L Edd and L X /L Edd , respectively.

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The 1.4-GHz radio properties of hard X-ray-selected AGN

Cited by 58 publications

References 61 publications

Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

The properties of radio and mid-infrared detected galaxies and the effect of environment on the co-evolution of AGN and star formation at z ∼ 1

Fundamental Plane of Black Hole Activity in the Quiescent Regime

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