The evolution of the hard X-ray luminosity function of AGN

Aird, James; Nandra, K.; Laird, E. S.; Georgakakis, A.; Ashby, M. L. N.; Barmby, P.; Coil, Alison L.; Huang, Jia-Sheng; Koekemoer, Anton M.; Steidel, Charles C.; Willmer, C. N. A.

doi:10.1111/j.1365-2966.2009.15829.x

Cited by 384 publications

(649 citation statements)

References 104 publications

(224 reference statements)

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“…There are a number of pieces of evidence that support a global evolutionary connection between the star formation and AGN activity, for example, 1) the differential redshift evolution of the AGN luminosity function, or "AGN downsizing" is also found for the star-forming galaxy population (e.g. Hasinger et al 2005;Hopkins & Hernquist 2006;Aird et al 2010;Kalfountzou et al 2014a), 2) the redshift distribution of strongly star-forming galaxies follows that of powerful AGN (e.g. Willott et al 2001;Chapman et al 2005; Wardlow et al…”

Section: Introductionmentioning

confidence: 99%

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Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1 which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that: 1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, 2) the RLQs show a SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radio AGN triggering are linked to star-formation triggering and 3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power.

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Section: Introductionmentioning

confidence: 99%

“…Boyle & Terlevich 1998;Merloni et al 2004;Aird et al 2010;Madau & Dickinson 2014) and 4) a tight correlation is found between the BH and stellar mass of the host galaxy bulge (e.g. Magorrian et al 1998;McConnell & Ma 2013;Graham & Scott 2013;Kormendy & Ho 2013).…”

Section: Introductionmentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Magorrian et al 1998). An intimate connection between AGN and star formation in galaxies is further suggested by the similar decline in AGN activity (Hasinger et al 2005;Aird et al 2010) and star formation (Hopkins & Beacom 2006) from when the Universe was half its current age to today. Additionally, this connection between galaxy and AGN E-mail: minh.huynh@uwa.edu.au evolution is reflected in the general shift of these processes from high mass galaxies in the distant Universe to low mass galaxies locally (Cowie et al 1996;Hasinger et al 2005;Juneau et al 2005;Mobasher et al 2009), commonly referred to as downsizing.…”

Section: Introductionmentioning

confidence: 99%

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

Huynh¹,

Bell²,

Hopkins³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a new image of the 5.5 GHz radio emission from the extended Chandra Deep Field South. Deep radio observations at 5.5 GHz were obtained in 2010 and presented in the first data release. A further 76 hours of integration has since been obtained, nearly doubling the integration time. This paper presents a new analysis of all the data. The new image reaches 8.6 µJy rms, an improvement of about 40% in sensitivity. We present a new catalogue of 5.5 GHz sources, identifying 212 source components, roughly 50% more than were detected in the first data release. Source counts derived from this sample are consistent with those reported in the literature for S 5.5GHz > 0.1 mJy but significantly lower than published values in the lowest flux density bins (S 5.5GHz < 0.1 mJy), where we have more detected sources and improved statistical reliability. The 5.5 GHz radio sources were matched to 1.4 GHz sources in the literature and we find a mean spectral index of −0.35 ± 0.10 for S 5.5GHz > 0.5 mJy, consistent with the flattening of the spectral index observed in 5 GHz sub-mJy samples. The median spectral index of the whole sample is α med = −0.58, indicating that these observations may be starting to probe the star forming population. However, even at the faintest levels (0.05 < S 5.5GHz < 0.1 mJy), 39% of the 5.5 GHz sources have flat or inverted radio spectra. Four flux density measurements from our data, across the full 4.5 to 6.5 GHz bandwidth, are combined with those from literature and we find 10% of sources (S 5.5GHz 0.1 mJy) show significant curvature in their radio spectral energy distribution spanning 1.4 to 9 GHz.

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“…Therefore, modified versions of these models are used, either extending the form of the luminosity or density evolution, or formulating a combination of the two (see e.g. Ueda et al 2003;Aird et al 2010). The blazar population is found to be best described in terms of a modified pure luminosity evolution (MPLE) model (Ajello et al 2009) on a double power-law presentday XLF (Equation 25), where the evolution factor is a power law with two free parameters, υ1 and υ2, giving a general behaviour with respect to redshift, of a form first given in Wall et al (2008),…”

Section: The X-ray Luminosity Functionmentioning

confidence: 99%

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

Jacobsen

et al. 2015

Mon. Not. R. Astron. Soc.

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High-energy neutrinos and photons are complementary messengers, probing violent astrophysical processes and structural evolution of the Universe. X-ray and neutrino observations jointly constrain conditions in active galactic nuclei (AGN) jets: their baryonic and leptonic contents, and particle production efficiency. Testing two standard neutrino production models for local source Cen A (Koers & Tinyakov 2008; Becker & Biermann 2009), we calculate the high-energy neutrino spectra of single AGN sources and derive the flux of high-energy neutrinos expected for the current epoch. Assuming that accretion determines both X-rays and particle creation, our parametric scaling relations predict neutrino yield in various AGN classes. We derive redshift-dependent number densities of each class, from Chandra and Swift/BAT X-ray luminosity functions (Silverman et al. 2008;Ajello et al. 2009). We integrate the neutrino spectrum expected from the cumulative history of AGN (correcting for cosmological and source effects, e.g. jet orientation and beaming). Both emission scenarios yield neutrino fluxes well above limits set by IceCube (by " 4-10 6ˆa t 1 PeV, depending on the assumed jet models for neutrino production). This implies that: (i) Cen A might not be a typical neutrino source as commonly assumed; (ii) both neutrino production models overestimate the efficiency; (iii) neutrino luminosity scales with accretion power differently among AGN classes and hence does not follow X-ray luminosity universally; (iv) some AGN are neutrino-quiet (e.g. below a power threshold for neutrino production); (v) neutrino and X-ray emission have different duty cycles (e.g. jets alternate between baryonic and leptonic flows); or (vi) some combination of the above.

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The evolution of the hard X-ray luminosity function of AGN

Cited by 384 publications

References 104 publications

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

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