THE EVOLUTION OF<i>SWIFT</i>/BAT BLAZARS AND THE ORIGIN OF THE MeV BACKGROUND

Ajello, M.; Costamante, L.; Sambruna, R. M.; Gehrels, N.; Chiang, J.; Rau, A. R. P.; Escala, Andrés; Greiner, J.; Tueller, J.; Wall, J. V.; Mushotzky, R. F.

doi:10.1088/0004-637x/699/1/603

Cited by 222 publications

(370 citation statements)

References 123 publications

(215 reference statements)

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“…We use the X-ray survey observations of AGN by Chandra (Silverman et al 2008) and Swift (Ajello et al 2009) and derive the populations of various AGN at different cosmologi-cal epochs. We next apply the neutrino production models and determine the neutrino emission from individual AGN.…”

Section: 31mentioning

confidence: 99%

“…We consider AGN number evolutions from two X-ray surveys, selecting X-ray emitting AGN (thus across the entire population, regardless of radio-loudness; Silverman et al 2008), and blazars (Ajello et al 2009). The two give us sets of widely different samples of AGN, both varying in luminosity and viewing angle, and where the former contains both RL and RQ AGN, and the latter contains only a fraction of the RL population.…”

Section: Evolving Agn Populationsmentioning

confidence: 99%

“…They use the Chandra multi-wavelength project to detect high redshift luminous AGN (LX ą 10 44 erg s´1), and the Chandra deep field to cover the lower luminosity range. Ajello et al (2009) have used 3 yrs of data from the Swift/BAT survey to select a complete sample of X-ray blazars to determine the evolution of blazars in the 15-55 keV band. The sample consists of 26 FSRQs and 12 BL Lac objects in a redshift range of 0.03 ă z ă 4.0.…”

Section: Evolving Agn Populationsmentioning

confidence: 99%

“…The number density can therefore be derived using the XLF, assuming that the luminosity distribution of the neutrino sources are complete and as inferred by Silverman et al (2008) and Ajello et al (2009), and can be extrapolated to redshifts up to z " 10.…”

Section: Evolving Agn Populationsmentioning

confidence: 99%

“…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.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: 31mentioning

confidence: 99%

Section: Evolving Agn Populationsmentioning

confidence: 99%

Section: Evolving Agn Populationsmentioning

confidence: 99%

Section: Evolving Agn Populationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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Evolution of Supermassive Black Holes

Volonteri

ESO Astrophysics Symposia

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Summary. Supermassive black holes (SMBHs) are nowadays believed to reside in most local galaxies, and the available data show an empirical correlation between bulge luminosity -or stellar velocity dispersion -and black hole mass, suggesting a single mechanism for assembling black holes and forming spheroids in galaxy halos. The evidence is therefore in favour of a co-evolution between galaxies, black holes and quasars. In cold dark matter cosmogonies, small-mass subgalactic systems form first to merge later into larger and larger structures. In this paradigm galaxy halos experience multiple mergers during their lifetime. If every galaxy with a bulge hosts a SMBH in its center, and a local galaxy has been made up by multiple mergers, then a black hole binary is a natural evolutionary stage. The evolution of the supermassive black hole population clearly has to be investigated taking into account both the cosmological framework and the dynamical evolution of SMBHs and their hosts. The seeds of SMBHs have to be looked for in the early Universe, as very luminous quasars are detected up to redshift higher than z = 6. These black holes evolve then in a hierarchical fashion, following the merger hierarchy of their host halos. Accretion of gas, traced by quasar activity, plays a fundamental role in determining the two parameters defining a black hole: mass and spin. A particularly intriguing epoch is the initial phase of SMBH growth. It is very challenging to meet the observational constraints at z = 6 if BHs are not fed at very high rates in their infancy.

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