Flat-spectrum Radio Quasars and BL Lacs Dominate the Anisotropy of the Unresolved Gamma-Ray Background
The Astrophysical Journal, vol. 933, pp. 221
Abstract
Abstract We analyze the angular power spectrum (APS) of the unresolved gamma-ray background (UGRB) emission and combine it with the measured properties of the resolved gamma-ray sources of the Fermi-LAT 4FGL catalog. Our goals are to dissect the composition of the gamma-ray sky and to establish the relevance of different classes of source populations of active galactic nuclei in determining the observed size of the UGRB anisotropy, especially at low energies. We find that, under physical assumptions for the spectral energy distribution, i.e., by using the 4FGL catalog data as a prior, two populations are required to fit the APS data, namely flat-spectrum radio quasars at low energies and BL Lacs at higher energies. The inferred luminosity functions agree well with the extrapolation of the flat-spectrum radio quasar and BL Lac ones obtained from the 4FLG catalog. We use these luminosity functions to calculate the UGRB intensity from blazars, finding a contribution of 20% at 1 GeV and 30% above 10 GeV. Finally, bounds on an additional gamma-ray emission due to annihilating dark matter are also derived.
Authors 5
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RWTH Aachen University · Stockholm University · AlbaNova · Istituto Nazionale di Fisica Nucleare, Sezione di Torino · University of Turin
Affiliation as printed
Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, I-10125 Torino, Italy; elena.pinetti@unito.it, elena.pinetti@to.infn.it
Institute for Theoretical Particle Physics and Cosmology, RWTH Aachen University, Sommerfeldstr. 16, D-52056 Aachen, Germany
Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via P. Giuria 1, I-10125 Torino, Italy; marco.regis@unito.it, nicolao.fornengo@to.infn.it
The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden; michael.korsmeier@fysik.su.se
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Centre National de la Recherche Scientifique · Sorbonne Université · University of Chicago · Fermi National Accelerator Laboratory · Istituto Nazionale di Fisica Nucleare, Sezione di Torino · University of Turin · Laboratoire de Physique Théorique et Hautes Energies
Affiliation as printed
Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, I-10125 Torino, Italy; elena.pinetti@unito.it, elena.pinetti@to.infn.it
Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via P. Giuria 1, I-10125 Torino, Italy; marco.regis@unito.it, nicolao.fornengo@to.infn.it
Laboratoire de Physique Théorique et Hautes Energies, CNRS & Sorbonne Université, 4 place Jussieu, F-75252 Paris, France
Theoretical Astrophysics Department, Fermi National Accelerator Laboratory, Batavia, IL 60510, USA
University of Chicago, Kavli Institute for Cosmological Physics, Chicago, IL 60637, USA
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Goddard Space Flight Center · University of Maryland, Baltimore County
Affiliation as printed
Center for Research and Exploration in Space Science and Technology, NASA/GSFC, Greenbelt, MD 20771, USA
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
University of Maryland, Baltimore County, Baltimore, MD 21250, USA; mnegro1@umbc.edu
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Istituto Nazionale di Fisica Nucleare, Sezione di Torino · University of Turin
Affiliation as printed
Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, I-10125 Torino, Italy; elena.pinetti@unito.it, elena.pinetti@to.infn.it
Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via P. Giuria 1, I-10125 Torino, Italy; marco.regis@unito.it, nicolao.fornengo@to.infn.it
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Istituto Nazionale di Fisica Nucleare, Sezione di Torino · University of Turin
Affiliation as printed
Dipartimento di Fisica, Università di Torino, Via P. Giuria 1, I-10125 Torino, Italy; elena.pinetti@unito.it, elena.pinetti@to.infn.it
Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Via P. Giuria 1, I-10125 Torino, Italy; marco.regis@unito.it, nicolao.fornengo@to.infn.it
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