DECIPHERING CONTRIBUTIONS TO THE EXTRAGALACTIC GAMMA-RAY BACKGROUND FROM 2 GeV TO 2 TeV

• Published in: The Astrophysical journal 2016-12, Vol.832 (2), p.117
• Main Authors: Lisanti, Mariangela, Mishra-Sharma, Siddharth, Necib, Lina, Safdi, Benjamin R.
• Format: Article
• Language: English
• Subjects: Active galactic nuclei; Astronomy & Astrophysics; ASTRONOMY AND ASTROPHYSICS; Astrophysics; BL Lacertae objects: general; Blazars; Correlation analysis; dark matter; Galaxies; galaxies: active; galaxies: statistics; Gamma rays; gamma rays: diffuse background; Milky Way; Neutrinos; Observatories; Point sources; Star formation; Statistical analysis
• ISSN: 0004-637X; 1538-4357; 1538-4357
• DOI: 10.3847/0004-637X/832/2/117

ABSTRACT Astrophysical sources outside the Milky Way, such as active galactic nuclei and star-forming galaxies, leave their imprint on the gamma-ray sky as nearly isotropic emission referred to as the extragalactic gamma-ray background (EGB). While the brightest of these sources may be individually resolved, their fainter counterparts contribute diffusely. In this work, we use a recently developed analysis method, called the Non-Poissonian Template Fit, on up to 93 months of publicly available data from the Fermi Large Area Telescope to determine the properties of the point sources (PSs) that comprise the EGB. This analysis takes advantage of photon-count statistics to probe the aggregate properties of these source populations below the sensitivity threshold of published catalogs. We measure the source-count distributions and PS intensities, as a function of energy, from ∼2 GeV to 2 TeV. We find that the EGB is dominated by PSs, likely blazars, in all seven energy sub-bins considered. These results have implications for the interpretation of IceCube's PeV neutrinos, which may originate from sources that contribute to the non-blazar component of the EGB. Additionally, we comment on implications for future TeV observatories such as the Cherenkov Telescope Array. We provide sky maps showing locations most likely to contain these new sources at both low ( 50 GeV) and high ( 50 GeV) energies for use in future observations and cross-correlation studies.