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Fermi observations of TeV-selected AGN

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arxiv 0910.4881 v1 pith:4NO75SSV submitted 2009-10-26 astro-ph.HE astro-ph.CO

S. J. Fegan , D. Sanchez , Fermi LAT Collaboration: A. A. Abdo , et al This is my paper · ORCID
classification astro-ph.HEastro-ph.CO
keywords fermiobservationssourcestev-selectedbeendetectedenergiesinstruments
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abstract

We report on observations of TeV-selected AGN made during the first 5.5 months of observations with the Large Area Telescope (LAT) on-board the Fermi Gamma-ray Space Telescope (Fermi). In total, 96 AGN were selected for study, each being either (i) a source detected at TeV energies (28 sources) or (ii) an object that has been studied with TeV instruments and for which an upper-limit has been reported (68 objects). The Fermi observations show clear detections of 38 of these TeV-selected objects, of which 21 are joint GeV-TeV sources and 29 were not in the third EGRET catalog. For each of the 38 Fermi-detected sources, spectra and light curves are presented. Most can be described with a power law of spectral index harder than 2.0, with a spectral break generally required to accommodate the TeV measurements. Based on an extrapolation of the Fermi spectrum, we identify sources, not previously detected at TeV energies, which are promising targets for TeV instruments. Evidence for systematic evolution of the $\gamma$-ray spectrum with redshift is presented and discussed in the context of interaction with the EBL.

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Cited by 2 Pith papers

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  1. A Search for Hard X-ray/Soft $\gamma$-ray Emission from SPT-CL J2012-5649 (Abell 3667) Using INTEGRAL/ISGRI

    astro-ph.HE 2025-12 conditional novelty 5.0 of 10

    INTEGRAL/ISGRI finds no 30–300 keV emission from the merging galaxy cluster Abell 3667, yielding a 3σ upper limit of 4.4×10^-10 erg cm^-2 s^-1 in the 30–100 keV band.

  2. Comprehensive Variability Analysis of Blazars Using Fermi Light Curves Across Multiple Timescales

    astro-ph.HE 2025-05 conditional novelty 4.0 of 10

    A census of Fermi gamma-ray light curves shows FSRQs are more variable than BL Lacs, BCUs resemble BL Lacs, flux distributions are often log-normal, and PSD slopes are generally flat.

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