Radio and gamma-ray properties of extragalactic jets from the TANAMI sample
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Date
2016-05-04
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Citation of Original Publication
M. Böck, M. Kadler, C. Müller, G. Tosti, R. Ojha, J. Wilms, D. Bastieri, T. Burnett, B. Carpenter, E. Cavazzuti, M. Dutka, J. Blanchard, P. G. Edwards, H. Hase, S. Horiuchi, D. L. Jauncey, F. Krauß, M. L. Lister, J. E. J. Lovell, B. Lott, D. W. Murphy, C. Phillips, C. Plötz, T. Pursimo, J. Quick, E. Ros, G. Taylor, D. J. Thompson, S. J. Tingay, A. Tzioumis and J. A. Zensus ,Radio and gamma-ray properties of extragalactic jets from the TANAMI sample, A&A, 590 (2016) A40 DOI: https://doi.org/10.1051/0004-6361/201424773
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© ESO 2016
© ESO 2016
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Abstract
The TANAMI program has been observing parsec-scale radio jets of southern (declination south of − 30°) γ-ray bright AGN, simultaneously with Fermi/LAT monitoring of their γ-ray emission, via high-resolution radio imaging with Very Long Baseline Interferometry techniques. We present the radio and γ-rayproperties of the TANAMI sources based on one year of contemporaneous TANAMI and Fermi/LAT data. A large fraction (72%) of the TANAMI sample can be associated with bright γ-ray sources for this time range. Association rates differ for different optical classes with all BL Lacs, 76% of quasars, and just 17% of galaxies detected by the LAT. Upper limits were established on the γ-ray flux from TANAMI sources not detected by LAT. This analysis led to the identification of three new Fermi sources whose detection was later confirmed. The γ-ray and radio luminosities are related by Lγ ∝ Lᵣ⁰·⁸⁹±⁰·⁰⁴. The brightness temperatures of the radio cores increase with the average γ-ray luminosity and the presence of brightness temperatures above the inverse Compton limit implies strong Doppler boosting in those sources. The undetected sources have lower γ/radio luminosity ratios and lower contemporaneous brightness temperatures. Unless the Fermi/LAT-undetected blazars are much γ-ray-fainter than the Fermi/LAT-detected sources, their γ-ray luminosity should not be significantly lower than the upper limits calculated here.