The remarkable predictive power of infrared data in Blazars

P. Giommi; N. Sahakyan; D. Israyelyan; M. Manvelyan

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arXiv · 2401.10548

The remarkable predictive power of infrared data in Blazars

P. Giommi·N. Sahakyan·D. Israyelyan·M. Manvelyan

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Abstract

Blazars are the brightest and most abundant persistent sources in the extragalactic gamma-ray sky. Due to their significance, they are often observed across various energy bands to explore potential correlations between emissions at different energies, yielding valuable insights into the emission processes of their powerful jets. In this study we utilised infrared (IR) data at 3.4 and 4.6 microns from the Near-Earth Object Wide-field Infrared Survey Explorer Reactivation Mission (NEOWISE), spanning eight years of observations, Swift X-ray data collected throughout the satellite lifetime, and twelve years of gamma-ray measurements from the Fermi Large Area Telescope's all-sky survey. Our analysis reveals that the IR spectral slope reliably predicts the peak frequency and maximum intensity of the synchrotron component of blazars spectral energy distributions, provided it is uncontaminated by radiation unrelated to the jet. A notable correlation between the IR and gamma-ray fluxes was observed, with the BL Lac subclass of blazars displaying a strong correlation coefficient of r = 0.80. Infrared band variability is more pronounced in flat spectrum radio quasars than in BL Lacs, with mean fractional variability values of 0.65 and 0.35, respectively. We also observed that the synchrotron peak intensity of intermediate-high-energy-peaked objects blazars can forecast their detectability at very high energy gamma-ray, energies. We used this predicting power to identify objects in current catalogues that could meet the detection threshold of the Cerenkov telescope array extragalactic survey, which should encompass approximately 180 blazars.

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P. Giommi, N. Sahakyan, D. Israyelyan, M. Manvelyan. 2024-01-19. The remarkable predictive power of infrared data in Blazars. https://arxiv.org/abs/2401.10548

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