Absorption features in sub-TeV gamma-ray spectra of BL Lac objects
| Autor: | Foffano, L., Vittorini, V., Tavani, M., Menegoni, E. |
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| Rok vydání: | 2022 |
| Předmět: | |
| Zdroj: | ApJ 926 95 (2022) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.3847/1538-4357/ac46fc |
| Popis: | The production site of gamma rays in blazars is closely related to their interaction with the photon fields surrounding the active galactic nucleus. In this paper, we discuss an indirect method that may help to unveil the presence of ambient structures in BL Lac objects through the analysis of their gamma-ray spectrum. Gamma rays, passing through structures at different distances from the black hole, interact via $\gamma\gamma$ pair production with the corresponding photon fields and produce absorption features in their spectral energy distribution. An interaction with a putative broad-line region may reduce the gamma-ray flux only if its production site were very close to the central engine. However, if jet photons interact with a bath of optical-UV seed photons produced by a narrow-line region extended over the parsec scale, the consequent $\gamma\gamma$ process may cause absorption features detectable at a few hundreds GeV. The detection of such absorption features is facilitated in sources with spectra reaching TeV energies, and specifically HBLs and EHBLs (extreme blazars) may represent exceptional probes to investigate this topic. We discuss recent observations of an extreme blazar named 2WHSP J073326.7+515354 (or PGC 2402248), which shows evidence of such an absorption feature in its gamma-ray spectrum and narrow emission lines in the optical spectrum, suggesting the presence of narrow-line regions in its large-scale environment. Finally, we discuss how sub-TeV absorption features in the spectra of BL Lac objects may affect their broadband modeling, and eventually represent a powerful diagnostic tool to constrain the gamma-ray production site and the jet environment. Comment: Accepted for publication in ApJ |
| Databáze: | arXiv |
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