Abstract
Aims. The BL Lac object RGB J0152+017 () was predicted to be a very high-energy (VHE; >100 GeV) γ-ray source, due to its high X-ray and radio fluxes. Our aim is to understand the radiative processes by investigating the observed emission and its production mechanism using the High Energy Stereoscopic System (HESS) experiment.
Highlights
IntroductionFirst detected as a radio source (Becker et al 1991) by the NRAO Green Bank Telescope and in the Parkes-MIT-NRAO surveys (Griffith et al 1995), ROSAT-Green Bank (RGB) J0152+017 was later identified as a BL Lac object by Laurent-Muehleisen et al (1998), Supported by CAPES Foundation, Ministry of Education of Brazil
First detected as a radio source (Becker et al 1991) by the NRAO Green Bank Telescope and in the Parkes-MIT-NRAO surveys (Griffith et al 1995), RGB J0152+017 was later identified as a BL Lac object by Laurent-Muehleisen et al (1998), Supported by CAPES Foundation, Ministry of Education of Brazil.who located it at z = 0.080, and was claimed as an intermediatefrequency-peaked BL Lac object by Laurent-Muehleisen et al.(1999). Brinkmann et al (1997) report the first detection of RGB J0152+017 in X-rays in the ROSAT-Green Bank (RGB) sample
The broad-band spectral energy distribution (SED) of BL Lac objects is typically characterised by a double-peaked structure, usually attributed to synchrotron radiation in the radio-to-X-ray domain and inverse Compton scattering in the γ-ray domain, which is frequently explained by synchrotron self-Compton (SSC) models
Summary
First detected as a radio source (Becker et al 1991) by the NRAO Green Bank Telescope and in the Parkes-MIT-NRAO surveys (Griffith et al 1995), RGB J0152+017 was later identified as a BL Lac object by Laurent-Muehleisen et al (1998), Supported by CAPES Foundation, Ministry of Education of Brazil. F. Aharonian et al.: Discovery of VHE γ-rays from the high-frequency-peaked BL Lacertae object RGB J0152+017. The broad-band SED of BL Lac objects is typically characterised by a double-peaked structure, usually attributed to synchrotron radiation in the radio-to-X-ray domain and inverse Compton scattering in the γ-ray domain, which is frequently explained by SSC models (see, e.g., Aharonian et al 2005). The contemporaneous radio, optical, X-ray, and VHE observations presented here do not show any significant variability, and enable the first SSC modelling of the emission of RGB J0152+017
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