| Name: | Sandeep Godiyal |
| Affiliation: | Bhabha Atomic Research Centre, Mumbai |
| Conference ID : | ASI2024_781 |
| Title : | Hard Gamma-ray Spectrum Blazars as Potential Targets for MACE observations |
| Authors : | S Godiyal1, K K Singh1,2, A Tolamatti1,2, N Chouhan1 |
| Authors Affiliation: | 1 S Godiyal, K K Singh, A Tolamatti, N Chouhan Affiliation (Astrophysical Sciences Division, Bhabha Atomic Research Centre, Mumbai 400085, India)
2 K K Singh, A Tolamatti Affiliation (Homi Bhabha National Institute, Anushakti Nagar, Mumbai 400094, India) |
| Mode of Presentation: | Poster |
| Abstract Category : | High Energy Phenomena, Fundamental Physics and Astronomy |
| Abstract : | The high energy emission above 10 GeV is generally described by a power law with spectral index Γ ≤ 2 from an extreme class of blazars observed by the Fermi Gamma-ray Space Telescope. These sources are referred to as hard gamma-ray spectrum blazars. Due to their hard gamma-ray spectra, the peak of high energy component in their broadband spectral energy distribution is located at energies above 1 TeV. This challenges the standard model for gamma-ray emission from blazars involving the inverse Compton scattering of low energy (UV/Optical/IR) photons by the relativistic electrons. Therefore, detection of a large population of such blazars in the energy range above 10 GeV is of particular importance to probe the radiative processes and particle acceleration. However, these sources are expected to be very faint due to the upper edge of the peak energy location in the gamma-ray region. In this contribution, we present results from the study of a sample of hard gamma-ray spectrum blazars, which are deemed to be the promising candidates for detection by the newly commissioned MACE telescope. It has the capability of detecting cosmic gamma-ray photons with energies above ~20 GeV from sources located at cosmological distances. We use the spectral properties of sources reported in the recent fourth Fermi gamma-ray source catalogue (4FGL) to identify the target candidates for MACE observations. |
