| Name: Anisha Hazra |
| Affiliation: National Institute of Technology, Rourkela |
| Conference ID: ASI2026_435 |
| Title: Probing the Jet Power of the Blazar OJ 287 from Multiwavelength Broadband SED Modelling |
| Abstract Type: Poster |
| Abstract Category: Galaxies and Cosmology |
| Author(s) and Co-Author(s) with Affiliation: Anisha Hazra(National Institute of Technology Rourkela, Rourkela - 769008, India), Hritwik Bora(Tezpur University, Tezpur - 784028, India), Ranjeev Misra(Inter-University Centre for Astronomy and Astrophysics, Pune - 411007, India), Ananta C. Pradhan(National Institute of Technology Rourkela, Rourkela - 769008, India) |
| Abstract: OJ 287 is one of the best-studied blazars and is well known for its strong and rapid variability across the electromagnetic spectrum. This makes it an excellent source for exploring how relativistic jets are formed, powered, and linked to the central supermassive black hole. In this work, we investigate the jet energetics of OJ 287 using detailed multiwavelength spectral energy distribution (SED) modelling based on quasi-simultaneous observations from the optical/UV to X-ray and high-energy bands.
The observed emission is interpreted within a one-zone leptonic framework using the composite spectral model tbabs * sscicon, where Galactic absorption is accounted for by tbabs and the intrinsic jet emission is produced via synchrotron and inverse Compton processes. To probe the nature of the underlying electron energy distribution and to test the robustness of the inferred jet parameters, we employ multiple spectral parameterizations, including log-parabolic and broken power-law forms, as well as energy-distribution–based accretion-dominated (EDA) and disk-dominated (EDD) scenarios. Both synchrotron self-Compton and external Compton processes are considered to reproduce the observed X-ray and high-energy emission.
By fitting the model to the data, we derive key physical parameters of the jet, including the magnetic field strength, emission region size, bulk Lorentz factor, Doppler factor, and the electron energy distribution. From the best-fitting models, we estimate the total jet power by decomposing it into contributions from relativistic electrons, cold protons, magnetic fields, and radiation output. Our results indicate that the jet of OJ 287 is highly efficient, with kinetic power dominated by relativistic particles and a substantial contribution from magnetic energy. The total jet power is comparable to or exceeds the accretion power inferred from optical–UV emission, supporting efficient jet launching mechanisms in supermassive black hole systems. |
