Abstract Details
| Name: | AMAL ABDULRAHMAN |
| Affiliation: | FAROOK COLLEGE, KOZHIKODE, KERALA |
| Conference ID : | ASI2023_460 |
| Title : | Probing IC/CMB Interpretation for the X-ray knots of AGN through VHE observations |
| Authors : | Amal A. Rahman1 , S. Sahayanathan2,3 , Malik Zahoor4 and P. A Subha1 1 Department of Physics,Farook College, Calicut University, Kerala-673632, India 2 Astrophysical Sciences Division, Bhabha Atomic Research Centre, Mumbai - 400085, India 3 Homi Bhabha National Institute, Mumbai 400094, India 4 Department of Physics, University of Kashmir, Srinagar 190006, India |
| Mode of Presentation: | Oral |
| Abstract Category : | Extragalactic Astronomy |
| Abstract : | Detection of hard X-ray spectrum from the kilo-parsec scale jet of active galactic nuclei cannot be accounted to the synchrotron emission mechanism responsible for the radio/optical emission. Spectral modelling of the radio–optical–X-ray emission from the knot features suggested the jet to be relativistic even at this scale. A plausible X-ray emission mechanism can be the inverse Compton scattering process with the prominent target soft photons being the Lorentz boosted cosmic microwave background (IC/CMB). Under this interpretation, the Compton spectral component peaks at GeV energy and many such galaxies were predicted to be Fermi candidate sources. Non-detection of these sources raised serious questions regarding the validity of the IC/CMB interpretation for the X-ray emission. However, IC/CMB mechanism is still a preferred X-ray emission mechanism for the X-ray jets which were not ruled out by Fermi observations. We revisit the IC/CMB mechanism for these sources and predict their flux at VHE energies. Our study suggests the knots and/or the jet component of 3C 120 and 3C 111 fall within their sensitivity limits of the upcoming Cherenkov Telescope Array(CTA). Future observations of these sources can be an effective tool to substantiate the IC/CMB interpretation. |