Modeling the Shell of Cassiopeia A to find the TeV Gamma-ray Emission Region

TL;DR

This study models the shell of Cassiopeia A using multi-wavelength data to locate TeV gamma-ray emission regions, revealing the limitations of leptonic models and supporting a hadronic component.

Contribution

It introduces a multi-wavelength spectral analysis approach to pinpoint gamma-ray emission regions in Cassiopeia A, highlighting the need for hadronic models.

Findings

X-ray flux varies across the remnant regions.

Leptonic models cannot simultaneously explain GeV and TeV data.

A hadronic component is necessary to fit the gamma-ray observations.

Abstract

We will present the multi-wavelength modeling of the supernova remnant Cassiopeia A's shell based on radio, X-rays, and GeV-TeV gamma rays. Our aim is to estimate the location of TeV gamma rays with the help of spectral analysis of X-rays from different regions of the shell, because Chandra X-ray observations have a far better angular resolution than the gamma-ray measurements. Our analysis shows X-ray flux levels from various regions of the remnant to be different. We find that leptonic model is unable to explain the GeV and TeV data, simultaneously. So, we invoke a hadronic model as an additional component to explain the GeV and TeV data.