Abstract Details
| Name: Rupesh Behera Affiliation: Indian Institute of Astrophysics Conference ID: ASI2025_595 Title : A comprehensive X-ray study of Cygnus Loop. Authors and Co-Authors : Rupesh Behera 1,2, Firoza K. Sutaria 1 Abstract Type : Poster Abstract Category : Stars, Interstellar Medium, and Astrochemistry in Milky Way Abstract : Supernova remnants (SNRs) are a mix of ejected material in a supernova explosion and interstellar material swept up by the shock wave. SNRs offer a unique opportunity to study the interactions between relativistic ejecta and supernova shock waves with the local interstellar medium (ISM). These nebular structures are crucial in shaping the structure and thermodynamic properties of the ISM. Surprisingly, much remains unknown about how they eventually mix with the ISM, leading to its chemical enrichment. In our study, we examined various segments of the Cygnus Loop using proprietary X-ray and UV observations from SXT and UVIT, respectively. Additionally, we incorporated archival X-ray data from other observatories. The Cygnus Loop is thought to have originated from a core-collapse supernova; however, no compact stellar remnant has been confidently identified. We performed X-ray spectroscopy on 17 regions spanning most of this extended 3x4 degree object. We fitted the spectra with composite thermal models, and the best fit model was analyzed by creating distribution maps. This allowed us to investigate variations in parameters such as temperature and elemental abundances with prominent emission lines in the soft X-ray spectrum. Our analysis revealed notable differences in properties between the eastern, western, and southern regions of the Cygnus Loop, which were evident directly from the spectra as well. Additionally, we explored the inter-correlations among these parameters by running the MCMC chain on the best fit model. Previous studies focusing on select regions of the Cygnus Loop indicated the possible presence of charge-exchange (CX) emission in the soft X-ray band and enhanced abundances of certain elements. Our best-fit models similarly showed enhanced abundances across multiple regions. Due to the low resolution of the spectra, it is nearly impossible to identify each of the CX emission lines and highly resolved X-ray spectra will be required. |