Modeling the Multiwavelength Emission from G73.9+0.9: Gamma-Rays from an SNR-MC Interaction
Abstract
G73.9+0.9 has been classified as a probable shell-type supernova remnant, though it has also been suggested that it could have a pulsar wind nebula (PWN). Here, a broadband model of the non-thermal emission of G73.9+0.9 from radio to gamma rays is presented. The model includes a new gamma-ray observation obtained by the analysis of seven years of data from the Fermi/LAT telescope. Above 200 MeV, the source is detected with a significance of 13σ and the spectrum of the radiation is best described by a power law with an index of ∼2.5. The leptonic mechanisms are hard to reconcile with the measured radio and gamma-ray spectral energy distribution. A PWN origin for the high-energy emission is also not very likely, due to the lack of detection of pulsars and of X-ray emission in the region, as well as from the shape of the gamma-ray spectrum. Given the possibility that the object is interacting with molecular clouds, a hadronic origin of the high-energy emission is more likely, and the spectral properties of the cosmic rays responsible for this radiation are derived.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- November 2015
- DOI:
- 10.1088/0004-637X/813/1/3
- arXiv:
- arXiv:1509.03710
- Bibcode:
- 2015ApJ...813....3A
- Keywords:
-
- acceleration of particles;
- ISM: supernova remnants;
- ISM: clouds;
- gamma rays: general ISM: individual objects: G73.9+0.9;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- To appear in ApJ. Comments welcomed