Revisiting Gamma-Ray Emission of the Supernova Remnant RCW 103
Fuente:
arXiv
Guardado en:
| Autores principales: | , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2024
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866913406066360320 |
|---|---|
| author | Xing, Yi Wang, Zhongxiang Zheng, Dong |
| author_facet | Xing, Yi Wang, Zhongxiang Zheng, Dong |
| contents | We analyze more than 15 years of the \gr\ data, obtained with the Large Area Telescope (LAT) onboard {\it the Fermi Gamma-ray Space Telescope (Fermi)}, for the region of the young supernova remnant (SNR) RCW~103, since the nearby source 4FGL J1616.2$-$5054e, counterpart to HESS~J1616$-$518 and $\simeq$13\,arcmin away from the SNR, is determined to be extended in the more recent Fermi-LAT source catalog. Different templates for 4FGL J1616.2$-$5054e and RCW~103 are tested, and we find that a point source with a power-law (PL) spectrum at the southern limb of the SNR best describes the detected gamma-ray emission. The photon index of the PL emission is $Γ\simeq 2.31$(or $α\simeq 2.4$ in a Log-Parabola model) , softer than the previously reported $Γ\simeq 2.0$ when the counterpart to HESS~J1616$-$518 was considered to be a point source (which likely caused mis-identification of extended emission at RCW~103). In order to produce the \gr\ emission in a hadronic scenario, we estimate that protons with an index$\sim$2.4 PL energy distribution are needed. These results fit with those from multi-wavelength observations that have indicated the remnant at the southern limb is interacting with a molecular cloud. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_00903 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Revisiting Gamma-Ray Emission of the Supernova Remnant RCW 103 Xing, Yi Wang, Zhongxiang Zheng, Dong High Energy Astrophysical Phenomena We analyze more than 15 years of the \gr\ data, obtained with the Large Area Telescope (LAT) onboard {\it the Fermi Gamma-ray Space Telescope (Fermi)}, for the region of the young supernova remnant (SNR) RCW~103, since the nearby source 4FGL J1616.2$-$5054e, counterpart to HESS~J1616$-$518 and $\simeq$13\,arcmin away from the SNR, is determined to be extended in the more recent Fermi-LAT source catalog. Different templates for 4FGL J1616.2$-$5054e and RCW~103 are tested, and we find that a point source with a power-law (PL) spectrum at the southern limb of the SNR best describes the detected gamma-ray emission. The photon index of the PL emission is $Γ\simeq 2.31$(or $α\simeq 2.4$ in a Log-Parabola model) , softer than the previously reported $Γ\simeq 2.0$ when the counterpart to HESS~J1616$-$518 was considered to be a point source (which likely caused mis-identification of extended emission at RCW~103). In order to produce the \gr\ emission in a hadronic scenario, we estimate that protons with an index$\sim$2.4 PL energy distribution are needed. These results fit with those from multi-wavelength observations that have indicated the remnant at the southern limb is interacting with a molecular cloud. |
| title | Revisiting Gamma-Ray Emission of the Supernova Remnant RCW 103 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2406.00903 |