A sample of ionised Fe line-emitting X-ray sources in the inner Galactic disc
[Context] The origin of the unresolved X-ray emission towards the Galactic Centre and the Galactic disc is unclear. Previous studies suggest that the Galactic diffuse X-ray emission is composed of unresolved point sources, primarily magnetic cataclysmic variables (mCVs). However, mCVs have a much lo...
| Autores: | , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/398647 |
| Acceso en línea: | http://hdl.handle.net/10261/398647 |
| Access Level: | acceso abierto |
| Palabra clave: | Novae, cataclysmic variables White dwarfs Galaxy: bulge Galaxy: center Galaxy: disk X-rays: binaries |
| Sumario: | [Context] The origin of the unresolved X-ray emission towards the Galactic Centre and the Galactic disc is unclear. Previous studies suggest that the Galactic diffuse X-ray emission is composed of unresolved point sources, primarily magnetic cataclysmic variables (mCVs). However, mCVs have a much lower 6.7 keV line equivalent width (EW6.7) and a much higher line intensity ratio between Fe XXVI and Fe XXV (I6.9/I6.7) compared to the diffuse X-ray emission. Therefore, the primary contributors to the unresolved X-ray emission remain unclear. |
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