|Title||Probing the Dark Matter Nature of the 3.5 keV Line with Draco|
|Author||Prof Alexey Boyarsky|
|Description||In recent months, much excitement has been generated in the scientific community by the detection of an X-ray line at 3.5keV in galaxy clusters, M31, and the Galactic Center that is consistent with a decay product of light dark matter. It is very difficult to explain the properties of this line across all of these targets consistently with any known atomic transition line or instrumental anomaly. An important check on the nature of this signal may be obtained by observing classical dwarf spheroidals, which are strongly dark matter dominated and contain very little, if any, hot gas. We thus propose a 1.3Msec observation of the Draco dwarf galaxy, which we show to be a sufficient exposure to either detect a dark matter decay line or robustly exclude the dark matter hypothesis.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2015-10-20T22:00:00Z, 077018, 17.56_20190403_1200. https://doi.org/10.5270/esa-e4bn6gt|